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+page_content=' France  13Franco-Chilean Laboratory for Astronomy,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' IRL 3386,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' CNRS and U.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' de Chile, Casilla 36-D, Santiago, Chile  (Received .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=';' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Revised .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=';' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Accepted .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=')  Submitted to ApJ  ABSTRACT  We report the detection of stimulated hydrogen radio recombination line (RRL) emission from ionized  gas in a z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 galaxy using 580–1670 MHz observations from the MeerKAT Absorption Line  Survey (MALS).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The RRL emission originates in a galaxy that intercepts and strongly lenses the radio  blazar PKS 1830−211 (z = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' This is the second detection of RRLs outside of the local universe  and the first clearly associated with hydrogen.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We detect effective H144α (and H163α) transitions  at observed frequencies of 1156 (798) MHz by stacking 17 (27) RRLs with 21σ (14σ) significance.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The RRL emission contains two main velocity components and is coincident in velocity with H i  21 cm and OH 18 cm absorption.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We use the RRL spectral line energy distribution and a Bayesian  analysis to constrain the density (ne) and the volume-averaged pathlength (ℓ) of the ionized gas.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We determine log(ne) = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0+1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 cm−3 and log(ℓ) = −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7+1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1 pc towards the north east (NE) lensed  image, likely tracing the diffuse thermal phase of the ionized ISM in a thin disk.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Towards the south  west (SW) lensed image, we determine log(ne) = 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0 cm−3 and log(ℓ) = −2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7+1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2 pc, tracing  gas that is more reminiscent of H ii regions.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We estimate a star formation (surface density) rate of  ΣSFR ∼ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 M⊙ yr−1 kpc−2 or SFR ∼ 50 M⊙ yr−1, consistent with a star-forming main sequence  galaxy of M⋆ ∼ 1011 M⊙.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The discovery presented here opens up the possibility of studying ionized  gas at high redshifts using RRL observations from current and future (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', SKA and ngVLA) radio  facilities.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Keywords: galaxies: ISM  Corresponding author: Kimberly L.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Emig  kemig@nrao.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='edu  ∗ Jansky Fellow of the National Radio Astronomy Observatory  1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' INTRODUCTION  Radio recombination lines (RRLs) result from the ra-  diative de-excitation of electrons at high excitation lev-  els of atoms.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' RRLs with frequencies νrest ≲10 GHz in  arXiv:2301.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='03115v1  [astro-ph.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='GA]  8 Jan 2023  ID2  Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  extragalactic sources probe gas with relatively low den-  sity that can be stimulated by radio continuum (for an  overview, see Emig 2021), upon which the line emis-  sion is significantly enhanced compared with the local  thermodynamic equilibrium (LTE) Boltzmann distribu-  tion.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The physical conditions of the gas strongly influ-  ence which principal quantum numbers (thus frequen-  cies) show enhanced emission.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Accordingly, the relative  intensities of RRLs, the so-called spectral line energy  distribution (SLED), carry information on the temper-  ature, density, and pathlength of the diffuse gas com-  ponent (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Shaver 1975;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Salgado et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2017a;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Oonk  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2017).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Stimulated emission has the added benefit  that its intensity is proportional to the background con-  tinuum intensity at a given frequency, SRRL ∝ Sbkg cont.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Therefore, it is conceivable to observe these RRLs at  cosmological distances wherever bright radio sources are  present (Shaver 1978).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In contrast, RRLs at high radio  frequencies (≳ 10 GHz) typically trace spontaneous re-  combination emission (in LTE), making them a great  direct measure of ionizing photons and therefore star  formation rates.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' However, the flux of spontaneous tran-  sitions falls off with distance (D) and frequency (ν) as  S ∝ D−2ν−1, limiting the observation of this faint emis-  sion to galaxies in the nearby universe.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The very first extragalactic detections of RRLs, in  M82 and NGC253, found contributions from stimulation  (Shaver et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1977;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Seaquist & Bell 1977;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Shaver et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  1978).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In the case of M82, Bell & Seaquist (1978) mod-  eled the SLED of hydrogen RRLs and showed that the  increasing intensity of the RRL emission at ν < 10 GHz  can only result due to stimulation by the large-scale syn-  chrotron continuum of the galaxy.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  They determined  that the hydrogen RRLs originate in ionized gas with  ne ≈ 150 cm−3 and pathlength ℓ ≈ 110 pc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Soon after,  Churchwell & Shaver (1979) used the Arecibo 300 m  telescope to search 21 galaxies and active galactic nu-  clei (AGN) for RRL emission with the 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 GHz re-  ceiver and three AGN with the 430 MHz receiver, with  the set-up covering just a single RRL transition.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' They  did not detect emission with line-to-continuum ratios of  τRRL > 10−3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' To similar sensitivities, Bell et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (1984)  used the Effelsberg 100 m dish at 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 GHz to search ten  galaxies without clear success.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Bell & Seaquist (1980)  discovered the H83α and H99α lines at 10.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 GHz and 6.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  GHz, respectively, in the GHz peaked-spectrum source  OQ 208 at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0763, showing that this RRL emission  could also only arise due to stimulation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' These studies  used narrow bandwidth receivers and were only sensitive  to one RRL spectral line per observation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  To date, 8 of the 23 external galaxies with detected  RRL emission show evidence for stimulated emission by  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  10  1  100  101  102  103  104  105  Density (cm  3)  100  200  300  400  500  600  Principal quantum number  MALS, 0 < z < 3  6479  815.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='9  242.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3  102.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  52.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='45  30.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='37  HRRL Rest Frequency (MHz)  Figure 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The principal quantum numbers, n, of Hydrogen  RRLs at which the stimulated-only emission of gas with a  given density peaks.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The thick black region marks the maxi-  mum n in the peak of emission, for ionized gas temperatures  5000 K ≤ Te ≤ 12 000 K, and the thin black region indicates  the n for which the peak intensity is more than one half of  the maximum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The shaded blue region shows the parameter  space covered by MALS for RRL redshifts of 0 ≤ z ≤ 3, while  the red hatched region shows the coverage for a z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 ob-  servation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' To calculate the peak optical depths we do not  take into account an external radiation field (which has a  minimal effect), but do take into account collisional broad-  ening of the line profile occurring in dense gas.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  non-thermal emission (for an overview, see Emig 2021)1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  These were all local (D < 350 Mpc) and mostly star  forming galaxies, until recently, Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2019) used  the Low Frequency Array to detect stimulated RRLs  at z = 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='124 with a rest-frame frequency of 284 MHz.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  They argue that the RRL emission most likely arises  from carbon in an intervening galaxy along the line-of-  sight to 3C 190.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' However, they could not clearly discern  whether the emission was from carbon or hydrogen since  the lines are separated by 150 km s−1 and have compa-  rable intensities at those frequencies in the Milky Way  (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Anantharamaiah 1985).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The improved sensitiv-  ity of high-resolution interferometers and the large frac-  tional bandwidths that enable deeper searches through  line stacking are making extragalactic RRL detections  now feasible.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Furthermore, given that the frequency  separation between each RRL is unique, the develop-  ment of new cross-correlation techniques are enabling  blind searches of RRLs across redshift space (Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2020).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Current large-bandwidth spectral line surveys, such as  the MeerKAT Absorption Line Survey (MALS;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Gupta  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2016), the First Large Absorption line Survey  (FLASH;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Allison et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2022), the Search for HI Ab-  1 We  also  refer  the  reader  for  an  update  collection  of  extragalactic  RRL  detections  at  www.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='tinyurl.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='com/  DatabaseForExtragalacticRRLs  Radio Recombination Lines at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  3  sorption with APERTIF (SHARP;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', see  Morganti  & Oosterloo 2018) – and in the future with the Square  Kilometer Array (SKA;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Blyth et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2015) – can  observe tens of RRLs simultaneously, opening the way  for ionized gas studies with optimum sensitivity to gas  with electron densities of 1 cm−3 ≲ ne ≲ 104 cm−3  (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', see Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' These surveys can explore RRLs as  a tracer of (diffuse) ionized gas in external galaxies for  the first time in a large systematic way and address at  what level stimulated RRLs are present in galaxies.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Ul-  timately, these RRL observations will bring new insight  into the evolution of the (ionized) interstellar medium  of galaxies and the environment of AGN.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In particular, MALS is carrying out the most sensi-  tive search to date (σ ∼ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 mJy beam−1 per 6 km s−1  channel) of H i 21 cm and OH 18 cm absorption lines at  0 ≲ z ≲ 2 (Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2016).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' MALS is observing ∼500  pointings centered on the brightest (S1 GHz > 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2 Jy)  radio sources at declination δ ≲ +30◦ (see Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2022, for the survey footprint), using the MeerKAT  (Jonas & MeerKAT Team 2016) L band, nominally cov-  ering 900–1670 MHz, and UHF band, nominally cover-  ing 580–1015 MHz.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Towards each sight line, the sur-  vey is sensitive to peak RRL line to continuum ratios  of τRRL = (0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='08 − 1) × 10−3 through line stacking,  reaching the range of optical depths observed from ion-  ized gas in the Milky Way (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Roshi & Ananthara-  maiah 2000).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' For an electron temperature of 8000 K,  these optical depths convert into emission measures  102.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 ≳ EM/cm−6 pc ≳ 104.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 for densities 1 cm−3 ≲  ne ≲ 104 cm−3 (see Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The first science verification observations of MALS  (Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021) focused on  the bright (S1 GHz ≈ 11 Jy) z = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='507 (Lidman et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  1999) blazar, PKS 1830−211 (referred to hereafter as  PKS 1830).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  PKS 1830 has a radio spectral index of  α1−15 GHz ≈ −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='26, classifying it as a flat spectrum ra-  dio quasar (Pramesh Rao & Subrahmanyan 1988;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Sub-  rahmanyan et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1990), and at lower frequencies it is  known to have a spectral turnover (Lovell et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1996).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  PKS 1830 is strongly gravitationally lensed (Patnaik  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1993;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Nair et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1993) by a galaxy at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  (Wiklind & Combes 1996).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Its morphology reveals  two compact radio components, referred to as north-  east (NE) and southwest (SW), approximately 1′′ apart  and surrounded by a low surface-brightness Einstein ring  (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Jauncey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1991).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' While the NE and SW com-  ponents are images of the blazar core, the ring is mainly  due to the jet and a bright knot in the jet (Jin et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2003).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' PKS 1830 is known to be variable, by up to a  factor of two in radio, on timescales of hours to years  (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Pramesh Rao & Subrahmanyan 1988;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Mart´ı-Vidal  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2013;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Allison et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2017;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Marti-Vidal & Muller  2019), and these variations are seen in all three lensed  components — the NE, SW, and ring.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The continuum  flux is dominated by the NE and SW components at  least down to 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 GHz (Verheijen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2001;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Koopmans  & de Bruyn 2005), where the Einstein ring contributes  ∼1% to the continuum flux (Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Pat-  naik et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1993).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' For an overview image of the system,  we refer the reader to Nair et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (1993).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Two absorption line systems are present along the  line-of-sight to PKS 1830.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The lensing galaxy at z =  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 has become an extragalactic-prototype absorption  system, with the most molecular species detected to date  (towards the SW image) (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Wiklind & Combes 1996;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Muller et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2011;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Tercero et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2020).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  galaxy has been directly imaged with Hubble Space Tele-  scope and appears to be a barred-spiral (Courbin et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  1998, 2002), but remains weak and elusive.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' From a well-  constrained lensing model (Nair et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1993;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Koopmans  & de Bruyn 2005;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Muller et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2020;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2021), the kinematics (vrot ∼ 260 km s−1) and orienta-  tion also suggest a nearly face-on (i ∼ 25◦) barred-spiral  galaxy of ∼1011 M⊙.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The SW image of the blazar core  passes through the galaxy at a radius of Rg ∼ 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 kpc  and a central velocity (from spatially unresolved emis-  sion) at vcen ∼ 0 km s−1, and the NE image passes  through at Rg ∼ 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 kpc and vcen ∼ −150 km s−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The SW image intercepts a spiral arm of the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  galaxy and traces dense (nH2 ∼ 2000 cm−3) molecu-  lar gas (Wiklind & Combes 1996;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Courbin et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2002;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Muller et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2013).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The gas along the line of sight to the  NE image arises in the diffuse ISM (Muller et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2011)  and is bright in H i 21 cm and main OH 18 cm absorp-  tion (Chengalur et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1999;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Koopmans & de Bruyn 2005;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' No time varia-  tion is visible in the cm-line spectra from the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  galaxy (Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021), which contrasts strongly  with the variations detected in the mm-wave absorp-  tion spectra (Muller & Gu´elin 2008;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Muller et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2014;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Schulz et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2015).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The second absorption system to-  wards PKS 1830 at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='19 has been seen only in H i  21 cm absorption so far (Lovell et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1996;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Allison et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2017;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  MALS observations of PKS 1830 verified system per-  formance and led to the first detection of OH 18 cm  satellite lines at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89, which had previously only  been detected at z ≲ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='25 (Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Combes  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In this article, we use these MALS obser-  vations to search for radio recombination line emission.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We aim to understand whether RRLs are present and  detectable and what they can tell us about photoion-  ized gas in galaxies and AGN.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2, we describe  4  Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  the methods used to process the data.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 3, we  report (i) detections of hydrogen RRLs in both the L  and UHF bands originating from ionized gas in the z =  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 galaxy, (ii) tests we performed to verify these re-  sults, and (iii) non-detections at the additional redshifts  searched.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 4, we constrain physical conditions of  the ionized gas by modeling the stimulated RRL emis-  sion.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Finally, we discuss implications of the ionized gas  measured by the RRLs in Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 5 and conclude in Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 6.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In this article, velocities are reported using the helio-  centric frame, with respect to z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='88582 unless stated  otherwise, and are converted from frequency using the  relativistic definition.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We use ΛCDM cosmology with  Ωm = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='29, ΩΛ = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='71, and Ho = 70 km s−1 Mpc−1, for  which 1′′ ∼ 7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='860 kpc at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='88582.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' DATA AND PROCESSING  2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Observations and Data Reduction  PKS 1830 was observed with the MeerKAT Radio  Telescope (Jonas & MeerKAT Team 2016) as the first  science verification target of MALS (Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2016).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  For the work presented here, we used MALS L band  spectra originally presented by Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Hereafter, we refer to this L band dataset obtained on  2019 December 19 as “Night1”.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We also used UHF band  spectra from the dataset obtained on 2020 July 13 and  presented in Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In addition to these  previously published datasets, we observed PKS 1830 a  second time in L band on 2020 September 18 using 59  antennas, which we will refer to as “Night2” in the ar-  ticle.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  For both L band observations, the total bandwidth  of 856 MHz was centered at 1283.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='987 MHz, cover-  ing 856–1712 MHz, and split into 32 768 frequency  channels.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  This delivered a frequency resolution of  26.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='123 kHz, which is 6.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1 km s−1 at the center of the  band.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' For UHF band, the total observable bandwidth  of 544 MHz covering 544–1088 MHz was also split into  32 768 frequency channels, providing a channel resolu-  tion of 16.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='602 kHz, or 6.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1 km s−1 at the center of the  band, i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', 815.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='992 MHz.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' For all observations the cor-  relator dump time was 8 s and the data were acquired  for all four polarization products, labeled as XX, XY,  YX and YY.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We also observed PKS 1934–638 and/or  3C 286 for flux density scale and bandpass calibrations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Since PKS 1830 is a bonafide VLA gain calibrator at  this spatial resolution, a separate gain calibrator was  not observed.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The total on-source times on PKS 1830  are: 40 min (L band Night1), 90 min (UHF band) and  90 min (L band Night2).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  All MALS datasets have been processed using ARTIP,  the  Automated  Radio  Telescope  Imaging  Pipeline  (Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021), a Python-based pipeline using tasks  and tools from the Common Astronomy Software Appli-  cations (CASA;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' McMullin et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2007;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The CASA Team  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The specific details of the observations, cali-  bration, and imaging of L and UHF band datasets can be  found in Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2021) and Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2021),  respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The Stokes-I continuum flux densities of  PKS 1830 obtained from wideband radio continuum im-  ages in L Night1 and UHF band with robust=0 weight-  ing are 11.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='245±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='001 Jy at 1270 MHz and 11.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='40±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='01 Jy  at 832 MHz, respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The radio emission is un-  resolved in these images with a spatial resolution of  12.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='′′9 × 8.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='′′1 (position angle = −76.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='◦3) and 17.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='′′4 × 13.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='′′1  (position angle = +69.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='◦0), respectively (Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2021;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The quoted uncertainty of  the flux densities are based on a single 2D Gaussian fit  to the continuum emission.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The continuum flux den-  sity of PKS 1830 obtained using the Night2 dataset is  S1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='27 GHz = 11.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='86 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='02 Jy.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  This matches with the  Night1 measurement within the flux density uncertainty  (∼5%) expected at these low frequencies.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Therefore,  throughout the article we use the average flux density  from the Night1 and Night2 datasets as the representa-  tive L band flux density, i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', S1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='27 GHz ≈ 11.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 Jy.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The spectral line data products from ARTIP for RRL  analysis are continuum-subtracted XX and YY parallel  hand image cubes obtained with robust=0 weighting.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We also note that for spectral line processing ARTIP  splits the L and UHF bands into 15 spectral windows  (hereafter SPWs) (see Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2021, for details of SPW boundaries).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The pixel sizes  for L and UHF band image cubes are 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='′′0 and 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='′′0, re-  spectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  XX and YY spectra were extracted in all  SPWs from a single pixel at the location of PKS 1830  determined from the continuum images.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The residual  flux density in each continuum-subtracted spectrum is  on the order of 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5% and required additional spectral-  baseline subtraction.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Further details of RRL specific spectral line processing  are provided in the next section.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In passing, we note that  we also made use of a MALS L band dataset of another  radio source, PKS 1740-517 (hereafter PKS 1740), also  known as J1744-5144, observed on 2020 September 20  (two days after Night2 observations of PKS 1830) with  an on-source time of 56 min.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' This observation also used  PKS 1934-638 and 3C 286 for flux density and bandpass  calibrations, and the unresolved radio source has a flux  density of ∼7 Jy at 1270 MHz, comparable to PKS 1830.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We process this dataset following the procedures de-  scribed above and use the resultant spectra to establish  the genuineness of the results obtained for PKS 1830.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Radio Recombination Lines at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  5  2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' RRL Spectral Processing  Considering the rest frequencies of RRLs, 38 and 44  of the α (∆n = 1) recombination lines (per element)  fall within the MALS L and UHF band coverage, re-  spectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2 At z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89, for example, the observations  cover 31 α recombination lines in L band spanning prin-  cipal quantum numbers n = 128 − 158 and 36 α recom-  bination lines in UHF band spanning n = 148 − 183.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Because line properties of RRLs are correlated over a  sizeable frequency range, we stacked the spectral lines  to drive down the noise and increase the signal to noise  ratio, as is commonly done in Galactic and extragalactic  RRL observations (Balser 2006;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2020).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We began spectral processing by identifying the ob-  served frequency of an RRL and extracting a spectrum  equivalent to vsys ± 1500 km s−1 centered on the line.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We selected this velocity chunk and discarded coverage  outside of it in order to (i) have a sufficient number  of channels to minimize errors in the estimation of the  spectral-baseline continuum level (Sault 1994), while (ii)  ensuring that a low (≤ 5) order polynomial – with an or-  der determined by minimizing the reduced χ2 – could be  fit over a well-behaved bandpass.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' RRLs that fell within  ±1000 km s−1 from the edge of a spectral window were  excluded from subsequent processing.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We flagged chan-  nels with persistent radio frequency interference (RFI)  and/or at the HI 21 cm and OH 18 cm line features  (at relevant redshifts) (see Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Combes  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021), and we discarded the full spectral line chunk  when flagged channels fell within |v| ∼ 500 km s−1 from  the line center in order to ensure a reliable fit to the  spectral-baseline.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We also flagged spectral line chunks  that were clearly contaminated by broad-band RFI and  reliable estimates of the baseline could not be attained.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  After flagging, we next fit a low order (≤ 5) polyno-  mial to (line-free) channels in each spectral chunk and  subtracted the fit.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' For the results presented in Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 3,  we did not impose a line-blank region, except for the  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 stacks.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' For the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 results, we first stacked  the spectrum without a line-blank region.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Based on the  significant feature we obtained in that spectrum, we set  the line blank as -230 km s−1 to +55 km s−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2 shows the baseline-subtracted spectral chunks,  as an example, from L band Night2 observations pro-  cessed for z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 RRLs.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The spectral noise has a  median of 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 mJy across the 17 RRL spectral chunks  used in the stack.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The noise properties and number of  2 We refer to the reader to the CRRLpy module (Salas et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2016)  found at https://github.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='com/astrofle/CRRLpy for a list of RRL  line frequencies.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  lines used in the final stacks can be found in Table 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The noise properties are consistent across the bands and  between parallel hand spectra.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We next interpolated each spectral chunk to a com-  mon velocity grid with channel widths of 1 km s−1, in-  tentionally oversampling the spectral channels to avoid  artificially smoothing-out spectral features.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The spec-  tral line chunks were then averaged together using the  inverse noise squared in line-free channels as a weight  (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2020).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 We next smoothed the channel  resolution to 8 km s−1 using a boxcar averaging kernel,  to better match the lowest resolution achieved at the  low frequency end of the bands.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' At this stage, we had  obtained a single Hnα spectrum for each parallel hand  XX and YY.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Finally, we averaged the XX and YY spec-  tra to create a Stokes-I spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We chose to combine  the stacked XX spectrum and the stacked YY spectrum  rather than creating a Stokes-I spectrum for each line  before combining polarizations because it (i) resulted in  better-behaved, i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Gaussian-like noise properties and  (ii) had the benefit of independently examining the dif-  ferences in the signal detected in two parallel hand spec-  tra.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The latter is particularly useful in distinguishing  true astrophysical signal from RFI, which is often lin-  early polarized.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' RESULTS  We applied the spectral processing procedures de-  scribed in the previous section to PKS 1830 observations  at the redshifts (i) z = 0 for Galactic emission, (ii)  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='19259 for the low redshift intervening absorber,  (iii) z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='88582 for the high redshift intervening ab-  sorber, and (iv) z = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='507 for the intrinsic redshift of  PKS 1830.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We detect RRL emission from the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  absorber in both Nights of L band and in UHF band ob-  servations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We report non-detections and upper limits  at all other redshifts and bands.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 3, we show the L band detections obtained  from the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 absorber.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We overlay the parallel  hand spectra, showing that they are consistent within  the noise in both nights of observations and therefore not  due to low-level linearly-polarized RFI.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We also overlay  the Stokes-I spectrum obtained from each night of L  band observations;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' they are consistent within the noise,  giving further evidence that the signal is astrophysical  in nature.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Lastly, we averaged L band Stokes-I spec-  3 We tested combining the spectral chunks with an additional  weight that depended upon the (inverse) line frequency (raised to  a power), but this did not significantly change the S/N properties,  indicating that the line properties are similar and well-correlated  across the observing bands.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  6  Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  1000  750  500  250  0  250  500  750  1000  Velocity (km s  1)  0  40  80  120  160  200  240  280  320  360  400  440  480  520  560  600  Flux density (mJy)  XX  YY  3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  Noise (mJy)  0  500  Integrated Signal  (mJy km s  1)  0  5  Integrated  S/N  128  132  133  134  135  136  137  145  149  150  151  152  153  155  156  158  128  132  133  134  135  136  137  145  149  150  151  152  153  155  156  158  128  132  133  134  135  136  137  145  149  150  151  152  153  155  156  158  Principal Quantum Number, n  Figure 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Spectral properties prior to stacking RRL transitions for L band spectra from Night 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Velocities are shown with  respect to z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='88582 and spectra are shifted along the ordinate for display purposes.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The principal quantum number of each  spectrum is given on the right hand side ordinate.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The shaded gray region in the left most panel indicates the line blank region.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  “Noise”, σ, is the rms (outside of the line blank region) per 8 km s−1 channel of the XX (yellow circles) or YY (purple circles)  spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' “Integrated Signal” = ∆vΣN  i=0 Si, the sum of emission from the channels inside the line blank region.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' “Integrated  S/N” = (ΣN  i=0 Si)/(  √  Nσ), the integrated signal divided by the integrated noise;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' we note that corresponding to negative values  of Integral Signal, the Integrated S/N is also negative.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The vertical dashed line in the three right panels indicates the median  value.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' There are no obvious and significant spurious features that could contaminate the RRL spectrum in our final stacking.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Radio Recombination Lines at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  7  Table 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Spectral and Line Properties  Line-of-sight  z  Band  Nlines  RRL  noise  vcenter  Speak  FWHM  �  SRRL dv  �  τ dv  (mJy)  (km s−1)  (mJy)  (km s−1)  (mJy km s−1)  (km s−1)  PKS 1830-211  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='88582  L  17  H 144 α  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='34  −117.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 ± 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3  1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='86 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='12  131 ± 14  258 ± 33  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='045 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='006  7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 ± 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='54 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='19  62.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 ± 9.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  102 ± 20  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='018 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='003  UHF  27  H 163 α  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='57  −124.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 ± 9.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='59 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='15  155 ± 24  262 ± 47  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='046 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='008  7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='81 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='25  80 ± 28  70 ± 25  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='012 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='004  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  L  17  H 175 α  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='36  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  < 22.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  < |0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0020|  UHF  28  H 203 α  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='41  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
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+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  < 26.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5  < |0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0023|  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='19259  L  17  H 166 α  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='34  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  23.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 ± 7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='002 1 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='000 6  UHF  33  H 189 α  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='43  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
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+page_content='  < 27.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  < |0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0024|  2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='507  L  14  H 116 α  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='40  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
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+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  < 25.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5  < |0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0023|  UHF  19  H 132 α  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='55  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  < 34.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='9  < |0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0031|  PKS 1740-517  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='88582  L  17  H 142 α  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='39  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='..' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  < 24.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  < |0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='004|  Note— Uncertainties of the line properties are determined from the variance of each parameter as determined by the fit.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Nlines is the  effective number of recombination lines stacked in the final spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' “RRL” refers to the effective radio recombination line transition of  the stacked spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' “noise” is the weighted standard deviation of line-free channels in units of mJy per 8 km s−1channel.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' vcenter is the  central velocity of the best fit Gaussian and uncertainty.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Speak is the peak amplitude of the best fit Gaussian fit.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' FWHM is the full-width  half maximum of the best fit Gaussian.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  �  SRRL dv is the velocity-integrated flux density of the best-fit Gaussian profile, or in the case of  an upper limit, the reported value is equal to an integrated signal to noise ratio of 3 assuming a line width of 60 km s−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  �  τ dv is the  velocity-integrated optical depth computed as −  �  SRRL/Sc dv where the values used for the continuum flux density, Sc, are described in  Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  8  Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  tra from Nights 1 and 2, producing a spectrum with  the highest signal-to-noise ratio attainable which we re-  fer to as the total-I spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The reduction in spec-  tral noise of the incrementally combined spectra follows  root N statistics.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The total integrated flux density of  �  SH144α dv = 337±16 mJy km s−1 with a maximum in-  tegrated signal-to-noise ratio (S/N) = (ΣN  i=0 Si)/(  √  Nσ)  of 21 is computed from the total-I spectrum by integrat-  ing over the N channels covering the velocity range −230  to 55 km s−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The effective transition of the total-I spec-  trum presented in the bottom panel of Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 3 is H144α,  at a rest-frame frequency of 2179.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 MHz and observed  at 1155.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 MHz.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The effective transition is determined  from the noise-weighted average of the line transitions  included in the stack.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The line properties of the ob-  served emission are consistent with SH136α < 5 mJy  upper limits to the H136α line at νrest = 2585.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 MHz  (νobs = 1371.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1 MHz) — a transition which is included  in our stack — obtained by Mohan et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2002).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In addition to (1) multiple nights of observations and  (2) comparing XX and YY parallel hand spectra,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' we ver-  ified additional evidence that the signal is true recom-  bination line emission by (3) observing an independent  detection of RRL emission in UHF band (more details  below),' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (4) performing jackknife tests,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' in which one line  spectrum at a time is omitted from the stacked spec-  trum,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' showing that the signal is not dominated by a  single outlying spectral chunk4,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (5) splitting the lines in  the band into two groups creating two sub-stacks and  this resulted in consistent line properties,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (6) verifying  a signal is not reproducible by stacking RRLs at other  redshifts (more details at the end of the Section and  see Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 4), and (7) finding that an RRL spectrum of  PKS 1740 stacked at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 does not systematically  produce a signal.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We made use of additional MALS L  band observations of PKS 1740 and followed the spectral  processing procedures described in Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We created  an average RRL spectrum at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 with an effec-  tive transition of H142α and show it in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  This  spectrum reached a noise, σ = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='39 mJy, comparable to  the PKS 1830 stack.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' However, no emission or significant  spectral features are present in the PKS 1740 spectrum,  and it is consistent with noise.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  This lends additional  support to the physical and real nature of the emission  from the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 absorber in PKS 1830.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Two velocity components dominate the L band H144α  emission from PKS 1830.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In the bottom panel of Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 3,  we show the best fit of two Gaussian profiles and the  4 We also refer the reader to Figure 2, where the noise, integrated  signal, and integrated signal-to-noise properties also demonstrate  no single or few outlying spectra dominate.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2  0  2  2  0  2  2  0  2  Flux Density (mJy)  600  400  200  0  200  400  600  Velocity (km s  1)  2  0  2  Figure 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Comparison of RRL stacked spectra in L band at  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The top three panels compare spectra from parallel  hands and observing nights.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The bottom panel shows (i) the  final spectral result for the band with Gaussian profiles fit  to two components and (ii) underneath, the final spectrum  with the Gaussian profiles subtracted.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The vertical dashed  lines mark the velocities −230 km s−1 and 55 km s−1 within  which we integrate the signal of the Total component.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  spectrum that results when the two Gaussian profiles  are subtracted.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The properties of the Gaussian fits  are listed in Table 1;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' the errors of each quantity are  determined from the variance of each variable as de-  termined by the fit.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The H144α component centered  on −117.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 ± 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 km s−1 arises from the NE sight-line  (and thus we will refer to this velocity component as  the NE component hereafter).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The H144α component  centered on 7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 ± 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2 km s−1 arises from the SW sight-  line (and thus we will refer to this velocity compo-  nent as the SW component hereafter).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In Table 1,  we also include the integrated optical depth equal to  �  τ dv ≈ −  �  SRRL/Sc dv computed by letting Sc of each  component equal half the total continuum flux density  in the band, Sc ≈ 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='75 Jy.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We assume the continuum  flux is equally split between the two core components  following Koopmans & de Bruyn (2005) and Combes  Radio Recombination Lines at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  9  600  400  200  0  200  400  600  Velocity (km s  1)  2  0  2  4  6  8  10  12  14  Flux density (mJy)  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='19  z = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5  PKS 1740  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  L band  UHF band  Figure 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Non-detection RRL spectra in the spectrum of  PKS 1830 (top three) and in PKS 1740 (bottom).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Spectra  have been given an arbitrary offset in intensity in multiples  of 4 mJy.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Velocities are defined with respect to the labeled  redshift.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  600  400  200  0  200  400  600  Velocity (km s  1)  1  0  1  2  3  Flux Density (mJy)  HI absorption / -240  OH absorption / -30  0  1×10  4  2×10  4  Normalized Flux Density  Figure 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The H144α spectrum detected in L band overlaid  by the rescaled H i and OH absorption spectra.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The right-  hand ordinate shows the RRL flux density normalized by the  continuum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2021) which show this to be the case and that the  core components dominate the emission at least down  to 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 GHz.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Furthermore, ALMA observations measure  a NE/SW flux density ratio close to one in July 2019  (Muller et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 5 overlays the H144α spectrum with the H i  21 cm and OH 18 cm absorption spectra that have been  rescaled by factors of −240 and −30, respectively, in  flux density units and obtained from the same MALS  datasets.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The RRL emission appears to span a simi-  lar velocity range as these other diffuse gas tracers and  likewise, is also dominated by two main velocity compo-  nents.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The RRL line centroids of the NE and SW compo-  nents agree within error with the OH 18 cm profiles,  which have values of −110±3 km s−1 and 6±3 km s−1,  respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  However, the RRL centroids are signif-  icantly offset from the dominant H i components at  ∼ −150 km s−1 and 0 km s−1, respectively, albeit the H i  profile is more complex with perhaps five velocity com-  ponents best-fitting the observed profile.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The variation  in central velocity with H i could arise due to different  filling factors, intrinsic distributions, and shapes of the  continuum with the higher frequency tracers (OH and  RRLs) finding better agreement.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The RRL line width of the NE component also agrees  within error with the OH absorption width, but the  widths are significantly different for the SW component,  with the RRL FWHM of 63 ± 10 km s−1 and the OH  FWHM of 94.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2 ± 5 km s−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  An estimate of the H i  width is close to ∼ 100 km s−1 for both components,  which would be inconsistent with the RRL widths from  either component.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Given the smaller line width of the  warmer gas traced by the RRLs in the SW, the emis-  sion may likely have a smaller filling factor, which is to  say, fewer individual components contribute to the total  profile.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' This can be expected since the SW line of sight  is dominated by dense molecular gas.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  While the two dominant components of H144α emis-  sion generally agree with the H i and OH profiles, more  than two velocity components are discernible in the  higher S/N spectra of H i and OH.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' For example, OH  absorption has an additional component centered at  −211 ± 3 km s−1 with a FWHM of 28 ± 9 km s−1;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' the  RRL line profile fit to the NE component encompasses  some emission in this velocity range.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The H i absorp-  tion spectrum also shows two velocity features that are  blueshifted with respect to the main ∼ −150 km s−1  peak.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 6, we show the UHF band detections obtained  at the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 absorber.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We overlay the parallel  hand spectra, showing that they are consistent within  the noise and thus likely not a result of RFI.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Inte-  grating the Stokes-I spectrum over the velocity chan-  nels from −230 to 55 km s−1 results in  �  SH163α dv =  309 ± 22 mJy km s−1 and a maximum integrated S/N  of 14.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The effective transition of the final spectrum is  H163α, with a rest-frame frequency of 1504.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 MHz and  observed at 797.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='85 MHz.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The H163α emission arises across a similar velocity  range as the H144α emission, yet the peak intensities are  slightly lower.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The distinction of two components is less  obvious in the H163α stack (UHF band), as compared  with the H144α stack (L band).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We fit two Gaussian  components to the spectrum, fixing the central velocity  10  Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2  0  2  600  400  200  0  200  400  600  Velocity (km s  1)  4  2  0  2  Flux Density (mJy)  Figure 6.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' RRL stacked spectra in UHF band at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The top panel compares spectra from the two parallel hands.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The bottom panel is the same as in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 3 but for the UHF  band spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  of the SW component equal to that obtained from the  high S/N spectrum in L band, vcen = 7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 km s−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The  best fits are shown in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 6 and the fit parameters are  listed in Table 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' As in the L band spectrum, we com-  pute the integrated optical depth by assuming the UHF  band continuum flux is equally split towards each core  component, Sc ≈ 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 Jy.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 4, we show the L and UHF band stacked spec-  tra of PKS 1830 at each redshift where we obtained null  results: z = 0, z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='19, and z = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The spectral prop-  erties of the non-detections are included in Table 1 and  the integrated optical depth,  �  τ dv ≈ −  �  SRRL/Sc dv,  is computed by letting Sc equal the total continuum  flux density in the L and UHF bands, respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Mohan et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2002) previously reported a 5σ upper  limit to the H158α line from the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='19 absorber  of SH158α < 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 mJy.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In our L band spectrum of the  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='19 stack at an effective transition of H166α, we  reach a spectral noise of 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='34 mJy, and our 3σ upper  limit to the peak line emission of SH166α < 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0 mJy  is consistent with the results obtained by Mohan et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  (2002).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Lastly, we note that carbon RRL emission becomes  significantly enhanced only at frequencies ≲ 350 MHz,  and thus we do not expect to detect it at the frequen-  cies of our observations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The detected signal likely  arises only from hydrogen emission given that it is co-  incident in velocity with the HI 21 cm and OH 18 cm  absorption.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' A 3σ upper limit to the carbon RRLs at  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 in L band is  ���  SC144α dv < 22.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 mJy km s−1  and in UHF band is  �  SC163α dv < 37.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 mJy km s−1,  assuming a line width of 60 km s−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We searched for  Hβ emission by stacking all available lines in both L  and UHF band following the procedures described in  Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We report a 3σ upper limit to the Hβ emission  of  �  SH192β dv < 18.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 mJy km s−1 and an in-band ratio  of peak H192β/H144α < 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5, where typical in-band β/α  ratios are ∼ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2 (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Salas et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2017).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' PHYSICAL CONDITIONS OF IONIZED GAS IN  THE Z=0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 ABSORBER  Because PKS 1830 has a relatively low Galactic  latitude and is behind the Inner Galaxy,  (ℓ, b  =  12.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0◦, −5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7◦), it has not yet been feasible to observe ion-  ized gas tracers at UV through IR wavelengths from the  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 galaxy (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Djorgovski et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1992;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Courbin  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1998).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  However, there have been some indica-  tions for the presence of ionized gas that could be at-  tributed to the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 galaxy.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Firstly, the jet emis-  sion which forms an Einstein ring shows a complete  turnover at ∼ 300 MHz in its spectral energy distribu-  tion (SED), which could be due to free-free absorption  and would not arise from synchrotron self absorption  (Pramesh Rao & Subrahmanyan 1988;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Jauncey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  1991;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Jones et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1996;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Lovell et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1996, and for more  details, see Sec 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Secondly, jet emission in the Ein-  stein ring (i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', not the core emission) is strongly po-  larized (Pramesh Rao & Subrahmanyan 1988;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Subrah-  manyan et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1990), indicating ionized plasma lies along  the lines of sight.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' However, it is debated whether the  ionized gas originates in the Milky Way or the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  galaxy and if the blazar core components are free-free  or synchrotron-self absorbed (Jones et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1996;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Guirado  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1999;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Mart´ı-Vidal et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2015).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Stimulated hydrogen radio recombination lines pro-  vide strong constraints on the gas volume density of elec-  trons and volume-averaged pathlength.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In the following  sections we model the RRL emission to derive physi-  cal properties.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We use these constraints to estimate the  ionized gas mass per unit area and the ionizing photon  flux.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' RRL line width  The width of recombination lines as a function of fre-  quency provides insight into the physical properties of  the emitting gas.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  A Doppler-broadened profile has a  constant width in velocity units as a function of fre-  quency, and its Gaussian profile indicates broadening  from the intrinsic gas particle motions (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', due to the  temperature of the gas or turbulence) or from multi-  ple emitting regions rotating at different velocities in a  galaxy.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' However, collisional and radiation broadening  Radio Recombination Lines at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  11  create a Lorentzian line profile and have an increasing  line width towards lower frequency, thereby informing  on the electron density of the gas or the incident radia-  tion field strength, respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  For the NE component, widths of FWHMH144α =  131±14 km s−1 and FWHMH163α = 155±24 km s−1 are  consistent within error.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' For the SW component, widths  of FWHMH144α = 62.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3±9.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 km s−1 and FWHMH163α =  80±28 km s−1 are also consistent within error.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' This in-  dicates that the lines are Doppler broadened.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Gaussian  distributions do fit our observed line profiles reasonably  well (see Figs.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 3 and 6).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Assuming the line widths of each component are equal  at the two frequencies, the weighted average of the  FWHM for the NE component is 137 km s−1 and for  the SW component is 64 km s−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We then use the width  at the lowest frequency to put a firm upper limit on the  gas density, assuming pressure broadening dominates.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Note, there is no indication to expect an extreme ra-  diation field that would cause the line to be radiation  broadened.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Salgado et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2017b) provide the FWHM  of a collisionally broadened profile, ∆νcol = nenγ ·10a/π  where ∆νcol is in units of Hz, ne is in units of cm−3,  a = −7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='386, γ = 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='439 and n is the principal quantum  level.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We place an upper limit of ne ≲ 7900 cm−3 for  the NE component and ne ≲ 3700 cm−3 for the SW  component.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' RRL SLED  As shown in Shaver (1975) and Shaver (1978),' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' the  flux density of an optically thin RRL of principal quan-  tum number,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' n,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' and frequency,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' ν,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' observed in front of  a significantly-brighter background radio source of flux  density Sbkg,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='ν and which results from stimulated emis-  sion is given by  Sn,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='ν ≈ −τ ∗  n,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='ν (bnβ) Sbkg,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='ν  (1)  where τ ∗  n,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='ν is the LTE RRL optical depth,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' bn is the ra-  tio of the number of hydrogen atoms in level n between  the non-LTE and the LTE cases,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' and β characterizes  the effect of stimulated transitions.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  bn and β, collec-  tively referred to as departure coefficients, depend on the  atomic physics of the hydrogen atom, and their product  is dependent upon electron density, electron tempera-  ture, the radiation field, and pathlength.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Computation  of the departure coefficients has been thoroughly stud-  ied since the first observations of hydrogen RRLs (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=',  Shaver 1975;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Hummer & Storey 1987;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Salgado et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2017a;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Prozesky & Smits 2018).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Integrating over the line  profile and expressing the LTE optical depth of the line,  the integrated optical depth of an α transition (∆n = 1)  100  101  Rest Frequency (GHz)  10  2  dv  (km s  1)  NE  SW  Total  100  Observed Frequency (GHz)  Figure 7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The integrated optical depth as a function of fre-  quency for the NE, SW, and Total components.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We overlay  predicted line intensities from RRL models, from 100 model  combinations that fall within the reported uncertainties and  chosen at random.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We assume a redshift z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 for the  conversion between observed and rest frequencies.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  at high principal quantum numbers takes the form  �  τn dv ≈ 6.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='13 × 10−4 km s-1 (bnβ)  (2)  �  EM  104 cm-6 pc  � �  Te  104 K  �-2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 �  ν  GHz  �-1  where Te is the electron temperature and EM is the  emission measure equal to EM =  �  nenion dℓ for elec-  tron density ne and ion density nion integrated over the  pathlength ℓ.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Because the departure coefficients at each  principal quantum number are strongly dependent upon  density, they are key to breaking the degeneracy between  density and pathlength in the emission measure.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 7, we plot the RRL SLED using the inte-  grated optical depths corresponding to the NE and SW  Gaussian components from from Table 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We also  plot (and use for analysis in this section), the inte-  grated optical depth of the Total component computed  from the velocity-integrated emission over -230 to 55  km s−1 and setting the continuum flux density, Sc,  equal to the flux density in each respective band, i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  �  τH144α = −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='029 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='001 km s−1 and  �  τH163α =  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='027±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='002 km s−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' While it would be ideal to model  the two velocity components individually, the large er-  rors of the Gaussian fit parameters warrant caution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The  results from the Total component represent an average  of the two lines-of-sight.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  To model the recombination line emission, we calcu-  lated the departure coefficients for a range of electron  densities and electron temperatures using the code and  12  Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  framework described in Salgado et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2017a,b).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' When  computing bnβ we only consider the effect of the cosmic  microwave background on the level populations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The  grid in density was sampled at an interval of 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 dex  and the temperature in multiples of 100.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We then inter-  polate over the grid values using a cubic bivariate spline  for the following analysis.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We used Bayesian analysis to constrain the posterior  distribution of the parameters ne, Te, and ℓ, and we  assume the gas is fully ionized with nion = ne.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The  likelihood function describes the comparison of the ob-  served integrated optical depth with the model (Eq.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2),  assuming a Gaussian distribution function with disper-  sion equal to the measurement uncertainty (see Table 1).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The model is taken to be Eq.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2 in which the values of ν,  ne, Te, and corresponding bnβ are input, and the path-  length is left as a free parameter.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We used flat priors for  the parameters expressed in logarithmic scale.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We as-  sumed reasonable ranges of the parameters: for density,  log(ne) = [−1, 6] cm−3 for the Total component, and  we used the upper limits derived from the line width  for the NE and SW components, log(ne) = [−1, 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4]  and log(ne) = [−1, 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6], respectively, in units of cm−3;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  for pathlength, log(ℓ) = [−9, 6] pc;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' and for tempera-  ture, we select a strict range of log(Te) = [3, 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3] K,  given that theory and observations substantiate tem-  peratures of photoionized gas to have typical values of  Te ≈ 6000 − 10 000 K (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Wenger et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2019;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Tielens  2005).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We also used the prior that the departure coef-  ficients must be negative and thus the line appears in  emission.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' To sample the posterior distribution we used  an affine-invariant sampler within the package emcee  (Foreman-Mackey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2013).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We used 20 walkers, 105  iterations, and verified convergence using an autocorre-  lation time analysis.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The 2D and 1D marginal posterior distributions of  the parameters of the Total component are plotted in  Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 8.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' They show that density is constrained by the  models to within 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 dex with a maximum a posteriori  value of ne = 500 cm−3 and 68.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3% credible interval of  130 cm−3 ≤ ne ≤ 2000 cm−3, and that electron temper-  atures are not well constrained.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Typical temperatures  of photoionized gas have values of Te ≈ 6000−10 000 K,  with variations that are largely metallicity dependent  (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Shaver et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1983;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Wenger et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2019).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The RRL  modeling shows that typical temperatures are slightly  more likely than cooler temperatures.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The maximum a  posteriori value of the volume-averaged pathlength for  the Total component is ℓ = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='025 pc and the 68.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3% cred-  ible interval is 7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='9 × 10−3 pc ≤ ℓ ≤ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='13 pc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' It is reason-  able to infer that this ionized gas is not distributed in a  very thin sheet of ℓ ∼ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='025 pc, but instead has a volume  3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  log(Te)  1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  log(ne)  2  1  0  1  log( )  3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  log(Te)  2  1  0  1  log( )  Figure 8.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Corner plot showing the Total component con-  straints for the electron densities ne in units of cm−3, elec-  tron temperatures Te in units of K, and pathlength ℓ in  units of pc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Contours are drawn at 68% and 95% intervals.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The histograms show the marginalized distributions and the  shaded region marks the 68% credible intervals.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Table 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Constraints on physical conditions.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Temper-  ature is not well constrained within the allowed range  log(Te) = [3, 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3] K.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  vcen  log(ne)  log(ℓ)  log(EM)  (km s−1)  (cm−3)  (pc)  (cm−6 pc)  NE  120  2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0+1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7+1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  SW  8  3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  −2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7+1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='9+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  Total  (-230–55)  2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='9+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  filling factor less than unity, and the emission arises from  multiple, discrete clouds within the galaxy — either as  ionized clouds, interface layers of molecular clouds, H ii  regions (for further information see Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1), etc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 9, we show the marginal posterior distributions  for all three components and each of the parameters,  electron density (ne), electron temperature (Te), path-  length (ℓ), and emission measure (EM).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The parameter  constraints are listed in Table 2, with the maximum a  posteriori values and 68.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3% credible intervals.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We do  not list the temperature in Table 2 because it is not well  constrained by these measurements.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We take 100 RRL  models at random with properties that fall within the  Radio Recombination Lines at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  13  100  102  104  Density (cm  3)  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  Posterior Probability  NE  SW  Total  1000  10000  Temperature (K)  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  10  2  100  102  Pathlength (pc)  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  102  104  106  Emission Measure (cm  6 pc)  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3  0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  Figure 9.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Posterior probability distributions for the parameters constrained through the RRL observations: electron density ne,  electron temperature Te, pathlength ℓ, and emission measure EM, derived for the NE, SW, and Total components.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The shaded  regions represent the 68.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3% credible intervals.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In the left-most panel, the gray dashed (dotted) line marks the ne < 7900 cm−3  (<3700 cm−3) constraint for the NE (SW) component obtained from the line width.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  constraints of the 68.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3% credible intervals and plot the  SLEDs of these models in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 7, in order to demonstrate  the variation in the predicted integrated optical depth  for different models.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Mass of ionized gas  Using the most likely values of the physical quantities  in Table 2, we estimate the mass and mass per unit area  of ionized gas in each component.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' These mass estimates  are meant for qualitative comparisons as order of magni-  tude indications and do warrant caution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We assume the  volume of gas is effectively described by a cylinder, as  a circular region on the plane of the sky (core size) and  with a distance into the plane equal to the path length.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We also assume that the radio continuum emission is  dominated by the NE and SW components, as these  have been shown to account for ∼ 99% of the emission  at 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 GHz (Koopmans & de Bruyn 2005;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' To calculate the mass of ionized gas, we expect  Mion ≈ 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='36mH · ne · (πr2  c)ℓ  Mion ≈ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='11 M⊙  � ne  cm−3  � � rc  pc  �2 � ℓ  pc  �  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  (3)  where mH is the hydrogen atom mass and rc is the radius  of the radio continuum core.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Guirado et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (1999) con-  strained the source size of the SW component to follow  ∝ ν−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0 resulting in a size of 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1′′ at 1 GHz, which cor-  responds to the value we set of rc = 786 pc at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  For the NE component we adopt the separation of 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='05′′  between the two brightest emission peaks as the size,  rc = 393 pc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We do not include uncertainties for rc  when computing the mass;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' however, we note that their  errors are small in comparison to the large range un-  certainty of the credible intervals.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Using the posterior  distributions of ne and ℓ, we estimate a total mass for  the NE component of Mion ≈ 106.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 M⊙ and for the  SW component, Mion ≈ 105.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 M⊙.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' If we assume that  the area of the Total component is a summation of the  areas intercepted by the NE and SW lines-of-sight, the  estimated ionized mass is Mion ≈ 106.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 M⊙.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  It is informative to also calculate the gas mass per  unit area  Σion ≈ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='033 M⊙ pc−2 � ne  cm−3  � � ℓ  pc  �  .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  (4)  For the NE, SW, and Total components, we calculate  Σion to be 100.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 M⊙ pc−2, 10−0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 M⊙ pc−2, and  100.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 M⊙ pc−2, respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Using the surface densities of the NE, SW and Total  components, we calculate an estimate for the total ion-  ized gas mass of the galaxy within the Einstein ring of  Rg ∼ 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 kpc in units of M⊙ as log(Mion,g) ≈ 8.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7,  7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4, and 7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='9+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5, respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' While the mass esti-  mated from the SW is more equivalent to a true lower  limit of the total ionized gas mass, the estimates from  the NE and Total components are almost certainly lower  limits as well since we do not trace the bulk of the ionized  gas mass of the galaxy contained in the Warm Ionized  Medium (WIM;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' see Tielens 2005).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Ionizing photon flux  We use the ionized gas emission measure to infer the  ionizing photon flux.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The ionizing photon rate, Qo, per  unit area is,  Qo  area ≈ EM · αB  Qo  area ≈ 7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 × 1045 photons s−1 pc−2  EM  103 cm−6 pc (5)  where αB is the case B recombination coefficient.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Us-  ing the posterior distributions of the emission mea-  sure, we calculate ionizing photon fluxes in units of  14  Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  photons s−1 pc−2 of log (Qo/area) = 47.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2, 46.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0,  and 47.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 for the NE, SW, and Total components,  respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' These values are about an order of mag-  nitude or more higher than the ionizing photon flux in  the disk of the Milky Way (Kado-Fong et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2020, and  references therein).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  While the gas mass estimates (Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3) are likely lower  limits, the ionized photon fluxes are closer to realistic  values, since they are dominated by the large emission  measures that we are sensitive to.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' DISCUSSION  5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Star Formation Rate and ISM Properties  The posterior distributions for the emission mea-  sure and thus directly the ionizing photon flux are  constrained with fairly similar 68.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3% credible inter-  vals.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  To estimate a star formation rate (SFR) of  the galaxy, we adopt the log-average EM within the  credible intervals of the three components, EM  ≈  104.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 cm−6 pc, within a typical error of 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 dex, and  therefore we adopt an ionizing photon flux is Qo/area ≈  1046.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='9±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 photons s−1 pc−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We estimate the total ion-  izing photon rate for the galaxy within Rg = 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 kpc  as Qo = πR2  g · 1046.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='9±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 ≈ 1054.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 photons s−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' A  Starburst99 model (Leitherer et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1999) of continu-  ous star formation establishes the relation with the ion-  izing photon rate (which levels off after ∼50 Myr) of  SFR = 1 M⊙ yr−1 (Qo/1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 × 1053 photons s−1).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Using  this relation, an estimated SFR for the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 galaxy  is SFR ≈ 101.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 M⊙ yr−1 and the SFR per unit area  is ΣSFR ≈ 10−0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 M⊙ yr−1 kpc−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' A galaxy on the  main sequence at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 with SFR ∼50 M⊙ yr−1 has a  typical stellar mass of ∼ 1011 M⊙ (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Schreiber et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2015).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Current lensing models estimate the total mass  within the Einstein ring as ME ≈ 4 × 1011 M⊙ (Muller  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2020) and therefore a stellar mass of ∼ 8×1010 M⊙  given a typical mass to stellar light ratio of ∼ 5 (Treu &  Koopmans 2004).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' This is likely a main-sequence galaxy.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 we estimated the ionized gas mass per unit  area of the NE component to be Σion ∼ 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1 M⊙ pc−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  For comparison, the H i column density is estimated to  be NH I ≈ 5×1021 cm−2 assuming half of the continuum  flux comes from the NE component (Chengalur et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  1999;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Combes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Assuming the average parti-  cle mass is ≈ 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='36mH, the atomic gas mass per unit area  is ΣH I ≈ 50 M⊙ pc−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We use the OH column density of  NOH ≈ 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 × 1015 cm−2 (Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021) and assume  an abundance of 10−7 (Balashev et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021) given that  this line-of-sight has properties of a diffuse cloud (Muller  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2011) in order to estimate a molecular gas column  density of NH2 ∼ 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5×1022 cm−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' This H2 column den-  sity is higher than the NH2 ∼ 1021 cm−2 derived from  H2O absorption, with a smaller continuum cross section  at higher frequencies (Muller et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2014).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Assuming the  average particle mass is ≈ 2mH, the molecular gas mass  per unit area is ΣH2 ≈ 240 M⊙ pc−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  With these estimates, the neutral gas mass per unit  area is ΣHI+H2  ∼ 290 M⊙ pc−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The ionized gas  mass detected in RRLs of the NE component is a  small fraction (∼0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7%) of the total gas mass.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The  Kennicutt-Schmidt law (Kennicutt 1998) long estab-  lishes a direct correlation between the surface densi-  ties of the neutral gas mass ΣHI+H2 and the star for-  mation rate ΣSFR in galaxies on spatial scales 300–500  pc or more (Schruba et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2010;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Kruijssen & Long-  more 2014).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' It suggests that a region in a galaxy with  ΣSFR ∼ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 M⊙ yr−1 kpc−2 has a neutral gas mass per  unit area of ΣHI+H2 ∼ 270 M⊙ pc−2 (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Kennicutt  & De Los Reyes 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Our measured neutral gas mass  agrees to within 10% of the expected value, although our  measured SFR surface density has a large uncertainty.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Although the estimated densities of the NE, SW  and Total components are consistent within the er-  rors, the most likely density of the SW component,  ne ≈ 1600 cm−3, is typical of young, compact H ii re-  gions.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' If we assume the H ii regions are rH II ≈ 2 pc in  size, then the covering fraction through this cross section  of the galaxy is fc ≈ ℓSW/(4/3 · rH II) ≈ 7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 × 10−4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The  total number of H ii regions, NH II, is calculated from  the surface density estimates, πr2  C = NH II/fc · (π r2  H II),  which computes to NH II ∼ 116, where we recall from  Sec.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 that rC = 786 pc for the SW component.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Equiv-  alently, assuming all H ii regions have ne ≈ 1600 cm−3  and rH II ≈ 2 pc, the ionized gas mass per H ii region is  estimated to be MH II = 1860 M⊙, and from the total  ionized mass of the SW component, MSW = NH IIMH II,  also results in NH II ≈ (2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1×105 M⊙)/(1860 M⊙) ∼ 113.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  However, this calculation warrants caution because the  number of H ii regions changes dramatically depending  on the assumed size.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We set rH II ≈ 2 pc because it is  the typical size of young, massive star clusters (Ryon  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2017) that are expected to dominate star forma-  tion in galaxies of this epoch, i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', with high gas surface  densities and star formation rates (Kruijssen 2012).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The ne − ΣSFR relation  The star formation rate per unit area is shown to  be correlated with the electron density of ionized gas  in the region (Shimakawa et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2015;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Herrera-Camus  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2016;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Jiang et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2019).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Assuming H ii regions  thermalize with the ISM (Guti´errez & Beckman 2010),  i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', take on a pressure balance with others phases, then  the volume-average density of the ionized gas (along  with fairly consistent ionized gas temperatures) indi-  Radio Recombination Lines at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  15  cates the thermal pressure of the medium (Jiang et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2019;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Barnes et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' This results in a P −ΣSFR re-  lation that serves as an important test-bed for pressure-  regulated, feedback-modulated star formation (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Kim  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2013;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Ostriker & Kim 2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Using doublet ratios  of [SII] and [OII] in the optical (Kewley et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2019),  Shimakawa et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2015) and Jiang et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2019) find a  relation of ΣSFR ∝ n1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3  e  in a sample of z ∼ 1 − 3  starburst galaxies.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In the far IR, the ratio of [NII] fine  structure lines from a sample of nearby normal galax-  ies and (ultra) luminous infrared galaxies ((U)LIRGs;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  LIR ≥ 1011 L⊙) establish ΣSFR ∝ n1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5  e  (Herrera-Camus  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2016).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  For ΣSFR ∼ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 M⊙ yr−1 kpc−2, the electron den-  sity predicted by the Shimakawa et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2015) relation is  ∼ 110 cm−3 and by the Herrera-Camus et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' (2016) re-  lation is ∼ 200 cm−3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  These density estimates agree  well with the NE component and lie on the cusp of  the 68% credible intervals of the SW and Total com-  ponents.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  If the RRL emission is tracing the thermal  properties of the diffuse medium in the galaxy’s disk,  higher pressures and densities are typically found at  smaller galactic radii, i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', the SW component, than at  larger galactic radii, i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', the NE component.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' For exam-  ple, Guti´errez & Beckman (2010) measured the electron  density to increase towards smaller galactic radii, r, as  ⟨ne⟩ = ⟨ne⟩o exp (−r/Rg), where Rg is the scale length  of the disk at which star-formation and density drops off  and ⟨ne⟩o is inner most density.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' With Rg = 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 kpc and  ⟨ne⟩ = 100 cm−3 of the NE component, at r = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 kpc  the expected density is ne ∼ 160 cm−3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' While the con-  trast in density at the two radii is not as extreme as the  best fit densities of the components indicate, the general  trend is consistent and a density of 160 cm−3 does fall  within the 68% credible interval of the SW component.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The smaller pathlength in comparison to the NE com-  ponent might then indicate a smaller covering fraction  of the overall larger cross section of this line-of-sight, i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  only within or close to the spiral arm.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Radio Continuum SED  The radio continuum emission from PKS 1830 is com-  plex.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The lensing is achromatic and contains a small-  scale core-jet structure with regions of different spectral  indices and opacities.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In addition, the source is variable  on hourly to yearly timescales (Pramesh Rao & Sub-  rahmanyan 1988;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' van Ommen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1995;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Lovell et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  1996, 1998;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Garrett et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 1997;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Jin et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2003;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Mart´ı-  Vidal et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2013;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Allison et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2017), which makes it  difficult to compare observations and model the radio  continuum emission (Muller et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2020).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  10  1  100  101  Rest Frequency (GHz)  101  3 × 100  4 × 100  6 × 100  2 × 101  SC (Jy)  10  1  100  101  Observed Frequency (GHz)  Figure 10.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Compilation of continuum flux density mea-  surements from the bright and highly variable (factors of  ∼1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 on weeks and years timescales) PKS 1830.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The gray  shaded region encompasses the 1σ confidence region of a  best-fitting power-law that is attenuated by free-free absorp-  tion.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We also include the continuum SEDS (with colors cor-  responding to the components on the left hand plot) from a  fixed power-law and that is attenuated by ionized gas with  properties constrained by the RRL models.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We assume a  redshift z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 for the conversion between observed and  rest frequencies.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Ionized gas that is detectable in RRLs and has a  large covering fraction would also emit free-free emis-  sion and when it becomes optically thick, would ab-  sorb any background radio continuum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  A reliable  model and knowledge of the spatially-resolved radio  SED could independently constrain the physical con-  ditions of the gas through free-free absorption.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The  frequency at which radio emission becomes optically  thick to free-free absorption is defined by τν = 6.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='67 ×  10−2 EM T −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='323  e  (ν/GHz)−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='118 (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We  collected  radio  continuum  measurements  of  PKS 1830 at ν ≲ 22 GHz (using the NASA/IPAC  Extragalactic Database (NED) and Pramesh Rao &  Subrahmanyan 1988;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Henkel et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2008;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Intema et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2017) and plot these in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 10.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We fit the SED of  PKS 1830 as a power-law index with an external screen  of free-free absorption, using the functional form Sν =  So( ν  νo )α exp(−τν) with τν = τo( ν  νo )−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='118.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Setting νo =  40 GHz with respect to observed frequencies, the best fit  parameters with 1σ uncertainties are So = 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4 Jy,  α = −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='24 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='03 and τo = (1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2) × 10−5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 10, we also plot how ionized gas that has phys-  ical properties constrained by the RRL models — us-  ing the same selection of models presented in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 7 —  would attenuate a power-law continuum SED (normal-  ized by So and α of our fit).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The emission from the RRLs  16  Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  we detect at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 would result in free-free absorp-  tion at lower frequencies than is observed in PKS 1830.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  For the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 galaxy to cause the free-free absorp-  tion, volume-average pathlengths a factor of 5 larger are  needed.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' A smaller filling factor and larger pathlength  intercepting the radio emission is not unreasonable.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  It would still be possible for ionized gas in the envi-  ronment of the blazar at z = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 to create the absorp-  tion in the radio SED.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Even though we do not detect  hydrogen RRL emission at z = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5, ionized gas with dif-  ferent properties, for example higher densities, could be  present and still be consistent with the RRL constraints.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  We also note that ionized gas in the Milky Way with  EMs that result in a turnover at the observed frequen-  cies (especially, on < 1′′ scales) would be observable in  hydrogen RRL emission at z = 0, and we do not detect  any RRL emission from the Milky Way.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  6.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' CONCLUSIONS  We used MALS observations to detect RRL emission  in the spectrum of the radio blazar PKS 1830.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The RRL  emission is observed at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 from a galaxy that  lies along the line of sight and strongly lenses PKS 1830.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  This is the second detection of RRLs outside of the local  universe (i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', at z ≥ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='076) and the first clearly associ-  ated with hydrogen (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=', Emig et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 2019).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We detect  H144α by stacking 17 RRLs covered by the L band (856–  1712 MHz) with a S/N of 21 (see Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 3), and we detect  H163α by stacking 27 lines in the UHF band (544–1088  MHz) with a S/N of 14 (see Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 6).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Emission from the  H144α line is consistent over two separate observations,  when comparing the spectra in parallel hand polariza-  tions, and is robust against additional spectral stacking  verification methods.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Like the H i 21 cm and OH 18 cm  absorption spectra (see Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 5), the H144α and H163α  emission profiles span ∼250 km s−1 in velocity and are  dominated by two velocity components associated with  two physically distinct regions of the galaxy, the NE and  SW lines of sight.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We do not detect RRL emission in  either band intrinsic to PKS 1830 (z = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5), from the  z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='19 absorption system along this line of sight, or  from the Milky Way (see Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 4).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Hydrogen RRL emission typically arises from fully  ionized gas and only stimulated emission is observable  outside of the local universe.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The maser-like proper-  ties of stimulated emission enable the RRL SLED to  constrain the density and pathlength of the ionized gas  (see Table 2 and Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' 9).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Considering the total inte-  grated line intensity, referred to as the Total compo-  nent, we used a Bayesian analysis to constrain the elec-  tron density of the gas log(ne) = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 ± 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6 cm−3 and  a volume-averaged pathlength of log(ℓ) = −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='6+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='5 pc,  which likely has a non-unity filling factor.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Analyzed  separately, the NE line-of-sight appears to harbor less  dense gas with log(ne) = 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0+1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='9  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7 cm−3 and log(ℓ) =  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7±1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1 pc, and the SW line-of-sight appears to inter-  cept dense gas that is more typical of H ii regions with  log(ne) = 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2+0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='4  −1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='0 cm−3 and log(ℓ) = −2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='7+1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2 pc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' These  scenarios are consistent with the NE line-of-sight pass-  ing through diffuse clouds at a larger galactic radius, and  the SW component directly intercepting a spiral arm, as  has previously been determined.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The RRL components measure an ionizing pho-  ton flux of Qo/area  ≈  1046±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8  photons s−1 pc−2  and star formation rate surface density of ΣSFR ∼  10−0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='2±0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 M⊙ yr−1 kpc−2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Taken over the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  galaxy within Rg ∼ 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='3 kpc, the ionizing photon rate of  Qo ∼ 1054.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='8 photons s−1 yields an average star forma-  tion rate of SFR ∼ 50 M⊙ yr−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Despite the plethora of  molecular species observed, the ionized gas content and  SFR have not been previously measured for this source,  largely due to the highly reddened nature of PKS 1830  at optical and NIR wavelengths.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' In comparing the SFR  and the galaxy’s mass (from lensing), the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 sys-  tem is likely on the main sequence.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The ionized gas mass per unit area of the diffuse  NE component as measured by the RRL emission is  Σion ≈ 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='1 M⊙ pc−2, in comparison with gas masses of  ΣH I ≈ 50 M⊙ pc−2 and ΣH2 ≈ 240 M⊙ pc−2 (via OH)  estimated from only the MALS observations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Given our  estimated SFR, the H i+H2 gas mass surface density  is close to the gas content predicted by the Kennicutt-  Schmidt law.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Our measured electron densities also  match reasonably well with the ne − ΣSFR relation de-  termined from optical and FIR line ratios.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  PKS 1830 is the first source investigated with MALS,  and the detection of RRLs in the source is promising  for the remaining ∼500 targets of the survey.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' With the  first hydrogen RRL detection that breaks the redshift-  barrier, we show that this tracer can be an important  tool for investigating (a) the electron density (thermal  pressure) of ionized gas in the ISM of galaxies (and the  ne−ΣSFR relation) and (b) the SED of AGN, thus even-  tually AGN evolution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' We have also demonstrated the  unique science that can be achieved through H i 21 cm,  OH 18 cm, and RRL measurements that are simulta-  neously observed in the MALS survey.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The ionized gas  properties in the z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89 galaxy will be substantially  improved through RRL observations at higher and lower  radio frequencies and at higher (<1′′) spatial resolutions  which can separate the two main (velocity) components  of emission.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The new science afforded by high-redshift  RRL studies is accessible with on-going wide-bandwidth  spectral line surveys and will be explored in unprece-  Radio Recombination Lines at z = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='89  17  dented capacities with future facilities such as the next  generation Very Large Array (ngVLA;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' Murphy et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  2018) and the SKA (Carilli 2015).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  ACKNOWLEDGMENTS  The authors acknowledge and appreciate the efforts  and input of the anonymous reviewer of this article.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The  authors thank Peter Shaver for comments on the article  and for the inspiration and motivation to carry through  with this research.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  SAB was supported by RSF grant 18-12-00301.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content=' The  MeerKAT telescope is operated by the South African  Radio Astronomy Observatory, which is a facility of the  National Research Foundation, an agency of the De-  partment of Science and Innovation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  The MeerKAT  data were processed using the MALS computing facil-  ity at IUCAA (https://mals.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='iucaa.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='in/releases) The Na-  tional Radio Astronomy Observatory is a facility of the  National Science Foundation operated under coopera-  tive agreement by Associated Universities, Inc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  This  research has made use of the NASA/IPAC Extragalac-  tic Database (NED), which is funded by the National  Aeronautics and Space Administration and operated by  the California Institute of Technology.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
+page_content='  Facilities: MeerKAT  Software: ARTIP (Gupta et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
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+page_content=' The Astropy Collaboration  et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/ENE1T4oBgHgl3EQfWgSE/content/2301.03115v1.pdf'}
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