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Astronomy &Astrophysics A&A 658, A135 (2022) https://doi.org/10.1051/0004-6361/202141662 © J. M. Winters et al. 2022 Molecules, shocks, and disk in the axi-symmetric wind of the MS-type AGB star RS Cancri? J. M. Winters1 , D. T. Hoai2 , K. T. Wong1 , W.-J. Kim3,4 , P. T. Nhung2 , P. Tuan-Anh2 , P. Lesaffre5 , P. Darriu...	10.1051_0004-6361_202141662	page_0000
A&A 658, A135 (2022) We have concentrated our efforts on two relatively close (d150pc) sources that show composite proﬁles in CO rota- tional lines (Winters et al. 2003): EP Aqr (Winters et al. 2007, hereafter referred to as W2007), and RS Cnc (Libert et al. 2010). Data obtained at IRAM show that these two sources hav...	10.1051_0004-6361_202141662	page_0001
J. M. Winters et al.: Molecules, shocks, and disk in the axi-symmetric wind of the MS-type AGB star RS Cancri Table 1. Properties of the combined data sets for all detected lines. Line Frequency Eu=k Peak ﬂux FWHP beam size PA 1 noise vel.res Comments(a) (GHz) (K) (Jy) (arcsec) (arcsec2) (deg) (mJy beam1) ( km s1) 1...	10.1051_0004-6361_202141662	page_0002
A&A 658, A135 (2022) Fig. 1. Overview of the frequency ranges observed with PolyFiX using two spectral setups (setup1: red and setup2: blue, respectively). Lower diagrams : zoom onto the individual spectra covering 7.8 GHz each. Upper row : setup1, lower row : setup2. The central 20 MHz at the border between inner and ...	10.1051_0004-6361_202141662	page_0003
J. M. Winters et al.: Molecules, shocks, and disk in the axi-symmetric wind of the MS-type AGB star RS Cancri Fig. 2. Continuum map around 247 GHz from A-conﬁguration. Con- tours are plotted in 100 steps, where 1 is 47.6 Jy beam1. The synthesized beam is indicated in the lower left corner. Fig. 3. CO line proﬁles, ...	10.1051_0004-6361_202141662	page_0004
A&A 658, A135 (2022) Fig. 6. Proﬁle around the SiO( v=2,J=5–4) line frequency. A- conﬁguration and D-conﬁguration merged. The spectral resolution is 1 km s1and the emission is integrated over the central 100100aperture. the idea that the SiO masers are excited by infrared pumping as opposed to collisional pumping (se...	10.1051_0004-6361_202141662	page_0005
J. M. Winters et al.: Molecules, shocks, and disk in the axi-symmetric wind of the MS-type AGB star RS Cancri ). Fig. 8. HCN line proﬁles. Left: HCN(3–2); A-conﬁguration and D- conﬁguration merged with a spectral resolution of 0.5 km s1.Right : H13CN(3–2); A-conﬁguration and D-conﬁguration merged with a spec- tral res...	10.1051_0004-6361_202141662	page_0006
A&A 658, A135 (2022) Fig. 10. Proﬁles of the four detected SO lines, with A-conﬁguration and D-conﬁguration merged. The spectral resolution is 3 km s1and the emission is integrated over the central 200200aperture. Fig. 11. Proﬁles of the two34SO lines detected here, with A- conﬁguration and D-conﬁguration merged. The...	10.1051_0004-6361_202141662	page_0007
J. M. Winters et al.: Molecules, shocks, and disk in the axi-symmetric wind of the MS-type AGB star RS Cancri Table 2. Parameters of the detected SO 2lines used for the population diagram analysis. Frequency WI=R S(v)dv g ulog10(Aul) Eu=kab (GHz) (Jy km s1) (s1) (K) (arcsec2) 214.6894 0.1410.0385 33 –4.0043 147.8...	10.1051_0004-6361_202141662	page_0008
A&A 658, A135 (2022) AGB stars, such as W Hya (Vlemmings et al. 2017), EP Aqr (Tuan-Anh et al. 2019), oCet (Hoai et al. 2020), R Dor (Decin et al. 2018; Nhung et al. 2019a, 2021), and in 15 out of 17 sources observed in the ALMA Large Program ATOMIUM (Decin et al. 2020; Gottlieb et al. 2022), calling for a common mecha...	10.1051_0004-6361_202141662	page_0009
J. M. Winters et al.: Molecules, shocks, and disk in the axi-symmetric wind of the MS-type AGB star RS Cancri Fig. 17. First-moment maps of different lines, indicating a possibly rotating structure (see Sect. 3.4). Left: HCN(3–2), middle left : SO 2(14(0,14)– 13(1,13)), middle right : SiO(v=1,6–5), right : SO(7(6)–6(5)...	10.1051_0004-6361_202141662	page_0010
A&A 587, A91 (2016) about their formation paths during the past evolution of the core. In particular, their degree of deuterium fractionation is a relic of the conditions that were prevailing in earlier, colder stages (e.g.Taquet et al. 2012 ,2014 ;Aikawa et al. 2012 ). Apart from methanol, relativ ely little is known ...	10.1051_0004-6361_201527268	page_0001
A. Belloche et al.: Deuterated complex organic molecules in Sgr B2(N2) Table 1. Observational setups of the EMoCA survey. Setup Frequency range Date of tstartaNabBaseline tintdCalibratorsePeakf LSB USB observation (UTC) rangecBA P ΔαΔδ GHz GHz yyyy-mm-dd hh:mm m min/prime/prime /prime/prime S1 84.1–87.8 96.2–99.8 2012-...	10.1051_0004-6361_201527268	page_0002
A&A 587, A91 (2016) Table 2. Beam sizes and noise levels. Setup SPWaFrequency Synthesized beam rmsc range HPBW PAbmJy MHz/prime/prime×/prime/prime ◦beam−1K S1 0 84 091–85 966 2 .1×1.5−85 3.0 0.16 1 85 904–87 779 2 .0×1.5−83 2.7 0.14 2 96 154–98 029 1 .8×1.4−85 3.0 0.16 3 97 904–99 779 1 .8×1.3−85 3.1 0.16 S2 0 87 729–8...	10.1051_0004-6361_201527268	page_0003
A. Belloche et al.: Deuterated complex organic molecules in Sgr B2(N2) based on Nguyen et al. (2013 ). Predictions for CH 3CN in its /v18=1 and 2 excited states are based on preliminary results from Müller et al. (2015 ), those in /v14=1 are preliminary data from a subsequent study (Müller et al., in prep.). Transition...	10.1051_0004-6361_201527268	page_0004
A&A 587, A91 (2016) Table 3. Rotational temperatures derived from population diagrams of selected (complex) organic molecules toward Sgr B2(N2). Molecule StatesaTﬁtb (K) CH 3CN /v18=1,/v18=2,/v14=1 253 (15) 13CH 3CN /v1=0,/v18=1 168 (13) CH 313CN /v1=0,/v18=1 165.5 (3.3) CH 2DCN /v1=0 136 (14) C2H5CN /v1=0 137.3 (1.6) ...	10.1051_0004-6361_201527268	page_0005
A. Belloche et al.: Deuterated complex organic molecules in Sgr B2(N2) Table 4. Parameters of our best-ﬁt LTE model (or upper limit) of selected (complex) organic molecules toward Sgr B2(N2). Molecule StatusaNdetbSizecTrotdNeCfΔVgVoﬀh Nref Ni30 mj (/prime/prime)( K ) ( c m−2)( k m s−1)( k m s−1) CH 3CN, /v18=1⋆d 20 1.4...	10.1051_0004-6361_201527268	page_0006
A&A 587, A91 (2016) Fig. 1. Deconvolved major, minor, and mean sizes (FWHM) derived for uncontaminated C 2H5CN transitions detected toward Sgr B2(N2) and plotted as a function of upper level energy. The symbols code for the spectral setup (S1 to S5, like in Table 2). In each panel, the dashed line indicates the median ...	10.1051_0004-6361_201527268	page_0007
A. Belloche et al.: Deuterated complex organic molecules in Sgr B2(N2) vibrationally excited state /v19=1. The detection of DC 3N is only tentative, and its column density should rather be considered as an upper limit. 5.4. Deuterated methanol CH 2DOH Methanol and its13Ca n d18O isotopologues are well detected toward S...	10.1051_0004-6361_201527268	page_0008
A&A 587, A91 (2016) Table 5. Deuterium fractionation of selected (complex) organic molecules toward Sgr B2(N2) compared to predictions of astrochem-ical models. Molecule Statusa[XD]/[XH] N2bT14cA12d %% % CH 2DCN d 0.38 3.6–0.15 2.3–6.3 CH 2DCH 2CN (oop) t 0.05 – – CH 2DCH 2CN (ip) n <0.024 – – CH 3CHDCN t 0.05 – – cis-...	10.1051_0004-6361_201527268	page_0009
A. Belloche et al.: Deuterated complex organic molecules in Sgr B2(N2) obtain for methyl cyanide, the d euterated species of which is securely identiﬁed in our ALMA spectrum of Sgr B2(N2) (Sect. 6.1.1 ). Therefore, even if the di ﬀerence in deuterium fractionation between methanol and methyl cyanide is a priori surpris...	10.1051_0004-6361_201527268	page_0010
174901-3 P.-M. Lam and Y. Zhen J. Chem. Phys. 143, 174901 (2015) g(f)+1 2Asin4α r2+U(r)−sin 2α 2rM=0. (10) Three equations (8)–(10) can be solved to obtain the remaining three unknowns quantities α,r, and M. In the high-force limit, Neukirch and Marko28have given the solutions in closed form. Define a quantity Kas K= ...	10.1063_1.4934988	page_0003
174901-4 P.-M. Lam and Y. Zhen J. Chem. Phys. 143, 174901 (2015) FIG. 3. Comparison of experimental and theoretical torque as a function of the applied force, for 50, 100, 200, and 500 mM salt (top to bottom). Circles are experimental data. Full lines are our theoretical results using a better form of the free energy. ...	10.1063_1.4934988	page_0004
174901-5 P.-M. Lam and Y. Zhen J. Chem. Phys. 143, 174901 (2015) limit in which the chain lengths are infinitely long, do the two ensembles yield identical results. 1D. Branzei and M. Foiani, Nat. Rev. Mol. Cell Biol. 11, 208 (2010). 2N. R. Cozzarelli, G. J. Cost, M. Nollmann, T. Viard, and J. E. Stray, Nat. Rev. Mol. ...	10.1063_1.4934988	page_0005
J. Chem. Phys. 145, 114901 (2016); https://doi.org/10.1063/1.4962516 145, 114901 © 2016 Author(s).On the influence of the intermolecular potential on the wetting properties of water on silica surfaces Cite as: J. Chem. Phys. 145, 114901 (2016); https://doi.org/10.1063/1.4962516 Submitted: 17 June 2016 • Accepted: 29 Au...	10.1063_1.4962516	page_0000
THE JOURNAL OF CHEMICAL PHYSICS 145, 114901 (2016) On the influence of the intermolecular potential on the wetting properties of water on silica surfaces E. Pafong,a)J. Geske, and B. Drossel Institut für Festkörperphysik, Technische Universität Darmstadt, Hochschulstr. 6, 64289 Darmstadt, Germany (Received 17 June 2016...	10.1063_1.4962516	page_0001
114901-2 Pafong, Geske, and Drossel J. Chem. Phys. 145, 114901 (2016) atoms has been added and the partial charges on each silica atom are increased. We probed the performance of both silica models by analyzing the wetting behaviour of water on silica surfaces and comparing to the experimental results.2,12,37–39 In the...	10.1063_1.4962516	page_0002
114901-3 Pafong, Geske, and Drossel J. Chem. Phys. 145, 114901 (2016) FIG. 1. Top view of the two initial con- figurations used in the MD simulations, labelled in the subsequent figures with “center” (a) and “surface” (b). Here the hydration level is 30%. Si, O Si,H, H are drawn in yellow, blue, and green, while water ...	10.1063_1.4962516	page_0003
114901-4 Pafong, Geske, and Drossel J. Chem. Phys. 145, 114901 (2016) FIG. 3. The water density at the pore surface, showing water molecules that are within a distance of 0.3 nm of the silica surface. For the GT surface ((e)-(h)), only filling ratios of 30% and 40% are shown, since for larger filling ratios the surface...	10.1063_1.4962516	page_0004
114901-5 Pafong, Geske, and Drossel J. Chem. Phys. 145, 114901 (2016) FIG. 4. Average number of hydrogen bonds per water molecule for water–silica ((a)-(b)) and water–water ((c)-(d)) contacts, for di fferent initial conditions and filling ratios, as indicated in the legends. The results for the GT silica surface are gi...	10.1063_1.4962516	page_0005
114901-6 Pafong, Geske, and Drossel J. Chem. Phys. 145, 114901 (2016) calculating numerically the volume and surface of the cut droplet for over 1 ×106different combinations of the sphere radius and the distance of the sphere center from the cylinder axis. Then, we used this database to find for a given filling ratio t...	10.1063_1.4962516	page_0006
A&A 641, A54 (2020) Fig. 6. Abundances relative to H2of MF, DE, F, and EC (Table 10) as a function of the total luminosity/mass ratio (see Sect. 6.3 for details) for the sources of our sample. The linear best-ﬁt to the data is shown for each molecule. luminosity and is not affected by any distance-induced observa- tion...	10.1051_0004-6361_202038212	page_0011
A. Coletta et al.: Evolution of COMs in star-forming regions Fig. 8. Average abundances relative to H2(with respective standard errors) of MF, DE, F, and EC (different colours), as a function of the evolutionary stage. Balucani et al. (2015) present instead a gas-phase route able to efﬁciently form MF from DE at low te...	10.1051_0004-6361_202038212	page_0012
A&A 641, A54 (2020) (Blake et al. 1987). We also note that, given the increasing abun- dance trend, molecular destruction routes seem to be less efﬁ- cient than formation/desorption mechanisms, especially at later evolutionary stages (i.e. higher luminosities). However, destruc- tion routes represent a less investigate...	10.1051_0004-6361_202038212	page_0013

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