dc.contributor.author | Yan, Y. T. | |
dc.contributor.author | Henkel, C. | |
dc.contributor.author | Kobayashi, C. | |
dc.contributor.author | Menten, K. M. | |
dc.contributor.author | Gong, Y. | |
dc.contributor.author | Zhang, J. S. | |
dc.contributor.author | Yu, H. Z. | |
dc.contributor.author | Yang, K. | |
dc.contributor.author | Xie, J. J. | |
dc.contributor.author | Wang, X.Y. | |
dc.date.accessioned | 2023-09-18T09:00:05Z | |
dc.date.available | 2023-09-18T09:00:05Z | |
dc.date.issued | 2023-02-14 | |
dc.identifier.citation | Yan , Y T , Henkel , C , Kobayashi , C , Menten , K M , Gong , Y , Zhang , J S , Yu , H Z , Yang , K , Xie , J J & Wang , X Y 2023 , ' Direct measurements of carbon and sulfur isotope ratios in the Milky Way ' , Astronomy & Astrophysics , vol. 670 , A98 , pp. 1/63 . https://doi.org/10.1051/0004-6361/202244584 | |
dc.identifier.issn | 0004-6361 | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/2212.03252v1 | |
dc.identifier.other | ORCID: /0000-0002-4343-0487/work/142860197 | |
dc.identifier.uri | http://hdl.handle.net/2299/26678 | |
dc.description | © 2023 The Author(s), published by EDP Sciences. This is an open access article distributed under the terms of the Creative Commons Attribution License (CC BY), https://creativecommons.org/licenses/by/4.0/ | |
dc.description.abstract | With the IRAM 30-m telescope, we performed observations of the $J$ = 2-1 transitions of CS, C$^{33}$S, C$^{34}$S, C$^{36}$S, $^{13}$CS, $^{13}$C$^{33}$S, and $^{13}$C$^{34}$S as well as the $J$ = 3-2 transitions of C$^{33}$S, C$^{34}$S, C$^{36}$S, and $^{13}$CS toward a large sample of 110 HMSFRs. We measured the $^{12}$C/$^{13}$C, $^{32}$S/$^{34}$S, $^{32}$S/$^{33}$S, $^{32}$S/$^{36}$S, $^{34}$S/$^{33}$S, $^{34}$S/$^{36}$S, and $^{33}$S/$^{36}$S abundance ratios with rare isotopologues of CS, thus avoiding significant saturation effects. With accurate distances obtained from parallax data, we confirm previously identified $^{12}$C/$^{13}$C and $^{32}$S/$^{34}$S gradients as a function of galactocentric distance (RGC). In the CMZ $^{12}$C/$^{13}$C ratios are higher than suggested by a linear fit to the disk values as a function of RGC. While $^{32}$S/$^{34}$S ratios near the Galactic center and in the inner disk are similar, this is not the case for $^{12}$C/$^{13}$C, when comparing central values with those near RGC of 5 kpc. As was already known, there is no $^{34}$S/$^{33}$S gradient but the average ratio of 4.35~$\pm$~0.44, derived from the $J$ = 2-1 transition lines of C$^{34}$S and C$^{33}$S, is well below previously reported values. A comparison between solar and local interstellar $^{32}$S/$^{34}$S and $^{34}$S/$^{33}$S ratios suggests that the solar system may have been formed from gas with a particularly high $^{34}$S abundance. For the first time, we report positive gradients of $^{32}$S/$^{33}$S, $^{34}$S/$^{36}$S, $^{33}$S/$^{36}$S and $^{32}{\rm S}/^{36}{\rm S}$ in our Galaxy. The predicted $^{12}$C/$^{13}$C ratios from the latest GCE models are in good agreement with our results, while $^{32}$S/$^{34}$S and $^{32}$S/$^{36}$S ratios show larger differences at larger RGC, $^{32}$S/$^{33}$S ratios show an offset across the entire inner 12 kpc of the Milky Way. | en |
dc.format.extent | 63 | |
dc.format.extent | 16942249 | |
dc.language.iso | eng | |
dc.relation.ispartof | Astronomy & Astrophysics | |
dc.subject | astro-ph.GA | |
dc.title | Direct measurements of carbon and sulfur isotope ratios in the Milky Way | en |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.contributor.institution | School of Physics, Engineering & Computer Science | |
dc.contributor.institution | Department of Physics, Astronomy and Mathematics | |
dc.description.status | Peer reviewed | |
rioxxterms.versionofrecord | 10.1051/0004-6361/202244584 | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |