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The ALMA-PILS survey: propyne (CH$_3$CCH) in IRAS 16293$-$2422

dc.contributor.authorCALCUTT, H.
dc.contributor.authorWILLIS, E. R.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorJØRGENSEN, J. K.
hal.structure.identifierforeign laboratories [FL]
dc.contributor.authorBJERKELI, P.
dc.contributor.authorLIGTERINK, N. F. W.
hal.structure.identifierAMOR 2019
dc.contributor.authorCOUTENS, Audrey
dc.contributor.authorMÜLLER, H. S. P.
hal.structure.identifierDepartment of Physics, The Ohio State University
dc.contributor.authorGARROD, R. T.
hal.structure.identifierInstitute of Astronomy [ETH Zürich]
dc.contributor.authorWAMPFLER, S. F.
dc.contributor.authorDROZDOVSKAYA, M. N.
dc.date.issued2019
dc.identifier.issn0004-6361
dc.description.abstractEnContext. Propyne (CH$_3$CCH) has been detected in a variety of environments, from Galactic star-forming regions to extragalactic sources. Such molecules are excellent tracers of the physical conditions in star-forming regions. Aims. This study explores the emission of CH$_3$CCH in the low-mass protostellar binary, IRAS 16293$-$2422, examining the spatial scales traced by this molecule, as well as its formation and destruction pathways. Methods. ALMA observations from the Protostellar Interferometric Line Survey (PILS) are used to determine the abundances and excitation temperatures of CH$_3$CCH towards both protostars, exploring spatial scales from 70 to 2400 au. The three-phase chemical kinetics model MAGICKAL is also used, to explore the chemical reactions of this molecule. Results. CH$_3$CCH is detected towards both IRAS 16293A and IRAS 16293B and is found to trace the hot corino component around each source in the PILS dataset. Eighteen transitions above 3$\sigma$ are detected, enabling robust excitation temperatures and column densities to be determined in each source. In IRAS 16293A, an excitation temperature of 90 K and a column density of 7.8$\times$10$^{15}$ cm$^{-2}$ best fits the spectra. In IRAS 16293B, an excitation temperature of 100 K and 6.8$\times$10$^{15}$ cm$^{-2}$ best fits the spectra. The chemical modelling finds that in order to reproduce the observed abundances, both gas-phase and grain-surface reactions are needed. Conclusions. CH$_3$CCH is a molecule whose brightness and abundance in many different regions can be utilised to provide a benchmark of molecular variation with the physical properties of star-forming regions. It is essential when making such comparisons, that the abundances are determined with a good understanding of the spatial scale of the emitting region, to ensure that accurate abundances are derived.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics - Solar and Stellar Astrophysics
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enThe ALMA-PILS survey: propyne (CH$_3$CCH) in IRAS 16293$-$2422
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201936323
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1909.13329
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.volume631
bordeaux.issueA137
bordeaux.peerReviewedoui
hal.identifierhal-02303193
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-02303193v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Astronomy%20and%20Astrophysics%20-%20A&A&rft.date=2019&rft.volume=631&rft.issue=A137&rft.eissn=0004-6361&rft.issn=0004-6361&rft.au=CALCUTT,%20H.&WILLIS,%20E.%20R.&J%C3%98RGENSEN,%20J.%20K.&BJERKELI,%20P.&LIGTERINK,%20N.%20F.%20W.&rft.genre=article


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