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The millimeter IRAM-30m line survey toward IK Tauri

dc.contributor.authorVELILLA PRIETO, L.,
dc.contributor.authorSÁNCHEZ CONTRERAS, C.,
hal.structure.identifierInstituto de Ciencia de Materiales de Madrid [ICMM]
dc.contributor.authorCERNICHARO, J.,
dc.contributor.authorAGÚNDEZ, M.,
hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
dc.contributor.authorQUINTANA-LACACI, G.,
dc.contributor.authorBUJARRABAL, V.,
dc.contributor.authorALCOLEA, J.,
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA]
dc.contributor.authorBALANÇA, Christian
hal.structure.identifierFORMATION STELLAIRE 2017
dc.contributor.authorHERPIN, Fabrice
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorMENTEN, K. M.,
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, F.,
dc.date.issued2017
dc.identifier.issn0004-6361
dc.description.abstractEnWe carried out a millimeter wavelength line survey between 79 and 356 GHz with the IRAM-30m telescope to investigate the physical and chemical properties of the molecular envelope of the oxygen-rich AGB star IK Tau. We analysed the molecular lines detected using the population diagram technique to derive rotational temperatures and column densities. Additionally, we conducted a radiative transfer analysis of the SO$_2$ lines detected. For the first time in this source we detected rotational lines in the ground vibrational state of HCO$^+$, NS, NO, and H$_2$CO, as well as several isotopologues of molecules previously identified. We also detected several rotational lines in vibrationally excited states of SiS and SiO isotopologues, and rotational lines of H$_2$O ($\nu_{\mathrm{2}}$=2). We have also increased the number of rotational lines detected of molecules that were previously identified, enabling a detailed study of the molecular abundances and excitation temperatures. IK Tau displays a rich chemistry for an oxygen-rich circumstellar envelope. We highlight the detection of NS and H$_2$CO with fractional abundances of f(NS)$\sim$10$^{-8}$ and f(H$_2$CO)$\sim$[10$^{-7}$--10$^{-8}$]. Most of the molecules display rotational temperatures between 15 and 40 K. NaCl and SiS isotopologues display rotational temperatures higher than the average (~65 K). In the case of SO$_2$ a warm component with $T_{\mathrm{rot}}$$\sim$290 K is also detected. This SO$_2$ warm component is probably arising from the inner regions of the envelope (at $\sim$8$R_{*}$) where SO$_2$ has a fractional abundance of f(SO$_2$)$\sim$10$^{-6}$. This result should be considered for future investigation of the main formation channels of this, and other, parent species in the inner winds of O-rich AGB stars, which at present are not well reproduced by current chemistry models.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics - Solar and Stellar Astrophysics
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enThe millimeter IRAM-30m line survey toward IK Tauri
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201628776
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv1609.01904
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.A25
bordeaux.volume597
bordeaux.peerReviewedoui
hal.identifierhal-01366048
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01366048v1
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