J/A+A/632/A19ivo://CDS.VizieR/J/A+A/632/A19doi:10.26093/cds/vizier.36320019CDSTaquet V.Bianchi E.Codella C.Persson M.V.Ceccarelli C.Cabrit S.,Jorgensen J.K.Kahane C.Lopez-Sepulcre A.Neri R.2020-01-29T15:59:09Z2019-11-22T06:40:49ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frprotostarschemical-abundancesinterferometryradio-astronomyinfrared-sourcesMethanol is a key species in astrochemistry since it is the most abundant organic molecule in the interstellar medium and is thought to be the mother molecule of many complex organic species. Estimating the deuteration of methanol around young protostars is of crucial importance because it highly depends on its formation mechanisms and the physical conditions during its moment of formation. We analyse several dozens of transitions from deuterated methanol isotopologues coming from various existing observational datasets obtained with the IRAM-PdBI and ALMA sub-mm interferometers to estimate the methanol deuteration surrounding three low-mass protostars on Solar System scales. A population diagram analysis allows us to derive a [CH_2_DOH]/[CH_3_OH] abundance ratio of 3-6% and a [CH_3_OD]/[CH_3_OH] ratio of 0.4-1.6% in the warm inner (<100-200AU) protostellar regions. These values are typically ten times lower than those derived with previous single-dish observations towards these sources but they are one to two orders of magnitude higher than the methanol deuteration measured in massive hot cores. Dust temperature maps obtained from Herschel and Planck observations show that massive hot cores are located in warmer molecular clouds than low-mass sources, with temperature differences of about 10K. The comparison of our measured values with the predictions of the gas-grain astrochemical model GRAINOBLE shows that such a temperature difference is sufficient to explain the different deuteration observed in low- to high-mass sources. This suggests that the physical conditions of the molecular cloud at the origin of the protostars mostly govern the present observed deuteration of methanol and, therefore, of more complex organic molecules. Finally, the methanol deuteration measured towards young solar-type protostars on Solar System scales seems to be higher by a factor of about 5 than the upper limit in methanol deuteration estimated in comet Hale-Bopp. If this result is confirmed by subsequent observations of other comets, this would imply that an important reprocessing of the organic material likely occurred in the solar nebula during the formation of the Solar System.2019A&A...632A..19Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/632/A19CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/632/A19https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/632/A19http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/632/A19https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/632/A19https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/632/A19http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/632/A19GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/632/A19/list (List of fits maps)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/632/A19/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/632/A19/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/632/A19/list?GETtext/xml+votable180.050000true52.2315431.24360.0055555555555555566/862 22866https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/632/A19?format=asciiInfraredRadiodefaultJ/A+A/632/A19/listList of fits mapsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right Ascension of center (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of center (J2000)degpos.eq.dec;meta.mainNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fits