J/A+A/575/A87ivo://CDS.VizieR/J/A+A/575/A87doi:10.26093/cds/vizier.35750087CDSFontani F.Busquet G.Palau A.Caselli P. Sanchez-Monge A.Tan J.C.,Audard M.2023-01-06T15:26:27Z2015-03-02T08:07:48ZCDS support team

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

cds-question@unistra.frinterstellar-mediumspectroscopymolecular-cloudsAn ever growing number of observational and theoretical evidence suggests that the deuterated fraction (column density ratio between a species containing D and its hydrogenated counterpart, Dfrac) is an evolutionary indicator both in the low- and the high-mass star formation process. However, the role of surface chemistry in these studies has not been quantified from an observational point of view. In order to compare how the deuterated fractions of species formed only in the gas and partially or uniquely on grain surfaces evolve with time, we observed rotational transitions of CH_3_OH, ^13^CH_3_OH, CH_2_DOH, CH_3_OD at 3 and 1.3mm, and of NH_2_D at 3mm with the IRAM-30m telescope, and the inversion transitions (1,1) and (2,2) of NH_3_ with the GBT, towards most of the cores already observed by Fontani et al. (2011A&A...529L...7F, 2014MNRAS.440..448F) in N_2_H^+^, N_2_D^+^, HNC, DNC. NH_2_D is detected in all but two cores, regardless of the evolutionary stage. Dfrac(NH_3_) is on average above 0.1, and does not change significantly from the earliest to the most evolved phases, although the highest average value is found in the protostellar phase (~0.3). Few lines of CH_2_DOH and CH_3_OD are clearly detected, and only towards protostellar cores or externally heated starless cores. This work clearly confirms an expected different evolutionary trend of the species formed exclusively in the gas (N_2_D^+^ and N_2_H^+^) and those formed partially (NH_2_D and NH_3_) or totally (CH_2_DOH and CH_3_OH) on grain mantles. The study also reinforces the idea that Dfrac(N_2_H^+^) is the best tracer of massive starless cores, while high values of Dfrac(CH_3_OH) seem rather good tracers of the early protostellar phases, at which the evaporation/sputtering of the grain mantles is most efficient.2015A&A...575A..87Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/575/A87CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/575/A87https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/575/A87http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/575/A87https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/575/A87https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/575/A87http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/575/A87GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/575/A87/sources (List of the observed sources, with the NH_2D_ spectra)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/575/A87/sources?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/575/A87/sources?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/575/A87/sources?GETtext/xml+votable180.050000true3.60958364.4744440.0055555555555555566/1470 3068 14299 14307 14317 14353 14594 14622 14689 15430 15629 24507 24554 28912 29103 30256 30258 30318-30319 30425 30595https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/575/A87?format=asciidefaultJ/A+A/575/A87/sourcesList of the observed sources, with the NH_2D_ spectraONameOther designation (3)meta.idcharSeq.p[1/28]? Sequence number of para-NH_2_D spectrum (in file sp/NH2Dpara.fits)meta.numberintnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintVLSRLSR velocity (2)km/sphys.veloc;pos.lsrfloatTypeType of source (G1)src.classcharNameSource namemeta.id;meta.maincharn_Name[aw] Note on source (1)meta.notecharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainNtNumber of transitions observed for this sourcemeta.ref.urlintnullableSNameSimbad namemeta.idcharSourceNames as in FITS files (added by CDS)meta.idcharprimarysp-oplot of ortho-$NH_2D$ spectrummeta.ref.urlcharsp-pplot of para-$NH_2D$ spectrummeta.ref.urlcharVelVelocity (LSR) of reference channelkm/sphys.veloc;pos.lsrfloatSc.oScan identification number of ortho spectrummeta.idintObs.oObservation date and time of ortho spectrumstime.epoch;obsnullableSeq.o[1/28] Sequence number of ortho-NH_2_D spectrum (in file sp/NH2Dortho.fits)meta.numberintSc.p? Scan identification number of ortho spectrummeta.idintnullableObs.p? Observation date and time of para spectrumstime.epoch;obsnullableJ/A+A/575/A87/tablebTransitions and line parameters (derived from Gaussian fits) for CH_3_OH,^13^CH_3_OH, CH_2_DOH and CH_3_OD detected at 3mm (tableB1) and 1mm (tableB2)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTypeType of source (G1)src.classcharNameSource namemeta.id;meta.maincharBandWavelength domain, 3mm (95GHz) or 1mm (219GHz)mminstr.filter;em.wl.centralcharFreq[89275/223423]? FrequencyMHzem.freqdoublenullableTransTransitionmeta.id;phys.atmol.transitionSint? Line Integrated intensity {int}T_MB_.dvK.km/sphot.flux.densityfloatnullablee_Sint[0.002/2]? rms uncertainty on SintK.km/sstat.errorfloatnullableDV[0.4/8]? Full width at half maximum {Delta}Vkm/sspect.line.widthfloatnullablee_DV? rms uncertainty on DeltaVkm/sstat.errorfloatnullableTpk[0/4]? Main beam temperature at line peakKobs.paramfloatnullableSourceName as in FITS files (added by CDS)meta.idcharu_Tpk[ab] problems in Tpeak estimation (1)meta.code.errorcharfig2plot added by VizieRmeta.ref.urlcharbzFileName of rotation diagram (Fig.2) in subdirectory "img" (added by CDS)meta.idchar