J/other/ApSS/361ivo://CDS.VizieR/J/other/ApSS/361.191CDSZhang Y.-J.Zhou J.-J.Esimbek J.He Y.-X.Li D.-L.Tang X.-D.,Ji W.-G.Yuan Y.Guo W.-H.2020-02-06T15:06:52Z2020-02-06T15:07:50ZCDS support team

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

cds-question@unistra.frchemical-abundancesmolecular-cloudsstar-forming-regionsinterstellar-mediummolecular-physicsradio-astronomyA total of 197 relatively isolated high-mass star-forming clumps were selected from the Millimeter Astronomy Legacy Team 90GHz (MALT90) survey data and their global chemical evolution investigated using four molecular lines, N_2_H^+^(1-0), HCO^+^(1-0), HCN(1-0), and HNC(1-0). The results suggest that the global averaged integrated intensity ratios I(HCO^+^)/I(HNC), I(HCN)/I(HNC), I(N_2_H^+^)/I(HCO^+^), and I(N_2_H^+^)/ I(HCN) are promising tracers for evolution of high-mass star-forming clumps. The global averaged column densities and abundances of N_2_H^+^, HCO^+^, HCN, and HNC increase as clumps evolve. The global averaged abundance ratios X(HCN)/X(HNC) could be used to trace evolution of high-mass star forming clumps, X(HCO^+^)/X(HNC) is more suitable for distinguishing high-mass star-forming clumps in prestellar (stage A) from those in protostellar (stage B) and HII/PDR region (stage C). These results suggest that the global averaged integrated intensity ratios between HCN(1-0), HNC(1-0), HCO^+^(1-0) and N_2_H^+^(1-0) are more suitable for tracing the evolution of high-mass star forming clumps. We also studied the chemical properties of the target high-mass star-forming clumps in each spiral arm of the Galaxy, and got results very different from those above. This is probably due to the relatively small sample in each spiral arm. For high-mass star-forming clumps in Sagittarius arm and Norma-Outer arm, comparing two groups located on one arm with different Galactocentric distances, the clumps near the Galactic Center appear to be younger than those far from the Galactic center, which may be due to more dense gas concentrated near the Galactic Center, and hence more massive stars being formed there.2016Ap&SS.361..191Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/other/ApSS/361.191CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/293 : GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)J/A+A/291/943 : Protostellar cores (Ossenkopf+, 1994)J/AJ/136/2391 : GLIMPSE Extended Green Objects catalog (Cyganowski+, 2008)J/A+A/527/A88 : Chemistry in infrared dark clouds (Vasyunina+, 2011)J/ApJ/756/60 : A 3mm line survey in 37 IR dark clouds (Sanhueza+, 2012)J/ApJ/777/157 : 90GHz obs. of high-mass star-forming regions (Hoq+, 2013)J/A+A/549/A45 : ATLASGAL Compact Source Catalog: 330<l<21 (Contreras+, 2013)J/A+A/563/A97 : IRAM 30m reduced spectra of 59 sources (Gerner+, 2014)J/A+A/568/A41 : ATLASGAL Compact Source Catalog: 280<l<60 (Urquhart+, 2014)J/MNRAS/443/1555 : ATLASGAL massive star forming clumps (Urquhart+, 2014)J/AJ/149/64 : MIPSGAL 24{mu}m point source catalog (Gutermuth+, 2015)J/ApJ/815/130 : High-mass molecular clumps from MALT90 (Guzman+, 2015)J/ApJ/824/29 : ATLASGAL clumps with IRAS flux & MALT90 data (Stephens+, 2016)J/other/PASA/33.30 : MALT90 Catalogue (Rathborne+, 2016)J/AJ/154/140 : MALT90 kinematic distances to clumps (Whitaker+, 2017)J/ApJS/231/11 : High-mass starless clump candidates from ATLASGAL (Yuan+, 2017)J/ApJ/839/113 : GLIMPSE/MIPSGAL data of molecular clouds (Retes-Romero+, 2017)J/MNRAS/473/1059 : Complete sample of Galactic clumps (Urquhart+, 2018)http://www3.mpifr-bonn.mpg.de/div/atlasgal/ : ATLASGAL home pagehttp://malt90.bu.edu/ : MALT90 home pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/other/ApSS/361.191https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/other/ApSS/361.191http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/other/ApSS/361.191https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/other/ApSS/361.191https://vizier.iucaa.in/viz-bin/votable?-source=J/other/ApSS/361.191http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/other/ApSS/361.191GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/other/ApSS/361.191/clumps (Integrated intensities and abundances data of the MALT90 clumps (Tables 1, 2 and 5))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/other/ApSS/361.191/clumps?https://vizier.iucaa.in/viz-bin/conesearch/J/other/ApSS/361.191/clumps?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/other/ApSS/361.191/clumps?GETtext/xml+votable180.050000true266.25655-28.849690.0055555555555555565/7202 10615 6/28802 28803 28806 28812 28813 28814 28824 28826 28827 28828 28830 28831 28852 28875 28879 28896 28897 28901 28912 28913 28916 28918 28919 29090 29091 29094 29096 29097 29100 29101 29103 29112 29113 29115 42207 42229 42378 42379 42381 42383 42390 42392 42396 42397 42434 42435 42438 42440 42441 42444 42445 42447 42450 42451 42454 42456 42457 42458https://cdsarc.cds.unistra.fr/viz-bin/moc/J/other/ApSS/361.191?format=asciiRadiodefaultJ/other/ApSS/361.191/clumpsIntegrated intensities and abundances data of the MALT90 clumps (Tables 1, 2 and 5)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDistDisplay the derived distances for this clump (link to Table 7)meta.ref.urlcharNameSource name (GLLL.lll+BB.bbb)meta.id;meta.maincharprimaryGLONGalactic longitudedegpos.galactic.lonGLAT[-1.1/1.1] Galactic latitudedegpos.galactic.latStageEvolutionary stage (G1)src.classcharFWHM[-121.1/154] Full line width at half maximum (FWHM) of N_2_H^+^(1-0) ({Delta}V(N_2_H^+^))km/sspect.line.widthfloate_FWHM[0.01/0.6] dVN2H uncertaintykm/sstat.error;phys.angSizefloatVlsr[0.4/24.4] LSR velocity of N_2_H^+^(1-0)km/sphys.veloc;pos.lsrfloate_Vlsr[0.02/1.2] Vlsr uncertaintykm/sstat.error;phys.veloc;pos.lsrfloatIN2H[1/8.7] N_2_H^+^ integrated intensityK.km/sphot.flux.density;em.radiofloatIHCO[1/8.7] HCO^+^ integrated intensityK.km/sphot.flux.density;em.radiofloatIHCN[0.9/10] HCN integrated intensityK.km/sphot.flux.density;em.radiofloatIHNC[1/7.3] HNC integrated intensityK.km/sphot.flux.density;em.radiofloatIN2H/HCO[0.03/20] N_2_H^+^ to HCO^+^ integrated intensity ratiospect.line.intensity;arith.ratiofloatIN2H/HCN[0.03/53] N_2_H^+^ to HCN integrated intensity ratiospect.line.intensity;arith.ratiofloatIN2H/HNC[0.09/14] N_2_H^+^ to HNC integrated intensity ratiospect.line.intensity;arith.ratiofloatIHCO/HCN[0.04/16] HCO^+^ to HCN integrated intensity ratiospect.line.intensity;arith.ratiofloatIHCO/HNC[0.07/15] HCO^+^ to HNC integrated intensity ratiospect.line.intensity;arith.ratiofloatIHCN/HNC[0.02/8] HCN to HNC integrated intensity ratiospect.line.intensity;arith.ratiofloatN2H[0.05/1.1] Abundance of N_2_H^+^(1-0)phys.abundfloatHCO[0.01/1.5] Abundance of HCO^+^(1-0)phys.abundfloatHCN[0.04/5] Abundance of HCN(1-0)phys.abundfloatHNC[0.02/0.8] Abundance of HNC(1-0)phys.abundfloatN2H/HCO[0.2/10.2] N_2_H^+^ to HCO^+^ abundance ratiophys.abund;arith.ratiofloatN2H/HCN[0.06/4.3] N_2_H^+^ to HCN abundance ratiophys.abund;arith.ratiofloatN2H/HNC[0.3/17.5] N_2_H^+^ to HNC abundance ratiophys.abund;arith.ratiofloatHCO/HCN[0.02/3] HCO^+^ to HCN abundance ratiophys.abund;arith.ratiofloatHCO/HNC[0.2/5.5] HCO^+^ to HNC abundance ratiophys.abund;arith.ratiofloatHCN/HNC[0.2/27.7] HCN to HNC abundance ratiophys.abund;arith.ratiofloat_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.ranullableindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decnullableindexedJ/other/ApSS/361.191/table7*Kinematic distances of 162 clumpsArm[1/4] Spiral arm (1)meta.codeintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource name (GLLL.lll+BB.bbb)meta.id;meta.maincharStageEvolutionary stage (G1)src.classcharDist[0.6/25.3] Kinematic distancekpcpos.distance;pos.heliocentricfloatRgc[3/16.8] Distance from the Galactic Center of the sourcekpcpos.distancefloat