J/A+A/663/A177ivo://CDS.VizieR/J/A+A/663/A177doi:10.26093/cds/vizier.36630177CDSWang Y.X.Zhang J.S.Yan Y.T.Qiu J.J.Chen J.L.Zhao J.Y.Zou Y.P.,Wu X.C.He X.L.Gong Y.B.Cai J.H.2023-02-22T09:02:11Z2023-02-22T09:39:01ZCDS support team

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

cds-question@unistra.frstar-forming-regionsmillimeter-astronomyphotometrysubmillimeter-astronomychemical-abundancesastrophysical-masersradio-astronomyCyanopolyynes (HC_2n+1_N, n=1,2,3), which are the linear carbon chain molecules, are precursors for the prebiotic synthesis of simple amino acids. They are important for understanding prebiotic chemistry and may be good tracers of the star formation sequence. We aim to search for cyanopolyynes in high-mass star-forming regions (HMSFRs) at possibly different evolutionary stages, investigate the evolution of HC_3_N and its relation with shock tracers, and detect the existence of HC_5_N and HC_7_N in HMSFRs with a formed protostar. We carried out a cyanopolyyne line survey towards a large sample of HMSFRs using the Shanghai Tian Ma 65m Radio Telescope (TMRT). Our sample consisted of 123 targets taken from the TMRT C band line survey. It included three kinds of sources, namely those with detection of the 6.7GHz CH_3_OH maser alone, with detection of the radio recombination line (RRL) alone, and with detection of both (hereafter referred to as Maser-only, RRL-only, and Maser-RRL sources, respectively). For our sample with detection of cyanopolyynes, their column densities were derived using the rotational temperature measured from the NH_3_ lines. We constructed and fitted the far-infrared (FIR) spectral energy distributions (SED; obtained from the Herschel FIR data and the Atacama Pathfinder Experiment data at 870 um) of our HC_3_N sources. Moreover, by analysing the relation between HC_3_N and other shock tracers, we also investigate whether HC_3_N is a good tracer of shocks. We detected HC_3_N in 38 sources, HC_5_N in 11 sources, and HC_7_N in G24.790+0.084, with the highest detection rate being found for Maser-RRL sources and a very low detection rate found for RRL-only sources. The mean column density of HC_3_N was found to be (1.75+/-0.42)x10^13^, (2.84+/-0.47)x10^13^, and (0.82+/-0.15)x10^13^cm^-2^ for Maser-only, Maser-RRL, and RRL-only sources, respectively. Based on a fit of the FIR SED, we derive their dust temperatures, H_2_ column densities, and abundances of cyanopolyynes relative to H_2_. The mean relative abundance of HC_3_N was found to be (1.22+/-0.52)x10^-10^ for Maser-only, (5.40+/-1.45)x10^-10^ for Maser-RRL, and (1.65+/-1.50)x10^-10^ for RRL-only sources, respectively. The detection rate, the column density, and the relative abundance of HC_3_N increase from Maser-only to Maser-RRL sources and decrease from Maser-RRL to RRL-only sources. This trend is consistent with the proposed evolutionary trend of HC_3_N under the assumption that our Maser-only, Maser-RRL, and RRL-only sources correspond to massive young stellar objects, ultracompact HII regions, and normal classical HII regions, respectively. Our detections enlarge the sample of HC_3_N in HMSFRs and support the idea that unsaturated complex organic molecules can exist in HMSFRs with a formed protostar. Furthermore, a statistical analysis of the integrated line intensity and column density of HC_3_N and shock-tracing molecules (SiO, H_2_CO) enabled us to find positive correlations between them. This suggests that HC_3_N may be another tracer of shocks, and should therefore be the subject of further observations and corresponding chemical simulations. Our results indirectly support the idea that the neutral-neutral reaction between C_2_H_2_ and CN is the dominant formation pathway of HC_3_N.2022A&A...663A.177Whttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/663/A177CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/568/A41 : ATLASGAL Compact Source Catalog: 280<l<60 (Urquhart+, 2014)J/ApJ/783/130 : Parallaxes of high mass star forming regions (Reid+, 2014)J/A+A/586/A149 : SiO in ATLASGAL-selected massive clumps (Csengeri+, 2016)J/MNRAS/473/1059 : Complete sample of Galactic clump propertiesJ/ApJ/885/131 : ~200 high-mass SFR plx + proper motion with VLBIhttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/663/A177https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/663/A177http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/663/A177https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/663/A177https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/663/A177http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/663/A177GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/663/A177/tableb1 (The HC_3_N (J = 2-1) transitions detected with the TMRT)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/663/A177/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/663/A177/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/663/A177/tableb1?GETtext/xml+votable180.050000true278.6509167-8.70738890.005555555555555556Cone search capability for table J/A+A/663/A177/tableb2 (The HC_5_N (J=3-2) and HC_7_N (J=15-14) transitions detected with TMRT)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/663/A177/tableb2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/663/A177/tableb2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/663/A177/tableb2?GETtext/xml+votable180.050000true276.9356667-11.24838890.005555555555555556Cone search capability for table J/A+A/663/A177/tableb3 (The column density and the relative abundance for HC_3_N, HC_5_N, and HC_7_N.)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/663/A177/tableb3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/663/A177/tableb3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/663/A177/tableb3?GETtext/xml+votable180.050000true276.9166-11.241940.005555555555555556Cone search capability for table J/A+A/663/A177/tablec1 (Sources without HC_3_N (J=2-1) detection)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/663/A177/tablec1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/663/A177/tablec1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/663/A177/tablec1?GETtext/xml+votable180.050000true277.3386667-10.87736110.0055555555555555565/7383 6/1783 3011 3630 3649 14317 14353-14354 14594 14622 14644 14646 14671 14682 14689 14691 14693 14696-14697 14704-14705 15362 15368 15390 15458 15473 15683 21458 22805 23969 24507 24554 29511 29522 30218-30219 30241 30244-30245 30256 30258-30259 30262-30263 30268-30269 30313 30317-30319 30417 30420 30422 30425 30616 30618 30622 30644 30692 30694 307122.283270615984385e-22 2.837779945223663e-21https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/663/A177?format=asciiMillimeterRadiodefaultJ/A+A/663/A177/table2Far infrared properties of our HC_3_N sourcesF160Herschel flux density at 160umJyphot.flux.density;em.mm.1500-3000GHzinte_F70Herschel flux density at 70um errorJystat.errorintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClassClassificationssrc.classcharNameSource name, GLL.lll+B.bbbmeta.id;meta.maincharF70Herschel flux density at 70umJyphot.flux.density;em.IR.30-60uminte_F160Herschel flux density at 160um errorJystat.errorintF250Herschel flux density at 250umJyphot.flux.density;em.mm.750-1500GHzinte_F250Herschel flux density at 250um errorJystat.errorintF350Herschel flux density at 350umJyphot.flux.density;em.mm.750-1500GHzinte_F350Herschel flux density at 350um errorJystat.errorintF500Herschel flux density at 500umJyphot.flux.density;em.mm.400-750GHzinte_F500Herschel flux density at 500um errorJystat.errorintF870APEX flux density at 870um (1)Jyphot.flux.density;em.mm.200-400GHzinte_F870APEX flux density at 870um error (1)Jystat.errorintReffEffective radius of sources at 870um (1)arcsecphys.angSize;em.mm.200-400GHzintgammaGas-to-dust ratiophys.mass;arith.ratiointTdustDust temperatureKphys.temperaturefloate_TdustDust temperature errorKstat.errorfloatMTotal (gas + dust) core masssolMassphys.massinte_MTotal (gas + dust) core mass errorsolMassstat.errorintT0dustDust temperature from Urquhart et al. (2018MNRAS.473.1059U, Cat. J/MNRAS/473/1059)Kphys.temperaturefloatMaTotal mass from Urquhart et al. (2018MNRAS.473.1059U, Cat. J/MNRAS/473/1059)solMassphys.massintN(H2)Column density of H_2_1e+23cm**-2phys.columnDensityfloate_N(H2)Column density of H_2_ error1e+23cm**-2stat.errorfloatJ/A+A/663/A177/tableb1The HC_3_N (J = 2-1) transitions detected with the TMRTe_VlsrLSR velocity errorkm/sstat.error;phys.veloc;pos.lsrfloatDeltanuFull width at half maximumkm/sspect.line.widthfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource Name (GLLL.lll+B.bbb)meta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainVlsrLSR velocitykm/sphys.veloc;pos.lsrfloate_DeltanuFull width at half maximum errorkm/sstat.errorfloatTmbPeak mean brigthness temperature valuemKphys.temperatureintrms? rms noise valuemKstat.stdev;instr.det.noiseintnullableIntTmbdvIntegrated line intensityK.km/sphot.flux.densityfloate_IntTmbdvIntegrated line intensity errorK.km/sstat.errorfloatDist? Heliocentric distance D is taken from the trigonometric parallax measurements (1)kpcpos.distancefloatnullablen_Dist[*] * for Dist obtained from the latest Parallax-based Distance Calculator V2meta.notecharDgc? Galactocentric distancekpcpos.distancefloatnullableClassClassificationssrc.classcharJ/A+A/663/A177/tableb2The HC_5_N (J=3-2) and HC_7_N (J=15-14) transitions detected with TMRTMolMolecule speciesmeta.notecharDeltanuFull width at half maximumkm/sspect.line.widthfloate_DeltanuFull width at half maximum errorkm/sstat.errorfloatTmbPeak mean brightness temperature valuemKphys.temperatureintrms? rms noise valuemKstat.stdev;instr.det.noiseintnullableIntTmbdvIntegrated line intensityK.km/sphot.flux.densityfloate_IntTmbdvIntegrated line intensity errorK.km/sstat.errorfloatClassClassificationssrc.classcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource Name (GLL.lll+B.bbb)meta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainVlsrLSR velocitykm/sphys.veloc;pos.lsrfloate_VlsrLSR velocity errorkm/sstat.error;phys.veloc;pos.lsrfloatJ/A+A/663/A177/tableb3The column density and the relative abundance for HC_3_N, HC_5_N, and HC_7_N._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.decnullableindexedrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintmoreindicates data in other tablesmeta.ref.urlcharClassClassificationssrc.classcharNameSource Name (GLLL.lll+BB.bbb)meta.id;meta.maincharprimaryTrotRotational temperature of NH_3_Kphys.temperaturefloatn_Trot[*] Note on Trot (1)meta.notecharN(HC3N)Column density of HC_3_N1e+13cm**-2phys.columnDensityfloate_N(HC3N)Column density of HC_3_N error1e+13cm**-2stat.errorfloatX(HC3N)? Relative abundance of HC_3_Nphys.abundfloatnullablee_X(HC3N)? Relative abundance of HC_3_N errorstat.errorfloatnullableN(HC5N)? Column density of HC_5_N1e+13cm**-2phys.columnDensityfloatnullablee_N(HC5N)? Column density of HC_5_N error1e+13cm**-2stat.errorfloatnullableX(HC5N)? Relative abundance of HC_5_Nphys.abundfloatnullablee_X(HC5N)? Relative abundance of HC_5_N errorstat.errorfloatnullableN(HC7N)? Column density of HC_7_N1e+13cm**-2phys.columnDensityfloatnullablee_N(HC7N)? Column density of HC_7_N error1e+13cm**-2stat.errorfloatnullableX(HC7N)? Relative abundance of HC_7_Nphys.abundfloatnullablee_X(HC7N)? Relative abundance of HC_7_N errorstat.errorfloatnullableN(HC3N)/N(HC5N)? Abundance ratio of N(HC_3_N)/N(HC_5_N)phys.abundfloatnullabler_Trot? Reference (2)meta.ref;pos.frameintnullable_GlonGalactic Longitude (derived from Name)degpos.galactic.lon_GlatGalactic Latitude (derived from Name)degpos.galactic.latJ/A+A/663/A177/tableb4The integrated line intensities of other moleculese_NH2C? Column density of H_2_CO error1e+13cm**-2stat.errorfloatnullableISiO? Integrated line intensity of SiO, taken from Csengeri et al. (2016A&A...586A.149C, Cat. J/A+A/586/A149)K.km/sspect.line.intensityfloatnullablee_ISiO? Integrated line intensity of SiO errorK.km/sstat.errorfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClassClassificationssrc.classcharNameSource Name (GLLL.lll+BB.bbb)Source namemeta.id;meta.maincharIH2CO? Integrated line intensity of H_2_CO (taken from TMRT C band survey)K.km/sphot.flux.densityfloatnullablee_IH2CO? Integrated line intensity of H_2_CO errorK.km/sstat.errorfloatnullableNH2C? Column density of H_2_CO, which is derived as done for cyanopolyynes in Sect. 3.11e+13cm**-2phys.columnDensityfloatnullableNSiO? Column density of SiO1e+13cm**-2phys.columnDensityfloatnullableJ/A+A/663/A177/tablec1Sources without HC_3_N (J=2-1) detectionrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource Name (GLLL.lll+BB.bbb)meta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainClassClassificationssrc.classcharrmsrms noise valuestat.stdev;instr.det.noiseint