J/A+A/713/A137ivo://CDS.VizieR/J/A+A/713/A137CDSMazurek H.J.Gerin M.Gratier P.Pety J.Bron E.Roueff E.Roueff A.,Beslic I.Einig L.Orkisz J. H.Palud P.Santa-Maria M. G.Segal L.,Zakardjian A.Bardeau S.Chainais P.Coude S.Demyk K.,de Souza Magalhaes V.Goicoechea J.R.Hughes A.Languignon D.,Levrier F.Le Petit F.C.L. Dariusz C.Liszt H.S.Peretto N.,Sievers A.Thouvenin P.-A.2026-09-16T08:14:08Z2026-09-16T09:02:18ZCDS support team

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

cds-question@unistra.frinterstellar-mediummolecular-cloudsspectroscopyyoung-stellar-objectsmillimeter-astronomysubmillimeter-astronomymolecular-physicsastrometryphotometryultraviolet-astronomyPre-stellar cores are the sites of the earliest stages of star formation. Dust continuum observations are often used to identify and characterize their properties yet only a small fraction of them was observed and studied in terms of their composition and dynamical status. Pre-stellar cores are often analysed as being analogous to template objects such as L1544 in Taurus, which could create an observational bias if this template is not representative of all possible prestellar cores. We explore the chemical diversity of prestellar cores and protostellar cores residing in the Orion B giant molecular cloud selected on their dust continuum emission to provide an unbiased view of their line emission properties and how they vary as function of the core parameters and environment. We make use of the large scale maps of Orion B in 25 molecular lines from which we extract information for a sample of 1001 cores selected using positions extracted from Herschel dust continuum observations. The main properties of the core sample are derived using the Principal Component Analysis and additional maps of physical parameters: column density N_H2_, far-ultraviolet (FUV) radiation field G0 and mean volume gas density n. Additional high spectral resolution observations of C^18^O(1-0) serve to evaluate the dynamical status of cores. The average line width of the cores is larger than what is typically expected for prestellar cores of closer star forming regions, which suggests that cores in Orion B are subjected to stronger turbulence affecting their stability. The first factor of the PCA analysis explaining the variation of the detected line intensities is the core column density of molecular gas. The second factor explains how the core chemical composition is strictly linked to their environment, which can be traced by the ratio of the external FUV radiation field over the core volume density, G0/n. Cold and shielded cores exhibit strong emission of N_2_H^+^, CH_3_OH and deuterated species, whereas cores exposed to radiation are devoid of typical core tracers, but exhibit emission of ^12^CN, HCO^+^ and HCN. The third factor explaining the core chemical diversity is the mean density along the core line of sight, which is also associated with freeze-out and fractionation signatures. Pre-stellar cores selected based on their dust emission exhibit a wide range of line emission patterns, which can be related to their intrinsic properties (column density N_H2_, mean volume density n) and environment (presence or lack of FUV). The key parameter that distinguishes cores of different emission patterns is G0/n.2026A&A...713A.137Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/713/A137CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/635/A34 : Catalog of dense cores in Orion B from Herschel (Konyves+ 2020)J/A+A/566/A45 : Orion optical-depth and column-density maps (Lombardi+, 2014)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/713/A137https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/713/A137http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/713/A137https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/713/A137https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/713/A137http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/713/A137GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/713/A137/tablea1 (Core information)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/713/A137/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/713/A137/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/713/A137/tablea1?GETtext/xml+votable180.050000true84.829875-1.39941670.0055555555555555565/5713 5716 6/22861 22872https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/713/A137?format=asciiUVMillimeterdefaultJ/A+A/713/A137/tablea1Core informationrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIndexRunning index of cores introduced in this work (1)meta.id;meta.maincharK20[5/1613] Core running index introduced by Konyves et al. (2020A&A...635A..34K, Cat. J/A+A/635/A34)meta.id.associntCoreType[1/3] Core type introduced by Konyves et al. (2020A&A...635A..34K, Cat. J/A+A/635/A34) (2)src.classintHGBSCore name from the HGBS catalogue (HGBS_J*) (Konyves et al. (2020A&A...635A..34K, Cat. J/A+A/635/A34)meta.idcharSimbadSimbad column added by the CDSmeta.ref.urlcharRcoreObserved core radius, extracted from Konyves et al. (2020A&A...635A..34K, Cat. J/A+A/635/A34)pcphys.size.radiusfloatRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainNH2Core column density, extracted from Lombardi et al. (2014A&A...566A..45L, Cat. J/A+A/566/A45) mapscm**-2phys.columnDensitydoubleTdustCore dust temperatures, extracted from Lombardi et al. (2014A&A...566A..45L, Cat. J/A+A/566/A45) mapsKphys.temperaturedoubleG0Far-ultraviolet radiation field measured on cores, based on maps from Santa-Maria et al. (2023A&A...679A...4S) in Habing units (3)phot.flux;em.UVdoublenMean core volume densities measured on maps from (Orkisz & Kainulainen, 2025A&A...697A..20O)cm**-3phys.densitydoubleJ/A+A/713/A137/table2Core intensity measurementsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIndexRunning index of cores introduced in this workmeta.id;meta.maincharK20[5/1613] Core running index introduced by Konyves et al. (2020A&A...635A..34K, Cat. J/A+A/635/A34)meta.id.associntHGBSCore name from the HGBS catalogue (Konyves et al. (2020A&A...635A..34K, Cat. J/A+A/635/A34)meta.idchar12CO10Integrated intensity for ^12^CO(1-0)K.km/sphot.flux.densitydouble13CO10Integrated intensity for ^13^CO(1-0)K.km/sphot.flux.densitydoubleC18O10Integrated intensity for C^18^O(1-0)K.km/sphot.flux.densitydoubleC17O10Integrated intensity for C^17^O(1-0)K.km/sphot.flux.densitydoubleN2Hp10Integrated intensity for N_2_H+(1-0)K.km/sphot.flux.densitydoubleHCOIntegrated intensity for HCOK.km/sphot.flux.densitydoubleHCOp10Integrated intensity for HCO+(1-0)K.km/sphot.flux.densitydoubleH13COp10Integrated intensity for H^13^CO+(1-0)K.km/sphot.flux.densitydoubleH2CO? Integrated intensity for H_2_COK.km/sphot.flux.densitydoublenullableDCOp10? Integrated intensity for DCO+K.km/sphot.flux.densitydoublenullableHCN10Integrated intensity for HCN(1-0)K.km/sphot.flux.densitydoubleHNC10Integrated intensity for HNC(1-0)K.km/sphot.flux.densitydoubleH13CN10Integrated intensity for H^13^CN(1-0)K.km/sphot.flux.densitydoubleHN13C10Integrated intensity HN^13^C(1-0)K.km/sphot.flux.densitydoubleDNC10? Integrated intensity for DNC(1-0)K.km/sphot.flux.densitydoublenullableCCH10Integrated intensity for CCH(1-0)K.km/sphot.flux.densitydoubleC3H2Integrated intensity for C_3_H_2_K.km/sphot.flux.densitydouble12CN10Integrated intensity for ^12^CN(1-0)K.km/sphot.flux.densitydouble12CS21Integrated intensity for ^12^CS(2-1)K.km/sphot.flux.densitydouble32SO21Integrated intensity for ^32^SO(2-1)K.km/sphot.flux.densitydoubleCCS? Integrated intensity for CCSK.km/sphot.flux.densitydoublenullableHCSp10Integrated intensity for HCS+(1-0)K.km/sphot.flux.densitydoubleSIO21Integrated intensity for SiO(2-1)K.km/sphot.flux.densitydoubleHNCOIntegrated intensity for HNCOK.km/sphot.flux.densitydoubleCH3OH21Integrated intensity for CH_3_OH(2-1)K.km/sphot.flux.densitydoublee_12CO10Intensity uncertainty for ^12^CO(1-0)K.km/sstat.errordoublee_13CO10Intensity uncertainty for ^13^CO(1-0)K.km/sstat.errordoublee_C18O10Intensity uncertainty for C^18^O(1-0)K.km/sstat.errordoublee_C17O10Intensity uncertainty for C^17^O(1-0)K.km/sstat.errordoublee_N2Hp10Intensity uncertainty for N_2_H+(1-0)K.km/sstat.errordoublee_HCOIntensity uncertainty for HCOK.km/sstat.errordoublee_HCOp10Intensity uncertainty for HCO+(1-0)K.km/sstat.errordoublee_H13COp10Intensity uncertainty for H^13^CO+(1-0)K.km/sstat.errordoublee_H2CO? Intensity uncertainty for H_2_COK.km/sstat.errordoublenullablee_DCOp10? Intensity uncertainty for ^12^CO(1-0)K.km/sstat.errordoublenullablee_HCN10Intensity uncertainty for HCN(1-0)K.km/sstat.errordoublee_HNC10Intensity uncertainty for HNC(1-0)K.km/sstat.errordoublee_H13CN10Intensity uncertainty for H^13^CN(1-0)K.km/sstat.errordoublee_HN13C10Intensity uncertainty for HN^13^C(1-0)K.km/sstat.errordoublee_DNC10? Intensity uncertainty for DNC(1-0)K.km/sstat.errordoublenullablee_CCH10Intensity uncertainty for CCH(1-0)K.km/sstat.errordoublee_C3H2Intensity uncertainty for C_3_H_2_K.km/sstat.errordoublee_12CN10Intensity uncertainty for ^12^CN(1-0)K.km/sstat.errordoublee_12CS21Intensity uncertainty for ^12^CS(2-1)K.km/sstat.errordoublee_32SO21Intensity uncertainty for ^32^SO(2-1)K.km/sstat.errordoublee_CCS? Intensity uncertainty for CCSK.km/sstat.errordoublenullablee_HCSp10Intensity uncertainty for HCS+(1-0)K.km/sstat.errordoublee_SIO21Intensity uncertainty for SiO(2-1)K.km/sstat.errordoublee_HNCOIntensity uncertainty for HNCOK.km/sstat.errordoublee_CH3OH21Intensity uncertainty for CH_3_OH(2-1)K.km/sstat.errordouble