J/A+A/677/A92ivo://CDS.VizieR/J/A+A/677/A92doi:10.26093/cds/vizier.36770092CDSValdivia-Mena M.T.Pineda J.E.Segura-Cox D.M.Caselli P.,Schmiedeke A.Choudhury S.Offner S.Neri R.Goodman A.Fuller G.2024-11-06T20:06:01Z2023-09-08T07:56:14ZCDS support team

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

cds-question@unistra.frmolecular-cloudsyoung-stellar-objectsinfrared-sourcesinterferometryThe infall of gas from outside natal cores has proven to feed protostars after the main accretion phase (Class 0). This changes our view of star formation to a picture that includes asymmetric accretion (streamers), and a larger role of the environment. However, the connection between streamers and the filaments that prevail in star-forming regions is unknown. We investigate the flow of material toward the filaments within Barnard 5 (B5) and the infall from the envelope to the protostellar disk of the embedded protostar B5-IRS1. Our goal is to follow the flow of material from the larger, dense core scale, to the protostellar disk scale. We present new HC_3_N line data from the NOEMA and 30m telescopes covering the coherence zone of B5, together with ALMA H_2_CO and C^18^O maps toward the protostellar envelope. We fit multiple Gaussian components to the lines so as to decompose their individual physical components. We investigated the HC3N velocity gradients to determine the direction of chemically fresh gas flow. At envelope scales, we used a clustering algorithm to disentangle the different kinematic components within H_2_CO emission. At dense core scales, HC_3_N traces the infall from the B5 region toward the filaments. HC_3_N velocity gradients are consistent with accretion toward the filament spines plus flow along them. We found a ~2800 au streamer in H_2_CO emission, which is blueshifted with respect to the protostar and deposits gas at outer disk scales. The strongest velocity gradients at large scales curve toward the position of the streamer at small scales, suggesting a connection between both flows. Our analysis suggests that the gas can flow from the dense core to the protostar. This implies that the mass available for a protostar is not limited to its envelope, and it can receive chemically unprocessed gas after the main accretion phase.2023A&A...677A..92Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/677/A92CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/677/A92https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/677/A92http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/677/A92https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/677/A92https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/677/A92http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/677/A92GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/677/A92/list (List of fits datacubes)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/677/A92/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/677/A92/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/677/A92/list?GETtext/xml+votable180.050000true56.9000832.870130.0055555555555555566/1542https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/677/A92?format=asciiInfrareddefaultJ/A+A/677/A92/listList of fits datacubesNzNumber of slicesmeta.numberintbVRAD? Lower value of VRAD intervalm/sphys.veloc;pos.heliocentricdoublenullableBVRAD? Upper value of VRAD intervalm/sphys.veloc;pos.heliocentricdoublenullabledVRAD? bVRAD resolutionm/sspect.resolutiondoublenullablebFreq? Lower value of frequency intervalHzem.freq;stat.mindoublenullableBFreq? Upper value of frequency intervalHzem.freq;stat.maxdoublenullabledFreq? Frequency resolutionHzspect.resolutionfloatnullablesizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitsrecnoRecord 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.numberintObs.dateObservation datestime.epoch;obsnullable