J/A+A/637/A63ivo://CDS.VizieR/J/A+A/637/A63doi:10.26093/cds/vizier.36370063CDSTaquet V.Codella C.De Simone M.Lopez-Sepulcre A.Pineda J.E.,Segura-Cox D.Ceccarelli C.Caselli P.Gusdorf A.Persson M.V.,Alves F.Caux E.Favre C.Fontani F.Neri R.Oya Y.Sakai N.,Vastel C.Yamamoto S.Bachiller R.Balucani N.Bianchi E.Bizzocchi L.,Chacon-Tanarro A.Dulieu F.Enrique-Romero J.Feng S.Holdship J.,Lefloch B.Jaber Al-Edhari A.Jimenez-Serra I.Kahane C.Lattanzi V.,Ospina-Zamudio J.Podio L.Punanova A.Rimola A.Sims I.R.Spezzano S.,Testi L.Theule P.Ugliengo P.Vasyunin A.I.Vazart F.Viti S.,Witzel A.2020-09-30T10:42:03Z2020-05-15T07:53:50ZCDS support team

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

cds-question@unistra.fryoung-stellar-objectsinfrared-sourcesinterstellar-mediumLow-mass protostars drive powerful molecular outflows that can be observed with millimetre and submillimetre telescopes. Various sulfuretted species are known to be bright in shocks and could be used to infer the physical and chemical conditions throughout the observed outflows. The evolution of sulfur chemistry is studied along the outflows driven by the NGC1333-IRAS4A protobinary system located in the Perseus cloud to constrain the physical and chemical processes at work in shocks. We observed various transitions from OCS, CS, SO, and SO_2_ towards NGC1333-IRAS4A in the 1.3, 2, and 3mm bands using the {IRAM NOrthern Extended Millimeter Array (NOEMA)} and we interpreted the observations through the use of the Paris-Durham shock model. The targeted species clearly show different spatial emission along the two outflows driven by IRAS4A. OCS is brighter on small and large scales along the south outflow driven by IRAS4A1, whereas SO_2_ is detected rather along the outflow driven by IRAS4A2 that is extended along the north east - south west (NE-SW) direction. SO is detected at extremely high radial velocity up to +25km/s relative to the source velocity, clearly allowing us to distinguish the two outflows on small scales. Column density ratio maps estimated from a rotational diagram analysis allowed us to confirm a clear gradient of the OCS/SO_2_ column density ratio between the IRAS4A1 and IRAS4A2 outflows. Analysis assuming non Local Thermodynamic Equilibrium of four SO$_2$ transitions towards several SiO emission peaks suggests that the observed gas should be associated with densities higher than 10^5^cm^-3^ and relatively warm (T>100K) temperatures in most cases. The observed chemical differentiation between the two outflows of the IRAS4A system could be explained by a different chemical history. The outflow driven by IRAS4A1 is likely younger and more enriched in species initially formed in interstellar ices, such as OCS, and recently sputtered into the shock gas. In contrast, the longer and likely older outflow triggered by IRAS4A2 is more enriched in species that have a gas phase origin, such as SO_2_.2020A&A...637A..63Thttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/637/A63CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/605/A57 : SOLIS. II. OMC2-FIR4 HC_3_N and HC_5_N images (Fontani+, 2017)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/637/A63https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/637/A63http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/637/A63https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/637/A63https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/637/A63http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/637/A63GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/637/A63/list (List of fits files)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/637/A63/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/637/A63/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/637/A63/list?GETtext/xml+votable180.050000true52.2936931.225190.005555555555555556Associated datahttps://cdsarc.cds.unistra.fr/assocdata/?obs_collection=J/A+A/637/A636/862https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/637/A63?format=asciiInfrareddefaultJ/A+A/637/A63/listList of fits filesrecnoRecord 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.numberintsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitsAssocDataAssociated Data web pagemeta.ref.urlchar