ALMA [N II] 205 mu m Imaging Spectroscopy of the Interacting Galaxy System BRI 1202-0725 at Redshift 4.7

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dc.contributor.authorLu, Nanyao
dc.contributor.authorZhao, Yinghe
dc.contributor.authorDiaz Santos, Tanio
dc.contributor.authorKevin Xu, C.
dc.contributor.authorCharmandaris, Vassilis
dc.contributor.authorGao, Yu
dc.contributor.authorvan der Werf, Paul P.
dc.contributor.authorPrivon, George C.
dc.contributor.authorInami, Hanae
dc.contributor.authorRigopoulou, Dimitra
dc.contributor.authorSanders, David B.
dc.contributor.authorZhu, Lei
dc.date.accessioned2024-01-10T13:11:00Z
dc.date.available2024-01-10T13:11:00Z
dc.date.issued2017
dc.description.abstractWe present the results from Atacama Large Millimeter/submillimeter Array imaging in the [N II] 205 mu m fine-structure line (hereafter [N II]) and the underlying continuum of BRI 1202-0725, an interacting galaxy system at z = 4.7, consisting of a quasi-stellar object (QSO), a submillimeter galaxy (SMG), and two Ly alpha emitters, all within similar to 25 kpc of the QSO. We detect the QSO and SMG in both [N II] and continuum. At the similar to 1 '' (or 6.6 kpc) resolution, both the QSO and SMG are resolved in [N II], with the de-convolved major axes of similar to 9 and similar to 14 kpc, respectively. In contrast, their continuum emissions are much more compact and unresolved even at an enhanced resolution of similar to 0 ''.7. The ratio of the [N II] flux to the existing CO(7-6) flux is used to constrain the dust temperature (T-dust) for a more accurate determination of the FIR luminosity L-FIR. Our best estimated T-dust equals 43 (+/- 2) K for both galaxies (assuming an emissivity index beta = 1.8). The resulting LCO(7-6)/LFIR ratios are statistically consistent with that of local luminous infrared galaxies, confirming that LCO(7-6) traces the star formation (SF) rate (SFR) in these galaxies. We estimate that the ongoing SF of the QSO (SMG) has an SFR of 5.1 (6.9) x 10(3) M-circle dot yr(-1) (+/- 30%) assuming Chabrier initial mass function, takes place within a diameter (at half maximum) of 1.3 (1.5) kpc, and will consume the existing 5 (5) x 10(11) M-circle dot of molecular gas in 10 (7) x 10(7) years.
dc.description.funderNSFC
dc.description.funderALMA-CONICYT
dc.description.funderFONDECYT
dc.fechaingreso.objetodigital2024-05-30
dc.format.extent6 páginas
dc.fuente.origenWOS
dc.identifier.doi10.3847/2041-8213/aa77fc
dc.identifier.eissn2041-8213
dc.identifier.issn2041-8205
dc.identifier.urihttps://doi.org/10.3847/2041-8213/aa77fc
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/77975
dc.identifier.wosidWOS:000403940100001
dc.information.autorucFísica;Privon G;S/I;1031484
dc.issue.numero2
dc.language.isoen
dc.nota.accesoContenido parcial
dc.publisherIOP PUBLISHING LTD
dc.revistaASTROPHYSICAL JOURNAL LETTERS
dc.rightsacceso restringido
dc.subjectgalaxies: active
dc.subjectgalaxies: ISM
dc.subjectgalaxies: star formation
dc.subjectinfrared: galaxies
dc.subjectISM: molecules
dc.subjectsubmillimeter: galaxies
dc.subjectLUMINOUS INFRARED GALAXIES
dc.subjectWARM MOLECULAR GAS
dc.subjectSTAR-FORMATION LAW
dc.subjectZ GREATER-THAN
dc.subjectC II
dc.subjectEMISSION
dc.subjectDUST
dc.subjectZ=4.7
dc.subjectQUASAR
dc.subjectRADIO
dc.titleALMA [N II] 205 mu m Imaging Spectroscopy of the Interacting Galaxy System BRI 1202-0725 at Redshift 4.7
dc.typeartículo
dc.volumen842
sipa.codpersvinculados1031484
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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