J/ApJ/825/25ivo://CDS.VizieR/J/ApJ/825/25doi:10.26093/cds/vizier.18250025CDSMisawa T.Saez C.Charlton J.C.Eracleous M.Chartas G.Bauer F.E.,Inada N.Uchiyama H.2022-11-21T06:59:21Z2016-10-05T15:09:49ZCDS support team

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

cds-question@unistra.frquasarsspectroscopygravitational-lensingredshiftedWe exploit the widely separated images of the lensed quasar SDSSJ1029+2623 (z_em_=2.197, {theta}=22.5") to observe its outflowing wind through two different sightlines. We present an analysis of three observations, including two with the Subaru telescope in 2010 February and 2014 April, separated by four years, and one with the Very Large Telescope, separated from the second Subaru observation by ~2 months. We detect 66 narrow absorption lines (NALs), of which 24 are classified as intrinsic NALs that are physically associated with the quasar based on partial coverage analysis. The velocities of intrinsic NALs appear to cluster around values of {nu}_ej_~59000, 43000, and 29000km/s, which is reminiscent of filamentary structures obtained by numerical simulations. There are no common intrinsic NALs at the same redshift along the two sightlines, implying that the transverse size of the NAL absorbers should be smaller than the sightline distance between two lensed images. In addition to the NALs with large ejection velocities of {nu}_ej_>1000km/s, we also detect broader proximity absorption lines (PALs) at z_abs_~z_em_. The PALs are likely to arise in outflowing gas at a distance of r<=620pc from the central black hole with an electron density of n_e_>=8.7x10^3^/cm^3^. These limits are based on the assumption that the variability of the lines is due to recombination. We discuss the implications of these results on the three-dimensional structure of the outflow.2016ApJ...825...25Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/825/25CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJ/779/161 : MgII absorbers in 0.4<z<2.3 SDSS QSOs (Seyffert+, 2013)J/ApJ/763/37 : Metals in SDSS QSOs I. 1.5<z<4.5 CIV absorbers (Cooksey+, 2013)J/AJ/143/119 : SDSS Quasar Lens Search. V. Final catalog (Inada+, 2012)J/A+A/546/A67 : Catalog of strong MgII absorbers (Lawther+, 2012)J/MNRAS/410/860 : Redshift dependence of BAL QSOs (Allen+, 2011)J/ApJS/171/1 : Census of QSOs Narrow Absorption Lines (Misawa+, 2007)J/A+A/427/107 : Polarization in BAL QSOs (Lamy+, 2004)J/ApJ/613/129 : Equivalent widths of QSOs (Wise+, 2004)J/ApJ/599/116 : UV properties of absorbed quasars (Vestergaard+, 2003)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/825/25https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/825/25http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/825/25https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/825/25https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/825/25http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/825/25GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/825/25/table3Line parameters of narrow absorption componentsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintImgImage identifier (A or B)meta.id;meta.maincharIonIon designation (C IV, Mg II, N V or Si IV)phys.atmol.ionStagecharf_Ion[g-k] Flag on Ion (1)meta.codecharlambda[3956.2/5376.1]? Wavelength of flux-weighted line center; Angstroms0.1nmem.wl;spect.linefloatnullablezabs[0.5/2.2] Redshift of flux weighted line centersrc.redshiftfloatvej[-100/190464] Ejection velocity from quasar emission redshiftkm/sphys.velocintlogN[11.9/17.4]? Log column density of Ionlog(cm**-2)phys.columnDensityfloatnullablee_logN[0.01/9.99]? Uncertainty in logNlog(cm**-2)stat.errorfloatnullablesigv/b[2.2/428.4] Flux-weighted line width, sigmav, or Doppler parameter, bkm/sspect.line.widthfloate_sigv/b[0.1/26]? Uncertainty in sigmav/bkm/sstat.errorfloatnullableCf[0.04/1]? Covering factor (2)stat.fit.paramfloatnullableE_Cf[0.02/0.5]? Upper uncertainty in Cf (3)stat.error;stat.maxfloatnullablee_Cf[0.02/0.4]? Lower uncertainty in Cfstat.errorfloatnullableOtherOther ion designations and associated wavelengths (4)meta.note