Multi-Sightline Observation of Narrow Absorption Lines in Lensed Quasar SDSS J1029+2623* †

Abstract

We exploit the widely-separated images of the lensed quasar SDSS J1029+2623 (z em =2.197, θ = 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 April (Misawa et al. 2014b, separated by 4 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 v ej ∼ 59,000, 43,000, and 29,000 km s −1 , 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 v ej > 1,000 km s −1 , 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 ≤ 620 pc from the central black hole with an electron density of n e ≥ 8.7×10 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.

Μελέτη των πλατιών γραμμών απορρόφησης των Si IV και C IV στα υπεριώδη φάσματα των Broad Absorption Line Quasars

“…Such cases have also been observed in UV absorption lines of Seyfert 1 galaxies (Crenshaw et al 1999 and references therein), some of which show as many as 7 distinct, kinematic components (e.g., Mrk 509 Kriss et al 2000). It should be noted, that the physical model we described above is confirmed, observationally, by the works of Misawa et al (2016) and Lu& . Misawa et al (2016) by observing multiple sight lines of the lensed quasar SDSS J1029+2623 resolved the clumpy structure of the outflow.…”

“…On the one hand we have the smooth wind models (Scargle et al 1970;Shlosman & Vitello 1993;Murray et al 1995;Fukumura et al 2018), according to which BAL troughs are the product of a smooth continuous flow. On the other hand we encounter models which assume that BALs are due to a flow of many individual substructures in the wind called density enhancements or clumps or clouds, indicating that accretion disc outflows are clumpy (McKee & Tarter 1975;Turnshek 1984;Lyratzi et al 2009Lyratzi et al , 2011Hamann et al 2013;Takeuchi et al 2013;Capellupo et al 2012Capellupo et al , 2014Misawa et al 2014Misawa et al , 2016Stathopoulos et al 2015;Waters & Proga 2016).…”

“…The main idea is that quasar winds are pervaded by a large number of multiscale structures (clumps, clouds), whose origin is probably some kind of radiative instability (Takeuchi et al 2013(Takeuchi et al , 2014Moscibrodzka & Proga 2013;Proga et al 2014;Proga & Waters 2015;Waters & Proga 2016;Kobayashi et al 2018). From an observational point of view Misawa et al (2014Misawa et al ( , 2016 by observing multiple sight lines, with the aid of strong gravitational lensing, managed to resolve the clumpy structure of the outflow winds in individual quasars. Hamann et al (2011) identified five high-velocity outflow Narrow Absorption Lines (NALs) in SDSS J212329.46-005052.9 which require five distinct clumpy structures of the outflow with similar physical conditions, characteristic sizes and kinematics.…”

Spectroscopic Observations of the Outflowing Wind in the Lensed Quasar SDSS J1001+5027∗

“…• Because BAL absorbers are believed to be located very close to the flux source (at a distance of order parsecs or less, much smaller than the boundary distance), the sightlines of the images of small-separation lensed quasars, such as SDSS J1001+5027, are not distinct. Nonetheless, the sightlines to NAL absorbers that are several kiloparsec away from the quasar are distinct (as in SDSS J1029+2623 Misawa et al 2013Misawa et al , 2014bMisawa et al , 2016.…”

“…In addition to these three methods of identifying intrinsic NALs, Misawa et al (2016) introduced a new method by exploiting multi-sightline observations. If NALs with identical line profiles are detected at the same redshift (i.e., at a common apparent ejection velocity from the quasar) along two sightlines with a large physical distance in the transverse direction, the corresponding absorber is very likely to be intrinsic to the quasar, because both cylinders of sight to the two lensed images can go through the same gas parcels only if these parcels are located in the vicinity of the flux source.…”