J/ApJ/825/25 Narrow absorption lines of lensed QSO J1029+2623 (Misawa+, 2016)
Multi-sightline observation of narrow absorption lines in lensed quasar
SDSS J1029+2623.
Misawa T., Saez C., Charlton J.C., Eracleous M., Chartas G., Bauer F.E.,
Inada N., Uchiyama H.
<Astrophys. J., 825, 25-25 (2016)>
=2016ApJ...825...25M 2016ApJ...825...25M (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Spectroscopy ; Gravitational lensing ; Redshifts
Keywords: quasars: absorption lines; quasars: individual: "SDSS J1029+2623"
Abstract:
We exploit the widely separated images of the lensed quasar
SDSSJ1029+2623 (zem=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
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 νej∼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 νej>1000km/s, we also detect broader proximity
absorption lines (PALs) at zabs∼zem. 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 ne≥8.7x103/cm3. 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.
Description:
We acquired high-resolution spectra of the brightest two of the three
lensed images of the quasar SDSS J1029+2623, A and B with V=18.72 and
18.67mags, with the VLT using the Ultraviolet and Visual Echelle
Spectrograph (UVES) in queue mode (ESO program 092.B-0512(A)). The
observations were performed from 2014 January 28 to February 26, which
is ∼4yrs after the first observation on 2010 February 10 (Misawa+
2013AJ....145...48M 2013AJ....145...48M), and ∼2 months before the third observation on
2014 April 4 (Misawa+ 2014ApJ...794L..20M 2014ApJ...794L..20M) with Subaru using the High
Dispersion Spectrograph (HDS). The wavelength coverage is
3300-6600Å with R∼33000.
Log of observations:
--------------------------------------------------------------
Target Obs. date Instrument R Ref
--------------------------------------------------------------
SDSS J1029+2623 A 2010 Feb 10 Subaru/HDS 30000 1
SDSS J1029+2623 A 2014 Jan 28-Feb 3 VLT/UVES 33000 2
SDSS J1029+2623 A 2014 Apr 4 Subaru/HDS 36000 3
SDSS J1029+2623 B 2010 Feb 10 Subaru/HDS 30000 1
SDSS J1029+2623 B 2014 Feb 4-26 VLT/UVES 33000 2
SDSS J1029+2623 B 2014 Apr 4 Subaru/HDS 36000 3
--------------------------------------------------------------
Ref: 1 = Misawa et al. 2013AJ....145...48M 2013AJ....145...48M, 2 = This paper,
3 = Misawa et al. 2014ApJ...794L..20M 2014ApJ...794L..20M
--------------------------------------------------------------
Objects:
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RA (ICRS) DE Designation(s)
-------------------------------------------------------------------
10 29 13.96 +26 23 18.2 SDSS J1029+2623 = QSO J1029+2623
10 29 13.94 +26 23 17.9 Image A = [IOM2006] SDSS J1029+2623 A
10 29 14.2 +26 23 40 Image B = [IOM2006] SDSS J1029+2623 B
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 218 239 Line parameters of narrow absorption components
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See also:
J/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)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- --- [Image]
7 A1 --- Img Image identifier (A or B)
9- 13 A5 --- Ion Ion designation (C IV, Mg II, N V or Si IV)
15 A1 --- f_Ion [g-k] Flag on Ion (1)
18- 23 F6.1 0.1nm lambda [3956.2/5376.1]? Wavelength of flux-weighted
line center; Angstroms
25- 30 F6.4 --- zabs [0.5/2.2] Redshift of flux weighted line center
32- 37 I6 km/s vej [-100/190464] Ejection velocity from
quasar emission redshift
39- 43 F5.2 [cm-2] logN [11.9/17.4]? Log column density of Ion
45- 48 F4.2 [cm-2] e_logN [0.01/9.99]? Uncertainty in logN
50- 54 F5.1 km/s sigv/b [2.2/428.4] Flux-weighted line width, sigmav,
or Doppler parameter, b
56- 59 F4.1 km/s e_sigv/b [0.1/26]? Uncertainty in sigmav/b
61- 64 F4.2 --- Cf [0.04/1]? Covering factor (2)
66- 69 F4.2 --- E_Cf [0.02/0.5]? Upper uncertainty in Cf (3)
71- 74 F4.2 --- e_Cf [0.02/0.4]? Lower uncertainty in Cf
76-218 A143 --- Other Other ion designations and associated
wavelengths (4)
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Note (1): Flag as follows:
g = Two C 4 PALs at zabs∼2.1898 and 2.1958 are fitted together as a
single absorption profile whose flux-weighted redshift is zabs∼2.1937.
h = Two N 5 PALs at zabs∼2.1900 and 2.1955 are fitted together as a single
absorption profile whose flux-weighted redshift is zabs∼2.1937.
i = We cannot fit this Si 4 NAL because both members of the doublet are
blending with other lines.
j = Two C 4 PALs at zabs∼2.1897 and 2.1957 are fitted together as a
single absorption profile whose flux-weighted redshift is zabs∼2.1937.
k = Two N 5 PALs at zabs∼2.1900 and 2.1955 are fitted together as a
single absorption profile whose flux-weighted redshift is zabs∼2.1935.
Note (2): The covering factor (Cf) is the fraction of photons from the
background source that pass through the absorber.
See section 3.2 for further explanations.
Note (3): When e_Cf is given but E_Cf is blank the upper limit is infinity.
Note (4): That are detected in the system. Lines in parenthesis are in
Lyα forest.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 23-Aug-2016