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A complete versionPreprint typeset using LATEX style emulateapj
v. 08/22/09
MULTI-SIGHTLINE OBSERVATION OF NARROW ABSORPTION LINES IN LENSED
QUASARSDSS J1029+26231,2
Toru Misawa3, Cristian Saez4,5, Jane C. Charlton6, Michael
Eracleous6,7, George Chartas8, Franz E.Bauer9,10,11, Naohisa
Inada12, and Hisakazu Uchiyama13
A complete version
ABSTRACTWe exploit the widely-separated images of the lensed
quasar SDSS J1029+2623 (zem=2.197, θ =
22′′.5) to observe its outflowing wind through two different
sightlines. We present an analysis of threeobservations, including
two with the Subaru telescope in 2010 February (Misawa et al. 2013)
and2014 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 quasarbased on partial coverage
analysis. The velocities of intrinsic NALs appear to cluster around
valuesof vej ∼ 59,000, 43,000, and 29,000 km s−1, which is
reminiscent of filamentary structures obtainedby numerical
simulations. There are no common intrinsic NALs at the same
redshift along the twosightlines, implying that the transverse size
of the NAL absorbers should be smaller than the sightlinedistance
between two lensed images. In addition to the NALs with large
ejection velocities of vej >1,000 km s−1, we also detect broader
proximity absorption lines (PALs) at zabs ∼ zem. The PALs arelikely
to arise in outflowing gas at a distance of r ≤ 620 pc from the
central black hole with an electrondensity of ne ≥ 8.7×103 cm−3.
These limits are based on the assumption that the variability of
thelines is due to recombination. We discuss the implications of
these results on the three-dimensionalstructure of the
outflow.Subject headings: quasars: absorption lines – quasars:
individual (SDSS J1029+2623)
1. INTRODUCTIONAGN outflows, potentially powered by one or more
of
a variety of mechanisms (e.g., radiation force,
magneticpressure, and magnetocentrifugal force), are
importantingredients of quasar central engines and likely play a
rolein quasar and galaxy formation/evolution because: 1)they
extract angular momentum from accretion disks al-lowing gas
accretion to proceed (e.g., Blandford & Payne1982; Emmering,
Blandford, and Shlosman 1992; Konigl& Kartje 1994; Everett
2005), leading to the growth of
Electronic address: [email protected] Based on data
collected at Subaru Telescope, which is operated
by the National Astronomical Observatory of Japan.2 Based on
observations obtained at the European Southern
Observatory at La Silla, Chile in programs 092.B-0512(A)3 School
of General Education, Shinshu University, 3-1-1 Asahi,
Matsumoto, Nagano 390-8621, Japan4 Korea Astronomy and Space
Science Institute (KASI), 61-1,
Hwaam-dong, Yuseong-gu, Deajeon 305-348, Republic of Korea5
Department of Astronomy, University of Maryland, College
Park, MD 20742-24216 Department of Astronomy and Astrophysics,
Pennsylvania
State University, University Park, PA 168027 Department of
Astronomy & Astrophysics and Center for
Gravitational Wave Physics, The Pennsylvania State
University,525 Davey Lab, University Park, PA 16802
8 Department of Physics and Astronomy, College of Charleston,SC
29424
9 Instituto de Astrof́ısica, Facultad de F́ısica, Pontificia
Univer-sidad Católica de Chile, Casilla 306, Santiago 22,
Chile
10 Millennium Institute of Astrophysics (MAS), NuncioMonseñor
Sótero Sanz 100, Providencia, Santiago, Chile
11 Space Science Institute, 4750 Walnut Street, Suite
205,Boulder, Colorado 80301
12 Department of Physics, National Institute of Technology,Nara
College, Yamatokohriyama, Nara 639-1080, Japan
13 Department of Astronomy, School of Science,
GraduateUniversity for Advanced Studies, Mitaka, Tokyo 181-8588,
Japan
black holes, 2) they also provide energy and momentumfeedback to
the interstellar medium of host galaxies andto the intergalactic
medium (IGM), and inhibit star for-mation (e.g., Springel, Di
Matteo, & Hernquist 2005),and 3) they may promote metal
enrichment of the in-tergalactic medium (IGM) (e.g., Hamann et al.
1997b;Gabel, Arav, & Kim 2006). These outflowing gases,which
are difficult to observe directly, have been detectedas absorption
lines in the spectra of about 50% of allquasars (e.g., Vestergaard
2003; Wise et al. 2004; Mis-awa et al. 2007a; Nestor et al. 2008;
Muzahid et al. 2013).However, a limitation of these past studies is
that theyobserve the outflowing gas only along a single
sightline(i.e., one dimension) toward the nucleus of each
quasar,although the absorber’s physical conditions probably de-pend
on the location/orientation at which we observe it(e.g., Ganguly et
al. 2001; Elvis 2000). Thus, the internalstructure of outflowing
winds is still largely unknown.
Multiple quasar images, produced by gravitationallensing,
provide a unique way to study the outflowing gasalong more than one
sightline. Lensed quasars with largeimage separation angles have a
higher chance of revealingstructural differences in the outflowing
winds, especiallyin the vicinity of the continuum source. In this
sense,the quasar images that are lensed by a cluster of
galaxies(rather than a single massive galaxy) are very promis-ing
targets. Among three such lensed quasars, SDSSJ1029+2623 at zem
∼2.197 (Inada et al. 2006; Oguri etal. 2008) is the best target
because i) it has the largestlensed quasar image separation (θ ∼
22′′.5) ever observed(see Figure 1 of Inada et al. 2006), and ii)
it exhibitsabsorption features in the blue wings of the C IV, N
V,and Lyα emission lines with ejection velocity of vej ≤
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2 Misawa et al.
1,000 km s−1, which could be the result of outflowing gasmoving
toward us from the central region. We call themProximity Absorption
Lines (PALs) throughout this pa-per. We define PALs as a
subcategory of Narrow Ab-sorption Lines (NALs) with ejection
velocity of vej ≤1,000 km s−1. We use this terminology throughout
thepaper to separate PALs from NALs with larger
ejectionvelocities.
Misawa et al. (2013) obtained high-resolution spectraof the
brighter two of the lensed images (images A andB) with the Subaru
telescope in 2010 February and foundseveral clear signs that the
origin of the PALs is indeedin the outflowing gas. First, they show
the signature ofpartial coverage, which means the absorbers do not
coverthe background flux source completely. There also existsa
clear difference in the absorption profiles between thespectra of
images A and B, which can be explained by ei-ther of the following
two scenarios: (a) time variability ofthe absorption features over
a time scale correspondingto the time delay between the two images
(time varia-tion scenario; Chartas et al. 2007)14, or (b) a
difference inthe absorption between the different sightlines of the
out-flowing wind (multi-sightline scenario; Chelouche 2003;Green
2006). However, with a single-epoch observationwe cannot
distinguish between these scenarios. Misawaet al. (2014b) performed
a second observation about fouryears (1514 days in the observed
frame) after the first ob-servation (which is longer than the time
delay betweenimages A and B, ∆tAB ∼ 744 days), and found that
thePALs were nearly stable and that most of the differencesbetween
images A and B still remained. This evidencesuggests a
multi-sightline scenario where the absorber’ssize should be smaller
than the physical distance betweenthe sightlines of the lensed
images, thus not covering bothsightlines. A possible explanation is
that there are anumber of small clumpy clouds in the outflowing
stream.Indeed, some of the outflowing gas is expected to consistof
small gas clouds (dcloud ≤ 10−3 pc) with very largegas densities
(ne ≥ 106 cm−3; Hamann et al. 2013; Joshiet al. 2014). Furthermore,
recent radiation-MHD simula-tions by Takeuchi et al. (2013)
reproduce variable clumpystructures with typical sizes of 20 times
the gravita-tional radius (Rg), corresponding to dcloud ∼ 5×10−4
pc,assuming a black-hole mass for SDSS J1029+2623 ofMBH ∼ 108.72 M�
(Misawa et al. 2013).
Such clumpy clouds can be examined more easilythrough narrow
absorption lines (NALs, hereafter) withlarge offset velocities from
the quasar because the cor-responding absorbers are (i) probably
smaller than thePAL absorbers and (ii) not so crowded in velocity
spaceas the PAL absorbers. Indeed, there are many NALsdetected in
the spectra of both images A and B ofSDSS J1029+2623. Their origin
is not only the out-flowing wind (intrinsic NALs, hereafter) but
also cos-mologically intervening gas such as foreground galaxiesand
the IGM (intervening NALs, hereafter). Althoughit has been
traditionally believed that many NALs thatfall within 5,000 km s−1
of the quasar emission redshift(termed associated absorption lines
or AALs) are physi-cally associated with the quasar (e.g., Weymann
et al.
14 The time delay between images A and B is ∆tAB ∼ 774 daysin
the sense of A leading B, while the time delay between images Band
C ∆tBC is only a few days (Fohlmeister et al. 2013).
1979), we can separate intrinsic NALs from interven-ing ones
more effectively by performing partial coverageanalysis. In order
to form a global picture of the outflow-ing wind, we need to
understand the physical conditionsof NAL absorbers (i.e., highly
accelerated gas) as well asPAL absorbers (i.e., weakly accelerated
gas).
In this paper, we present the results from our new
spec-troscopic observation of SDSS J1029+2623 taken withthe Very
Large Telescope (VLT), which enables us forthe first time to
identify intrinsic NALs in a high qualityspectrum of this object.
In §2, we describe the obser-vations and data reduction. The
methods used for ab-sorption line detection and covering factor
analysis areoutlined in §3. The results and discussion are
presentedin §4 and §5. Finally, we summarize our results in §6.
Weuse a cosmology with H0=70 km s−1 Mpc−1, Ωm=0.3,and ΩΛ=0.7
throughout the paper.
2. OBSERVATIONSWe acquired high resolution spectra of the
brightest
two of the three lensed images of SDSS J1029+2623, Aand B with V
= 18.72 and 18.67 mags, with the VLTusing the Ultraviolet and
Visual Echelle Spectrograph(UVES) in queue mode (ESO program
092.B-0512(A)).The observations were performed from 2014 January
28to February 26 (epoch E2, hereafter), which is ∼4 yearsafter the
first observation on 2010 February 10 (epochE1, hereafter; Misawa
et al. 2013), and ∼2 months beforethe third observation on 2014
April 4 (epoch E3, here-after; Misawa et al. 2014b) with Subaru
using the HighDispersion Spectrograph (HDS). We used a slit width
of1.′′2, corresponding to R ∼ 33,000, while Misawa et al.(2013,
2014b) took R ∼ 30,000 and 36,000 spectra usingSubaru/HDS. The
wavelength coverage is 3300–6600 Åin the 390/564 nm setting, which
covers the O VI, N V,Si IV, and C IV doublets as well as the Lyα
absorptionline at zabs ∼ zem. We also adopted 2×2 pixel binningin
both the spatial and dispersion directions to increasethe S/N
ratio. The total integration time is 26,670s andthe final S/N ratio
is about 23 pix−1 around 4700Å forboth images.
We reduced the data to extract the one-dimensionalspectra in a
standard manner using the UVES CommonPipeline Library (CPL release
6.6). We could not sepa-rate the third image (image C, V = 20.63)
from image Bcompletely because the typical seeing of our
observation(∼ 1.′′0–1.′′8) was comparable to the separation angle
be-tween images B and C (θ ∼ 1.′′85)15.
Table 1 gives a log of the current observation withVLT/UVES as
well as our past observations with Sub-aru/HDS, in which we list
the target name, date of obser-vation, telescope/instrument used,
spectral resolution,total exposure time, and signal-to-noise ratio
(S/N). TheS/N is evaluated around 4700 Å, close to the C IV
mini-BAL. In Figure 1, we show normalized spectra over thefull
wavelength range of our observations for images Aand B. These
spectra were binned every 0.5Å for displaypurposes, and the 1σ
errors are also shown.
3. DATA ANALYSIS
15 On the other hand, a flux contamination from the image Cis
almost negligible in the image B spectrum because the former ismuch
fainter than the latter.
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Multi-Sightline Observation of NALs 3
First, using the line detection code search, writ-ten by Chris
Churchill, we detect all absorption fea-tures whose confidence
level is greater than 5σ in thenormalized spectrum of each lensed
image. We thenidentify N V, C IV, and Si IV doublets in the
regionsfrom −1,000 km s−1 to 5,000 km s−1 (N V), from−1,000 km s−1
to 70,000 km s−1 (C IV), and from−1,000 km s−1 to 40,000 km s−1 (Si
IV) around the corre-sponding emission lines, with the maximum
velocity setin order to avoid the Lyα forest16. We also search for
theMg II doublet in the whole range of the spectra. Absorp-tion
troughs that are separated by nonabsorbed regionsare considered to
be separate lines. In total, 4 Mg II, 19C IV, 2 N V, and 7 Si IV
doublets are identified in the im-age A spectrum, while 3 Mg II, 22
C IV, 2 N V, and 7 Si IVdoublets are identified in the image B
spectrum. Theequivalent widths of both blue and red members of
dou-blets are measured for each line by integrating across
theabsorption profile and these are listed in Table 2. We
alsosearched for 10 single metal lines (O I λ1302, Si II λ1190,Si
II λ1193, Si II λ1260, Si II λ1527, Al II λ1671,C II λ1036, C II
λ1335, Si III λ1207, and C III λ1548)as well as Lyα and Lyβ and
detected about 200 lines atthe same redshift as the doublet lines.
These are sum-marized in Table ??. Other single lines or
unidentifiedlines are not shown in Figure 1 and Tables 1–?? even
ifthey are detected at a confidence greater than 5σ.
3.1. dN/dz AnalysisOne of the important properties of intrinsic
NALs is
a number density excess of high-ionization doublets perunit
redshift (i.e., dN/dz; Hamann et al. 1997a, and ref-erences
therein). In order to compare the dN/dz fromour spectra with those
from our previous study based on37 quasar spectra (Misawa et al.
2007a), we construct acomplete sample including only NALs whose
blue dou-blet members would be detected even in the lowest
S/Nspectrum in Misawa et al. (2007a). The correspondinglower limits
of rest-frame equivalent widths (EWs) areEWrestmin = 0.056 Å,
0.038 Å, and 0.054 Å for C IV, N V,and Si IV, respectively. Here,
the values of EWrestmin de-pend on the S/N ratio of the observed
spectrum as
EW restmin =−U2 + U
√U2 + 4(S/N)2(M2LM
−1c + ML)
2(S/N)2(1 + zabs)×∆λ(Å),
(1)where U is the confidence level of the EW defined asEW/σ(EW),
and ML and MC are the numbers of pixelsover which the equivalent
width and the continuum levelare determined (Young et al. 1979;
Tytler et al. 1987).Using equation (1), we confirm that the S/N of
our VLTspectra is always larger than the required values exceptfor
the region between λobs ∼ 4500 – 4525 Å (Figure 2).After removing
weak NALs with EWrest < EWrestmin, wehave 12 C IV, 2 N V, and 3
Si IV doublets in image Aspectrum and 11 C IV, 2 N V, and 3 Si IV
doublets in theimage B spectrum. We will call this the
“homogeneous”NAL sample, hereafter. Following Misawa et al.
(2007a),we also combined multiple NALs lying within 200 km s−1
16 Here, we define the velocity offset as positive for
blueshiftedNALs from the quasar emission redshift that is
determined fromMg II emission line (Inada et al. 2006).
of each other into a single NAL “system” because clus-tered
lines are probably not independent even if theyhave a
cosmologically intervening origin (e.g., Sargent,Steidel, &
Boksenberg 1988).
All identified doublets (including both the homoge-neous and
inhomogeneous NAL samples) are listed inTable 2, in which multiple
NALs within 200 km s−1 ofeach other are separated by horizontal
lines. The tablegives the ion name (ion), flux-weighted absorption
red-shift (zabs), ejection velocity (vej) supposing they orig-inate
in the outflow, rest frame EWs of blue and redmembers of the
doublet (EWrestb , EW
restr ), identification
number in Figure 1 (ID), reliability class of intrinsic
lines(described later), ionization class (described later),
andvelocity difference from the first doublet at the lowestredshift
in each absorption system (∆v). Table ?? sum-marizes other
information including the flux-weightedline width of each system on
a velocity scale, σ(v), asdefined in Misawa et al. (2007a), and
other transitionsthat are detected at the same redshift, as well as
the col-umn density (log N), Doppler parameter, b, and
coveringfactor, Cf , for each absorption component in the
system.
3.2. Partial Coverage AnalysisAmong several criteria, i) time
variability, ii) par-
tial coverage, and iii) line locking are the most
reliableproperties to distinguish intrinsic NALs from
interveningNALs (Barlow & Sargent 1997; Hamann et al. 1997a,
andreferences therein). When compared with broad intrin-sic
absorption lines, intrinsic NALs are less likely to vary(Misawa et
al. 2014a; Chen et al. 2015) and when theydo vary, their variation
amplitude is small (Wise et al.2004; Misawa et al. 2014a).
Therefore, the variabilitycriterion does not offer an efficient way
of identifying in-trinsic NALs.
Partial coverage analysis is quite useful for our spectrabecause
the resolving power is high enough to deblendNALs into multiple
components. Using the Voigt pro-file fitting code minfit (Churchill
1997; Churchill et al.2003), we deblended NALs into 86 and 91
components inimages A and B, respectively. We do not include the Si
IVNAL at zabs = 1.8909 because the blue and red membersof the
doublet are both blended with other lines. Withminfit, we fit each
NAL profile using the redshift (z),column density (log N in cm−2),
Doppler parameter (bin km s−1), and covering factor (Cf) as free
parameters.The covering factor (Cf) is the fraction of photons
fromthe background source that pass through the absorber. Ifthe
background source is uniformly bright, then Cf alsorepresents the
fraction of the background source (i.e.,the continuum source and/or
broad emission line regions,BELRs) that is occulted by foreground
absorbers alongour sightline. If Cf is less than unity, it is
likely thatthe absorbers are part of a quasar outflow because
cos-mologically intervening absorbers like substructures
inforeground galaxies and the IGM are less likely to haveinternal
structures as small as a size of the backgroundflux sources (e.g.,
Wampler et al. 1995; Barlow & Sargent1997). The covering factor
is evaluated in an unbiasedmanner as
Cf =(Rr − 1)2
1 + Rb − 2Rr, (2)
where Rb and Rr are the residual (i.e., unabsorbed) fluxes
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4 Misawa et al.
of the blue and red members of a doublet in the nor-malized
spectrum (c.f., Hamann et al. 1997b; Barlow &Sargent 1997;
Crenshaw et al. 1999). If minfit givesunphysical covering factors
for some components, e.g.,negative or greater than 1, we rerun the
code assumingCf = 1 only for those components because the Cf
valuesare very sensitive to continuum level errors, especiallyfor
full coverage doublets (Misawa et al. 2005). In addi-tion to the
fitting method above, we evaluate Cf valuesfor each pixel as
Ganguly et al. (1999) did (pixel-by-pixelmethod). The fitting
results by both methods are shownin Figure 3 and the fit parameters
by the fitting methodare summarized in Table ??. We have confirmed
thatthe Cf values provided by the two methods are in goodagreement
with each other.
4. RESULTS4.1. Narrow Absorption Lines (NALs)
Using our NAL sample toward the lensed images ofSDSS J1029+2623,
we perform several statistical anal-yses. In these analyses, in
order to avoid any possiblebiases we do not include the two C IV
NALs at zabs ∼1.9322 and 1.9788 that are covered in the Subaru
spec-trum (Misawa et al. 2013) but not covered by our VLTdata.
4.1.1. dN/dz analysisIn Table 4, we summarize the number density
of homo-
geneous NAL systems per unit redshift (dN/dz) or perunit
velocity offset from the quasar (dN/dβ) for C IV,N IV, and Si IV,
along with the Poisson noise in thesequantities (Gehrels 1986). All
systems are also classifiedinto one of two categories according to
the offset veloc-ity from the quasar; associated absorption lines
(AALs)with vej ≤ 5,000 km s−1, and non-AALs with vej >5,000 km
s−1, following Misawa et al. (2007a). We foundthat the dN/dz values
for C IV, N V, and Si IV toward thisone quasar, SDSS J1029+2623,
are larger than the aver-age values in the larger sample of Misawa
et al. (2007a)by factors of ∼3, ∼6, and ∼2, respectively, although
thisenhancement is not statistically significant because of
thesmall number of NALs in our spectra. Because Misawa etal.
(2007a) discovered that at least ∼20% of C IV NALsoriginate from
winds based on partial coverage analysis,statistically we expect to
detect two or more intrinsicC IV NALs among ∼10 homogeneous C IV
NALs in thespectra of images A and B.
4.1.2. Intrinsic or Intervening NALsHigh-velocity NALs
blueshifted with vej > 1000 km s−1
are expected to be outside of the range of velocities whereBELs
are found, and thus, they absorb mostly continuumlight. The
existence of partial coverage in high-velocityNALs suggests that
the size of absorbers is comparableto or smaller than the continuum
source (i.e., dcloud ≤Rcont). Following Misawa et al. (2007a), we
separateall NALs (including those in the inhomogeneous sample)into
three classes (classes-A, B, and C) based on partialcoverage
analysis, where class-A includes NALs most re-liably classified as
intrinsic while class-C includes NALsthat are consistent with full
coverage or that cannot beclassified. Class-B contains NALs that
show line-locking,which is a signature of a radiatively driven
outflowing
wind and is only detectable if our sightline is approxi-mately
parallel to the gas motion, as often seen in NALs(e.g., Benn et al.
2005; Bowler et al. 2014). Class-Balso contains systems that have
tentative evidence forpartial coverage. As a result, 4 C IV NALs
(includingPALs) are classified as intrinsic (two class-A and
twoclass-B) among the 12 C IV NALs in the homogeneoussample from
the spectrum of image A, while 3 C IV NALsare classified as
intrinsic (two class-A and one class-B)among 11 NALs in the
spectrum of image B. The frac-tion of intrinsic NALs (27 – 33%) is
somewhat largerthan the average value of ∼20% (Misawa et al.
2007a),although our sample size is small. If we include the
in-homogeneous sample, 5 C IV NALs are classified as 3class-A and 2
class-B among 19 NALs toward image A,while 9 out of 22 C IV NALs
are classified into 4 class-Aand 5 class-B NALs toward image B. In
addition to in-trinsic C IV NALs, we detected two class-B Si IV
NALsonly toward image A in homogeneous sample, and threeclass-B Si
IV NALs in each of the image A and B spectraafter including systems
from the inhomogeneous sample.It is also noteworthy that we detect
a large number ofline-locked NALs: 2 C IV and 3 Si IV NALs in image
Aand 5 C IV and 3 Si IV NALs in image B, while only fivesystems are
line-locked among 138 homogeneous NALstoward 37 quasars (Misawa et
al. 2007a). This resultstrongly suggests that our sightline toward
the centralsource is almost parallel to the outflowing
streamline.
4.1.3. Ionization Conditions
The outflowing winds in the vicinity of the flux sourceare
probably more highly ionized than most interveningabsorbers due to
strong UV radiation from the contin-uum source, although it depends
on the gas density ofthe absorbers. Indeed, a high ionization state
has beenused as one indicator of the intrinsic properties of
ab-sorbers (Hamann et al. 1997a, and references therein).Broad
absorption lines (BALs) are often classified intothree categories
according to their ionization level: high-ionization BALs (HiBALs),
low-ionization BALs (LoB-ALs), and extremely low-ionization BALs
showing Fe IIlines (FeLoBALs) (Weymann et al. 1991). A similar
clas-sification has also been performed for NALs (Bergeron etal.
1994; Misawa et al. 2007a). Motivated by the liter-ature, we
classify our NALs into three categories, basedon the detection of
absorption lines in low (ionization po-tential; IP < 25 eV),
intermediate (IP = 35 – 50 eV), andhigh (IP > 60 eV) ionization
levels17. Interestingly, someclass-A NAL systems include low
ionization lines (see Ta-ble 2), which suggests that intrinsic NAL
absorbers havemultiple phases with different ionization states, as
notedin Misawa et al. (2007a).
4.1.4. Similarities in NALs between Sightlines
Here, we present a new method of identifying intrin-sic NALs by
exploiting our multi-sightline observation.If NALs with similar
line profiles are detected at thesame redshift toward two
sightlines, the corresponding
17 An important caveat here is that we do not necessarily
de-tect all absorption lines because of the detection limits due to
linestrength, observed wavelength coverage, and line blending
(e.g., inLyα forest).
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Multi-Sightline Observation of NALs 5
absorber must have a size larger than the physical dis-tance
between the two sightlines. The absorber also can-not have any
internal structures on the scale of the sight-line separation.
Although foreground galaxies and IGMstructures also can cover both
sight lines (whose physi-cal separation is ∼kpc or ∼Mpc scale),
they usually havesignificant internal velocity structures on those
scales, asoften seen in the spectra of lensed quasars (e.g.,
Ellisonet al. 2004). Only intrinsic absorbers can satisfy the
re-quirement of having very similar profiles because theirsizes can
be larger than the sightline separation (e.g.,sub-parsec scale) if
they are at a small distance from theflux source (e.g., r < 1
kpc). Based on the ejection ve-locity distribution of class-A, B,
and C NALs (Figure 4),in Figure 5 we summarize the distribution of
velocity dif-ferences between NALs and PALs in the two
sightlines(∆v) for systems within ∆v ≤ 200 km s−1 between thetwo
sightlines. The distribution is almost uniform up to∆v ∼ 200 km s−1
with a clear peak near ∆v ∼ 0 km s−1.Among eight NAL pairs with ∆v
≤ 10 km s−1, four areC IV and N V PALs at zabs ∼ zem, which we will
discusslater. The other four NAL pairs are C IV NALs at zabs∼
1.8909, 2.1349, and 2.1819, and a Si IV pair at zabs∼ 1.8909.
Although the velocity shift is very small forthese NAL pairs, their
line profiles are clearly different ascompared in Figure 6. This
means our two sightlines gothrough different absorbers or different
regions of a sin-gle absorber. In either event, we cannot conclude
thatthese are intrinsic NALs based only on this analysis. Onthe
other hand, it is intriguing that no NAL pairs thatare classified
into class-A/B have a common ejection ve-locity or line profile.
For example, the C IV NALs atzabs = 1.7652 toward image A and at
zabs = 1.7650 to-ward image B are both classified as class-A NALs.
Al-though their ejection velocities are very close each other,their
line centers and profiles are obviously different, asshown in
Figure 7. We also note that the difference is re-markable in all
three epochs (see Figure 8). This meansthe multi-sightline scenario
(i.e., that two sightlines passthrough different regions of the
outflow) is also applica-ble for intrinsic NALs with large ejection
velocity as wellas for PALs as already confirmed in Misawa et al.
(2013,2014b).
4.1.5. Time Variability of NALs
Because of the lower data quality (S/N ∼ 10 pixel−1)and narrower
effective wavelength coverage of the Sub-aru/HDS spectra taken in
epochs E1 and E3, we cannotmonitor NALs for time variability
analysis with only afew exceptions. As an example, we compare
spectra ob-tained at three epochs around the strong C IV NALs
atzabs = 1.8909–1.9138 (ID = 35–44) in image A and C IVNALs at zabs
= 1.8909–1.9119 (ID = 41–48) in image Bas shown in Figure 9. These
NALs are obviously not vari-able, which is consistent with the past
result that NALswith large ejection velocities are rarely variable
(Chen etal. 2015).
4.2. Proximity Absorption Lines (PALs)The absorption line group
at zabs ∼ zem with an ejec-
tion velocity of vej < 1000 km s−1 has already been ob-served
twice in 2010 February (epoch E1) and 2014 April(epoch E3) with
Subaru/HDS. Its origin is probably in
the outflowing gas because: i) there is evidence for par-tial
coverage (e.g., there exists a clear residual flux at thebottom of
the Lyα and N V absorption lines even thoughthey appear to be
saturated.), ii) the profiles are vari-able, and iii) the profiles
show signatures of line-locking(Misawa et al. 2013, 2014b). The
most important resultfrom these past observations is that the
absorption pro-files of the Lyα, N V, and C IV PALs in the spectra
ofimages A and B are clearly different, especially for linesat vej
< 0 km s−1 (see Figure 10). There are at least threepossible
origins for the difference: a) a micro-lensing ef-fect, b) time
delay between the images, and c) differentabsorber structure along
the different sightlines. Amongthese, the first idea is immediately
rejected because thelensed images show a common ratios between the
radio,optical, and X-ray fluxes (Ota et al. 2012; Oguri et
al.2012), which is not expected for micro-lensing. We canalso
reject the time delay effect because the variability isalmost
negligible between epochs E1 and E3 (Misawa etal. 2014b). A
difference in column density between thetwo sightlines is the only
acceptable explanation. To ourknowledge, this is the first time
that an outflowing windhas been observed along multiple sightlines.
Hereafter,we call the PALs at vej < 0 km s−1 (showing
sightlinedifference) narrow PALs and those at vej > 0 km
s−1(showing similar line profiles between sightlines) broadPALs
(see Figure 10).
Our observation with VLT/UVES not only gives anadditional epoch
for monitoring the PALs but enables usto study the detailed
velocity structure of PALs usinghigher quality spectra with a S/N
ratio double that ofthe past observations with Subaru. We first
confirm theline-locking pattern in velocity plots of the C IV PAL
asshown in Figure 11, which was already noted in Misawaet al.
(2013). Like the other NAL absorbers, the PALabsorbers also appear
to be outflowing almost parallelto our sightline. We also reconfirm
that the C IV PALsbecame shallower (i.e., decreasing in equivalent
width)over a large velocity range of the profile between epochsE1
and E2/E3 (see Figure 11) at ∆trest ∼1.3 years inthe quasar
rest-frame. However, these lines are almoststable on the shorter
time scales of ∆trest ∼0.05 yearsbetween epochs E2 and E3. The
broad spectral coverageof the VLT/UVES spectra allows us to detect
for thefirst time the O VI doublet corresponding to the PALabsorber
(see Figure 10). There is also a hint of the Si IVdoublet detected,
but it appears blended with other linesat lower redshift.
4.2.1. Comparison of Covering Factors
In addition to line profiles and strengths, we also com-pare
covering factors for the clean part of the C IV andN V PALs in the
three epochs. The fitting parameters tothe PALs in epoch E2 with
minfit are summarized in Ta-ble ??. The total column densities of C
IV and N V PALsafter summing all Voigt components are
log(NNV/cm−2)= 15.62 and log(NCIV/cm−2) = 15.90 in image A and16.04
and 15.89 in image B spectrum. These values areall consistent with
the corresponding values that we mea-sured in epoch E1 (Misawa et
al. 2013) with differencesof a factor of ≤ 2. Because all PALs have
small offsetvelocities and are located on the BELs in the
spectra,we should consider the BELRs as well as the contin-
-
6 Misawa et al.
uum source as the background flux source. Because theC IV PAL is
partially self-blended (i.e., blending of theblue members of one
doublet with the red member ofanother doublet), we can compare
covering factors effec-tively only for the narrow PALs at vej ∼
−100–0 km s−1(corresponding to ∆v ∼ 400–500 km s−1 in Figure
12),for which self-blending is negligible18.
We show the fitting results for the PALs in epoch E2in Figure 12
and Table ??. The average covering fac-tors of C IV and N V at vej
∼ −100–0 km s−1 (i.e., ∆v∼ 400–500 km s−1 in Figure 12) are Cf =
0.47±0.03and 0.58±0.05 toward image A, and Cf = 0.23±0.02
and0.39±0.08 toward image B. These values are all consis-tent with
the corresponding values in epoch E1 towardimage A (Cf = 0.47±0.05
and 0.61±0.07) and image B(Cf ∼ 0.2 and 0.35±0.05)19 and in epoch
E3 toward im-age A (Cf = 0.45±0.09 and 0.54±0.09) and image B (Cf=
0.20±0.05 and 0.34±0.19). Thus, covering factors arenot variable at
least on a timescale of ∆trest ∼ 1.3 years.
The N V PALs all have larger Cf values than that forC IV, which
is consistent with past results that higherionization transitions
tend to have larger coverage frac-tions (e.g., Petitjean &
Srianand 1999; Srianand & Pe-titjean 2000; Misawa et al. 2007a;
Muzahid et al. 2015).This result suggests that i) the size (i.e.,
distance fromthe central black hole) of the N V BELR is smaller
thanthat of the C IV BELR, and/or ii) the size of the N Vabsorbers
is larger than that of the C IV absorbers. It isalso interesting
that the PALs in the image A spectrumalways have larger Cf values
than those in the image Bspectrum, which is additional evidence for
variations inthe structure along multiple sightlines.
5. DISCUSSION5.1. Velocity anisotropies in NAL absorbers
Line-locking is seen in both NALs and PALs, thus weare likely to
be observing the quasar almost along thedirection of the outflow.
Nonetheless, we discovered avelocity difference between the two
sightlines (see Ta-ble 2). Given the redshifts of the lens (zl =
0.58; Oguriet al. 2008) and the source (zs = 2.197) the
separationangle of the light rays that form images A and B, as
seenfrom the source20, is θ′ ∼14.′′6. This velocity
gradientsuggests that the outflowing wind has internal
velocityanisotropies on a scale of ∼1 km s−1 arcsec−1 on aver-age.
Indeed, the hydrodynamic simulations of Proga &Kallman (2004)
show this type of internal velocity vari-ations. A recent
radiation-MHD simulation by Takeuchiet al. (2013) also reproduced
such velocity variations over
18 Negative ejection velocity for these components could be
dueto our underestimation of these values because the emission
redshiftis determined from broad UV emission lines, as done for
this quasarby Inada et al. (2006), which are systematically
blueshifted fromthe systemic redshift that is measured by narrow,
forbidden lines(see, e.g., Corbin 1990; Tytler & Fan 1992;
Brotherton et al. 1994;Marziani et al. 1996) by about 260 km
s−1.
19 Because no absorption component was used for C IV PAL atvej ≤
0 km s−1 in the epoch E1 spectrum (Misawa et al. 2013), weadopt an
average line depth for this region as a covering factor.
20 The separation angle as seen by the source is given by θ′
= (Dol/Dsl) × θ, where θ is the observed separation angle of
theimages (22.′′5) and Dol and Dsl = ((1 + zs)/(1 + zl)) × Dls
areangular diameter distances from the observer to the lens and
fromthe source to the lens, respectively.
a typical spatial scale of ∼ 5×10−4 pc. This is consistentwith
the size of NAL absorbers, which is also compara-ble to the size of
the continuum source (∼ 2.5×10−4 pc;Misawa et al. 2013). However,
we should note that thevelocity variations in the simulations are
found in theinner part of the wind at distances of ∼50Rg from
thecenter.
The velocity distribution of intrinsic NALs that areclassified
into Class-A or B appears to cluster aroundvalues of vej ∼ 59,000,
43,000, and 29,000 km s−1, exceptfor two intrinsic NALs at vej ∼
49,500 km s−1 (class-A)and ∼ 8,500 km s−1 (class-B) in the image B
spectrum(Figure 4). These clustering patterns are reminiscent ofthe
filamentary structures obtained by numerical simu-lations (e.g.,
Proga, Stone, & Kallman 2000). If thesepatterns are indeed due
to filamentary structures, thereshould exist some velocity
anisotropies within them. Ve-locity dispersions in the three
intrinsic NAL clusters areδv ∼ 900, 260, and 1200 km s−1
respectively, which cor-respond to about 1.6%, 0.6%, and 4.0% of
their averageejection velocity.
5.2. Ionization condition in PAL absorbersThe Lyα, C IV, and N V
PALs have been monitored
at three epochs (E1, E2, and E3) between 2010 Febru-ary and 2014
April. Between epochs E1 and E2/E3,C IV PALs show a clear variation
in their strength (i.e.,depth). There are several possible reasons
for this timevariability: (a) gas motion across our line of sight
(e.g.,Hamann et al. 2008; Gibson et al. 2008; Muzahid et al.2015),
(b) changes in the ionization state of the absorber(e.g., Hamann et
al. 2011; Misawa et al. 2007b), and (c)redirection of photons
around the absorber by scatter-ing material (e.g., Lamy &
Hutsemékers 2004; Misawaet al. 2010). Among these, the first
scenario can be re-jected because all absorption components in the
C IVPAL vary in concert, which requires the implausible sit-uation
in which all clouds cross our sightline simulta-neously (c.f.
Misawa et al. 2007b). The third scenariois also less likely because
it requires a variation in thecovering factor while the Cf values
remain almost sta-ble both in C IV and N V PALs between epochs E1
andE2/E3. Thus, only the scenario involving a change inionization
state deserves further investigation. This sce-nario is further
separated into two variants: i.e., C3+ions are ionized to C4+ or
they recombine to C2+. Bothvariants of this scenario can explain
the decreasing EWof the C IV PALs. Without knowing an absorber’s
ion-ization parameter21, we cannot tell which one is morelikely. If
the latter variant applies, we can place con-straints on the
electron density and the distance fromthe ionizing photon source by
the same prescription asused in Narayanan et al. (2004), taking the
variabilitytime scale as an upper limit to the recombination
time.Based on the observation that the C IV PALs vary be-tween
epochs E1 and E3 over ∆tobs = 1514 days (i.e.,∆trest = 474 days)22
we can place a lower limit on the
21 The ionization parameter U is defined as the ratio of
hydrogenionizing photon density (nγ) to the electron density
(ne).
22 We compare spectra in epochs E1 and E3 instead of epochsE1
and E2 because the E2 observation spans the time range 2014January
28 to February 26, which gives an additional uncertaintyfor
measuring the variation time scale.
-
Multi-Sightline Observation of NALs 7
electron density of the absorber as ne > 8.7× 103 cm−3,and an
upper limit on the distance from the flux sourceas r < 620 pc,
assuming U ∼ 0.02, the value at whichthe C IV and N V ions are
close to the optimal ionizationstates for those elements (e.g.,
Hamann et al. 1995).
5.3. Global Picture of the Outflow fromSDSS J1029+2623
In Table 5, we summarize the physical properties ofbroad PALs,
narrow PALs, and intrinsic NALs. We alsopresent a possible geometry
of the outflow along our twosightlines in Figure 13 based on our
previous constraints.
First, we see almost the same absorption profiles ofLyα, N V,
and C IV PALs in the two lensed images ex-cept for a clear
difference in the narrow PALs at vej ∼−100–0 km s−1. We also
confirm that none of the in-trinsic NALs have common absorption
profiles betweenthe images. These results suggest that the size of
thebroad PAL absorbers are larger than the projected sepa-ration
between sightlines at the distance of the absorbers,rθ, while the
narrow PAL absorbers and NAL absorbershave sizes smaller than rθ.
Such common absorption pro-files are, however, observable
regardless of the absorber’ssize, if their distance from the flux
source is smaller thanthe boundary radius rb at which the two
sightlines oflensed images become fully separated with no
overlap(Misawa et al. 2013). The boundary distance is ∼3.5 pcfor
SDSS J1029+2623 if only the continuum source iscounted. If we also
consider the BELR (whose size isestimated to be ∼0.09 pc)23 as the
background source,rb would be ∼1200 pc (see Figure 13).
We can also place constraints on the absorber sizebased on
partial covering analysis. Intrinsic NALs withlarge ejection
velocities have partial coverage, althoughthey absorb only the
continuum photons. This meanstheir physical scale is comparable to
or smaller than thesize of the continuum source, dcloud ≤ 2.5×10−4
pc. Onthe other hand, broad PAL absorbers cover almost en-tirely
both the BELR and the continuum source, whichmeans the size of the
absorbers as a whole is compara-ble to or larger than the BELR
size, ≥ 0.09 pc. NarrowPAL absorbers may consist of a number of
small clumpyclouds because they show partial coverage.
In our VLT/UVES spectra, we detected high-ionization transitions
like O VI and N V in the PALsystems, while the intrinsic NAL
systems are in variousionization states, with or without
high-ionization tran-sitions, as already noted in the literature
(e.g., Misawaet al. 2007a; Ganguly et al. 2013). Some C IV NAL
ab-sorbers also show N V transitions, while others do not.Because
Lyα and N V in the PAL system are less vari-able than C IV and
because N V has larger covering factorthan C IV, the cross-section
of Lyα and N V should belarger than that of C IV. PAL absorbers
with strong O VIlines are probably located much closer to the
ionizing fluxsource than NAL absorbers, although this conclusion
de-pends on the density of the absorber.
It is well known that both broad and narrow absorptionlines at
zabs ∼ zem tend to vary (Wise et al. 2004; Misawaet al. 2014a),
while NALs with large ejection velocitiesare rarely variable (e.g.,
Chen et al. 2015). Indeed, the
23 This is calculated by Misawa et al. (2013) based on the
em-pirical equation in McLure & Dunlop (2004).
PALs in our spectra are variable, while most of the C IVNALs are
probably stable between the three epochs, aswe observed for a few
strong C IV NALs. Misawa etal. (2014a) suggest that broader
absorption lines like thebroad PALs can vary mainly due to a change
in theirionization state while narrow absorption lines like
narrowPALs and NALs vary primarily due to the gas motiontransverse
to our sightlines. The gas motion scenariocould explain why narrow
PALs are variable but high-velocity NALs are not. Based on the
dynamical model ofMurray et al. (1995) and more recent
investigations (e.g.,Misawa et al. 2005; Hall et al. 2011), the
absorbers atlarger distance from the center have small transverse
(i.e.,orbital) velocities compared to their radial velocities.
Ifintrinsic NALs lie at larger distances than narrow PALs,their
small transverse velocities would rarely lead to timevariability,
while the large transverse velocities of narrowPALs can lead to
time variability more frequently.
6. SUMMARYIn this study, we performed a spectroscopic
observa-
tion for images A and B of the gravitationally lensedquasar SDSS
J1029+2623, and monitored the absorp-tion profiles in these spectra
as well as in the previ-ous two observations. Using high quality
spectra takenwith VLT/UVES, we detected intrinsic narrow
absorp-tion lines (NALs) as well as broader, proximity absorp-tion
lines (PALs), and fit models to the line profiles.Based on the
results of our multi-sightline spectroscopy,we discuss a possible
geometry and internal structure ofthe outflowing wind along our
sightlines. Our main re-sults are as follows.
We detected 66 NALs, of which 24 are classifiedas intrinsic NALs
(physically associated with thequasar) based on partial coverage
analysis.
Class-A and B NALs cluster at vej ∼ 59,000,43,000, and 29,000 km
s−1, which is reminiscent ofthe filamentary structures that are
often obtainedin numerical simulations.
Our multiple sightline observation suggests thatthe size of the
broad PAL absorbers are larger thanthe projected distance between
sightlines (rθ) whilethe narrow PAL absorbers and intrinsic NAL
ab-sorbers have sizes smaller than rθ if their radialdistances are
greater than the boundary distance.
While PAL systems show only high ionization tran-sitions,
including O VI, intrinsic NAL systems showa wide range of
ionization conditions with andwithout low ionization transitions
like O I, Al II,and Si II, as noted in the literature.
No class-A/B NALs (i.e., candidates for intrinsicNALs) have
common absorption profiles in the twolensed images, which means
that the outflow hasan internal velocity structure whose typical
spatialscale is smaller than the physical distance betweenthe
sightlines (i.e., ≤ rθ).
Short-time variation in the PALs is probably dueto a change in
the ionization state of the gas. If thisis the case, we can place a
lower limit on the gas
-
8 Misawa et al.
density as ne ≥ 8.7× 103 cm−3 and an upper limiton the
absorber’s distance from the flux source asr ≤ 620 pc.
Based on our best knowledge, we present a possiblegeometry of
the outflow along our two sightlines,in which we identify different
structures in the out-flowing wind that can produce, respectively,
broadPALs, narrow PALs, and NALs with large ejectionvelocities.
For further investigations of the outflow’s internalstructure,
especially in the transverse direction, weshould perform the same
observations for image C ofSDSS J1029+2623. We also aim to observe
several lensedquasars with smaller separation angles (θ ∼ 2′′) by a
sin-gle massive galaxy to examine ∼10 times finer internalstructure
in an outflow, as already mentioned in Misawaet al. (2014b).
We thank the anonymous referee for comments thathelped us
improve the paper. We would like to thank
Masamune Oguri, Poshak Gandhi, and Chris Cullitonfor their
valuable comments. We also would like tothank Christopher Churchill
for providing us with theminfit and search software packages. The
researchwas supported by the Japan Society for the Promotionof
Science through Grant-in-Aid for Scientific Research15K05020, JGC-S
Scholarship Foundation, and partiallysupported by MEXT Grant-in-Aid
for Scientific Researchon Innovative Areas (No. 15H05894). CS
acknowledgessupport from CONICYT-Chile through Becas Chile74140006.
FEB acknowledges support from CONICYT-Chile (Basal-CATA
PFB-06/2007, FONDECYT Regular1141218, ”EMBIGGEN” Anillo ACT1101)
and the Min-istry of Economy, Development, and Tourism’s
Millen-nium Science Initiative through grant IC120009, awardedto
The Millennium Institute of Astrophysics, MAS. JCCand ME
acknowledge support from the National ScienceFoundation through
award AST-1312686.
REFERENCES
Arav, N., Borguet, B., Chamberlain, C., Edmonds, D.,
&Danforth, C. 2013, MNRAS, 436, 3286
Benn, C. R., Carballo, R., Holt, J., et al. 2005, MNRAS, 360,
1455Barlow, T. A., & Sargent, W. L. W. 1997, AJ, 113,
136Bergeron, J., et al. 1994, ApJ, 436, 33Blandford, R.D. &
Parne, D.G., 1982, MNRAS, 199, 883Bowler, R. A. A., Hewett, P. C.,
Allen, J. T., & Ferland, G. J.
2014, MNRAS, 445, 359Brotherton, M. S., Wills, B. J., Steidel,
C. C., & Sargent,
W. L. W. 1994, ApJ, 423, 131Chartas, G., Eracleous, M., Dai, X.,
Agol, E., & Gallagher, S.
2007, ApJ, 661, 678Chen, Z.-F., Gu, Q.-S., Chen, Y.-M., &
Cao, Y. 2015, MNRAS,
450, 3904Chelouche, D. 2003, ApJ, 596, L43Churchill, C. W.,
Vogt, S. S., & Charlton, J. C. 2003, AJ, 125, 98Churchill, C.
W. 1997, Ph.D. Thesis, Univ. California, Santa CruzCorbin, M. R.
1990, ApJ, 357, 346Crenshaw, D. M., Kraemer, S. B., Boggess, A.,
Maran, S. P.,
Mushotzky, R. F., & Wu, C.-C. 1999, ApJ, 516, 750Gehrels, N.
1986, ApJ, 303, 336Dorodnitsyn, A. V. 2009, MNRAS, 393, 1433Dunn,
J. P., Bautista, M., Arav, N., et al. 2010, ApJ, 709, 611Ellison,
S. L., Ibata, R., Pettini, M., et al. 2004, A&A, 414, 79Elvis,
M. 2000, ApJ, 545, 63Emmering, R.T., Bladford, R.D., &
Shlosman, I., 1992, ApJ, 385,
460Everett, J. E., 2005, ApJ, 631, 689Fohlmeister, J., Kochanek,
C. S., Falco, E. E., et al. 2013, ApJ,
764, 186Foltz, C., Wilkes, B., Weymann, R., & Turnshek, D.
1983, PASP,
95, 341Gabel, J.R., Arav, N., & Kim, T.-S. 2006, ApJ, 646,
742Ganguly, R., Lynch, R. S., Charlton, J. C., et al. 2013,
MNRAS,
435, 1233Ganguly, R., Bond, N. A., Charlton, J. C., et al. 2001,
ApJ, 549,
133Ganguly, R., Eracleous, M., Charlton, J. C., & Churchill,
C. W.
1999, AJ, 117, 2594Gibson, R. R., Brandt, W. N., Schneider, D.
P., & Gallagher,
S. C. 2008, ApJ, 675, 985Green, P. J. 2006, ApJ, 644, 733Hall,
P. B., Brandt, W. N., Petitjean, P., et al. 2013, MNRAS,
434, 222Hall, P. B., Anosov, K., White, R. L., et al. 2011,
MNRAS, 411,
2653Hamann, F., Chartas, G., McGraw, S., et al. 2013, MNRAS,
435,
133Hamann, F., Kanekar, N., Prochaska, J. X., et al. 2011,
MNRAS,
410, 1957Hamann, F., Kaplan, K. F., Rodŕıguez Hidalgo, P.,
Prochaska,
J. X., & Herbert-Fort, S. 2008, MNRAS, 391, L39Hamann, F.,
& Sabra, B. 2004, AGN Physics with the Sloan
Digital Sky Survey, 311, 203
Hamann, F., Barlow, T. A., Junkkarinen, V., & Burbidge, E.
M.1997a, ApJ, 478, 80
Hamann, F., Barlow, T. A., & Junkkarinen, V. 1997b, ApJ,
478,87
Hamann, F., Barlow, T. A., Beaver, E. A., et al. 1995, ApJ,
443,606
Inada, N., Oguri, M., Morokuma, T., et al. 2006, ApJ, 653,
L97Jannuzi, B. T., Hartig, G. F., Kirhakos, S., et al. 1996, ApJ,
470,
L11Joshi, R., Chand, H., Srianand, R., & Majumdar, J.
2014,
MNRAS, 442, 862Konigl, A., & Kartje, J. F. 1994, ApJ, 434,
446Kurosawa, R. & Proga, D. 2009, ApJ, 693, 1929Lamy, H., &
Hutsemékers, D. 2004, A&A, 427, 107Marziani, P., Sulentic, J.
W., Dultzin-Hacyan, D., Calvani, M., &
Moles, M. 1996, ApJS, 104, 37McLure, R. J., & Dunlop, J. S.
2004, MNRAS, 352, 1390Misawa, T., Charlton, J. C., & Eracleous,
M. 2014a, ApJ, 792, 77Misawa, T., Inada, N., Oguri, M., et al.
2014b, ApJ, 794, L20Misawa, T., Inada, N., Ohsuga, K., et al. 2013,
AJ, 145, 48Misawa, T., Kawabata, K. S., Eracleous, M., Charlton, J.
C., &
Kashikawa, N. 2010, ApJ, 719, 1890Misawa, T., Charlton, J. C.,
Eracleous, M., Ganguly, R., Tytler,
D., Kirkman, D., Suzuki, N., & Lubin, D. 2007a, ApJS, 171,
1Misawa, T., Eracleous, M., Charlton, J. C., & Kashikawa,
N.
2007b, ApJ, 660, 152Misawa, T., Eracleous, M., Charlton, J.C.,
& Tajitsu, A., 2005,
ApJ, 629, 115Murray, N., Chiang, J., Grossman, S. A., &
Voit, G. M., 1995,
ApJ, 451, 498Muzahid, S., Srianand, R., Charlton, J., &
Eracleous, M. 2015,
arXiv:1509.07850Muzahid, S., Srianand, R., Arav, N., Savage, B.
D., & Narayanan,
A. 2013, MNRAS, 431, 2885Narayanan, D., Hamann, F., Barlow, T.,
Burbidge, E.M., Cohen,
R.D., Junkkaribeb, V., & Lyons, R., 2004, ApJ, 601,
715Nestor, D., Hamann, F., & Rodriguez Hidalgo, P. 2008,
MNRAS,
386, 2055Nomura, M., Ohsuga, K., Wada, K., Susa, H., &
Misawa, T.
2013, PASJ, 65,Oguri, M., Schrabback, T., Jullo, E., et al.
2012, arXiv:1209.0458Oguri, M., Ofek, E. O., Inada, N., et al.
2008, ApJ, 676, L1Ota, N., Oguri, M., Dai, X., et al. 2012,
arXiv:1202.1645Petitjean, P. & Srianand, R., 1999, A&A,
345, 73Proga, D., & Kallman, T. R. 2004, ApJ, 616, 688Proga,
D., Stone, J. M., & Kallman, T. R., 2000, ApJ, 543, 686Sargent,
W.L.W., Boksenberg, A., & Steidel, C.C., 1988, ApJS,
68, 539Springel, V., Di Matteo, T., & Hernquist, L. 2005,
ApJ, 620, L79Srianand, R. & Petitjean, P., 2000, A&A, 357,
414Takeuchi, S., Ohsuga, K., & Mineshige, S. 2013, PASJ, 65,
88Tytler, D., & Fan, X.-M. 1992, ApJS, 79, 1Tytler, D.,
Boksenberg, A., Sargent, W. L. W., Young, P., &
Kunth, D., 1987, ApJS, 64, 667
-
Multi-Sightline Observation of NALs 9
Vestergaard, M., 2003, ApJ, 599, 116Wampler, E. J., Chugai, N.
N., & Petitjean, P. 1995, ApJ, 443,
586Weymann, R. J., Morris, S. L., Foltz, C. B., & Hewett, P.
C.
1991, ApJ, 373, 23Weymann, R. J., Williams, R. E., Peterson, B.
M., & Turnshek,
D. A. 1979, ApJ, 234, 33
Wise, J. H., Eracleous, M., Charlton, J. C., & Ganguly, R.
2004,ApJ, 613, 129
Young, P. J., Sargent, W. L. W., Boksenberg, A., Carswell, R.
F.,& Whelan, J. A. J., 1979, ApJ, 229, 891
-
10 Misawa et al.
TABLE 1Log of Observations
Target Obs Date Instrument R Texp S/Na Referenceb
(sec) (pix−1)
SDSS J1029+2623 A 2010 Feb 10 Subaru/HDS 30000 14400 13 12014
Jan 28 – Feb 3 VLT/UVES 33000 26670 23 2
2014 Apr 4 Subaru/HDS 36000 11400 14 3SDSS J1029+2623 B 2010 Feb
10 Subaru/HDS 30000 14200 13 1
2014 Feb 4 – 26 VLT/UVES 33000 26670 23 22014 Apr 4 Subaru/HDS
36000 11400 14 3
a Signal to noise ratio at λobs ∼ 4700Å.b References. (1)
Misawa et al. 2013, (2) This paper, (3) Misawa et al. 2014b.
-
Multi-Sightline Observation of NALs 11TA
BLE
2A
bso
rptio
nSyst
ems
wit
hD
oublet
Lin
es
Image
AIm
age
BIo
nz a
bs
vej
EW
rest
ba
EW
rest
rb
IDC
lass
-1c
Cla
ss-2
dIo
nz a
bs
vej
EW
rest
ba
EW
rest
rb
IDC
lass
-1c
Cla
ss-2
d∆
ve
(km
s−1)
(Å)
(Å)
(km
s−1)
(Å)
(Å)
(km
s−1)
Mg
II0.5
111
190431
0.6
04±
0.0
08
0.4
95±
0.0
08
27,2
9C
1L
Mg
II0.5
124
190276
0.0
95±
0.0
04
0.0
52±
0.0
04
31,3
2C
3L
0.0
Mg
II0.5
125
190265
0.2
21±
0.0
05
0.1
45±
0.0
04
28,3
0C
1L
+19.8
Mg
II0.6
731
171003
1.6
89±
0.0
08
1.4
44±
0.0
08
49,5
0C
1L
Mg
II0.9
176
141245
0.1
93±
0.0
02
0.1
20±
0.0
02
61,6
3C
3L
0.0
Mg
II0.9
184
141157
0.1
86±
0.0
05
0.0
92±
0.0
05
67,6
8C
1L
+125.1
Mg
II0.9
187
141116
1.4
72±
0.0
06
1.3
66±
0.0
06
62,6
4C
1+
172.0
CIV
1.6
085
60206
0.0
35±
0.0
02
0.0
26±
0.0
02
7,1
0B
2H
CIV
1.6
149
59493
0.1
05±
0.0
04
≤0.1
32
12,1
3B
2IH
0.0
CIV
1.6
151
59472
0.3
08±
0.0
03
0.2
97±
0.0
03
8,1
1B
2,H
IH+
22.9
CIV
1.6
160
59378
0.0
47±
0.0
03
≤0.0
33
9,1
2C
2+
126.2
CIV
1.6
221
58699
≤0.2
84
0.1
44±
0.0
02
16,2
0C
2,H
H0.0
CIV
1.6
230
58601
≤0.5
12
0.1
90±
0.0
07
16,1
8B
2,H
H+
103.0
CIV
1.6
253
58350
0.0
21±
0.0
02
0.0
14±
0.0
02
18,2
2B
2H
CIV
1.6
556
55033
0.1
33±
0.0
04
0.0
81±
0.0
03
25,2
6C
1H
CIV
1.6
924
51029
0.0
84±
0.0
02
0.0
46±
0.0
02
27,2
8C
2H
0.0
CIV
1.6
930
50965
0.4
98±
0.0
05
0.1
85±
0.0
07
23,2
4C
2,H
LIH
+66.8
CIV
1.7
065
49509
0.0
42±
0.0
02
0.0
32±
0.0
02
29,3
0A
2H
CIV
1.7
212
47932
0.4
93±
0.0
05
0.0
53±
0.0
04
25,2
6C
2,H
HC
IV1.7
617
43596
0.0
10±
0.0
02
0.0
11±
0.0
02
33,3
6C
3LIH
0.0
CIV
1.7
627
43496
0.0
94±
0.0
02
0.0
66±
0.0
02
34,3
7B
1+
108.6
CIV
1.7
650
43250
0.0
41±
0.0
02
0.0
22±
0.0
02
35,3
8A
2H
0.0
CIV
1.7
652
43224
0.0
47±
0.0
02
0.0
35±
0.0
02
31,3
2A
2LIH
+21.7
CIV
1.8
909
30091
0.3
55±
0.0
04
0.3
09±
0.0
03
35,3
7C
1,H
LIH
0.0
CIV
1.8
909
30088
0.4
56±
0.0
06
≤0.5
01
41,4
3C
2,H
IH0.0
SiIV
1.8
909
30088
0.1
81±
0.0
03
≤0.2
68
5,1
0B
2,H
0.0
SiIV
1.8
909
30087
0.1
21±
0.0
04
0.1
19±
0.0
04
5,1
4B
20.0
SiIV
1.8
944
29737
0.3
80±
0.0
05
≤0.3
83
6,1
7C
2,H
LIH
0.0
CIV
1.8
945
29723
≤0.6
69
≤0.5
92
42,4
4C
2,H
+10.4
CIV
1.8
949
29686
0.4
13±
0.0
04
0.3
18±
0.0
04
36,3
9C
2,H
LIH
+51.8
SiIV
1.8
949
29685
0.1
37±
0.0
03
≤0.4
64
6,1
4B
2+
51.8
SiIV
1.8
975
29413
0.0
32±
0.0
02
0.0
19±
0.0
02
8,1
9B
2LIH
0.0
CIV
1.8
982
29343
0.1
93±
0.0
04
0.1
46±
0.0
05
38,4
0C
1,H
IH+
72.5
SiIV
1.8
982
29342
0.0
29±
0.0
03
0.0
13±
0.0
02
7,1
7C
2+
72.5
SiIV
1.9
016
28991
0.1
62±
0.0
03
0.1
42±
0.0
02
9,2
1C
1,H
LIH
0.0
CIV
1.9
019
28964
0.4
57±
0.0
05
0.3
63±
0.0
06
45,4
6C
1,H
+31.0
SiIV
1.9
024
28917
0.0
23±
0.0
02
0.0
13±
0.0
02
11,2
3B
2+
82.7
CIV
1.9
115
27981
0.5
72±
0.0
08
0.4
48±
0.0
07
41,4
3C
1,H
LIH
0.0
SiIV
1.9
115
27987
0.4
39±
0.0
04
0.3
18±
0.0
04
13,1
9C
1,H
0.0
SiIV
1.9
118
27949
≤0.2
48
≤0.1
97
15,2
4C
2,H
+30.9
CIV
1.9
119
27946
0.8
37±
0.0
09
0.6
79±
0.0
09
47,4
8C
1,H
LIH
+41.2
CIV
1.9
138
27745
0.4
84±
0.0
09
0.3
59±
0.0
09
42,4
4C
3,H
+236.9
SiIV
1.9
141
27718
≤0.4
61
0.2
05±
0.0
05
15,2
0B
2,H
LIH
+267.8
SiIV
1.9
420
24880
0.0
41±
0.0
02
0.0
19±
0.0
03
21,2
2C
2LI
CIV
2.1
081
8460
0.2
09±
0.0
04
0.1
10±
0.0
04
51,5
2B
1,H
IH0.0
CIV
2.1
084
8426
0.1
30±
0.0
02
0.0
74±
0.0
02
45,4
6C
2IH
+29.0
CIV
2.1
196
7348
≤0.0
65
0.0
24±
0.0
01
47,4
8C
2LH
0.0
CIV
2.1
209
7223
0.5
52±
0.0
03
0.4
70±
0.0
03
53,5
4C
1,H
LIH
+125.0
CIV
2.1
270
6643
0.1
45±
0.0
01
0.1
14±
0.0
01
49,5
0C
1H
0.0
CIV
2.1
276
6585
0.0
29±
0.0
02
0.0
14±
0.0
02
55,5
7C
2IH
+57.5
CIV
2.1
285
6500
0.1
83±
0.0
02
0.1
55±
0.0
02
56,5
8C
1,H
+143.9
CIV
2.1
349
5884
0.0
93±
0.0
03
0.0
46±
0.0
02
51,5
2C
1H
0.0
CIV
2.1
349
5886
0.0
73±
0.0
02
0.0
32±
0.0
02
59,6
0C
2H
0.0
-
12 Misawa et al.TA
BLE
2A
bso
rptio
nSyst
ems
wit
hD
oublet
Lin
es
CIV
2.1
800
1604
0.0
11±
0.0
01
0.0
08±
0.0
01
53,5
5C
2IH
0.0
SiIV
2.1
815
1458
0.1
15±
0.0
06
0.0
41±
0.0
05
33,3
4C
1+
141.5
CIV
2.1
818
1428
0.2
98±
0.0
02
0.2
09±
0.0
02
61,6
2C
1,H
LIH
+169.7
CIV
2.1
819
1416
0.4
25±
0.0
04
≤0.2
97
54,5
6C
1,H
+179.2
SiIV
2.1
821
1403
0.0
88±
0.0
02
0.0
62±
0.0
03
39,4
0C
1+
198.0
CIV
2.1
897
686
0.8
48±
0.0
03
≤1.4
05
63,6
4A
1,H
H0.0
CIV
2.1
898
676
0.9
02±
0.0
03
≤1.2
53
57,5
8A
1,H
H+
9.4
NV
2.1
900
657
0.9
45±
0.0
04
≤0.8
82
1,3
A1,H
+28.2
NV
2.1
900
658
0.8
88±
0.0
04
≤0.7
17
1,3
A1,H
+28.2
NV
2.1
955
141
≤1.4
94
1.3
41±
0.0
04
2,4
A1,H
H0.0
NV
2.1
955
141
≤1.2
31
1.2
01±
0.0
03
2,4
A1,H
H0.0
CIV
2.1
957
122
1.5
69±
0.0
03
1.2
24±
0.0
03
65,6
6A
1,H
+18.8
CIV
2.1
958
113
≤1.5
90
1.3
03±
0.0
03
59,6
0A
1,H
+28.2
aR
est-
fram
eeq
uiv
ale
nt
wid
thofblu
eco
mponen
tofdouble
tline.
bR
est-
fram
eeq
uiv
ale
nt
wid
thofre
dco
mponen
tofdouble
tline.
cR
elia
bility
class
ofin
trin
sic
lines
base
don
part
ialco
ver
age
analy
sis,
defi
ned
inM
isaw
aet
al.
(2007a).
Ifan
equiv
ale
nt
wid
this
larg
een
ough,w
ecl
ass
ify
the
double
tashom
ogen
eous
sam
ple
with
am
ark
of“H
”.
dIo
niz
ation
class
ofabso
rption
syst
emw
ith
hig
h(H
;IP
>60
eV),
inte
rmed
iate
(I;IP
=35
–50
eV),
and/or
low
(L;IP
<25
eV)
ioniz
ation
transi
tions.
eVel
oci
tydiff
eren
cefr
om
the
firs
tdouble
tin
each
abso
rption
syst
em.
-
Multi-Sightline Observation of NALs 13TA
BLE
3Lin
eParameters
of
Narrow
Abso
rptio
nC
omponents
λobsa
z absb
vejc
log
Nσ(v
)/bd
Oth
erIo
n(Å
)(k
ms−
1)
(cm
−2)
(km
s−1)
Cfe
Ionsf
Image
A
Mg
II4225.6
0.5
111
190431
47.3
Mg
Iλ2853,Fe
IIλ2600
(Fe
IIλ2383)
0.5
108
190464
12.9
6±
0.0
65.1±
0.2
0.9
3+
0.0
7−
0.0
6
0.5
112
190426
13.5
1±
0.0
510.5±
0.5
1.0
0+
0.0
6−
0.0
6
0.5
112
190423
13.6
9±
0.3
337.1±
7.2
0.1
9+
0.1
0−
0.0
90.5
113
190408
12.6
0±
0.0
27.6±
0.3
1.0
0
Mg
II4229.5
0.5
125
190265
17.9
Mg
Iλ2853,Fe
IIλ2600
(Fe
IIλ2344,Fe
IIλ2383)
0.5
125
190269
12.6
9±
0.0
26.0±
0.4
1.0
00.5
126
190261
12.7
0±
0.2
713.3±
4.2
0.8
3+
0.4
6−
0.2
8
Mg
II5376.1
0.9
176
141245
14.1
Mg
Iλ2853,Fe
IIλ2600
(AlII
Iλ1863)
0.9
176
141246
12.9
5±
0.0
24.7±
0.2
1.0
0
Mg
II5365.3
0.9
187
141116
68.1
Mg
Iλ2853,Fe
IIλ2344,2
600
(AlII
Iλ1863)
0.9
181
141190
12.5
0±
0.0
24.1±
0.3
1.0
00.9
185
141146
14.0
3±
0.0
216.9±
0.2
1.0
00.9
189
141094
14.9
4±
0.0
722.0±
0.5
0.9
9+
0.0
3−
0.0
3
CIV
4048.7
1.6
151
59472
26.0
SiIV
λ1394,1
403
1.6
151
59473
17.3
3±
0.0
68.7±
0.1
1.0
0+
0.0
4−
0.0
4
CIV
4050.1
1.6
160
59378
13.1
1.6
160
59379
13.6
6±
0.1
510.3±
1.1
0.4
2+
0.0
8−
0.0
8
CIV
4067.7
1.6
230
58601
38.3
1.6
229
58617
13.8
4±
0.0
213.0±
0.8
1.0
01.6
231
58590
13.9
3±
0.0
65.4±
0.6
1.0
01.6
236
58538
12.8
8±
0.0
99.7±
3.0
1.0
0
CIV
4169.3
1.6
930
50965
58.4
SiII
λ1527,A
lII
λ1671
(OI
λ1302,SiII
λ1260,C
IIλ1335,SiIV
λ1394)
1.6
928
50991
13.6
9±
0.0
239.0±
1.8
1.0
01.6
934
50925
13.5
2±
0.0
217.9±
0.7
1.0
0
CIV
4212.9
1.7
212
47932
41.9
Lyα
1.7
209
47955
13.2
5±
0.0
211.1±
0.7
1.0
01.7
214
47908
13.1
6±
0.0
29.2±
0.7
1.0
0
CIV
4281.1
1.7
652
43224
10.0
Lyα(O
Iλ1302,SiII
λ1207,SiIV
λ1394)
1.7
652
43223
13.7
1±
0.1
16.1±
0.5
0.5
8+
0.0
6−
0.0
6
CIV
4475.7
1.8
909
30091
30.8
Lyα,SiII
λ1527,A
lII
λ1671,(S
iII
λ1190,1
192,1
260,C
IIλ1335,SiII
Iλ1207)
1.8
909
30090
14.8
3±
0.0
520.9±
0.5
0.9
6+
0.0
5−
0.0
5
SiIV
4029.3
1.8
909
30088
27.1
Lyα,SiII
λ1527,A
lII
λ1671,(S
iII
λ1190,1
192,1
260,C
IIλ1335,SiII
Iλ1207)
1.8
906
30121
12.4
8±
0.1
12.8±
0.9
1.0
01.8
907
30111
12.4
9±
0.1
48.8±
3.1
1.0
01.8
910
30081
13.5
6±
0.0
211.2±
0.4
1.0
0
CIV
4481.8
1.8
949
29686
36.5
Lyα(C
IIλ1335,SiII
Iλ1207,N
Vλ1239,1
243)
1.8
945
29728
12.8
5±
0.2
67.7±
3.0
1.0
0
-
14 Misawa et al.TA
BLE
3Lin
eParameters
of
Narrow
Abso
rptio
nC
omponents
1.8
947
29703
14.1
4±
0.2
212.5±
4.2
1.0
01.8
949
29684
14.5
7±
0.2
39.0±
1.3
1.0
01.8
952
29654
13.7
4±
0.0
28.7±
0.4
1.0
0
SiIV
4034.7
1.8
949
29685
38.2
Lyα(C
IIλ1335,SiII
Iλ1207,N
Vλ1239,1
243)
1.8
949
29684
16.1
7±
0.0
52.2±
0.4
1.0
0
CIV
4487.0
1.8
982
29343
22.5
Lyα
1.8
981
29353
13.8
7±
0.0
711.9±
1.0
0.8
8+
0.0
7−
0.0
71.8
983
29332
13.4
5±
0.0
212.8±
0.6
1.0
0
SiIV
4039.4
1.8
982
29342
19.9
Lyα
1.8
980
29360
11.9
5±
0.0
94.8±
1.6
1.0
01.8
983
29337
12.4
0±
0.0
49.3±
1.2
1.0
0
CIV
4507.6
1.9
115
27981
48.8
Lyα,SiII
λ1527,A
lII
λ1671
(OI
λ1302,SiII
λ1190,1
193,1
260,SiII
Iλ1207)
1.9
115
27984
14.7
9±
0.0
436.0±
0.9
0.9
8+
0.0
8−
0.0
8
SiIV
4057.9
1.9
115
27987
44.5
Lyα,SiII
λ1527,A
lII
λ1671
(OI
λ1302,SiII
λ1190,1
193,1
260,SiII
Iλ1207)
1.9
112
28017
13.4
3±
0.0
413.7±
1.2
1.0
01.9
114
27995
13.3
5±
0.0
47.5±
0.7
1.0
01.9
115
27979
13.4
6±
0.0
346.9±
2.4
1.0
01.9
116
27973
13.8
4±
0.0
712.3±
1.4
0.9
6+
0.0
6−
0.0
6
CIV
4511.2
1.9
138
27745
64.0
Lyα,SiII
λ1527,A
lII
λ1671,C
IIλ1335
(SiII
λ1190,1
193,1
260,SiII
Iλ1207,N
Vλ1239,1
243)
1.9
133
27797
14.1
0±
0.0
823.1±
1.4
0.6
9+
0.0
9−
0.0
81.9
141
27716
14.3
4±
0.0
221.2±
0.6
1.0
0
SiIV
4087.8
1.9
141
27718
17.2
Lyα,SiII
λ1527,A
lII
λ1671,C
IIλ1335
(SiII
λ1190,1
193,1
260,SiII
Iλ1207,N
Vλ1239,1
243)
1.9
141
27720
13.6
1±
0.0
210.9±
0.4
1.0
01.9
143
27694
12.3
8±
0.0
94.9±
1.7
1.0
0
SiIV
4100.4
1.9
420
24880
13.2
Lyα,SiII
λ1527,A
lII
λ1671,C
IIλ1335
(OI
λ1302,SiII
λ1190,1
193,1
260,SiII
Iλ1207)
1.9
420
24879
12.7
0±
0.0
210.2±
0.7
1.0
0
CIV
4812.5
2.1
084
8426
21.2
Lyα,SiIV
λ1394
(SiII
Iλ1207)
2.1
083
8435
13.4
6±
0.0
311.8±
0.7
1.0
02.1
086
8415
13.1
9±
0.0
610.8±
1.0
1.0
0
CIV
4829.8
2.1
196
7348
17.1
Lyα,C
IIλ1335
2.1
196
7349
13.6
3±
0.1
413.9±
1.0
0.4
3+
0.1
2−
0.0
9
CIV
4841.2
2.1
270
6643
16.4
Lyα(N
Vλ1239,1
243)
2.1
270
6644
13.6
8±
0.1
014.5±
0.6
0.9
0+
0.1
2−
0.1
22.1
270
6638
13.8
6±
0.0
25.2±
0.1
1.0
0
CIV
4853.4
2.1
349
5884
35.3
Lyα
2.1
347
5903
13.0
3±
0.0
220.9±
1.5
1.0
02.1
351
5866
13.3
4±
0.1
811.3±
0.8
0.7
0+
0.4
5−
0.2
4
CIV
4923.2
2.1
800
1604
14.3
Lyα
2.1
799
1606
13.4
8±
0.3
510.2±
2.3
0.1
5+∞
−0.0
8
SiIV
4434.2
2.1
815
1458
73.3
Lyα(S
iII
Iλ1207)
2.1
810
1502
12.7
2±
0.0
35.8±
0.8
1.0
0
-
Multi-Sightline Observation of NALs 15TA
BLE
3Lin
eParameters
of
Narrow
Abso
rptio
nC
omponents
2.1
818
1427
12.5
4±
0.0
719.5±
4.4
1.0
02.1
822
1395
12.9
4±
0.2
53.0±
1.1
0.7
2+
0.2
3−
0.2
3
CIV
4926.3
2.1
819
1416
34.0
Lyα(S
iII
Iλ1207)
2.1
817
1436
13.6
9±
0.0
916.5±
1.7
0.8
8+
0.1
0−
0.1
02.1
820
1409
13.8
9±
0.0
129.1±
0.3
1.0
02.1
822
1394
13.6
1±
0.0
16.0±
0.3
1.0
0
CIV
g4944.5
2.1
937
347
400.1
Lyα,SiIV
λ1394,O
VI
λ1032,1
038
2.1
881
878
13.2
4±
0.0
125.6±
0.8
1.0
02.1
886
831
14.4
9±
0.0
711.6±
0.6
0.4
3+
0.0
2−
0.0
2
2.1
889
795
14.2
7±
0.2
38.6±
1.3
0.3
8+
0.0
2−
0.0
2
2.1
892
773
13.7
7±
0.2
011.1±
1.4
0.5
2+
0.0
8−
0.0
8
2.1
894
748
14.3
0±
0.1
77.8±
1.0
0.4
4+
0.0
2−
0.0
2
2.1
900
693
14.4
9±
0.0
225.3±
0.6
0.8
4+
0.0
2−
0.0
2
2.1
909
613
14.0
4±
0.0
320.3±
0.5
0.9
8+
0.0
3−
0.0
32.1
914
567
13.3
1±
0.0
116.6±
0.3
1.0
02.1
943
287
14.5
3±
0.0
217.8±
0.2
0.9
1+
0.0
2−
0.0
2
2.1
947
254
14.8
4±
0.1
810.0±
1.0
0.5
2+
0.0
2−
0.0
2
2.1
953
201
14.6
3±
0.0
222.5±
0.7
0.8
9+
0.0
2−
0.0
2
2.1
961
124
14.8
8±
0.0
329.4±
0.9
0.8
1+
0.0
2−
0.0
2
2.1
968
61
14.4
8±
0.0
225.9±
0.6
0.8
4+
0.0
2−
0.0
2
2.1
975
−11
14.2
8±
0.0
219.6±
0.5
0.4
6+
0.0
2−
0.0
2
2.1
981
−63
13.9
1±
0.0
314.9±
0.6
0.4
7+
0.0
3−
0.0
3
2.1
985
−100
14.0
9±
0.0
911.5±
1.0
0.1
8+
0.0
2−
0.0
2
NV
h3956.5
2.1
937
343
428.4
Lyα,SiIV
λ1394,O
VI
λ1032,1
038
2.1
879
889
13.3
8±
0.0
223.8±
1.2
1.0
02.1
885
834
13.8
1±
0.1
317.4±
1.0
0.8
5+
0.1
8−
0.1
7
2.1
893
762
14.2
6±
0.0
442.5±
1.7
0.9
7+
0.0
6−
0.0
6
2.1
900
691
14.8
8±
0.0
320.6±
0.5
0.8
8+
0.0
3−
0.0
3
2.1
909
614
14.5
5±
0.0
223.5±
0.5
0.9
7+
0.0
3−
0.0
32.1
914
567
13.9
0±
0.0
115.0±
0.2
1.0
02.1
944
285
14.8
3±
0.0
222.1±
0.4
0.9
7+
0.0
3−
0.0
3
2.1
953
201
14.9
2±
0.0
141.1±
1.6
0.9
7+
0.0
3−
0.0
3
2.1
961
125
15.4
5±
0.3
314.9±
1.8
0.8
4+
0.0
4−
0.0
4
2.1
966
75
15.2
1±
0.0
526.7±
0.8
0.9
2+
0.0
3−
0.0
3
2.1
976
−14
14.3
8±
0.0
425.6±
1.4
0.6
2+
0.0
3−
0.0
3
2.1
981
−61
14.2
1±
0.0
910.9±
1.2
0.5
3+
0.0
6−
0.0
62.1
984
−91
13.6
6±
0.0
126.3±
0.7
1.0
0
Image
B
Mg
II4229.3
0.5
124
190276
11.7
Fe
IIλ2600
0.5
124
190275
12.6
8±
0.1
811.3±
0.9
0.6
9+
0.2
9−
0.2
0
Mg
II4678.6
0.6
731
171003
78.2
Mg
Iλ2853,Fe
IIλ2344,2
383,2
600
0.6
725
171070
13.0
2±
1.0
32.4±
1.9
0.3
1+
0.1
0−
0.0
9
0.6
726
171059
13.4
9±
0.1
47.5±
1.7
0.9
2+
0.0
8−
0.0
8
-
16 Misawa et al.TA
BLE
3Lin
eParameters
of
Narrow
Abso
rptio
nC
omponents
0.6
727
171047
12.8
3±
0.5
216.5±
18.7
1.0
0+
0.2
1−
0.1
8
0.6
729
171032
13.0
3±
0.2
48.1±
2.4
1.0
0+
0.0
6−
0.0
60.6
730
171018
13.2
7±
0.0
112.0±
0.3
1.0
00.6
731
171008
14.2
9±
9.7
93.2±
9.0
0.9
8+
0.0
6−
0.0
60.6
732
170994
13.2
9±
0.0
116.5±
0.4
1.0
00.6
733
170980
13.6
7±
0.1
620.7±
5.0
1.0
0+
0.0
5−
0.0
50.6
735
170955
13.2
9±
0.0
117.6±
0.3
1.0
00.6
736
170947
13.3
8±
0.4
46.0±
2.0
0.5
5+
0.1
4−
0.1
4
Mg
II5364.4
0.9
184
141157
33.1
0.9
181
141186
12.4
5±
0.5
99.1±
2.0
0.2
9+∞
−0.3
2
0.9
184
141158
12.6
5±
0.1
29.6±
1.0
0.6
8+
0.1
8−
0.1
30.9
185
141142
12.2
2±
0.0
211.8±
0.7
1.0
0
CIV
4038.4
1.6
085
60206
11.2
1.6
085
60206
13.5
7±
0.1
88.0±
0.9
0.4
4+
0.1
0−
0.1
0
CIV
4048.4
1.6
149
59493
20.6
(SiIV
λ1394,1
403)
1.6
150
59491
12.3
8±
0.0
82.5±
4.5
1.0
01.6
150
59487
14.0
4±
0.0
69.2±
0.4
0.7
1+
0.0
6−
0.0
6
CIV
4066.3
1.6
221
58699
19.0
1.6
222
58699
14.1
2±
0.0
213.4±
0.4
1.0
0
CIV
4064.5
1.6
253
58350
13.7
1.6
253
58348
13.5
7±
0.2
46.0±
0.9
0.2
8+
0.0
8−
0.0
8
CIV
4111.4
1.6
556
55033
22.1
1.6
556
55033
13.8
2±
0.0
614.7±
0.5
0.8
5+
0.0
7−
0.0
6
CIV
4168.4
1.6
924
51029
14.7
1.6
925
51027
13.4
2±
0.0
111.4±
0.5
1.0
0
CIV
4190.2
1.7
065
49509
11.7
1.7
065
49508
13.6
8±
0.1
47.8±
0.8
0.4
6+
0.0
7−
0.0
6
CIV
4275.7
1.7
617
43596
11.1
Lyα
1.7
617
43596
14.1
7±
9.9
94.5±
25.6
0.1
5+
0.1
1−
0.1
1
CIV
4277.1
1.7
627
43496
20.9
Lyα,SiII
λ1527
(SiII
λ1260,C
IIλ1335,SiII
Iλ1207,SiIV
λ1394,1
403)
1.7
626
43503
13.7
8±
0.0
77.6±
0.7
0.8
3+
0.0
7−
0.0
6
1.7
628
43479
13.9
2±
0.3
722.0±
16.2
0.1
7+∞
−0.0
7
CIV
4280.7
1.7
650
43250
15.8
Lyα
1.7
650
43249
13.6
4±
0.2
011.7±
1.4
0.3
6+
0.1
2−
0.1
0
CIV
4475.7
1.8
909
30088
48.6
Lyα(S
iII
Iλ1207)
1.8
904
30140
13.4
2±
0.0
311.4±
0.8
1.0
01.8
910
30084
14.3
1±
0.0
625.0±
2.3
1.0
01.8
913
30055
13.1
5±
0.5
910.4±
6.0
1.0
01.8
915
30027
13.0
0±
0.0
811.3±
2.2
1.0
0
SiIV
i4029.3
1.8
909
30087
38.2
Lyα(S
iII
Iλ1207)
-
Multi-Sightline Observation of NALs 17TA
BLE
3Lin
eParameters
of
Narrow
Abso
rptio
nC
omponents
SiIV
4034.0
1.8
944
29737
76.4
Lyα,SiII
λ1527,A
lII
λ1671
(SiII
λ1190,1
193,1
260,C
IIλ1335,SiII
Iλ1207)
1.8
940
29771
13.8
7±
0.0
222.5±
0.4
1.0
01.8
947
29700
12.3
3±
0.0
810.1±
2.1
1.0
01.8
950
29675
12.9
2±
0.0
211.3±
0.7
1.0
01.8
954
29629
12.7
0±
0.0
312.6±
0.9
1.0
0
CIV
4488.7
1.8
945
29723
75.2
Lyα,SiII
λ1527,A
lII
λ1671
(SiII
λ1190,1
193,1
260,C
IIλ1335,SiII
Iλ1207)
1.8
939
29785
14.1
4±
0.0
916.9±
1.9
1.0
01.8
942
29753
14.5
1±
0.0
518.7±
1.4
1.0
01.8
946
29708
13.2
3±
0.1
47.7±
1.7
1.0
01.8
949
29682
14.2
5±
0.0
316.6±
1.2
1.0
01.8
953
29638
13.7
6±
0.0
731.2±
5.3
1.0
0
SiIV
4038.4
1.8
975
29413
11.2
Lyα,C
IVλ1548,1
551
(SiII
λ1260,SiII
Iλ1207)
1.8
975
29414
13.0
7±
0.2
07.4±
0.9
0.5
0+
0.1
6−
0.1
3
SiIV
4044.2
1.9
016
28991
18.5
Lyα,SiII
λ1527,A
lII
λ1671
(SiII
λ1190,1
193,1
260,C
IIλ1335,SiII
Iλ1207)
1.9
016
28992
13.8
7±
0.0
412.8±
0.3
0.9
2+
0.0
5−
0.0
5
CIV
4492.7
1.9
019
28964
52.4
Lyα,SiII
λ1527,A
lII
λ1671
(SiII
λ1190,1
193,1
260,C
IIλ1335,SiII
Iλ1207)
1.9
017
28988
14.5
1±
0.0
321.6±
0.5
0.9
6+
0.0
7−
0.0
7
1.9
024
28918
13.8
7±
0.0
512.5±
0.4
0.9
7+
0.0
8−
0.0
7
SiIV
4045.2
1.9
024
28917
11.1
Lyα,C
IVλ1548,1
551
1.9
023
28918
13.1
9±
0.2
56.8±
1.2
0.3
1+
0.1
0−
0.0
9
SiIV
4058.4
1.9
118
27949
26.7
Lyα