J/ApJ/931/154 High-quality UV & X-ray quasar spectral data (Rivera+, 2022)
Exploring changes in quasar spectral energy distributions across CIV parameter
space.
Rivera A.B., Richards G.T., Gallagher S.C., McCaffrey T.V., Rankine A.L.,
Hewett P.C., Shemmer O.
<Astrophys. J., 931, 154 (2022)>
=2022ApJ...931..154R 2022ApJ...931..154R
ADC_Keywords: QSOs; X-ray sources; Spectra, optical; Surveys; Redshifts;
Equivalent widths; Black holes; Ultraviolet
Keywords: Quasars ; Spectral energy distribution ; Black hole physics ;
X-ray active galactic nuclei
Abstract:
We examine the UV/X-ray properties of 1378 quasars in order to link
empirical correlations to theoretical models of the physical
mechanisms dominating quasars as a function of mass and accretion
rate. The clarity of these correlations is improved when (1) using CIV
broad emission line equivalent width (EQW) and blueshift (relative to
systemic) values calculated from high signal-to-noise ratio
reconstructions of optical/UV spectra and (2) removing quasars
expected to be absorbed based on their UV/X-ray spectral slopes. In
addition to using the traditional CIV parameter space measures of CIV
EQW and blueshift, we define a "CIV|| distance" along a
best-fit polynomial curve that incorporates information from both CIV
parameters. We find that the CIV|| distance is linearly
correlated with both the optical-to-X-ray slope, αox, and
broad-line HeII EQW, which are known spectral energy distribution
indicators, but does not require X-ray or high spectral resolution UV
observations to compute. The CIV|| distance may be a better
indicator of the mass-weighted accretion rate, parameterized by
L/LEdd, than the CIV EQW or blueshift alone, as those relationships
are known to break down at the extrema. Conversely, there is only a
weak correlation with the X-ray energy index (Γ), an alternate
L/LEdd indicator. We find no X-ray or optical trends in the direction
perpendicular to the CIV distance that could be used to reveal
differences in accretion disk, wind, or corona structure that could be
widening the CIV EQW-blueshift distribution. A different parameter
(such as metallicity) not traced by these data must come into play.
Description:
The majority of our sample is drawn from archival X-ray observations
of quasars from SDSS, specifically Data Release 14
(Paris+ 2014, VII/286 superseded by VII/289).
Timlin+ 2020, J/MNRAS/492/719 use X-ray data from the Chandra
archives, while Lusso+ 2020, J/A+A/642/A150 use data from the
SDSS-4XMM catalog (see IX/69), and these two investigations are
largely complementary to each other. The union of these two data sets
provides the foundation for our investigation. See Section 2.1.
We additionally include a subsample of multiepoch data from the
SDSS-RM sample (Shen+ 2015, J/ApJS/216/4 quasars analyzed in
Rivera+ 2020ApJ...899...96R 2020ApJ...899...96R); see Section 2.2.
To construct our full sample, we additionally selected 25 quasars for
new observations with both HST and Chandra. Observations with Chandra
ACIS occurred between 2016 December and 2017 August. See Section 2.3
We define a "good" subset in Section 3.4.3 with 779 objects.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
fig13.dat 205 779 The "Good" sample that underlies the Bokeh
interactive plots in Figure 13
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Description of file:
Rivera2022GoodSampleRevised.fits is the original FITS file of the
sample as downloaded in the Data behind Figure 13.
See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
IX/57 : The Chandra Source Catalog (CSC), Release 2.0 (Evans+, 2019)
IX/69 : XMM-Newton Serendipitous Source Catalogue 4XMM-DR13 (Webb+, 2023)
VII/289 : SDSS quasar catalog, sixteenth data release (DR16Q) (Lyke+, 2020)
J/ApJS/166/470 : SDSS-Spitzer type I QSOs IR photometry (Richards+, 2006)
J/ApJ/666/757 : CIV 1549Å emission line in AGNs (Sulentic+, 2007)
J/ApJ/685/773 : X-ray-UV relations in SDSS DR5 QSOs (Gibson+, 2008)
J/ApJ/705/1336 : X-ray measurements of ChaMP-SDSS gal. (Constantin+, 2009)
J/MNRAS/405/2302 : Improved redshifts for SDSS quasar spectra (Hewett+, 2010)
J/ApJ/726/20 : X-ray emission from quasars (Miller+, 2011)
J/ApJS/194/45 : QSO properties from SDSS-DR7 (Shen+, 2011)
J/A+A/548/A66 : SDSS Quasar Catalog, DR9Q (Paris+, 2012)
J/MNRAS/449/1593 : CIV absorption in BAL QSOs (Baskin+, 2015)
J/AJ/149/203 : Reddening of ∼35000 quasars from SDSS (Krawczyk+, 2015)
J/ApJ/805/122 : X-ray properties of PHL1811 analogs and WLQs (Luo+, 2015)
J/ApJ/815/33 : A Hubble diagram for quasars (Risaliti+, 2015)
J/ApJS/216/4 : SDSS-RM project: technical overview (Shen+, 2015)
J/ApJ/819/154 : SDSS-DR7 QSOs with X-ray and UV luminosities (Lusso+, 2016)
J/ApJ/865/56 : Emission line & R-band cont. LCs of 17 QSOs (Lira+, 2018)
J/ApJ/886/42 : Reverberation mapping & opt. spectra of AGNs (Du+, 2019)
J/A+A/642/A150 : Quasars as standard candles. III. (Lusso+, 2020)
J/ApJ/900/141 : X-ray weak quasars from SDSS & Chandra (Pu+, 2020)
J/MNRAS/498/4033 : Extreme quasar X-ray variability (Timlin+, 2020)
J/MNRAS/492/719 : Chandra observations of radio-quiet QSOs (Timlin+, 2020)
J/ApJ/915/129 : 13yr of spectrophotometrically monitored QSOs (Kaspi+, 2021)
J/ApJS/252/15 : GNRIS-Distant Quasar Survey (GNRIS-DQS) (Matthews+, 2021)
J/MNRAS/504/5556 : X-ray data of 26 high-luminosity quasars (Timlin+, 2021)
Byte-by-byte Description of file: fig13.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SDSS]
5- 23 A19 --- SDSSo SDSS identifier (original designations
from SDSS-DR14, VII/286) (SDSS) (8)
25- 33 E9.3 --- logRedd [-99/0.8]? Log(L/LEdd) from Shen+ 2011,
J/ApJS/194/45 (LOGEDD_RATIO) (1)
35- 41 F7.5 --- Gamma [1.2/2.8] Photon index Γ for the
Timlin+ 2020, J/MNRAS/492/719 and
Chandra/HST samples (Gamma) (2)
43- 49 F7.3 mW/m2/Hz F2keV [-32.1/-29.9] Log of the observed flux
density at 2keV, in erg/cm2/s/Hz
(f2keV_ergs) (3)
51- 57 F7.3 --- aOX [-1.92/-1.14] Measured αox value
(Alpha_ox) (4)
59- 64 F6.3 --- DelaOX-T20 [-0.25/0.3] Δαox calculated
using alphaox and equation 3 from
Timlin+ 2020, J/MNRAS/492/719
(DeltaAlphaox)
66- 71 F6.3 --- DelaOX [-0.3/0.24] Δαox calculated
using alphaox and equation 4 from this
paper (NewDeltaAlpha_ox)
73- 78 F6.3 --- Del(g-i) [-0.3/0.3] Delta(g-i) from
Krawczyk+ 2015, J/AJ/149/203 (Delg-i)
80- 86 F7.3 0.1nm EWCIV-T20 [16/189]? Rest-frame CIV equivalent
width (in Angstroms) from Timlin+ 2020,
J/MNRAS/492/719 (TimlinCIVEQW)
88- 95 F8.3 km/s CIVshift-T20 [-587/3736]? CIV blueshift from
Timlin+ 2020, J/MNRAS/492/719
(TimlinCIVBlueshift)
97- 105 F9.3 km/s CIVshift [-1047/4874] CIV blueshift generated
from the independent component analysis
(ICA) reconstructed spectra (CIV_blue)
107- 113 F7.3 0.1nm EWCIV [6.8/228] Rest-frame CIV EQW (in
angstroms) generated from the ICA
reconstructed spectra (CIV_EW)
115- 121 F7.5 --- zold [0.46/3.42]? SDSS redshift (Old_redshift)
123- 129 F7.5 --- z [0.46/3.41] Independent component
analysis (ICA) calculated redshift
(Redshifts)
131- 136 F6.3 0.1nm EWHeII [-0.3/8.3] Rest-frame HeII EQW (in
angstroms) generated from the ICA
reconstructed spectra (HeII_EQW)
138- 144 F7.4 --- logMBH [0/10.5]? LogMBH from Shen+ 2011,
J/ApJS/194/45 (LOGBH)
146 I1 --- Ref [1/4] Reference (Data_source) (5)
148 I1 --- Clean [1] Clean flag (always "1") (Clean) (6)
150- 160 F11.7 deg RAdeg SDSS right ascension (J2000) (RA_1)
162- 172 F11.7 deg DEdeg [-15.1/70] SDSS declination (J2000)
(DEC_1)
174 I1 --- N19 [0/1] QSO from Nardini+
2019A&A...632A.109N 2019A&A...632A.109N (Nardini_Sample)
176 I1 --- Good [1] Part of this paper "Good" sample;
always "1" (Good)
178- 185 F8.5 --- Xdist [-0.94/-0.0038] Distance in
Γ-Δαox space from
the gray dotted line described by
equation 3 and shown in Figure 7
(XRayDist)
187- 191 F5.3 --- CIVpadist [0.085/1.21]? CIV parallel distance
(CIV_Dist) (7)
193- 198 F6.3 --- CIVpedist [-0.26/0.15]? CIV perpendicular distance
(CIVPerpDist) (7)
200- 205 F6.3 [10-7W/Hz] logL2500 [29.6/32.5] Log of the luminosity at
2500Å in erg/s/Hz (L2500) (4)
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Note (1): A null value indicates there was no match from
Shen+ 2011, J/ApJS/194/45
A value of -99.0 indicates that there was a match to the sample,
however a calculation of Log(L/LEdd) was unable to be performed.
Note (2): the Gamma values were derived from hardness ratios generated by the
Park+ 2006ApJ...652..610P 2006ApJ...652..610P Bayesian Estimation of Hardness Ratios
(BEHR) code. For the SDSSRM sample flux ratios were instead used to
estimate Gamma (see Appendix B of this paper for details).
The Lusso+ 2020, J/A+A/642/A150 Gammas were calculated from an
estimation of the slope of the power law connecting the observed soft
and hard monochromatic fluxes. The Nardini+ 2019A&A...632A.109N 2019A&A...632A.109N sample
had Gamma values measured directly from their spectra.
The Nardini+ 2019A&A...632A.109N 2019A&A...632A.109N, Timlin+ 2020, J/MNRAS/492/719 and
Lusso+ (2020, J/A+A/642/A150) values were taken from the original papers.
Note (3): Values from the Nardini+ 2019A&A...632A.109N 2019A&A...632A.109N,
Timlin+ 2020, J/MNRAS/492/719 and Lusso+ (2020, J/A+A/642/A150)
samples were taken from those papers. The SDSSRM and Chandra/HST
samples had F2keV values as calculated in Appendix B of this paper.
Note (4): The Nardini+ 2019A&A...632A.109N 2019A&A...632A.109N and Timlin+ 2020, J/MNRAS/492/719
values were taken directly from those papers, the values for
Lusso+ (2020, J/A+A/642/A150) were calculated from the data table
provided. The SDSSRM and Chandra/HST samples had alpha_ox values
calculated as in Appendix B of this paper.
Note (5): Data source as follows:
1 = Timlin et al. 2020, J/MNRAS/492/719
2 = SDSSRM, this paper
3 = Chandra/HST
4 = Lusso et al. 2020, J/A+A/642/A150
Note (6): Flag as follows:
1 = part of the Lusso+ 2020, J/A+A/642/A150 "clean sample" or the
Timlin+ 2020, J/MNRAS/492/719 "sensitive sample"
Note (7): The CIV parameter space are described in Section 3.1
Note (8): At row 311, the object SDSSJ141056.25+541023.7 is a misprint for
SDSSJ141056.25+541608.5; corrected at CDS.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 17-Apr-2024