J/ApJ/692/758 BAL QSOs in SDSS-DR5 (Gibson+, 2009)
A catalog of broad absorption line quasars in Sloan Digital Sky Survey Data
Release 5.
Gibson R.R., Jiang L., Brandt W.N., Hall P.B., Shen Y., Wu J.,
Anderson S.F., Schneider D.P., Vanden Berk D., Gallagher S.C., Fan X.,
York D.G.
<Astrophys. J., 692, 758-777 (2009)>
=2009ApJ...692..758G 2009ApJ...692..758G
ADC_Keywords: Active gal. nuclei ; Line Profiles ; X-ray sources ; Surveys ;
Equivalent widths
Keywords: galaxies: active - galaxies: nuclei - quasars: absorption lines -
quasars: emission lines - X-rays: general
Abstract:
We present a catalog of 5039 broad absorption line (BAL) quasars
(QSOs) in the Sloan Digital Sky Survey (SDSS) Data Release 5 (DR5) QSO
catalog that have absorption troughs covering a continuous velocity
range ≥2000km/s. We have fitted ultraviolet (UV) continua and line
emission in each case, enabling us to report common diagnostics of BAL
strengths and velocities in the range -25000 to 0km/s for SiIV1400,
CIV1549, AlIII1857, and MgII2799. We calculate these diagnostics using
the spectrum listed in the DR5 QSO catalog, and also for spectra from
additional SDSS observing epochs when available. In cases where BAL
QSOs have been observed with Chandra or XMM-Newton, we report the
X-ray monochromatic luminosities of these sources. We confirm and
extend previous findings that BAL QSOs are more strongly reddened in
the rest-frame UV than non-BAL QSOs, and that BAL QSOs are relatively
X-ray weak compared to non-BAL QSOs.
Description:
This BAL catalog is constructed from SDSS DR5 (Adelman-McCarthy et al.
2007, Cat. VII/252). The SDSS uses a CCD camera on a dedicated 2.5m
telescope at Apache Point Observatory, New Mexico, to obtain images in
five broad optical bands (ugriz) over approximately 10000deg2 of the
high Galactic latitude sky.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 265 5035 DR5 BAL Catalog
table2.dat 251 569 DR5 BAL catalog duplicate spectra
table3.dat 45 118 DR5 non-BALs with CIV BlueWingAbs flag set
table4.dat 51 92 BALs with absorption from other ions
table5.dat 90 73 X-ray source information
--------------------------------------------------------------------------------
See also:
VII/260 : The SDSS-DR7 quasar catalog (Schneider+, 2010)
VII/23 : Absorption Lines in QSO Spectra (Ellis+ 1978)
J/MNRAS/399/2231 : SDSS DR5 BALQSO catalog (Scaringi+, 2009)
J/ApJ/665/990 : SDSS DR2 BAL QSOs (Ganguly+, 2007)
J/ApJS/165/1 : BAL QSOs from SDSS DR3 (Trump+, 2006)
J/A+A/427/107 : Polarization in BAL QSOs (Lamy+, 2004)
J/ApJ/599/116 : UV properties of absorbed quasars (Vestergaard+, 2003)
J/AJ/125/1711 : Broad Absorption Line Quasars from SDSS (Reichard+, 2003)
J/ApJS/97/1 : HST Quasar Absorption Line Key Project. X. (Lockman+ 1995)
http://www.sdss.org/ : SDSS home page
Byte-by-byte Description of file: table[12].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- SDSS SDSS-DR5 identification (HHMMSS.ss+DDMMSS.s)
20- 29 F10.6 deg RAdeg Right Ascension in decimal degrees (J2000)
31- 40 F10.6 deg DEdeg Declination in decimal degrees (J2000)
42- 45 F4.2 --- z SDSS-DR5 redshift (1)
47- 51 I5 d MJD ? Modified Julian date of observation (only
for table 2)
53- 56 I4 --- Plate ? SDSS plate number (only for table 2)
58- 60 I3 --- Fiber ? SDSS fiber number (only for table 2)
62- 68 F7.1 km/s BI(Si) ? SiIV balnicity index
70- 76 F7.1 km/s BIO(Si) ? SiIV modified balnicity index; see text
78- 82 F5.1 0.1nm EW(Si) ? SiIV rest-frame absorption equivalent width
84- 89 I6 km/s vmin(Si) ? SiIV minimum velocity
91- 96 I6 km/s vmax(Si) ? SiIV maximum velocity
98-101 F4.2 --- fd(Si) ? SiIV BAL bin fraction below 50% of continuum
103-109 F7.1 km/s BI(C) ? CIV balnicity index
111-117 F7.1 km/s BIO(C) ? CIV modified balnicity index; see text
119-124 F6.1 0.1nm EW(C) ? CIV rest-frame absorption equivalent width
126-131 I6 km/s vmin(C) ? CIV minimum velocity
133-138 I6 km/s vmax(C) ? CIV maximum velocity
140-143 F4.2 --- fd(C) ? CIV BAL bin fraction below 50% of continuum
145-151 F7.1 km/s BI(Al) ? AlIII balnicity index
153-159 F7.1 km/s BIO(Al) ? AlIII modified balnicity index; see text
161-166 F6.1 0.1nm EW(Al) ? AlIII rest-frame absorption equivalent width
168-173 I6 km/s vmin(Al) ? AlIII minimum velocity
175-180 I6 km/s vmax(Al) ? AlIII maximum velocity
182-185 F4.2 --- fd(Al) ? AlIII BAL bin fraction below 50% of continuum
187-193 F7.1 km/s BI(Mg) ? MgII balnicity index
195-201 F7.1 km/s BIO(Mg) ? MgII modified balnicity index; see text
203-208 F6.1 0.1nm EW(Mg) ? MgII rest-frame absorption equivalent width
210-215 I6 km/s vmin(Mg) ? MgII minimum velocity
217-222 I6 km/s vmax(Mg) ? MgII maximum velocity
224-227 F4.2 --- fd(Mg) ? MgII BAL bin fraction below 50% of continuum
229 I1 --- f_SiIVEmL [0/1] SiIV EmLost flag (2)
231 I1 --- f_CIVEmL [0/1] CIV EmLost flag (2)
233 I1 --- f_AlIIIEmL [0/1] AlIII EmLost flag (2)
235 I1 --- f_MgIIEmL [0/1] MgII EmLost flag (2)
237 I1 --- f_SiIVBB [0/1]? SiIV BALManyBadBins flag (2)
239 I1 --- f_CIVBB [0/1]? CIV BALManyBadBins flag (2)
241 I1 --- f_AlIIIBB [0/1]? AlIII BALManyBadBins flag (2)
243 I1 --- f_MgIIBB [0/1]? MgII BALManyBadBins flag (2)
245 I1 --- f_CIV4BWA [0/1] CIV BlueWingAbs flag (2)
247-251 F5.1 --- SN1700 ? Signal-to-noise (3)
253-258 F6.2 [mW/m2/Hz] logF1400 ? Log of 1400 monochromatic luminosity (4)
260-265 F6.2 [mW/m2/Hz] logF2500 ? Log of 2500 monochromatic luminosity (4)
--------------------------------------------------------------------------------
Note (1): The redshifts for our QSOs are taken from the DR5 QSO catalog
(Cat. VII/252, superseded by VII/260), with the exception of two
sources, J100424.88+122922.2 and J153029.05+553247.9, which we
consider to be misclassified. We assign these sources redshifts of
4.66 and 1.73, respectively.
Note (2): There are cases, such as strongly absorbed emission-line
profiles, for which we were unable to accurately determine the
underlying emission. We define a set of flags that we use to indicate
when the fit model is particularly uncertain due to such effects.
EmLost = The profile of the emission line at (nearly) zero velocity has been
strongly absorbed and may not have been accurately reconstructed.
BlueWingAbs = Additional "blue wing" emission occurs on the blue side
of the C emission line, and absorption is apparent between the blue
wing and the line core. Since we fit only the line core and cannot
accurately reconstruct the "blue wing" emission, we could potentially
miss BAL absorption in these cases.
BALManyBadBins = Some putative BALs consist of a large number of
spectral bins that have been flagged as "bad" in the SDSS pipeline.
See text for further details.
Note (3): Median of the flux divided by the noise for all spectral bins in
the 1650-1750Å range. See text for further details.
Note (4): Only for table 1. Corrected for Galactic reddening.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table[34].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- SDSS SDSS-DR5 name (HHMMSS.ss+DDMMSS.s)
20- 29 F10.6 deg RAdeg Right ascension in decimal degrees (J2000)
31- 40 F10.6 deg DEdeg Declination in decimal degrees (J2000)
42- 45 F4.2 --- z Redshift
47 I1 --- SiIV [0/1]? SiIV contamination? (only for table 4)
49 I1 --- AlIII [0/1]? AlIII contamination? (only for table 4)
51 I1 --- MgII [0/1]? MgII contamination? (only for table 4)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- SDSS SDSS source (HHMMSS.ss+DDMMSS.s)
20- 29 A10 --- ObsID Chandra or XMM-Newton observation
identification number (1)
31- 34 F4.1 ks Exp X-ray exposure time (2)
36- 42 A7 ct Sct 0.5-2keV counts source/BG
44- 50 A7 ct Hct 2-8keV counts source/BG
52 I1 --- Det [0/1] X-ray detected? (0 for no detection)
54 A1 --- l_logR* Limit flag on logR*
55- 59 F5.2 [-] logR* Radio loudness parameter (3)
61 A1 --- l_logLx Limit flag on log(L2keV)
62- 66 F5.2 [10-7W/m2/Hz] logLx The 2keV monochromatic luminosity in erg/s/Hz
68 A1 --- l_aox Limit flag on aox
69- 73 F5.2 --- aox Optical-to-X-ray spectral index (4)
75- 78 F4.2 --- e_aox ? aox uncertainty (5)
80 A1 --- l_Daox Limit flag on Daox
81- 85 F5.2 --- Daox Difference in X-ray luminosity (6)
87- 90 F4.2 --- e_Daox ? Delaox uncertainty (5)
--------------------------------------------------------------------------------
Note (1): Ten-digit numbers correspond to XMM-Newton observations, while
shorter numbers correspond to Chandra observations.
Note (2): The effective X-ray exposure reported by the CIAO or SAS
toolchains for the extraction of the source region.
Note (3): log(R*)=log(Lν(5GHz)/L2500). See section 4.6 for further
details.
Note (4): αox is usually expressed in terms of the logarithm of the
ratio between the monochromatic luminosities Lν at 2keV and
2500Å with the parameter:
αox=0.3838log(Lν(2keV)/Lν(2500Å)). For typical
QSOs, αox is a function of L2500, the monochromatic
luminosity at 2500Å. Just et al. (2007ApJ...665.1004J 2007ApJ...665.1004J) found the
equation (3):
αox(L2500)=(-0.140±0.007)log(L2500)+(2.705±0.212).
Note (5): The error is assumed to be dominated by the error on X-ray luminosity.
Note (6): Equation (3) enables quantitative measurement of how the X-ray
luminosity of a given QSO differs from that expected for a typical
QSO of the same UV luminosity. This difference is parameterized by:
Δαox=αox-αox(L2500), where αox
is the value observed for a particular source observed to have a UV
luminosity of L2500, and αox(L2500) is determined for a
typical QSO from Equation (3).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 25-Feb-2011