Access to Astronomical Catalogues

← Click to display the menu
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
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 265 569 DR5 BAL catalog duplicate spectra table3.dat 51 118 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) : SDSS home page Byte-by-byte Description of file: table[12].dat
Bytes Format Units Label Explanations
1- 18 A18 --- SDSS SDSS-DR5 identification ( 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 ( 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 ( 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) 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: Δαoxoxox(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
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service