J/MNRAS/427/1135 Properties of radio-loud BAL quasars (DiPompeo+, 2012)
The rest-frame ultraviolet properties of radio-loud broad absorption line
quasars.
DiPompeo M.A., Brotherton M.S., Cales S.L., Runnoe J.C.
<Mon. Not. R. Astron. Soc., 427, 1135-1152 (2012)>
=2012MNRAS.427.1135D 2012MNRAS.427.1135D
ADC_Keywords: QSOs ; Ultraviolet ; Equivalent widths
Keywords: quasars: absorption lines - quasars: emission lines - quasars: general
Abstract:
We recently presented radio observations of a large sample of
radio-loud broad absorption line (BAL) quasars from the Sloan Digital
Sky Survey (SDSS) and Faint Images of the Radio Sky at Twenty-cm
surveys, as well as a well matched sample of unabsorbed quasars,
primarily to measure their radio spectral indices and estimate
ensemble orientations. Here, we analyse the SDSS spectra of these
samples and compare the rest-frame ultraviolet properties of
radio-loud BAL and non-BAL quasars. Ultraviolet properties include the
continuum shape, emission-line measurements of CIV, AlIII, CIII],
FeII and MgII, and BAL properties including the balnicity index,
absorption index and minimum and maximum outflow velocities. We find
that radio-loud BAL quasars have similar ultraviolet properties
compared to radio-loud non-BAL sources, though they do appear to have
redder continua and stronger FeII emission, which is consistent with
what is found for radio-quiet BAL sources. No correlations exist
between outflow properties and orientation (radio spectral index),
suggesting that BAL winds along any line of sight are driven by the
same mechanisms. There are also few correlations between spectral
index and other properties. We conclude that BAL outflows occur along
all lines of sight with similar strengths and velocities.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 80 146 Sample properties
table2.dat 135 146 Line measurements
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See also:
J/A+A/427/107 : Polarization in BAL QSOs (Lamy+, 2004)
J/ApJS/165/1 : BAL QSOs from SDSS DR3 (Trump+, 2006)
J/ApJ/665/990 : SDSS DR2 BAL QSOs (Ganguly+, 2007)
J/ApJ/692/758 : BAL QSOs in SDSS-DR5 (Gibson+, 2009)
J/MNRAS/410/860 : Redshift dependence of BAL QSOs (Allen+, 2011)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1 A1 --- Note [n] n for non-BAL sample
3- 6 A4 --- --- [SDSS]
8- 26 A19 --- SDSS SDSS name (JHHMMSS.ss+DDMMSS.s)
28- 31 F4.2 --- z Redshift
33- 36 F4.2 [-] logR* [0.98/3.25] Radio loudness
38- 41 F4.1 [10-7W] logLr Radio luminosity, k-corrected to rest-frame 5GHz
43- 46 F4.1 [10-7W] logLbol Bolometric luminosity
48- 50 F3.1 [Msun] logMbh ? Black-hole mass
52- 55 F4.2 --- fEdd [0/3.1]? Eddington fraction (Lbol/Ledd)
57 A1 --- l_BI Limit flag on BI
58- 61 I4 km/s BI ? Balnicity index (1)
63 A1 --- l_AI Limit flag on AI
64- 67 I4 km/s AI ? Absorption index (1) (2)
69 A1 --- l_vmax Limit on vmax
70- 74 I5 km/s vmax ? Maximum velocity (1)
76- 80 I5 km/s vmin ? Minimum velocity (1)
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Note (1): measurements of the CIV BAL trough. In some cases the trough extends
off the blue edge of the spectrum, and so lower limits are given.
The absorption index AI is similar to the Balnicity index BI, but allows
for lower velocities (<3000km/s)
Note (2): AI measured using a criteria of continuous absorption for 800km/s,
instead of 2000km/s.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1 A1 --- Note [n] n for non-BAL sample
3- 11 A9 --- Object Object short name (HHMM+DDMM)
13- 17 F5.1 10-19W/m2/nm f1000 Continuum normalized flux density at
1000km/s, in 10-17erg/cm2/s/Å (1)
19- 23 F5.2 --- alphaUV Power-law slope αUV,
Fλ∝λ-α (1)
25- 28 F4.2 --- FeII FeII scaling factor (1) (2)
30- 34 F5.1 0.1nm EW(CIV) ? CIV equivalent width
36- 39 F4.1 0.1nm e_EW(CIV) ? rms uncertainty on EW(CIV)
41- 44 I4 km/s FW(CIV) ? CIV FWHM
46- 49 I4 km/s e_FW(CIV) ? rms uncertainty on FW(IV)
51- 56 F6.1 km/s BS(CIV) ? CIV blueshift
58- 61 F4.1 0.1nm EW(AlIII) ? AlIII equivalent width (3)
63- 66 F4.1 0.1nm e_EW(AlIII) ? rms uncertainty on EW(AlIII)
69- 73 I5 km/s FW(AlIII) ? AlIII FWHM
75- 78 I4 km/s e_FW(AlIII) ? rms uncertainty on FW(AlIII)
80- 83 F4.1 0.1nm EW[CIII] ? [CIII] equivalent width (3)
85- 87 F3.1 0.1nm e_EW[CIII] ? rms uncertainty on EW[CIII]
89- 93 I5 km/s FW[CIII] ? [CIII] FWHM
95- 98 I4 km/s e_FW[CIII] ? rms uncertainty on FW[CIII]
100-105 F6.1 km/s BS[CIII] ? [CIII] blueshift
107-111 F5.1 0.1nm EW(MgII) ? MgII equivalent width
113-117 F5.1 0.1nm e_EW(MgII) ? rms uncertainty on EWMgII
119-123 I5 km/s FW(MgII) ? MgII FWHM
125-128 I4 km/s e_FW(MgII) ? rms uncertainty on FW(MgII)
130-135 F6.1 km/s BS(MgII) ? MgII blueshift
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Note (1): Errors on f1000, alphaUV, and the FeII scaling are omitted because
they are typically quite small, on the order of one to a few percent.
Note (2): These values are scalings of the FeII flux in the I Zw 1 template.
Note (3): Line parameters are given as "0.0" when the final fit is
indistinguishable from a line not being present. In some cases lines could
not be measured, due to various factors like redshift, noisy or missing data,
intervening absorption, or BAL features.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 08-Aug-2013