J/A+A/603/A1 X-shooter spectra of 6 ∼2.2 quasars (Bisogni+, 2017)
Simultaneous detection and analysis of optical and ultraviolet broad emission
lines in quasars at z ∼ 2.2.
Bisogni S., di Serego Alighieri S., Goldoni P., Ho L.C., Marconi A.,
Ponti G., Risaliti G.
<Astron. Astrophys. 603, A1 (2017)>
=2017A&A...603A...1B 2017A&A...603A...1B (SIMBAD/NED BibCode)
ADC_Keywords: QSOs; Galaxies, optical; Spectra, ultraviolet; Spectra, infrared
Keywords: galaxies: active - galaxies: nuclei - galaxies: Seyfert -
quasars: emission lines - quasars: general
Abstract:
We studied the spectra of six z∼2.2 quasars obtained with the
X-shooter spectrograph at the Very Large Telescope. The redshift of
these sources and X-shooter's spectral coverage allow us to cover the
rest spectral range ∼1200-7000Å for the simultaneous detection of
optical and ultraviolet lines emitted by the Broad Line Region.
Simultaneous measurements, avoiding issues related to quasars
variability, help us understanding the connection between different
Broad Line Region line profiles generally used as virial estimators of
Black Holes masses in quasars. The goal of this work is comparing the
emission lines from the same object to check on the reliability of
Hα, MgII and CIV with respect to Hβ. Hα and MgII
linewidths correlate well with Hβ, while CIV shows a poorer
correlation, due to the presence of strong blueshifts and asymmetries
in the profile. We compare our sample with the only other two whose
spectra were taken with the same instrument and for all examined lines
our results are in agreement with the ones obtained with X-shooter at
z∼1.5-1.7.
We finally evaluate CIII] as a possible substitute of CIV in the same
spectral range and find that its behaviour is more coherent with those
of the other lines: we believe that, when a high quality spectrum such
as the ones we present is available and a proper modelization with the
FeII and FeIII emissions is performed, the use of this line is more
appropriate than that of CIV if not corrected for the contamination by
non-virialized components.
Description:
Reduced spectra for the six sources in the sample. Observations were
performed with slit widths of 1.3, 1.2 and 1.2 arcsec respectively for
the three arms resulting in resolving powers
R=λ/{DELTA}λ=4000, 6700 and 4300. The spectra were
processed using version 1.3.0 of the X-shooter data reduction pipeline
(Goldoni et al. 2006, Proc. SPIE, 6269, 62692K; Modigliani et al.
2010, Proc. SPIE, 7737, 773728).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 111 6 Sample and observations properties
sp/* . 18 Individual spectra
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See also:
J/ApJS/194/45 : QSO properties from SDSS-DR7 (Shen+, 2011)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 19 A19 -- Name Name (JHHMMSS.ss+DDMMSS.s)
21- 26 F6.4 --- zShen Redshift initially used to rest-frame the
spectra (Shen et al., 2011,
Cat. J/ApJS/194/45)
28- 34 F7.5 --- zfit Redshift we estimate from the central
wavelength of the [OIII]λ5007 line
36- 42 F7.5 --- e_zfit rms uncertainty on zfit
44- 49 F6.3 Gpc DL Luminosity distance (1)
51- 55 F5.2 mag rmag SDSS r-band PSF magnitude
57- 61 F5.3 mag E(B-V) Galactic extinction from
Schlafly & Finkbeiner (2011ApJ...737..103S 2011ApJ...737..103S)
63- 66 I4 s ExpTime Exposure time
68- 71 F4.2 --- Airmass Airmass
73- 75 F3.1 arcsec Seeing Seeing
77- 87 A11 --- UVB Name of UVB arm reduced spectrum in
subdirectory sp
89- 99 A11 --- VIS Name of VIS arm reduced spectrum in
subdirectory sp
101-111 A11 --- NIR Name of NIR arm reduced spectrum in
subdirectory sp
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Note (1): In determining the luminosity distance DL we use the following
cosmological parameters: H0=70km/s/Mpc1, {OMEGA}M=0.3 and {OMEGA}{LAMBDA}=0.7.
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Byte-by-byte Description of file: sp/*
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
5- 15 F11.5 nm lambda Wavelength
18- 29 E12.6 10mW/m2/nm sp ?=- Flux (erg/cm2/s/Å)
31- 42 E12.6 10mW/m2/nm e_sp []?=- Errors on flux (erg/cm2/s/Å)
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Acknowledgements:
Susanna Bisogni, susanna(at)arcetri.astro.it
References:
Goldoni, P., Royer, F., Francois, P., et al. 2006, in Presented at the
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference,
Vol. 6269, Society of Photo-Optical Instrumentation Engineers (SPIE)
Conference Series
Modigliani, A., Goldoni, P., Royer, F., et al. 2010, in Society of
Photo-Optical Instrumentation Engineers (SPIE) Conference Series,
Vol. 7737, Society of Photo-Optical Instrumentation Engineers (SPIE)
Conference Series
(End) Susanna Bisogni [Arcetri, Italia], Patricia Vannier [CDS] 08-Mar-2017