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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 (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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 111 6 Sample and observations properties sp/* 42 18 Individual spectra
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 ( 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) 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
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.
Byte-by-byte Description of file: sp/*
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)
Acknowledgements: Susanna Bisogni, susanna(at) 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
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

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