AA/2016/30143 Simultaneous detection and analysis of optical and ultraviolet broad emission lines in Quasars at z ~ 2.2 (Bisogni+, 2017) =============================================================================== Simultaneous detection and analysis of optical and ultraviolet broad emission lines in Quasars at z ~ 2.2 Susanna Bisogni, Sperello di Serego Alighieri, Paolo Goldoni, Luis C. Ho, Alessandro Marconi, Gabriele Ponti, Guido Risaliti =2017A&A...?..? =============================================================================== Keywords: galaxies: active - galaxies:nuclei - galaxies: Seyfert quasars: emission lines - quasars: general Abstract: We studied the spectra of six z \sim 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 \sim 1200-7000\AA 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 H$\alpha$, MgII and CIV with respect to H$\beta$. H$\alpha$ and MgII linewidths correlate well with H$\beta$, 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 \sim 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/∆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; Modigliani et al. 2010). File Summary: ------------------------------------------------------------------------------- filename Lrecl Records Explanations ------------------------------------------------------------------------------- readme 80 . This file UVB_J093147.dat 39 14845 J093147 UVB arm reduced spectrum VIS_J093147.dat 39 24457 J093147 VIS arm reduced spectrum NIR_J093147.dat 39 29701 J093147 NIR arm reduced spectrum UVB_J103325.dat 39 14845 J103325 UVB arm reduced spectrum VIS_J103325.dat 39 24457 J103325 VIS arm reduced spectrum NIR_J103325.dat 39 29700 J103325 NIR arm reduced spectrum UVB_J105239.dat 39 14845 J105239 UVB arm reduced spectrum VIS_J105239.dat 39 24457 J105239 VIS arm reduced spectrum NIR_J105239.dat 39 29701 J105239 NIR arm reduced spectrum UVB_J121911.dat 39 14845 J121911 UVB arm reduced spectrum VIS_J121911.dat 39 24457 J121911 VIS arm reduced spectrum NIR_J121911.dat 39 29701 J121911 NIR arm reduced spectrum UVB_J123120.dat 39 14845 J123120 UVB arm reduced spectrum VIS_J123120.dat 39 24457 J123120 VIS arm reduced spectrum NIR_J123120.dat 39 29181 J123120 NIR arm reduced spectrum UVB_J124220.dat 39 14845 J124220 UVB arm reduced spectrum VIS_J124220.dat 39 24457 J124220 VIS arm reduced spectrum NIR_J124220.dat 39 29181 J124220 NIR arm reduced spectrum -------------------------------------------------------------------------------- Byte-by-byte Description of file: ARM_NAME_sourcename.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1 F1 nm wl wavelength array 2 E1 ergs/cm2/s/AA sp array of fluxes 3 E1 ergs/cm2/s/AA sp_err array of errors on fluxes -------------------------------------------------------------------------------- Acknowledgements: Susanna Bisogni (susanna@arcetri.astro.it) References: Goldoni, P., Royer, F., Fran ̧cois, 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 8-Mar-2017