THE NEXT GENERATION ATLAS OF QUASAR SPECTRAL ENERGY DISTRIBUTIONS FROM RADIO TO X-RAYS

By Zhaohui Shang, M. Brotherton, B. Wills, D. Wills, S. Cales, D. Dale, R. Green, J. Runnoe, R. Nemmen, S. C. Gallagher and 7 more. 2011

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We have produced the next generation of quasar spectral energy distributions (SEDs), essentially updating the work of Elvis et al. by using high-quality data obtained with several space- and ground-based telescopes, including NASA's Great Observatories. We present an atlas of SEDs of 85 optically bright, non-blazar quasars over the electromagnetic spectrum from radio to X-rays. The heterogeneous sample includes 27 radio-quiet and 58 radio-loud quasars. Most objects have quasi-simultaneous ultraviolet–optical spectroscopic data, supplemented with some far-ultraviolet spectra, and more than half also have Spitzer mid-infrared Infrared Spectrograph spectra. The X-ray spectral parameters are collected from the literature where available. The radio, far-infrared, and near-infrared photometric data are also obtained from either the literature or new observations. We construct composite SEDs for radio-loud and radio-quiet objects and compare these to those of Elvis et al., finding that ours have similar overall shapes, but our improved spectral resolution reveals more detailed features, especially in the mid- and near-infrared.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/35e8208bd4f067801617d292d735d7161e198212

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Citations in the corpus

Erratum: Updating quasar bolometric luminosity corrections (2012, methodology): “There have been other recent investigations of quasar SEDs as well (Shang et al. 2011; Richards et al. 2006), those that focus on specific wavelength regimes (e.g., Mullaney et al. 2011; Nemmen & Brotherton 2010; Netzer et al. 2007; Vasudevan & Fabian 2007; Shang et al. 2005), those that focus on…”
THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: THE QUASAR LUMINOSITY FUNCTION FROM DATA RELEASE NINE (2012, background): “Often a break is added to the near UV where a softer spectrum is observed (αUV ∼ −1.7, Telfer et al. 2002; Shang et al. 2005, 2011).”
THE MAN BEHIND THE CURTAIN: X-RAYS DRIVE THE UV THROUGH NIR VARIABILITY IN THE 2013 ACTIVE GALACTIC NUCLEUS OUTBURST IN NGC 2617 (2013, unknown): “In the right panel of Figure 10 we also show the composite SED for radio-quiet quasars of Shang et al. (2011) scale to match in theSwift UV fluxes.”
A TWO-PARAMETER MODEL FOR THE INFRARED/SUBMILLIMETER/RADIO SPECTRAL ENERGY DISTRIBUTIONS OF GALAXIES AND ACTIVE GALACTIC NUCLEI (2014, methodology): “Shi et al. (2013) utilize Spitzer infrared spectral (5–30 µm) and imaging (24, 70, & 160 µm) data from all PG quasars to generate a median mid-infrared spectrum similar to that of Shang et al. (2011).”
The first ultraviolet quasar-stacked spectrum at z ≃ 2.4 from WFC3 (2015, background): “…and possible luminosity dependence of the BBB has not been properly estimated due to the lack of UV observations corrected for the intergalactic medium (IGM) absorption by neutral hydrogen along the line of sight (Richards et al. 2006a; Trammell et al. 2007; Shang et al. 2011; Elvis et al. 2012).”
The bright end of the galaxy luminosity function at z≃7: before the onset of mass quenching? (2013, background): “The average quasar SEDs from Shang et al. (2011) suggests that if one of our candidates was a typical radio-loud quasar, it would just be detectable in the X-ray and radio imaging (see Figure 6 of Ouchi et al. 2009b).”