A Near-Infrared Spectral Template for Quasars

By E. Glikman, D. Helfand, R. White. 2005

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We present a near-infrared quasar composite spectrum spanning the wavelength range 0.58-3.5 μm. The spectrum has been constructed from observations of 27 quasars obtained at the NASA IRTF telescope and satisfying the criteria Ks < 14.5 and Mi < -23; the redshift range is 0.118 < z < 0.418. The signal-to-noise ratio is moderate, reaching a maximum of 150 between 1.6 and 1.9 μm. While a power-law fit to the continuum of the composite spectrum requires two breaks, a single power-law slope of α = -0.92 plus a 1260 K blackbody provides an excellent description of the spectrum from Hα to 3.5 μm, strongly suggesting the presence of significant quantities of hot dust in this blue-selected quasar sample. We measure intensities and line widths for 10 lines, finding that the Paschen line ratios rule out case B recombination. We compute K-corrections for the J, H, K, and Spitzer 3.6 μm bands, which will be useful in analyzing observations of quasars up to z = 10.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/303af3ca1ddc854254c5c2fd4540530694282b3c

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Citations in the corpus

Spitzer Quasar and ULIRG Evolution Study (QUEST). II. The Spectral Energy Distributions of Palomar-Green Quasars (2007, result): “We also compared our data with the recent Glikman et al. (2006) composite obtained from a sample of 27 AGNs that cover a redshift and luminosity range similar to the QUEST QSOs.”
Formation of z~6 Quasars from Hierarchical Galaxy Mergers (2006, background): “…al. 2003); and (4) a lack of evolution in the spectral energy distribution (SED) compared to lower redshift counterparts (e.g., Elvis et al. 1994; Glikman et al. 2006; Richards et al. 2006), which demonstrates the existence of ‘‘mature’’ quasars at early times and comparable metal enrichment in…”
CONSTRAINING EMISSION MODELS OF LUMINOUS BLAZAR SOURCES (2009, background): “On the other hand, we note that the nearIR quasar continua join the harder optical ones almost always around the same frequency, namely ∼1 μm, in both radio-quiet and radio-loud sources (Barvainis 1987; Glikman et al. 2006; Netzer et al. 2007; Labita et al. 2008).”
THE WIDE-FIELD INFRARED SURVEY EXPLORER (WISE): MISSION DESCRIPTION AND INITIAL ON-ORBIT PERFORMANCE (2010, background): “One of the highest redshift QSOs, SDSS 1148+5251, is shown in Figure 15, with data from Jiang et al. (2006) and a scaled composite spectrum constructed from Vanden Berk et al. (2001) and Glikman et al. (2006).”
The FIRST-2MASS Red Quasar Survey (2007, methodology): “Here we fit to each object a reddened quasar composite from the FIRST Bright Quasar Survey (Brotherton et al. 2001) combinedwith a near-infrared quasar composite (Glikman et al. 2006), resulting in wavelength coverage from 800 to 35000 8.”
THE NEXT GENERATION ATLAS OF QUASAR SPECTRAL ENERGY DISTRIBUTIONS FROM RADIO TO X-RAYS (2011, background): “…the comparison between our SEDs from Far-UV to Mid-IR and other quasar composite spectra, including the HST ultraviolet composites (Telfer et al. 2002), the composite from Sloan Digital Sky Survey (SDSS, Vanden Berk et al. 2001), and a Near-IR composite of 27 SDSS quasars (Glikman et al. 2006).”
A Census of Photometrically Selected Little Red Dots at 4 < z < 9 in JWST Blank Fields (2024, methodology): “The first one is the empirical model based on a composite of 2200 SDSS quasar spectra (Vanden Berk et al. 2001), and the second is derived from 27 near-infrared quasar spectra by Glikman et al. (2006).”