Bolometric Quasar Luminosity Function: Data & Routines | Phil Hopkins’ Research Group

Various routines, etc. from the paper: 

An Observational Determination of the Bolometric Quasar Luminosity Function

Hopkins, P. F., Richards, G. T., & Hernquist, L., 2006, ApJ, astro-ph/0605678


    A C script to return the quasar luminosity function from any of the analytic fits in the paper above, at arbitrary frequency (or the integrated bolometric, B-band, mid-IR, soft X-ray, or hard X-ray bands) and redshift. The beginning lines of the code explain its use and range of applicability.


    Another C script, this one returns the model intrinsic (un-reddened) quasar SED which we construct from various observations in the paper above, as a function of frequency and bolometric quasar luminosity. The beginning lines of the code describe its functionality. It is straightforward to use the C-code as a standalone, or there is a version designed to compiled as a shared library and called with an IDL script, available here.

Binned Bolometric QLF Data:

    This table contains the binned bolometric QLF data from the paper. At each of the redshifts z = 0.0, 0.1, 0.2, 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.5, 4.0, 4.5, 5.0, 5.5, 6.0, we include all binned data points from overlapping redshift intervals, from the entire collection of compiled luminosity functions given in Table 1 of the paper. Each point is rescaled as n_observed/n_model to a point on the bolometric QLF, given our best-fit SED, obscuration, and QLF shape/evolution model. Essentially, these are calculated just as the binned observations in the “bolometric luminosity” column of Figures 6 & 7. 

    The file header describes the format. One caution: the different redshifts listed are *not* independent, since many of the observations are binned in very large redshift intervals (e.g. z = 1.6 - 3.2), in which cases they appear at several of the more finely sampled redshifts here. 

Please, email me if you have any questions about using these routines and/or data, or would like to use the compiled observations in a different format. I’m happy to oblige. 

© Philip Hopkins 2015