QSOSED_MODELS#
Name#
QSOSED_MODELS
Purpose#
Generates the spectra and X-ray parameters for the QSOSED model as described in Kubota & Done (2018). The spectra can include or not include Galactic absorption.
Calling Sequence#
model_agn_count_rate = qsosed_models(redshift, wave_rest, arf_interp, exp_neg_tau_xray_MW, $
galactic_nH, lumin_dist [, Lnu_x_agn=Lnu_x_agn, $
L2500=L2500, agn_mass=agn_mass, agn_logmdot=agn_logmdot])
Inputs#
redshift
int, float, or double scalarThe redshift of the model.
wave_rest
int, float or double array(Nwave)The rest-frame wavelengths at which to interpolate the qsosed models \([\mu \rm m]\).
arf_interp
double array(Nwave)A grid of ARF values interpolated from the input ARF file \([{\rm cm}^2]\).
exp_neg_tau_xray_MW
float or double array(Nwave)The attenuation from the Milky Way to be applied to the X-ray data in terms of \(e^{-\tau}\).
galactic_nH
int, float, or double scalarGalactic, i.e. Milky Way, neutral Hydrogen column density along the line of sight \([10^{20}\ {\rm cm}^2]\).
lumin_dist
int, float, double scalarThe luminosity distance of the model \([{\rm Mpc}]\).
Output#
model_agn_count_rate
double array(Nwave, Nmass, Nmdot)Instrumental count rate density produced by qsosed model grid \([{\rm counts\ s^{-1}\ Hz^{-1}}]\).
Optional Outputs#
Lnu_x_agn
double array(Nwave, Nmass, Nmdot)The qsosed model luminosity \([L_\odot\ {\rm Hz}^{-1}]\).
L2500
double array(Nmass, Nmdot)The rest-frame 2500 Angstrom monochromatic luminosity shifted to the observed frame \([L_\odot\ {\rm Hz}^{-1}]\).
agn_mass
double array(Nmass, Nmdot)The SMBH mass grid \([M_\odot]\).
agn_logmdot
double array(Nmass, Nmdot)The Log10 of SMBH accretion rate grid, normalized by the Eddington rate.
Reference#
Modification History#
2021/09/21: Created (Erik B. Monson).
2022/06/22: Moved to separate file and documentation improved (Keith Doore).
2022/06/22: Major update to include new implementation (Keith Doore)
2022/11/02: Galactic NH is now in units of 1e20 cm-2 (Erik B. Monson)