Xray luminosities scaling relations

class XrayLuminosity.XrayLuminosity[source]

The class XrayLuminosity is a wrapper to add Xray luminosity to the Multidark simulations results / outputs.

It adds Xray luminosity to simulations following the Bongiorno et al. 2016 model.

See http://adsabs.harvard.edu/abs/2016A%26A...588A..78B equations 7, 10, 11, 12

class XrayLuminosity.XrayLuminosity(Lbox=<Quantity 2500.0 Mpc>, boxDir='/home/comparat/data/MultiDark', snl=[], Hbox=<Quantity 67.77 km / (Mpc s)>, Melement=23593750000.0)[source]

Loads the environement to assign stellar masses to halos from dark matter only simulations, here MultiDark simulations.

  • Lbox – length of the box in Mpc/h
  • wdir – Path to the multidark lightcone directory
  • boxDir – box directory name
  • snl – list of snapshots available
  • zsl – list of redshift corresponding to the snapshots
  • zArray – redshift array to be considered to interpolate the redshift – distance conversion
  • Hbox – Hubble constant at redshift 0 of the box
  • Melement – Mass of the resolution element in solar masses.
  • columnDict – dictionnary to convert column name into the index to find it in the snapshots
fM(logM, z)[source]

Computes stellar mass component of the model $f_*$ (equation 10)

  • logM – stellar mass array
  • z – redshift array
fll(logM, z, ll)[source]

Computes the specific accretion rate component of the model $f_lambda$ (equation 11) :param logM: stellar mass :param z: redshift :param ll: log lambda SAR, specific accretion rate


Computes the redshift component of the model $f_z(z)$ (equation 12)

  • z – redshift array
  • z0 – redshift turn over
psi(logM, z, ll)[source]

Computes the bivariate distribution function (equation 7) :param logM: stellar mass :param z: redshift :param ll: log lambda SAR, specific accretion rate