Pop III X-ray Binary Emissivities

Specific X-ray emissivities from Pop III XRBs calculated for "The Mass Distribution of the First Stars can be Determined via the 21-cm Signal" using the methodology of Sartorio et al. 2023. Separate emissivities are given for each of the six potential Pop III IMFs considered in that work, along with the corresponding integrated luminosity and specific abundance of XRBs. See the above paper for details of this data set's modelling and assumptions.

The data set is stored in a hdf5 file, xray_emissivities.hdf5, divided into six top-level groups, one for each of the considered Pop III IMFs. The naming of these groups follows the convention of starting with  pop_III_ followed by the IMFs minimum mass, maximum mass, and exponent (as outlined in the paper) separated by underscores, e.g.,

pop_III_0.8_250_2.35 : Sal IMF

pop_III_2_180_2 : Int-2 IMF

pop_III_2_180_1 : Int-1 IMF

pop_III_2_180_0.5 : Int-0.5 IMF

pop_III_2_180_0 : Int-0 IMF

pop_III_10_500_0 : Top IMF

Each of these six top-level groups contains four data sets:

specific_xray_emissivity : The X-ray emissivity of Pop III XRBs per unit Pop III star formation in erg Hz^-1 Msol^-1 (as depicted in Fig 1b)

frequencies_hz : The frequencies the above is stored at in Hz

fX_III : The integrated specific X-ray emissivity in the band 0.20 to 95.65 keV (as listed in Table 1)

XRBs_per_SFR : Average abundace of Pop III XRBs per Pop III SFR in yr Msol^-1 (see Sartorio et al. 2023 Table 2)