Mason, Trenti & Treu (2015, 2022) UV luminosity function model 0 <= z <= 20
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LF/
contains the UV LF model, both with and without dust attenuation and for ST and Reed+07 hmf (see Assumptions below). Uncertainties are approx. 0.2-0.4 dex based on the calibration at z~5 (I would assume 0.2 dex at z<9, 0.3 dex at 9 < z < 13 and 0.4 dex at z>13). Columns are:- Muv[mag]
- log10_Phi_max (100% efficiency LF)
- log10_Phi_dust
- log10_Phi_nodust Phi units are #/mag/Mpc^3.
e.g. to plot the 'dust' model below at z=12 using the Reed+07 hmf use
z = 12
LF = np.genfromtxt(f'../../UVLF_model/LF/LF_z={z}_Reed07.txt')
plt.semilogy(LF[:,0], 10**LF[:,2])
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MUV_Mh/
contains the UV magnitude - halo mass relation, both with and without dust attenuation Muv_Mh. Columns are:- logMh [Msun]
- Muv[mag]
- Muv_dust[Mag] (which includes dust attenuation following Mason+15 eqn 4)
- We use hmf to calculate halo mass functions and use the Eisenstein & Hu 1998 (EH) transfer function as it works better than CAMB at high z
- We provide LFs calculated using both both Sheth-Tormen and Reed+07 halo mass functions. These are almost identical at z<10, but at z>10 ST predicts a higher abundance of massive halos. Reed+07 hmfs were derived using N-body simulations at z~10-30.
- Flat LCDM cosmology with h=0.7, Om0=0.3,
- For z<10 we use metallicity = 0.02 Z_sun, z>=10 we use Z = 0.01 Z_sun
If you use these models please include a citation to Mason, Trenti & Treu (2015) (for z < 10) and Mason, Trenti & Treu (2022) (for z >= 10).