lsst_inaf_agile.zou2024
Implements Zou+2024 p(lambda_SAR | M_star, z).
The specific accretion rate is defined as the ratio of the 2-10 keV intrinsic X-ray luminosity and the host galaxy stellar mass lambda_SAR = LX / Mstar.
Zou+2024 model the p(lambda_SAR | Mstar, z) as a piecewise double power law function, where the power law index depends on the critical lambda_SAR,c.
Their observed sample is based on 8000 X-ray AGN and 1.3M normal galaxies compiled from the CANDELS, LSST DDFs, and eFEDS. Nominally the sample is valid for z < 4 and M_star > 1e9.5 Msun.
References
https://ui.adsabs.harvard.edu/abs/2024ApJ…964..183Z/abstract
Attributes
Functions
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Return power law index gamma. |
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Return log10 of p(lambda) = A * (lambda / lambda_c)^gamma. |
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Return analytic integral of $p(lambda)$ up to specific accretoin rate $lambda$. |
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Return inverse of the analytic integral of $p(lambda)$ i.e. $P^{-1}$. |
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Return Zou+2024 parameters at the given physical parameters. |
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Return log10 of $p(lambda)$ for the given physical parameters. |
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Return log10 of $P(lambda)$ for the given physical parameters. |
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Return log10 of $P^{-1}(lambda)$ for the given physical parameters. |
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Return a (double) Schechter function. |
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Return the analytic form of the X-ray luminosity function. |
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Return Wright+2018 stellar mass function. |
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Return the X-ray luminosity function implied by $p(lambda)$. |
Return the specific accretion rate distribution function. |
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Return the fraction of CTK AGN from Ueda+2014. |
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Return the accretion rate distribution of the CTK AGN population. |
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Return the total (CTN + CTK) $log p(lambda)$. |
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Return log_lambda_sar sampled from the p(lambda). |
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Return the AGN fraction given the physical parameters. |
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Return $lambda_mathrm{min}$ at which $p(lambda)$ integrates to unity. |
Plot Fig. 10 from Zou+2024. |
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Plot the $lambda_mathrm{min}$ in terms of $z$ and $M_mathrm{star}$. |
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Plot $p(lambda)$ separately for CTN and CTK AGN. |
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Plot the X-ray luminosity function. |
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Test the extrapolation accuracy from different extrapolation strategies. |
Module Contents
- _get_gamma(loglambda, loglambdac, gamma1, gamma2)[source]
Return power law index gamma.
- Parameters:
loglambda (float or array_like) – log10 of the specific accretion rate.
loglambdac (float) – log10 of the critical specific accretion rate.
gamma1 – gamma, where loglambda < loglambdac
gamma2 – gamma, where loglambda < loglambdac
- Returns:
gamma – power law index defined as gamma1 if loglambda < loglambdac else gamma2.
- Return type:
float
- _get_log_plambda(loglambda, logA, loglambdac, gamma1, gamma2)[source]
Return log10 of p(lambda) = A * (lambda / lambda_c)^gamma.
- _get_log_Plambda(loglambda, logA, loglambdac, gamma1, gamma2)[source]
Return analytic integral of $p(lambda)$ up to specific accretoin rate $lambda$.
- _get_inv_log_Plambda(log_Plambda, logA, loglambdac, gamma1, gamma2)[source]
Return inverse of the analytic integral of $p(lambda)$ i.e. $P^{-1}$.
- _get_parameters(log_mstar, z, t, log_mstar_lim=(-np.inf, np.inf), z_lim=(-np.inf, np.inf))[source]
Return Zou+2024 parameters at the given physical parameters.
- Parameters:
log_mstar (float) – log10 of the galaxy stellar mass
z (float) – redshift
t (str) – galaxy type, one of “main”, “starforming”, or “quiescent”
log_mstar_lim (tuple[float, float]) – stellar mass limits for controlling boundary extrapolation
z_lim (tuple[float, float]) – redshift limits for controlling boundary extrapolation
- Returns:
(A, loglambdac, gamma1, gamma2) – Zou+2024 parameters.
- Return type:
tuple[float, float, float, float]
- get_log_plambda(loglambda, log_mstar, z, t, *args, **kwargs)[source]
Return log10 of $p(lambda)$ for the given physical parameters.
- get_log_Plambda(loglambda, log_mstar, z, t)[source]
Return log10 of $P(lambda)$ for the given physical parameters.
- get_inv_log_Plambda(log_Plambda, log_mstar, z, t)[source]
Return log10 of $P^{-1}(lambda)$ for the given physical parameters.
- get_schechter(logM, logMstar, alpha1, phi1, alpha2=np.nan, phi2=np.nan, factor=LN10)[source]
Return a (double) Schechter function.
Implements Eq. 8 from Weaver+2020.
- get_xray_luminosity_function_analytic(log_lx, z, log_mstar_min, log_mstar_max, dlog_mstar)[source]
Return the analytic form of the X-ray luminosity function.
- get_stellar_mass_function_wright2018(log_mstar, z, t='all')[source]
Return Wright+2018 stellar mass function.
- get_xray_luminosity_function(log_lx, z, fun_phi_star=get_stellar_mass_function_wright2018, t='all', log_mstar_min=8.0, log_mstar_max=13.0, dlog_mstar=0.01, log_lambda_sar_min=-np.inf, log_lambda_sar_max=+np.inf, check_plambda_ctk=False, *args, **kwargs)[source]
Return the X-ray luminosity function implied by $p(lambda)$.
The X-ray luminosity function may be derived as the product of the galaxy stellar mass function and $p(lambda)$.
- get_specific_accretion_rate_distribution_function(loglambda, log_mstar, z, t='all', dlog_mstar=0.1)[source]
Return the specific accretion rate distribution function.
The specific accretion rate distribution is the product of the galaxy stellar mass function and the accretion rate probability.
- get_log_plambda_ctk(loglambda, m, z, t, test_integral=True, *args, **kwargs)[source]
Return the accretion rate distribution of the CTK AGN population.
Combines the accretion rate distribution of Zou+2024 (CTN AGN) and the CTK AGN fraction of Ueda+2014. The p_CTK is defined as:
p_tot = p_ctn + p_ctk
p_tot = p_ctn / (1 - f_CTK_AGN)
so that
p_CTK = f_CTK_AGN / (1 - f_CTK_AGN) * p_CTN
where the CTK AGN fraction is defined as
f_CTK_AGN equiv N_CTK / (N_CTN + N_CTK)
and p_CTN is the accretion rate distribution of CTN AGN.
- get_log_plambda_total(loglambda, mstar, z, t, test_integral=True, *args, **kwargs)[source]
Return the total (CTN + CTK) $log p(lambda)$.
- get_log_lambda_SAR(m, z, t, add_ctk=True, dlog_lambda=0.001, Nsample=1, *args, **kwargs)[source]
Return log_lambda_sar sampled from the p(lambda).
- get_fraction_agn(xmin, mstar, z, t, add_ctk=True, *args, **kwargs)[source]
Return the AGN fraction given the physical parameters.
The AGN fraction is defined as the integral of $p(lambda)$ from $lambda = 10^{32}$ (erg/s/Msun).
- get_log_lambda_min(mstar, z, t, *args, **kwargs)[source]
Return $lambda_mathrm{min}$ at which $p(lambda)$ integrates to unity.