In this tutorial, we will give an overview of the phenomenological galaxy population model that is used in the galsbi package. It will explain how galaxy catalogs are generated and how the model can be customized. Generally, we assume that galaxies are split into two populations: star-forming (or blue) galaxies and quiescent (or red) galaxies.
The first step in generating a galaxy catalog is to define the luminosity function for each galaxy population as a function of redshift. We use two independent Schechter functions for both populations parametrized by the following parameters:
where the parameter \(\alpha\) can be defined in galsbi with lum_fct_alpha_blue
and lum_fct_alpha_red
.
For \(M^*(z)\) and \(\phi^*(z)\), GalSBI offers the following parametrizations:
The parameters \(M^*_1\), \(M^*_2\), \(\phi^*_1\), \(\phi^*_2\), and \(z_0\) can be defined using the following names:
\(M^*_1\): lum_fct_m_star_blue_intcpt
and lum_fct_m_star_red_intcpt
\(M^*_2\): lum_fct_m_star_blue_slope
and lum_fct_m_star_red_slope
\(\phi^*_1\): lum_fct_phi_star_blue_amp
and lum_fct_phi_star_red_amp
\(\phi^*_2\): lum_fct_phi_star_blue_exp
and lum_fct_phi_star_red_exp
\(z_0\): lum_fct_z_const_blue
and lum_fct_z_const_red
Sampling galaxies from the luminosity function creates a catalog of galaxies with redshifts and absolute magnitude. Changing the parameters of the luminosity function therefore changes the number of galaxies, the redshift distribution and the magnitude distribution. The impact of the different parameters on the luminosity function is illustrated in the interactive figure below.
This figure shows the luminosity function for star-forming galaxies (blue) and quiescent galaxies (red) for different redshifts and a simulated HSC deep field images generated with these luminosity functions (with the other parameters following the posterior from Fischbacher+2024). The sliders allow you to change the parameters of the luminosity function and see how the galaxy population and the images change. Since deep fields are typically dominated by blue galaxies, the impact of changing the parameters is more pronounced for the blue galaxy population. Intuitively, \(M^*_1\) controls the knee of the luminosity function at redshift 0 and \(M^*_2\) controls the evolution of the knee with redshift. \(\phi^*_1\) controls the amplitude of the luminosity function at redshift 0 and \(\phi^*_2\) controls the evolution of the amplitude with redshift. And \(\alpha\) controls the slope of the luminosity function at the faint end.
In a next step, we assign a spectrum to each galaxy. Given the spectrum and the redshift, the apparent magnitude in each filter band can be computed by integrating the redshifted spectrum over the filter throughput. The spectra are assigned as a linear combination of the kcorrect template from Blanton and Roweis (2007), see the figure below.
The template coefficients describe the relative contribution of each template to the galaxy spectrum.
After defining the spectra, it is rescaled to match the absolute magnitude of the galaxy.
Since only the relative contribution of the templates is important, the sum of these coefficients can be set to 1.
This is exactly the support of a Dirichlet distribution with the number of components equal to the number of templates.
The standard Dirichlet distribution of order 5 is parametrized by the concentration parameter \(\alpha=(\alpha_1, \ldots, \alpha_5)\).
The concentration parameters are sampled at redshift 0 and and at a redshift defined by template_coeff_z1_blue
and template_coeff_z1_red
.
Redshifts in between are interpolated by
The concentration parameters can be defined by the following names:
template_coeff_alpha0_blue_i
and template_coeff_alpha0_red_i
for \(\alpha_{i,z=0}\) with \(i=1, \ldots, 5\)
template_coeff_alpha1_blue_i
and template_coeff_alpha1_red_i
for \(\alpha_{i,z=z_1}\) with \(i=1, \ldots, 5\)
GalSBI offers different parametrizations of the Dirichlet distribution:
This is the standard Dirichlet distribution with the concentration parameter \(\alpha\) following the text book definition and was used in Herbel+2018.
In this parameterization, the distribution is parametrized by the modes of each component and the standard deviation.
Both mode and standard deviation are clearly defined for a Dirichlet distribution such that given
the mode and standard deviation, the concentration parameter can be computed.
The modes are still defined with the same GalSBI parameters as above.
The standard deviation is defined by template_coeff_alpha0_std_blue
and template_coeff_alpha1_std_blue
and for red correspondingly.
This parametrization has the advantage that defining the distribution by its mode and
standard deviation increases the interpretability of the parameters.
The last step in generating a galaxy catalog is to assign a morphological parameters to each galaxy. This includes the size, the ellipticity, and the light profile.
In GalSBI, we sample the the half-light radius \(r_{50}\) from a lognormal distribution with mean \(\mu_{\log r_{50}}(M)\) and standard deviation \(\sigma_{\log r_{50}}(M)\), where both mean and standard deviation can depend on the absolute magnitude \(M\). The following parametrizations are currently available:
In this parametrization, the standard deviation is constant across all magnitudes and
defined by the parameter logr50_phys_std
.
and the mean is parametrized as a linear function of the absolute magnitude with the following parameters:
logr50_phys_mean_intcpt
, logr50_phys_mean_slope
This parametrization is similar to the single parametrization but the parameters are
different for red and blue galaxies. The parameters are:
logr50_phys_mean_intcpt_blue
, logr50_phys_mean_slope_blue
, logr50_phys_std_blue
,
logr50_phys_mean_intcpt_red
, logr50_phys_mean_slope_red
, logr50_phys_std_red
This parametrization follows the fitting function Shen et al. (2003). It adds a non-linear dependence of the mean on the absolute magnitude for blue galaxies and a non-constant standard deviation. The mean and standard deviation are parametrized as follows:
The parameters in GalSBI are logr50_sdss_fit_sigma1_blue
, logr50_sdss_fit_sigma2_blue
,
logr50_sdss_fit_M0_blue
, logr50_sdss_fit_alpha_blue
, logr50_sdss_fit_beta_blue
,
logr50_sdss_fit_gamma_blue
for blue galaxies and
logr50_sdss_fit_sigma1_red
, logr50_sdss_fit_sigma2_red
,
logr50_sdss_fit_M0_red
, logr50_sdss_fit_a_red
, logr50_sdss_fit_b_red
for red galaxies.
Furthermore, GalSBI includes a parametrization of the size evolution with redshift.
For this the sampled size is rescaled by a factor \((1+z)^{\alpha_{r_{50}}}\).
The parameter \(\alpha_{r_{50}}\) can be defined by logr50_alpha
for the single and
by logr50_alpha_blue
and logr50_alpha_red
for the other two parametrizations.
An interactive figure showing the impact of the different parameters of the sdss_fit parametrization is shown below including the redshift evolution of the size (with the parameter called eta to avoid confusion with the alpha parameter). Because we increase the half-light radius of the galaxies but keep the magnitude fixed, the galaxies become fainter when the size increases. At the same time, decreasing the size makes the galaxies more compact and more round as soon as the size is comparable to the PSF. The plot also highlights that changing some of these parameters, although the varied ranges exceed the posterior distribution of these parameters dramatically, lead to changes in the image that are barely visible by eye. This demonstrates how sophistacted the inference of these parameters has to be.
439:<iframe src=”/galsbi-dash/run-dash-sersic” width=900 height=900 style=”border: 1px solid #aaa;”></iframe>
The ellipticity of a galaxy is defined as a complex number \(e = e_1 + i e_2\). The magnitude of the ellipticity (typically called absolute ellipticity) is defined as \(e_\mathrm{abs}= \sqrt{e_1^2 + e_2^2}\). The shape of a galaxy for different ellipticities is shown in the figure below.
To sample the ellipticity, GalSBI offers the following parametrizations:
In this parametrization, the ellipticity is sampled from a gaussian distribution with mean
and standard deviation parametrized by e1_mean
, e1_sigma
, e2_mean
, e2_sigma
.
It is made sure that the absolute ellipticity is smaller than 1.
Same as the default parametrization but the parameters are different for blue and red galaxies.
The parameters are e1_mean_blue
, e1_sigma_blue
, e2_mean_blue
, e2_sigma_blue
,
e1_mean_red
, e1_sigma_red
, e2_mean_red
, e2_sigma_red
.
This parametrization follows the parametrization of Miller et al. (2013), see Equation B2 and B3. The blue galaxies are sampled from the following distribution:
with \(e_\mathrm{max} = 0.8\) and the other parameters can be defined using
ell_disc_log_a
for \(\log(a)\), ell_disc_pow_alpha
for \(\alpha\) and ell_disc_min_e
for \(e_\mathrm{min}\).
The red galaxies are sampled from the following distribution:
with the parameters ell_bulge_b
for \(b\) and \(c=6.691\).
After sampling the absolute ellipticity, the phase is sampled uniformly between 0 and 2pi and the complex ellipticity is converted to the real and imaginary part \(e_1\) and \(e_2\).
This parametrization samples the absolute ellipticity from a beta distribution which is
bounded between 0 and 1 and is parametrized by two shape parameters \(\alpha\) and \(\beta\).
The parameters are ell_beta_ab_ratio
and ell_beta_ab_sum
where the ratio is
computed as \(\alpha / (\alpha + \beta)\) and the sum as \(\alpha + \beta\).
For all ellipticity methods based on the beta distribution, there is also an additional parameter
ell_beta_emax
which defines the maximum value of the ellipticity.
This parametrization samples the absolute ellipticity from a beta distribution using two parameters
ell_beta_ab_sum
and ell_beta_ab_mode
.
The sum is the same as in the beta_ratio parametrization and the mode is definded as \(\frac{\alpha-1}{\alpha+\beta-2}\).
Same as the beta_mode parametrization but the parameters are different for blue and red galaxies.
The parameters are ell_beta_ab_sum_blue
, ell_beta_ab_mode_blue
, ell_beta_ab_sum_red
, ell_beta_ab_mode_red
.
The light profile of galaxies is defined by the Sersic profile:
where \(I_0\) is the intensity at the center, \(R_e\) is the effective radius, \(n\) is the Sersic index, and \(b_n\) is a constant that depends on \(n\). GalSBI offers the following parametrizations for the Sersic profile:
In this parametrization, the Sersic index is sampled from the distribution proposed by Berge et al. (2013),
see Appendix A.1.
It defines two distributions, one for the bright galaxies and one for the faint galaxies.
The bright sample is sampled from two lognormal distributions with the following parameters:
sersic_n_mean_1_hi
, sersic_n_sigma_1_hi
, sersic_n_mean_2_hi
, sersic_n_sigma_2_hi
.
The faint sample is based on one lognormal distribution with the following parameters:
sersic_n_mean_low
, sersic_n_sigma_low
.
All the distributions are offset by the parameter sersic_n_offset
.
In this parametrization, the Sersic index is fixed to the values sersic_index_blue
and sersic_index_red
for blue and red galaxies, respectively.
In this parametrization, the Sersic index is fixed to the value sersic_single_value
.
In this parametrization, the Sersic index is sampled from a beta prime distribution.
The parameters are sersic_betaprime_blue_mode
, sersic_betaprime_blue_size
and sersic_betaprime_blue_mode_alpha
(and correspondingly for red galaxies).
The size relates directly to the classical beta parameter \(\beta\) of the beta prime distribution.
The mode characterizes the peak of the distribution at redshift 0 and
the mode alpha characterizes the redshift evolution of the mode.
The traditional \(\alpha\) parameter of the beta prime distribution is therefore
The impact of the different parameters for the blue_red_betaprime
parametrization is illustrated in the interactive figure below.
No, if a specific model is passed to the GalSBI class, all the configurations and parameter values are set automatically based on the model. For example, the following code snippet will
from galsbi import GalSBI
model = GalSBI(model="Fischbacher+24", model_index=96)
sets all the parametrizations based on the fiducial model of Fischbacher et al. (2024) and sets all the parameter values to the 96th sample of the posterior distribution.
GalSBI is based on the following papers:
Fischbacher et al. (2024): GalSBI: Phenomenological galaxy population model for cosmology using simulation-based inference
Moser et al. (2024): Simulation-based inference of deep fields: galaxy population model and redshift distributions
Tortorelli et al. (2021): The PAU Survey: Measurement of Narrow-band galaxy properties with Approximate Bayesian Computation
Tortorelli et al. (2020): Measurement of the B-band Galaxy Luminosity Function with Approximate Bayesian Computation
Kacprzak et al. (2020): Monte Carlo Control Loops for cosmic shear cosmology with DES Year 1
Herbel et al. (2018): The redshift distribution of cosmological samples: a forward modeling approach
Further references used for the parametrizations are:
Berge et al. (2013): An Ultra Fast Image Generator (UFig) for wide-field astronomy
Miller et al. (2013): Bayesian galaxy shape measurement for weak lensing surveys – III. Application to the Canada–France–Hawaii Telescope Lensing Survey
Blanton and Roweis (2007): K-corrections and filter transformations in the ultraviolet, optical, and near infrared
Shen et al. (2003): The size distribution of galaxies in the Sloan Digital Sky Survey