An example showing how to scale a galaxy’s mass by luminosity/flux.

Parametric galaxies scale their brightness based on their initial stellar mass which is passed at instantiation. This example shows how a galaxy can later be scaled in terms of mass to achieve a particular brightness in a particular filter.

plot scale by luminosity
36307.8054770101 nJy

import matplotlib.pyplot as plt
import numpy as np
from astropy.cosmology import Planck18 as cosmo
from matplotlib.lines import Line2D
from unyt import Hz, Msun, Myr, erg, nJy, s

from synthesizer import galaxy
from synthesizer.conversions import apparent_mag_to_fnu, fnu_to_lnu
from synthesizer.emission_models import PacmanEmission
from synthesizer.emission_models.attenuation import PowerLaw
from synthesizer.filters import Filter
from synthesizer.grid import Grid
from synthesizer.parametric import SFH, Stars, ZDist

# Set up a figure to plot on
fig = plt.figure()
ax_lum = fig.add_subplot(111)

# Set up the flux y axis
ax_flux = ax_lum.twinx()

# Enforce logscale
ax_lum.loglog()
ax_flux.loglog()

# Define the grid
grid_name = "test_grid"
grid_dir = "../../tests/test_grid/"
grid = Grid(grid_name, grid_dir=grid_dir)

# Define the emission model
model = PacmanEmission(
    grid,
    fesc=0.5,
    fesc_ly_alpha=0.5,
    tau_v=0.1,
    dust_curve=PowerLaw(slope=-1),
)

# Set up the SFH
sfh = SFH.Constant(max_age=100 * Myr)

# Set up the metallicity distribution
metal_dist = ZDist.Normal(mean=0.01, sigma=0.005)

# Get the stellar population
stars = Stars(
    grid.log10age,
    grid.metallicity,
    sf_hist=sfh,
    metal_dist=metal_dist,
    initial_mass=10**9 * Msun,
)

# And make a galaxy containing this stellar population
redshift = 12
gal = galaxy(stars=stars, redshift=redshift)

# Generate spectra using pacman model (complex)
gal.stars.get_spectra(model)

# Get the observed spectra
gal.get_observed_spectra(cosmo=cosmo)

# Plot the original spectra
ax_lum.plot(
    gal.stars.spectra["attenuated"]._lam,
    gal.stars.spectra["attenuated"]._lnu,
    color="m",
    linestyle="--",
    alpha=0.7,
)
ax_flux.plot(
    gal.stars.spectra["attenuated"]._obslam,
    gal.stars.spectra["attenuated"]._fnu,
    color="m",
    label=(
        r"Original ($\log_{10}(M_\star / M_\odot)"
        + f"={np.log10(gal.stars.initial_mass):.2f})$"
    ),
    alpha=0.7,
)

# Define a filter in which we will scale the galaxy
f = Filter(filter_code="JWST/NIRCam.F150W", new_lam=grid.lam)

# First lets scale by luminosity
scale_lum = 10**25.0 * erg / s / Hz
gal.stars.scale_mass_by_luminosity(
    lum=scale_lum,
    scale_filter=f,
    spectra_type="attenuated",
)

# Plot the luminosity scaled spectra
ax_lum.plot(
    gal.stars.spectra["attenuated"]._lam,
    gal.stars.spectra["attenuated"]._lnu,
    color="c",
    linestyle="--",
    alpha=0.7,
)
ax_flux.plot(
    gal.stars.spectra["attenuated"]._obslam,
    gal.stars.spectra["attenuated"]._fnu,
    color="c",
    label=(
        r"Luminosity scaled ($\log_{10}(M_\star / M_\odot)"
        + f"={np.log10(gal.stars.initial_mass):.2f})$"
    ),
    alpha=0.7,
)

# And scale by flux
scale_flux = apparent_mag_to_fnu(20)
print(scale_flux)
gal.stars.scale_mass_by_flux(
    flux=scale_flux,
    scale_filter=f,
    spectra_type="attenuated",
)

# Plot the luminosity scaled spectra
ax_lum.plot(
    gal.stars.spectra["attenuated"]._lam,
    gal.stars.spectra["attenuated"]._lnu,
    color="orange",
    linestyle="--",
    alpha=0.7,
)
ax_flux.plot(
    gal.stars.spectra["attenuated"]._obslam,
    gal.stars.spectra["attenuated"]._fnu,
    color="orange",
    label=(
        r"Flux scaled ($\log_{10}(M_\star / M_\odot)"
        + f"={np.log10(gal.stars.initial_mass):.2f})$"
    ),
    alpha=0.7,
)

# Label axes
x_units = str(gal.stars.spectra["attenuated"].lam.units)
y_units_lnu = str(gal.stars.spectra["attenuated"].lnu.units)
y_units_fnu = str(gal.stars.spectra["attenuated"].fnu.units)
ax_lum.set_xlabel(r"$\lambda/[\mathrm{" + x_units + r"}]$")
ax_lum.set_ylabel(r"$L_{\nu}/[\mathrm{" + y_units_lnu + r"}]$")
ax_flux.set_ylabel(r"$F_{\nu}/[\mathrm{" + y_units_fnu + r"}]$")


# Make the legend
legend_handles = [
    Line2D([0], [0], color="k", linestyle="--"),
    Line2D([0], [0], color="k", linestyle="-"),
]
legend_labels = ["Luminosity", "Flux"]
ax_flux.legend(loc="upper right")
ax_lum.legend(handles=legend_handles, labels=legend_labels, loc="upper left")

ax_lum.set_ylim(
    fnu_to_lnu(10**-4 * nJy, cosmo, redshift=redshift),
    fnu_to_lnu(10**12.5 * nJy, cosmo, redshift=redshift),
)
ax_flux.set_ylim(10**-4, 10**12.5)
ax_lum.set_xlim(10**2, None)
ax_flux.set_xlim(10**2, None)
plt.show()

Total running time of the script: (0 minutes 0.767 seconds)

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