def abundanceMatchSnapshot(proxy,
scatter,
lf,
box_size,
minmag=-25.,
maxmag=10.,
debug=False,
figname=None):
af = AbundanceFunction(lf['mag'],
lf['phi'],
ext_range=(minmag, maxmag),
nbin=2000,
faint_end_fit_points=6)
# check the abundance function
if debug:
plt.clf()
plt.semilogy(lf['mag'], lf['phi'])
x = np.linspace(minmag, maxmag, 101)
plt.semilogy(x, af(x))
plt.savefig('abundance_fcn.png')
# deconvolution and check results (it's a good idea to always check this)
remainder = af.deconvolute(scatter * LF_SCATTER_MULT, 40)
x, nd = af.get_number_density_table()
if debug:
plt.clf()
plt.semilogy(x, np.abs(remainder / nd))
plt.savefig('nd_remainder.png')
# get number densities of the halo catalog
nd_halos = calc_number_densities(proxy, box_size)
# do abundance matching with some scatter
catalog_sc = af.match(nd_halos, scatter * LF_SCATTER_MULT)
if debug:
plt.clf()
c, e = np.histogram(catalog_sc[~np.isnan(catalog_sc)],
bins=np.linspace(minmag, maxmag, 101))
c = c / box_size**3 / (e[1:] - e[:-1])
me = (e[:-1] + e[1:]) / 2
plt.semilogy(me, c)
plt.semilogy(me, af(me))
plt.savefig('lf_in_v_out.png')
return catalog_sc
def comp_deconv_steps(lf, scatters, deconv_repeats, m_max=-25):
""" Generate the projected 2D correlation by abundance matching galaxies
Parameters:
lf: The luminosity function. The first column is the magnitudes and the
second column is the density in units of 1/Mpc^3.
scatters: The scatters to deconvolve / re-introduce in the am (must
be a list)
Returns:
w_p(r_p) at the r_p values specified by r_p_data.
"""
# Initialize abundance function and calculate the number density of the
# halos in the box
af = AbundanceFunction(lf[:, 0], lf[:, 1], (-25, -5))
f, ax = plt.subplots(len(scatters),
1,
sharex='col',
sharey='row',
figsize=(13, 16))
ax[-1].set_xlabel('Magnitude (M - 5 log h)')
x, nd = af.get_number_density_table()
# For each scatter and each number of deconvolution steps, plot the
# dependence of the remainder on the step.
for s_i in range(len(scatters)):
scatter = scatters[s_i]
y_max = 0
legend = []
for deconv_repeat in deconv_repeats:
remainder = af.deconvolute(scatter * LF_SCATTER_MULT,
deconv_repeat) / nd
ax[s_i].plot(x,
remainder,
lw=3,
c=custom_blues_complement[len(legend)])
y_max = max(y_max, np.max(remainder[x > m_max]))
legend.append('Deconvolution Steps = %d' % (deconv_repeat))
ax[s_i].set_ylabel('(LF (deconv $\Rightarrow$ conv) - LF) / LF')
ax[s_i].set_xlim([np.max(lf[:, 0]) - 2, m_max])
ax[s_i].set_ylim([-1.2, y_max * 1.2])
ax[s_i].set_title('Luminosity Function Remainder %.2f Scatter' %
(scatter))
ax[0].legend(legend)
def generate_wp(lf_list,
halos,
af_criteria,
r_p_data,
box_size,
mag_cuts,
pimax=40.0,
nthreads=1,
scatters=None,
deconv_repeat=20,
verbose=False):
""" Generate the projected 2D correlation by abundance matching galaxies
Parameters:
lf_list: A list of luminosity functions for each mag_cut. The first
column is the magnitudes and thesecond column is the density in
units of 1/Mpc^3.
halos: A catalog of the halos in the n-body sim that can be indexed
into using the quantity name.
af_criteria: The galaxy property (i.e. vpeak) to use for abundance
matching.
r_p_data: The positions at which to calculate the 2D correlation
function.
box_size: The size of the box (box length not volume)
mag_cuts: The magnitude cuts for w_p(r_p) (must be a list)
pimax: The maximum redshift seperation to use in w_p(r_p) calculation
nthreads: The number of threads to use for CorrFunc
scatters: The scatters to deconvolve / re-introduce in the am (must
be a list)
deconv_repeat: The number of deconvolution steps to conduct
verbose: If set to true, will generate plots for visual inspection
of am outputs.
Returns:
w_p(r_p) at the r_p values specified by r_p_data.
"""
# Repeat once for each magnitude cut
wp_binneds = []
for mag_cut_i in range(len(mag_cuts)):
mag_cut = mag_cuts[mag_cut_i]
lf = lf_list[mag_cut_i]
# Initialize abundance function and calculate the number density of the
# halos in the box
af = AbundanceFunction(lf[:, 0], lf[:, 1], (-25, -5))
nd_halos = calc_number_densities(halos[af_criteria], box_size)
if scatters is not None:
remainders = []
for scatter in scatters:
remainders.append(
af.deconvolute(scatter * LF_SCATTER_MULT, deconv_repeat))
# If verbose output the match between abundance function and input data
if verbose:
matplotlib.rcParams.update({'font.size': 18})
plt.figure(figsize=(10, 8))
plt.plot(lf[:, 0], lf[:, 1], lw=7, c=custom_blues[1])
x = np.linspace(np.min(lf[:, 0]) - 2, np.max(lf[:, 0]) + 2, 101)
plt.semilogy(x, af(x), lw=3, c=custom_blues[4])
plt.xlim([np.max(lf[:, 0]) + 2, np.min(lf[:, 0])])
plt.ylim([1e-5, 1])
plt.xlabel('Magnitude (M - 5 log h)')
plt.ylabel('Number Density (1/ (Mpc^3 h))')
plt.legend(['Input', 'Fit'])
plt.title('Luminosity Function')
plt.yscale('log')
plt.show()
# Plot remainder to ensure the deconvolution returned reasonable results
if verbose and scatters is not None:
f, ax = plt.subplots(2,
1,
sharex='col',
sharey='row',
figsize=(15, 12),
gridspec_kw={'height_ratios': [2, 1]})
x, nd = af.get_number_density_table()
ax[0].plot(x, nd, lw=3, c=custom_blues[4])
legend = []
for scatter in scatters:
ax[0].plot(af._x_deconv[float(scatter * LF_SCATTER_MULT)],
nd,
lw=3,
c=custom_blues_complement[2 * len(legend)])
legend.append('Scatter = %.2f' % (scatter))
ax[0].set_xlim([np.max(lf[:, 0]) + 2, np.min(lf[:, 0])])
ax[0].set_ylim([1e-5, 1])
ax[0].set_ylabel('Number Density (1/ (Mpc^3 h))')
ax[0].legend(['Fit'] + legend)
ax[0].set_title('Deconvolved Luminosity Function')
ax[0].set_yscale('log')
ax[1].set_xlabel('Magnitude (M - 5 log h)')
ax[1].set_ylabel('(LF (deconv $\Rightarrow$ conv) - LF) / LF')
ax[1].set_xlim([np.max(lf[:, 0]) + 2, np.min(lf[:, 0])])
y_max = 0
for r_i in range(len(remainders)):
remainder = remainders[r_i] / nd
ax[1].plot(x,
remainder,
lw=3,
c=custom_blues_complement[2 * r_i])
y_max = max(y_max, np.max(remainder[x > np.min(lf[:, 0])]))
ax[1].set_ylim([-1.2, y_max * 1.2])
plt.show()
# Conduct the abundance matching
catalogs = []
if scatters is not None:
for scatter in scatters:
catalogs.append(
af.match(nd_halos,
scatter * LF_SCATTER_MULT,
do_rematch=False))
else:
catalogs = [af.match(nd_halos)]
wp_scatts = []
for catalog in catalogs:
# A luminosity cutoff to use for the correlation function.
sub_catalog = catalog < mag_cut
print('Scatter %.2f catalog has %d galaxies' %
(scatters[len(wp_scatts)], np.sum(sub_catalog)))
x = halos['px'][sub_catalog]
y = halos['py'][sub_catalog]
z = halos['pz'][sub_catalog]
# Generate rbins so that the average falls at r_p_data
rbins = np.zeros(len(r_p_data) + 1)
rbins[1:-1] = 0.5 * (r_p_data[:-1] + r_p_data[1:])
rbins[0] = 2 * r_p_data[0] - rbins[1]
rbins[-1] = 2 * r_p_data[-1] - rbins[-2]
# Calculate the projected correlation function
wp_results = wp(box_size,
pimax,
nthreads,
rbins,
x,
y,
z,
verbose=False,
output_rpavg=True)
# Extract the results
wp_binned = np.zeros(len(wp_results))
for i in range(len(wp_results)):
wp_binned[i] = wp_results[i][3]
wp_scatts.append(wp_binned)
wp_binneds.append(wp_scatts)
return wp_binneds