139 research outputs found
Full-shape cosmology analysis of SDSS-III BOSS galaxy power spectrum using emulator-based halo model: a determination of
We present the results obtained from the full-shape cosmology analysis of the
redshift-space power spectra for 4 galaxy samples of the SDSS-III BOSS DR12
galaxy catalog over . For the theoretical template, we use an
emulator that was built from an ensemble set of -body simulations, which
enables fast and accurate computation of the redshift-space power spectrum of
halos. Combining with the halo occupation distribution to model the halo-galaxy
connection, we can compute the redshift-space power spectrum of BOSS-like
galaxies in the flat CDM cosmology. In our cosmology inference, we use
the power spectrum monopole, quadrupole and hexadecapole and include 7 nuisance
parameters to model uncertainties in the halo-galaxy connection for each galaxy
sample, but do not use any information on the abundance of galaxies. We
demonstrate a validation of our analysis pipeline using the mock catalogs of
BOSS-like galaxies, generated using different recipes of the halo-galaxy
connection and including the assembly bias effect. Assuming weak priors on
cosmological parameters, except for and , we
show that our model well reproduces the BOSS power spectra. Including the power
spectrum information up to , we find
, , and
, for the mode and 68\% credible interval,
after marginalization over nuisance parameters. We find little improvement in
the cosmological parameters beyond a maximum wavelength due to the shot noise domination and marginalization of
the halo-galaxy connection parameters. Our results are consistent with the
Planck CMB results within statistical uncertainties.Comment: 27 pages, 18 figures, accepted by Phys. Rev. D. The main results are
replaced with the analysis of the updated measurement of BOSS DR12 power
spectrum provided by Beutler & McDonald (2021, arXiv:2106.06324
Robustness of Baryon Acoustic Oscillations Measurements with Photometric Redshift Uncertainties
We investigate the robustness of baryon acoustic oscillations (BAO)
measurements with a photometric galaxy sample using mock galaxy catalogs with
various sizes of photometric redshift (photo-) uncertainties. We first
investigate the robustness of BAO measurements, assuming we have a perfect
knowledge of photo- uncertainties. We find that the BAO shift parameter
can be constrained in an unbiased manner for various sizes of
photometric redshift uncertainties at , , and as long as
the number density of galaxies is high. A sparse galaxy sample causes
additional noise in the covariance matrix calculation and it can bias the
constraint on . Next, we investigate the scenario where incorrect
photometric redshift uncertainties are assumed in the fitting model and find
that underestimating the photo- uncertainty leads to a degradation in the
constraining power on . In addition, we investigate BAO measurements
with a cross-correlation signal between a spec- sample and a photo-
sample. We find BAO constraints are unbiased and slightly tighter than the
auto-correlation signal of a photo- sample. We also quantify the
constraining power on assuming the LSST-like covariance and
find that the 95\% confidence level is -
corresponding to the photo- uncertainties of 1\% to 3\% respectively.
Finally, we examine whether the skewness in the photometric redshift can bias
the constraint on and confirm that the constraint on is
unbiased even if we use a fitting model assuming a Gaussian photo-
uncertainty.Comment: 10 pages, 11 figures, 3 table
On the Assembly Bias of Cool Core Clusters Traced by H Nebulae
Do cool-core (CC) and noncool-core (NCC) clusters live in different
environments? We make novel use of H emission lines in the central
galaxies of redMaPPer clusters as proxies to construct large (1,000's) samples
of CC and NCC clusters, and measure their relative assembly bias using both
clustering and weak lensing. We increase the statistical significance of the
bias measurements from clustering by cross-correlating the clusters with an
external galaxy redshift catalog from the Sloan Digital Sky Survey III, the
LOWZ sample. Our cross-correlations can constrain assembly bias up to a
statistical uncertainty of 6%. Given our H criteria for CC and NCC, we
find no significant differences in their clustering amplitude. Interpreting
this difference as the absence of halo assembly bias, our results rule out the
possibility of having different large-scale (tens of Mpc) environments as the
source of diversity observed in cluster cores. Combined with recent
observations of the overall mild evolution of CC and NCC properties, such as
central density and CC fraction, this would suggest that either the cooling
properties of the cluster core are determined early on solely by the local
(<200 kpc) gas properties at formation or that local merging leads to
stochastic CC relaxation and disruption in a periodic way, preserving the
average population properties over time. Studying the small-scale clustering in
clusters at high redshift would help shed light on the exact scenario.Comment: 17 pages, 9 figures, 2 tables, to be submitted to ApJ; comments
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