1,312 research outputs found
Dependence of Self-Assembled Peptide Hydrogel Network Structure on Local Fibril Nanostructure
Physically cross-linked, fibrillar hydrogel networks are formed by the self-assembly of β-hairpin peptide molecules with varying degrees of strand asymmetry. The peptide registry in the self-assembled state can be used as a design element to generate fibrils with twisting, nontwisting, or laminated morphology. The mass density of the networks varies significantly, and can be directly related to the local fibrillar morphology as evidenced by small angle neutron scattering (SANS) and in situ substantiation using cryogenic transmission electron microscopy (cryo-TEM) under identical concentrations and conditions. Similarly, the density of the network is dependent on changes in the peptide concentration. Bulk rheological properties of the hydrogels can be correlated to the fibrillar nanostructure, with the stiffer, laminated fibrils forming networks with a higher G′ as compared to the flexible, singular fibrillar networks
The Weak Lensing Signal and the Clustering of BOSS Galaxies I: Measurements
A joint analysis of the clustering of galaxies and their weak gravitational
lensing signal is well-suited to simultaneously constrain the galaxy-halo
connection as well as the cosmological parameters by breaking the degeneracy
between galaxy bias and the amplitude of clustering signal. In a series of two
papers, we perform such an analysis at the highest redshift () in
the literature using CMASS galaxies in the Sloan Digital Sky Survey-III Baryon
Oscillation Spectroscopic Survey Eleventh Data Release (SDSS-III/BOSS DR11)
catalog spanning 8300~deg. In this paper, we present details of the
clustering and weak lensing measurements of these galaxies. We define a
subsample of 400,916 CMASS galaxies based on their redshifts and stellar mass
estimates so that the galaxies constitute an approximately volume-limited and
similar population over the redshift range . We obtain a
signal-to-noise ratio for the galaxy clustering measurement. We
also explore the redshift and stellar mass dependence of the clustering signal.
For the weak lensing measurement, we use existing deeper imaging data from the
CFHTLS with publicly available shape and photometric redshift catalogs from
CFHTLenS, but only in a 105~deg area which overlaps with BOSS. This
restricts the lensing measurement to only 5,084 CMASS galaxies. After careful
systematic tests, we find a highly significant detection of the CMASS weak
lensing signal, with total . These measurements form the basis of
the halo occupation distribution and cosmology analysis presented in More et
al. (Paper II).Comment: 15 pages, 13 figures. Accepted for publication in the Astrophysical
Journa
The Stripe 82 Massive Galaxy Project II: Stellar Mass Completeness of Spectroscopic Galaxy Samples from the Baryon Oscillation Spectroscopic Survey
The Baryon Oscillation Spectroscopic Survey (BOSS) has collected spectra for
over one million galaxies at over a volume of 15.3 Gpc (9,376
deg) -- providing us an opportunity to study the most massive galaxy
populations with vanishing sample variance. However, BOSS samples are selected
via complex color cuts that are optimized for cosmology studies, not galaxy
science. In this paper, we supplement BOSS samples with photometric redshifts
from the Stripe 82 Massive Galaxy Catalog and measure the total galaxy stellar
mass function (SMF) at and . With the total SMF in hand,
we characterize the stellar mass completeness of BOSS samples. The
high-redshift CMASS ("constant mass") sample is significantly impacted by mass
incompleteness and is 80% complete at only in
the narrow redshift range . The low redshift LOWZ sample is 80%
complete at for . To construct
mass complete samples at lower masses, spectroscopic samples need to be
significantly supplemented by photometric redshifts. This work will enable
future studies to better utilize the BOSS samples for galaxy-formation science.Comment: 18 pages, 17 figures, 5 table
The large-scale Quasar-Lyman \alpha\ Forest Cross-Correlation from BOSS
We measure the large-scale cross-correlation of quasars with the Lyman
\alpha\ forest absorption in redshift space, using ~ 60000 quasar spectra from
Data Release 9 (DR9) of the Baryon Oscillation Spectroscopic Survey (BOSS). The
cross-correlation is detected over a wide range of scales, up to comoving
separations r of 80 Mpc/h. For r > 15 Mpc/h, we show that the cross-correlation
is well fitted by the linear theory prediction for the mean overdensity around
a quasar host halo in the standard \Lambda CDM model, with the redshift
distortions indicative of gravitational evolution detected at high confidence.
Using previous determinations of the Lyman \alpha\ forest bias factor obtained
from the Lyman \alpha\ autocorrelation, we infer the quasar bias factor to be
b_q = 3.64^+0.13_-0.15 at a mean redshift z=2.38, in agreement with previous
measurements from the quasar auto-correlation. We also obtain a new estimate of
the Lyman \alpha\ forest redshift distortion factor, \beta_F = 1.1 +/- 0.15,
slightly larger than but consistent with the previous measurement from the
Lyman \alpha\ forest autocorrelation. The simple linear model we use fails at
separations r < 15 Mpc/h, and we show that this may reasonably be due to the
enhanced ionization due to radiation from the quasars. We also provide the
expected correction that the mass overdensity around the quasar implies for
measurements of the ionizing radiation background from the line-of-sight
proximity effect.Comment: 24 pages, 6 figures, published in JCA
The High-Mass End of the Red Sequence at z~0.55 from SDSS-III/BOSS: completeness, bimodality and luminosity function
We have developed an analytical method based on forward-modeling techniques
to characterize the high-mass end of the red sequence (RS) galaxy population at
redshift , from the DR10 BOSS CMASS spectroscopic sample, which
comprises galaxies. The method, which follows an unbinned maximum
likelihood approach, allows the deconvolution of the intrinsic CMASS
colour-colour-magnitude distributions from photometric errors and selection
effects. This procedure requires modeling the covariance matrix for the i-band
magnitude, g-r colour and r-i colour using Stripe 82 multi-epoch data. Our
results indicate that the error-deconvolved intrinsic RS distribution is
consistent, within the photometric uncertainties, with a single point
() in the colour-colour plane at fixed magnitude, for a
narrow redshift slice. We have computed the high-mass end () of the -band RS Luminosity Function (RS LF) in several redshift
slices within the redshift range . In this narrow redshift range,
the evolution of the RS LF is consistent, within the uncertainties in the
modeling, with a passively-evolving model with Mpc mag, fading at a rate of mag per
unit redshift. We report RS completeness as a function of magnitude and
redshift in the CMASS sample, which will facilitate a variety of
galaxy-evolution and clustering studies using BOSS. Our forward-modeling method
lays the foundations for future studies using other dark-energy surveys like
eBOSS or DESI, which are affected by the same type of photometric
blurring/selection effects.Comment: 27 pages, 20 figures, accepted for publication in MNRA
Stochastic bias of colour-selected BAO tracers by joint clustering-weak lensing analysis
The baryon acoustic oscillation (BAO) feature in the two-point correlation
function of galaxies supplies a standard ruler to probe the expansion history
of the Universe. We study here several galaxy selection schemes, aiming at
building an emission-line galaxy (ELG) sample in the redshift range
, that would be suitable for future BAO studies, providing a highly
biased galaxy sample. We analyse the angular galaxy clustering of galaxy
selections at the redshifts 0.5, 0.7, 0.8, 1 and 1.2 and we combine this
analysis with a halo occupation distribution (HOD) model to derive the
properties of the haloes these galaxies inhabit, in particular the galaxy bias
on large scales. We also perform a weak lensing analysis (aperture statistics)
to extract the galaxy bias and the cross-correlation coefficient and compare to
the HOD prediction.
We apply this analysis on a data set composed of the photometry of the deep
co-addition on Sloan Digital Sky Survey (SDSS) Stripe 82 (225 deg), of
Canda-France-Hawai Telescope/Stripe 82 deep \emph{i}-band weak lensing survey
and of the {\it Wide-Field Infrared Survey Explorer}infrared photometric band
W1.
The analysis on the SDSS-III/constant mass galaxies selection at is
in agreement with previous studies on the tracer, moreover we measure its
cross-correlation coefficient . For the higher redshift bins, we
confirm the trends that the brightest galaxy populations selected are strongly
biased (), but we are limited by current data sets depth to derive
precise values of the galaxy bias. A survey using such tracers of the mass
field will guarantee a high significance detection of the BAO.Comment: 17 pages, 15 figures, submitted to MNRA
Beyond CDM constraints from the full shape clustering measurements from BOSS and eBOSS
We analyse the full shape of anisotropic clustering measurements from the
extended Baryon Oscillation Spectroscopic survey (eBOSS) quasar sample together
with the combined galaxy sample from the Baryon Oscillation Spectroscopic
Survey (BOSS). We obtain constraints on the cosmological parameters independent
of the Hubble parameter for the extensions of the CDM models,
focusing on cosmologies with free dark energy equation of state parameter .
We combine the clustering constraints with those from the latest CMB data from
Planck to obtain joint constraints for these cosmologies for and the
additional extension parameters - its time evolution , the physical
curvature density and the neutrino mass sum . Our
joint constraints are consistent with flat CDM cosmological model
within 68\% confidence limits. We demonstrate that the Planck data are able to
place tight constraints on the clustering amplitude today, , in
cosmologies with varying and present the first constraints for the
clustering amplitude for such cosmologies, which is found to be slightly higher
than the CDM value. Additionally, we show that when we vary and
allow for non-flat cosmologies and the physical curvature density is used,
Planck prefers a curved universe at significance, which is
higher than when using the relative curvature density
. Finally, when is varied freely, clustering provides only
a modest improvement (of 0.021 eV) on the upper limit of .Comment: 12 pages, 6 figures, submitted to MNRA
- …