175 research outputs found
The Dark Energy Survey
We describe the Dark Energy Survey (DES), a proposed optical-near infrared
survey of 5000 sq. deg of the South Galactic Cap to ~24th magnitude in SDSS
griz, that would use a new 3 sq. deg CCD camera to be mounted on the Blanco 4-m
telescope at Cerro Telolo Inter-American Observatory (CTIO). The survey data
will allow us to measure the dark energy and dark matter densities and the dark
energy equation of state through four independent methods: galaxy clusters,
weak gravitational lensing tomography, galaxy angular clustering, and supernova
distances. These methods are doubly complementary: they constrain different
combinations of cosmological model parameters and are subject to different
systematic errors. By deriving the four sets of measurements from the same data
set with a common analysis framework, we will obtain important cross checks of
the systematic errors and thereby make a substantial and robust advance in the
precision of dark energy measurements.Comment: White Paper submitted to the Dark Energy Task Force, 42 page
The Dark Energy Survey
We describe the Dark Energy Survey (DES), a proposed optical-near infrared survey of 5000 sq. deg of the South Galactic Cap to ~24th magnitude in SDSS griz, that would use a new 3 sq. deg CCD camera to be mounted on the Blanco 4-m telescope at Cerro Telolo Inter-American Observatory (CTIO). The survey data will allow us to measure the dark energy and dark matter densities and the dark energy equation of state through four independent methods: galaxy clusters, weak gravitational lensing tomography, galaxy angular clustering, and supernova distances. These methods are doubly complementary: they constrain different combinations of cosmological model parameters and are subject to different systematic errors. By deriving the four sets of measurements from the same data set with a common analysis framework, we will obtain important cross checks of the systematic errors and thereby make a substantial and robust advance in the precision of dark energy measurements
Maximizing survey volume for large-area multi-epoch surveys with Voronoi tessellation
The survey volume of a proper motion-limited sample is typically much smaller than a magnitude-limited sample. This is because of the noisy astrometric measurements from detectors that are not dedicated for astrometric missions. In order to apply an empirical completeness correction, existing works limit the survey depth to the shallower parts of the sky that hamper the maximum potential of a survey. The number of epoch of measurement is a discrete quantity that cannot be interpolated across the projected plane of observation, so that the survey properties change in discrete steps across the sky. This work proposes a method to dissect the survey into small parts with Voronoi tessellation using candidate objects as generating points such that each part defines a ‘mini-survey’ that has its own properties. Coupling with a maximum volume density estimator, the new method is demonstrated to be unbiased and recovered ∼20 per cent more objects than the existing method in a mock catalogue of a white dwarf-only solar neighbourhood with Pan–STARRS 1-like characteristics. Towards the end of this work, we demonstrate one way to increase the tessellation resolution with artificial generating points, which would be useful for analysis of rare objects with small number counts
Anisotropy in the matter distribution beyond the baryonic acoustic oscillation scale
Tracing the cosmic evolution of the Baryonic Acoustic Oscillation (BAO) scale
with galaxy two point correlation functions is currently the most promising
approach to detect dark energy at early times. A number of ongoing and future
experiments will measure the BAO peak with unprecedented accuracy. We show
based on a set of N-Body simulations that the matter distribution is
anisotropic out to ~150 Mpc/h, far beyond the BAO scale of ~100M pc/h, and
discuss implications for the measurement of the BAO. To that purpose we use
alignment correlation functions, i.e., cross correlation functions between high
density peaks and the overall matter distribution measured along the
orientation of the peaks and perpendicular to it. The correlation function
measured along (perpendicular to) the orientation of high density peaks is
enhanced (reduced) by a factor of ~2 compared to the conventional correlation
function and the location of the BAO peak shifts towards smaller (larger)
scales if measured along (perpendicular to) the orientation of the high density
peaks. Similar effects are expected to shape observed galaxy correlation
functions at BAO scales.Comment: 4 pages, 3 figures, accepted for publication in ApJ
Cosmological parameter constraints from galaxy–galaxy lensing and galaxy clustering with the SDSS DR7
Recent studies have shown that the cross-correlation coefficient between galaxies and dark matter is very close to unity on scales outside a few virial radii of galaxy haloes, independent of the details of how galaxies populate dark matter haloes. This finding makes it possible to determine the dark matter clustering from measurements of galaxy–galaxy weak lensing and galaxy clustering. We present new cosmological parameter constraints based on large-scale measurements of spectroscopic galaxy samples from the Sloan Digital Sky Survey (SDSS) data release 7. We generalize the approach of Baldauf et al. to remove small-scale information (below 2 and 4 h^(−1) Mpc for lensing and clustering measurements, respectively), where the cross-correlation coefficient differs from unity. We derive constraints for three galaxy samples covering 7131 deg^2, containing 69 150, 62 150 and 35 088 galaxies with mean redshifts of 0.11, 0.28 and 0.40. We clearly detect scale-dependent galaxy bias for the more luminous galaxy samples, at a level consistent with theoretical expectations. When we vary both σ_8 and Ω_m (and marginalize over non-linear galaxy bias) in a flat Λ cold dark matter model, the best-constrained quantity is σ_8(Ω_m/0.25)^(0.57) = 0.80 ± 0.05 (1σ, stat. + sys.), where statistical and systematic errors (photometric redshift and shear calibration) have comparable contributions, and we have fixed n_s = 0.96 and h = 0.7. These strong constraints on the matter clustering suggest that this method is competitive with cosmic shear in current data, while having very complementary and in some ways less serious systematics. We therefore expect that this method will play a prominent role in future weak lensing surveys. When we combine these data with Wilkinson Microwave Anisotropy Probe 7-year (WMAP7) cosmic microwave background (CMB) data, constraints on σ_8, Ω_m, H_0, w_(de) and ∑m_ν become 30–80 per cent tighter than with CMB data alone, since our data break several parameter degeneracies
Lensing Bias in Cosmic Shear
Only galaxies bright enough and large enough to be unambiguously identified
and measured are included in galaxy surveys used to estimate cosmic shear. We
demonstrate that because gravitational lensing can scatter galaxies across the
brightness and size thresholds, cosmic shear experiments suffer from lensing
bias. We calculate the effect on the shear power spectrum and show that -
unless corrected for - it will lead analysts to cosmological parameters
estimates that are biased at the 2-3\sigma level in DETF Stage III experiments,
such as the Dark Energy Survey.Comment: 14 pages; 4 figures (this version). Accepted for publication in ApJ.
v2: incorporating referee's comments; v3: updated acknowledgment
SDSS quasars in the WISE preliminary data release and quasar candidate selection with optical/infrared colors
We present a catalog of 37,842 quasars in the SDSS Data Release 7, which have
counterparts within 6" in the WISE Preliminary Data Release. The overall WISE
detection rate of the SDSS quasars is 86.7%, and it decreases to less than
50.0% when the quasar magnitude is fainter than . We derive the median
color-redshift relations based on this SDSS-WISE quasar sample and apply them
to estimate the photometric redshifts of the SDSS-WISE quasars. We find that by
adding the WISE W1- and W2-band data to the SDSS photometry we can increase the
photometric redshift reliability, defined as the percentage of sources with the
photometric and spectroscopic redshift difference less than 0.2, from 70.3% to
77.2%. We also obtain the samples of WISE-detected normal and late-type stars
with SDSS spectroscopy, and present a criterion in the versus
color-color diagram, , to separate quasars from stars.
With this criterion we can recover 98.6% of 3089 radio-detected SDSS-WISE
quasars with redshifts less than four and overcome the difficulty in selecting
quasars with redshifts between 2.2 and 3 from SDSS photometric data alone. We
also suggest another criterion involving the WISE color only, , to
efficiently separate quasars with redshifts less than 3.2 from stars. In
addition, we compile a catalog of 5614 SDSS quasars detected by both WISE and
UKIDSS surveys and present their color-redshift relations in the optical and
infrared bands. By using the SDSS , UKIDSS YJHK and WISE W1- and W2-band
photometric data, we can efficiently select quasar candidates and increase the
photometric redshift reliability up to 87.0%. We discuss the implications of
our results on the future quasar surveys. An updated SDSS-WISE quasar catalog
consisting of 101,853 quasars with the recently released WISE all-sky data is
also provided.Comment: 27 pages, 9 figures and 5 tables. Revised to match the published
version in the Astronomical Journal. 5 tables are available electronically at
(http://vega.bac.pku.edu.cn/~wuxb/sdsswiseqso.htm). A new SDSS-WISE quasar
catalog consisting of 101,853 quasars with the WISE all-sky data is available
as Table
Lensing is low: cosmology, galaxy formation or new physics?
We present high signal-to-noise galaxy-galaxy lensing measurements of the
BOSS CMASS sample using 250 square degrees of weak lensing data from CFHTLenS
and CS82. We compare this signal with predictions from mock catalogs trained to
match observables including the stellar mass function and the projected and two
dimensional clustering of CMASS. We show that the clustering of CMASS, together
with standard models of the galaxy-halo connection, robustly predicts a lensing
signal that is 20-40% larger than observed. Detailed tests show that our
results are robust to a variety of systematic effects. Lowering the value of
compared to Planck2015
reconciles the lensing with clustering. However, given the scale of our
measurement ( Mpc), other effects may also be at play and need
to be taken into consideration. We explore the impact of baryon physics,
assembly bias, massive neutrinos, and modifications to general relativity on
and show that several of these effects may be non-negligible
given the precision of our measurement. Disentangling cosmological effects from
the details of the galaxy-halo connection, the effects of baryons, and massive
neutrinos, is the next challenge facing joint lensing and clustering analyses.
This is especially true in the context of large galaxy samples from Baryon
Acoustic Oscillation surveys with precise measurements but complex selection
functions.Comment: 26 pages. Submitted to MNRAS. Comments welcom
The Dark Energy Survey Data Processing and Calibration System
The Dark Energy Survey (DES) is a 5000 deg2 grizY survey reaching
characteristic photometric depths of 24th magnitude (10 sigma) and enabling
accurate photometry and morphology of objects ten times fainter than in SDSS.
Preparations for DES have included building a dedicated 3 deg2 CCD camera
(DECam), upgrading the existing CTIO Blanco 4m telescope and developing a new
high performance computing (HPC) enabled data management system (DESDM).
The DESDM system will be used for processing, calibrating and serving the DES
data. The total data volumes are high (~2PB), and so considerable effort has
gone into designing an automated processing and quality control system. Special
purpose image detrending and photometric calibration codes have been developed
to meet the data quality requirements, while survey astrometric calibration,
coaddition and cataloging rely on new extensions of the AstrOmatic codes which
now include tools for PSF modeling, PSF homogenization, PSF corrected model
fitting cataloging and joint model fitting across multiple input images.
The DESDM system has been deployed on dedicated development clusters and HPC
systems in the US and Germany. An extensive program of testing with small rapid
turn-around and larger campaign simulated datasets has been carried out. The
system has also been tested on large real datasets, including Blanco Cosmology
Survey data from the Mosaic2 camera. In Fall 2012 the DESDM system will be used
for DECam commissioning, and, thereafter, the system will go into full science
operations.Comment: 12 pages, submitted for publication in SPIE Proceeding 8451-1
Multi-messenger Observations of a Binary Neutron Star Merger
On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of 1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg at a luminosity distance of Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Msun. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at 40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over 10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position 9 and 16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. (Abridged
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