167 research outputs found
The two-point correlation function covariance with fewer mocks
We present FITCOV an approach for accurate estimation of the covariance of two-point correlation functions that requires fewer mocks than the standard mock-based covariance. This can be achieved by dividing a set of mocks into jackknife regions and fitting the correction term first introduced in Mohammad & Percival (2022), such that the mean of the jackknife covariances corresponds to the one from the mocks. This extends the model beyond the shot-noise limited regime, allowing it to be used for denser samples of galaxies. We test the performance of our fitted jackknife approach, both in terms of accuracy and precision, using lognormal mocks with varying densities and approximate EZmocks mimicking the Dark Energy Spectroscopic Instrument LRG and ELG samples in the redshift range of z = [0.8, 1.1]. We find that the MohammadâPercival correction produces a bias in the two-point correlation function covariance matrix that grows with number density and that our fitted jackknife approach does not. We also study the effect of the covariance on the uncertainty of cosmological parameters by performing a full-shape analysis. We demonstrate that our fitted jackknife approach based on 25 mocks can recover unbiased and as precise cosmological parameters as the ones obtained from a covariance matrix based on 1000 or 1500 mocks, while the MohammadâPercival correction produces uncertainties that are twice as large. The number of mocks required to obtain an accurate estimation of the covariance for the two-point correlation function is therefore reduced by a factor of 40â60. The FITCOV code that accompanies this paper is available at this GitHub repository
Intrinsic alignment as an RSD contaminant in the DESI survey
We measure the tidal alignment of the major axes of luminous red galaxies (LRGs) from the Legacy Imaging Survey and use it to infer the artificial redshift-space distortion signature that will arise from an orientation-dependent, surface-brightness selection in the Dark Energy Spectroscopic Instrument (DESI) survey. Using photometric redshifts to downweight the shapeâdensity correlations due to weak lensing, we measure the intrinsic tidal alignment of LRGs. Separately, we estimate the net polarization of LRG orientations from DESIâs fibre-magnitude target selection to be of order 10-2 along the line of sight. Using these measurements and a linear tidal model, we forecast a 0.5 per cent fractional decrease on the quadrupole of the two-point correlation function for projected separations of 40â80 h-1 Mpc. We also use a halo catalogue from the ABACUSSUMMIT cosmological simulation suite to reproduce this false quadrupole
DAHe white dwarfs from the DESI survey
A new class of white dwarfs, dubbed DAHe, that present Zeeman-split Balmer
lines in emission has recently emerged. However, the physical origin of these
emission lines remains unclear. We present here a sample of 21 newly identified
DAHe systems and determine magnetic field strengths and (for a subset) periods
which span the ranges of ~ 6.5 -- 147 MG and ~ 0.4 -- 36 h respectively. All
but four of these systems were identified from the Dark Energy Spectroscopic
Instrument (DESI) survey sample of more than 47000 white dwarf candidates
observed during its first year of observations. We present detailed analysis of
the new DAHe WDJ161634.36+541011.51 with a spin period of 95.3 min, which
exhibits an anti-correlation between broadband flux and Balmer line strength
that is typically observed for this class of systems. All DAHe systems cluster
closely on the Gaia Hertzsprung-Russell diagram where they represent ~ 1 per
cent of white dwarfs within that region. This grouping further solidifies their
unexplained emergence at relatively late cooling times and we discuss this in
context of current formation theories. Nine of the new DAHe systems are
identifiable from SDSS spectra of white dwarfs that had been previously
classified as featureless DC-type systems. We suggest high S/N, unbiased
observations of DCs as a possible route for discovering additional DAHe
systems.Comment: 19 pages, 10 Figures, accepted for publication in MNRA
A framework to measure the properties of intergalactic metal systems with two-point flux statistics
The abundance, temperature, and clustering of metals in the intergalactic
medium are important parameters for understanding their cosmic evolution and
quantifying their impact on cosmological analysis with the Ly forest.
The properties of these systems are typically measured from individual quasar
spectra redward of the quasar's Ly emission line, yet that approach
may provide biased results due to selection effects. We present an alternative
approach to measure these properties in an unbiased manner with the two-point
statistics commonly employed to quantify large-scale structure. Our model
treats the observed flux of a large sample of quasar spectra as a continuous
field and describes the one-dimensional, two-point statistics of this field
with three parameters per ion: the abundance (column density distribution),
temperature (Doppler parameter) and clustering (cloud-cloud correlation
function). We demonstrate this approach on multiple ions (e.g., C IV, Si IV, Mg
II) with early data from the Dark Energy Spectroscopic Instrument (DESI) and
high-resolution spectra from the literature. Our initial results show some
evidence that the C IV abundance is higher than previous measurements and
evidence for abundance evolution over time. The first full year of DESI
observations will have over an order of magnitude more quasar spectra than this
study. In a future paper we will use those data to measure the growth of
clustering and its impact on the Ly forest, as well as test other DESI
analysis infrastructure such as the pipeline noise estimates and the resolution
matrix.Comment: 15 pages, 14 figure
A data compression and optimal galaxy weights scheme for Dark Energy Spectroscopic Instrument and weak lensing data sets
Combining different observational probes, such as galaxy clustering and weak lensing, is a promising technique for unveiling the physics of the Universe with upcoming dark energy experiments. The galaxy redshift sample from the Dark Energy Spectroscopic Instrument (DESI) will have a significant overlap with major ongoing imaging surveys specifically designed for weak lensing measurements: The Kilo-Degree Survey (KiDS), the Dark Energy Survey (DES), and the Hyper Suprime-Cam (HSC) survey. In this work, we analyse simulated redshift and lensing catalogues to establish a new strategy for combining high-quality cosmological imaging and spectroscopic data, in view of the first-year data assembly analysis of DESI. In a test case fitting for a reduced parameter set, we employ an optimal data compression scheme able to identify those aspects of the data that are most sensitive to cosmological information and amplify them with respect to other aspects of the data. We find this optimal compression approach is able to preserve all the information related to the growth of structures
Analysis of the impact of broad absorption lines on quasar redshift measurements with synthetic observations
Accurate quasar classifications and redshift measurements are increasingly important to precision cosmology experiments. Broad absorption line (BAL) features are present in 15-20 per cent of all quasars, and these features can introduce systematic redshift errors, and in extreme cases produce misclassifications. We quantitatively investigate the impact of BAL features on quasar classifications and redshift measurements with synthetic spectra that were designed to match observations by the Dark Energy Spectroscopic Instrument (DESI) survey. Over the course of 5 yr, DESI aims to measure spectra for 40 million galaxies and quasars, including nearly three million quasars. Our synthetic quasar spectra match the signal-to-noise ratio and redshift distributions of the first year of DESI observations, and include the same synthetic quasar spectra both with and without BAL features. We demonstrate that masking the locations of the BAL features decreases the redshift errors by about 1 per cent and reduces the number of catastrophic redshift errors by about 80 per cent. We conclude that identifying and masking BAL troughs should be a standard part of the redshift determination step for DESI and other large-scale spectroscopic surveys of quasars
Preliminary Target Selection for the DESI Milky Way Survey (MWS)
The DESI Milky Way Survey (MWS) will observe 8 million stars between mag, supplemented by observations of brighter targets under poor observing conditions. The survey will permit an accurate determination of stellar kinematics and population gradients; characterize diffuse substructure in the thick disk and stellar halo; enable the discovery of extremely metal-poor stars and other rare stellar types; and improve constraints on the Galaxy's 3D dark matter distribution from halo star kinematics. MWS will also enable a detailed characterization of the stellar populations within 100 pc of the Sun, including a complete census of white dwarfs. The target catalog from the preliminary selection described here is public
A data compression and optimal galaxy weights scheme for Dark Energy Spectroscopic Instrument and weak lensing datasets
Combining different observational probes, such as galaxy clustering and weak
lensing, is a promising technique for unveiling the physics of the Universe
with upcoming dark energy experiments. The galaxy redshift sample from the Dark
Energy Spectroscopic Instrument (DESI) will have a significant overlap with
major ongoing imaging surveys specifically designed for weak lensing
measurements: the Kilo-Degree Survey (KiDS), the Dark Energy Survey (DES) and
the Hyper Suprime-Cam (HSC) survey. In this work we analyse simulated redshift
and lensing catalogues to establish a new strategy for combining high-quality
cosmological imaging and spectroscopic data, in view of the first-year data
assembly analysis of DESI. In a test case fitting for a reduced parameter set,
we employ an optimal data compression scheme able to identify those aspects of
the data that are most sensitive to the cosmological information, and amplify
them with respect to other aspects of the data. We find this optimal
compression approach is able to preserve all the information related to the
growth of structure; we also extend this scheme to derive weights to be applied
to individual galaxies, and show that these produce near-optimal results.Comment: 14 pages, 12 Figures, DESI collaboration articl
Design and production of the DESI fibre cables
The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the Universe using the Baryonic Acoustic Oscillation technique. The spectra of 35 million galaxies and quasars over 14000 sq deg will be measured during the life of the experiment. A new prime focus corrector for the KPNO Mayall telescope will deliver light to 5000 fibre optic positioners. The fibres in turn feed 10 broad-band spectrographs. We will describe the design and production progress on the fibre cables, strain relief system and preparation of the slit end. In contrast to former projects, the larger scale of production required for DESI requires teaming up with industry to find a solution to reduce the time scale of production as well as to minimise the stress on the optical fibres
DESI and DECaLS (D&D): galaxyâgalaxy lensing measurements with 1 per cent survey and its forecast
The shear measurement from the Dark Energy Camera Legacy Survey (DECaLS) provides an excellent opportunity for galaxy-galaxy lensing study with the Dark Energy Spectroscopic Instrument (DESI) galaxies, given the large (âŒ9000 deg2) sky overlap. We explore this potential by combining the DESI 1 per cent survey and DECaLS Data Release 8 (DR8). With âŒ106 deg2 sky overlap, we achieve significant detection of galaxy-galaxy lensing for Bright Galaxy Survey (BGS) and luminous red galaxy (LRG) as lenses. Scaled to the full BGS sample, we expect the statistical errors to improve from to a promising level of at. This brings stronger requirements for future systematics control. To fully realize such potential, we need to control the residual multiplicative shear bias |m| < 0.006 and the bias in the mean redshift |Îz| < 0.008, requiring the introduced bias in the measurement is <0.31Ï. We also expect significant detection of galaxy-galaxy lensing with DESI LRG/emission line galaxy (ELG) full samples as lenses, and cosmic magnification of ELG through cross-correlation with low-redshift DECaLS shear. If such systematical error control can be achieved, we find the advantages of DECaLS, comparing with the Kilo Degree Survey (KiDS) and the Hyper Suprime-Cam (HSC), are at low redshift, large scale, and in measuring the shear ratio (to ÏR âŒ0.04) and cosmic magnification
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