Author
Kaylan J. Burleigh
Other affiliations: University of California, Berkeley, University of Arizona
Bio: Kaylan J. Burleigh is an academic researcher from Lawrence Berkeley National Laboratory. The author has contributed to research in topics: Observatory & Star formation. The author has an hindex of 6, co-authored 10 publications receiving 992 citations. Previous affiliations of Kaylan J. Burleigh include University of California, Berkeley & University of Arizona.
Papers
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TL;DR: The DESI Legacy Imaging Surveys project as discussed by the authors is a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image approximately 14,000 deg^2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory.
Abstract: The DESI Legacy Imaging Surveys are a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image approximately 14,000 deg^2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory. The combined survey footprint is split into two contiguous areas by the Galactic plane. The optical imaging is conducted using a unique strategy of dynamically adjusting the exposure times and pointing selection during observing that results in a survey of nearly uniform depth. In addition to calibrated images, the project is delivering a catalog, constructed by using a probabilistic inference-based approach to estimate source shapes and brightnesses. The catalog includes photometry from the grz optical bands and from four mid-infrared bands (at 3.4, 4.6, 12 and 22 micorons) observed by the Wide-field Infrared Survey Explorer (WISE) satellite during its full operational lifetime. The project plans two public data releases each year. All the software used to generate the catalogs is also released with the data. This paper provides an overview of the Legacy Surveys project.
711 citations
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TL;DR: The DESI Legacy Imaging Surveys (http://legacysurvey.org/) as mentioned in this paper is a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image ≈14,000 deg2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory.
Abstract: The DESI Legacy Imaging Surveys (http://legacysurvey.org/) are a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing–Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image ≈14,000 deg2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory. The combined survey footprint is split into two contiguous areas by the Galactic plane. The optical imaging is conducted using a unique strategy of dynamically adjusting the exposure times and pointing selection during observing that results in a survey of nearly uniform depth. In addition to calibrated images, the project is delivering a catalog, constructed by using a probabilistic inference-based approach to estimate source shapes and brightnesses. The catalog includes photometry from the grz optical bands and from four mid-infrared bands (at 3.4, 4.6, 12, and 22 μm) observed by the Wide-field Infrared Survey Explorer satellite during its full operational lifetime. The project plans two public data releases each year. All the software used to generate the catalogs is also released with the data. This paper provides an overview of the Legacy Surveys project.
517 citations
01 Jan 2019
TL;DR: The DESI Legacy Imaging Surveys (http://legacysurvey.org/) project is a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image ≈14,000 deg2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory.
Abstract: Author(s): Huang, L; Dey, A; Schlegel, DJ; Lang, D; Blum, R; Burleigh, K; Fan, X; Findlay, JR; Finkbeiner, D; Herrera, D; Juneau, S; Landriau, M; Levi, M; McGreer, I; Meisner, A; Myers, AD; Moustakas, J; Nugent, P; Patej, A; Schlafly, EF; Walker, AR; Valdes, F; Weaver, BA; Yeche, C; Zou, H; Zhou, X; Abareshi, B; Abbott, TMC; Abolfathi, B; Aguilera, C; Alam, S; Allen, L; Alvarez, A; Annis, J; Ansarinejad, B; Aubert, M; Beechert, J; Bell, EF; Benzvi, SY; Beutler, F; Bielby, RM; Bolton, AS; Briceno, C; Buckley-Geer, EJ; Butler, K; Calamida, A; Carlberg, RG; Carter, P; Casas, R; Castander, FJ; Choi, Y; Comparat, J; Cukanovaite, E; Delubac, T; Devries, K; Dey, S; Dhungana, G; Dickinson, M; Ding, Z; Donaldson, JB; Duan, Y; Duckworth, CJ; Eftekharzadeh, S; Eisenstein, DJ; Etourneau, T; Fagrelius, PA; Farihi, J; Fitzpatrick, M; Font-Ribera, A; Fulmer, L; Gansicke, BT; Gaztanaga, E; George, K; Gerdes, DW; A Gontcho, SG; Gorgoni, C; Green, G; Guy, J; Harmer, D; Hernandez, M; Honscheid, K; Huang, LW; James, DJ; Jannuzi, BT; Jiang, L | Abstract: © 2019. The American Astronomical Society. All rights reserved.. The DESI Legacy Imaging Surveys (http://legacysurvey.org/) are a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image ≈14,000 deg2 of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory. The combined survey footprint is split into two contiguous areas by the Galactic plane. The optical imaging is conducted using a unique strategy of dynamically adjusting the exposure times and pointing selection during observing that results in a survey of nearly uniform depth. In addition to calibrated images, the project is delivering a catalog, constructed by using a probabilistic inference-based approach to estimate source shapes and brightnesses. The catalog includes photometry from the grz optical bands and from four mid-infrared bands (at 3.4, 4.6, 12, and 22 μm) observed by the Wide-field Infrared Survey Explorer satellite during its full operational lifetime. The project plans two public data releases each year. All the software used to generate the catalogs is also released with the data. This paper provides an overview of the Legacy Surveys project.
193 citations
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TL;DR: In this paper, the authors mapped 12CO and 13CO J = 2-1 emission over 1.04 deg2 of the Serpens molecular cloud with 38'' spatial and 0.3 km s-1 spectral resolution using the Arizona Radio Observatory Heinrich Hertz Submillimeter Telescope.
Abstract: We mapped 12CO and 13CO J = 2-1 emission over 1.04 deg2 of the Serpens molecular cloud with 38'' spatial and 0.3 km s–1 spectral resolution using the Arizona Radio Observatory Heinrich Hertz Submillimeter Telescope. Our maps resolve kinematic properties for the entire Serpens cloud. We also compare our velocity moment maps with known positions of young stellar objects (YSOs) and 1.1 mm continuum emission. We find that 12CO is self-absorbed and 13CO is optically thick in the Serpens core. Outside of the Serpens core, gas appears in filamentary structures having LSR velocities which are blueshifted by up to 2 km s–1 relative to the 8 km s–1 systemic velocity of the Serpens cloud. We show that the known Class I, flat, and Class II YSOs in the Serpens core most likely formed at the same spatial location and have since drifted apart. The spatial and velocity structure of the 12CO line ratios implies that a detailed three-dimensional radiative transfer model of the cloud will be necessary for full interpretation of our spectral data. The "starless cores" region of the cloud is likely to be the next site of star formation in Serpens.
18 citations
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TL;DR: In this paper, a new tool called Obiwan is presented, which uses image simulations to determine the selection function of a galaxy redshift survey and calculate three-dimensional clustering statistics.
Abstract: This work presents the application of a new tool, Obiwan, which uses image simulations to determine the selection function of a galaxy redshift survey and calculate three-dimensional (3D) clustering statistics. Obiwan relies on a forward model of the process by which images of the night sky are transformed into a 3D large-scale structure catalogue, and offers several advantages over more traditional map-based techniques – such as operating on individual exposures and adopting a maximum likelihood approach. The photometric pipeline automatically detects and models galaxies and then generates a catalogue of such galaxies with detailed information for each one of them, including their location, redshift, and so on. Systematic biases in the imaging data are therefore imparted into the catalogues and must be accounted for in any scientific analysis of their information content. Obiwan simulates this process for samples selected from the Legacy Surveys imaging data. This imaging data will be used to select target samples for the next-generation Dark Energy Spectroscopic Instrument (DESI) experiment. Here, we apply Obiwan to a portion of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey emission-line galaxies (ELGs). Systematic biases in the data are clearly identified and removed. We compare the 3D clustering results to those obtained by the map-based approach applied to the complete eBOSS Data Release 16 (DR16) sample. We find the results are consistent, thereby validating the eBOSS DR16 ELG catalogues, which is used to obtain cosmological results.
15 citations
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Romina Ahumada1, Carlos Allende Prieto2, Carlos Allende Prieto3, Andres Almeida4 +342 more•Institutions (94)
TL;DR: The most recent data release from the Sloan Digital Sky Surveys (SDSS-IV) is DR16 as mentioned in this paper, which is the fourth and penultimate from the fourth phase of the survey.
Abstract: This paper documents the sixteenth data release (DR16) from the Sloan Digital Sky Surveys; the fourth and penultimate from the fourth phase (SDSS-IV). This is the first release of data from the southern hemisphere survey of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2); new data from APOGEE-2 North are also included. DR16 is also notable as the final data release for the main cosmological program of the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), and all raw and reduced spectra from that project are released here. DR16 also includes all the data from the Time Domain Spectroscopic Survey (TDSS) and new data from the SPectroscopic IDentification of ERosita Survey (SPIDERS) programs, both of which were co-observed on eBOSS plates. DR16 has no new data from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey (or the MaNGA Stellar Library "MaStar"). We also preview future SDSS-V operations (due to start in 2020), and summarize plans for the final SDSS-IV data release (DR17).
803 citations
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University of Edinburgh1, Autonomous University of Madrid2, Pierre-and-Marie-Curie University3, University of Portsmouth4, University of Cape Town5, University of Wisconsin-Madison6, Moscow State University7, New Mexico State University8, New York University9, University of Utah10, University of Toronto11, Université Paris-Saclay12, University of Waterloo13, Sejong University14, Stanford University15, Max Planck Society16, University College London17, Texas Christian University18, National Autonomous University of Mexico19, University of Barcelona20, Consejo Nacional de Ciencia y Tecnología21, Universidad de Guanajuato22, Liverpool John Moores University23, Lawrence Berkeley National Laboratory24, Ohio State University25, École Polytechnique Fédérale de Lausanne26, University of Wyoming27, Haverford College28, University of Oxford29, University of Pittsburgh30, Perimeter Institute for Theoretical Physics31, California Institute of Technology32, Ohio University33, Swinburne University of Technology34, Fermilab35, University of Washington36, Korea Astronomy and Space Science Institute37, Brookhaven National Laboratory38, University of St Andrews39, Durham University40
TL;DR: In this article, the authors present the cosmological implications from final measurements of clustering using galaxies, quasars, and Lyα forests from the completed SDSS lineage of experiments in large-scale structure.
Abstract: We present the cosmological implications from final measurements of clustering using galaxies, quasars, and Lyα forests from the completed Sloan Digital Sky Survey (SDSS) lineage of experiments in large-scale structure. These experiments, composed of data from SDSS, SDSS-II, BOSS, and eBOSS, offer independent measurements of baryon acoustic oscillation (BAO) measurements of angular-diameter distances and Hubble distances relative to the sound horizon, rd, from eight different samples and six measurements of the growth rate parameter, fσ8, from redshift-space distortions (RSD). This composite sample is the most constraining of its kind and allows us to perform a comprehensive assessment of the cosmological model after two decades of dedicated spectroscopic observation. We show that the BAO data alone are able to rule out dark-energy-free models at more than eight standard deviations in an extension to the flat, ΛCDM model that allows for curvature. When combined with Planck Cosmic Microwave Background (CMB) measurements of temperature and polarization, under the same model, the BAO data provide nearly an order of magnitude improvement on curvature constraints relative to primary CMB constraints alone. Independent of distance measurements, the SDSS RSD data complement weak lensing measurements from the Dark Energy Survey (DES) in demonstrating a preference for a flat ΛCDM cosmological model when combined with Planck measurements. The combined BAO and RSD measurements indicate σ8=0.85±0.03, implying a growth rate that is consistent with predictions from Planck temperature and polarization data and with General Relativity. When combining the results of SDSS BAO and RSD, Planck, Pantheon Type Ia supernovae (SNe Ia), and DES weak lensing and clustering measurements, all multiple-parameter extensions remain consistent with a ΛCDM model. Regardless of cosmological model, the precision on each of the three parameters, ωΛ, H0, and σ8, remains at roughly 1%, showing changes of less than 0.6% in the central values between models. In a model that allows for free curvature and a time-evolving equation of state for dark energy, the combined samples produce a constraint ωk=-0.0022±0.0022. The dark energy constraints lead to w0=-0.909±0.081 and wa=-0.49-0.30+0.35, corresponding to an equation of state of wp=-1.018±0.032 at a pivot redshift zp=0.29 and a Dark Energy Task Force Figure of Merit of 94. The inverse distance ladder measurement under this model yields H0=68.18±0.79 km s-1 Mpc-1, remaining in tension with several direct determination methods; the BAO data allow Hubble constant estimates that are robust against the assumption of the cosmological model. In addition, the BAO data allow estimates of H0 that are independent of the CMB data, with similar central values and precision under a ΛCDM model. Our most constraining combination of data gives the upper limit on the sum of neutrino masses at mν<0.115 eV (95% confidence). Finally, we consider the improvements in cosmology constraints over the last decade by comparing our results to a sample representative of the period 2000-2010. We compute the relative gain across the five dimensions spanned by w, ωk, mν, H0, and σ8 and find that the SDSS BAO and RSD data reduce the total posterior volume by a factor of 40 relative to the previous generation. Adding again the Planck, DES, and Pantheon SN Ia samples leads to an overall contraction in the five-dimensional posterior volume of 3 orders of magnitude.
575 citations
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TL;DR: The Extended Baryon Oscillation Spectroscopic Survey (eBOSS) as mentioned in this paper uses four different tracers of the underlying matter density field to expand the volume covered by BOSS and map the large-scale structures over the relatively unconstrained redshift range 0.6 0.87.
Abstract: In a six-year program started in 2014 July, the Extended Baryon Oscillation Spectroscopic Survey (eBOSS) will conduct novel cosmological observations using the BOSS spectrograph at Apache Point Observatory. These observations will be conducted simultaneously with the Time Domain Spectroscopic Survey (TDSS) designed for variability studies and the Spectroscopic Identification of eROSITA Sources (SPIDERS) program designed for studies of X-ray sources. In particular, eBOSS will measure with percent-level precision the distance-redshift relation with baryon acoustic oscillations (BAO) in the clustering of matter. eBOSS will use four different tracers of the underlying matter density field to vastly expand the volume covered by BOSS and map the large-scale-structures over the relatively unconstrained redshift range 0.6 0.6 sample of BOSS galaxies. With ~195,000 new emission line galaxy redshifts, we expect BAO measurements of d_A(z) to an accuracy of 3.1% and H(z) to 4.7% at an effective redshift of z = 0.87. A sample of more than 500,000 spectroscopically confirmed quasars will provide the first BAO distance measurements over the redshift range 0.9 2.1; these new data will enhance the precision of dA(z) and H(z) at z > 2.1 by a factor of 1.44 relative to BOSS. Furthermore, eBOSS will provide improved tests of General Relativity on cosmological scales through redshift-space distortion measurements, improved tests for non-Gaussianity in the primordial density field, and new constraints on the summed mass of all neutrino species. Here, we provide an overview of the cosmological goals, spectroscopic target sample, demonstration of spectral quality from early data, and projected cosmological constraints from eBOSS.
316 citations
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Princeton University1, Cardiff University2, Pontifical Catholic University of Chile3, Université Paris-Saclay4, University of Pennsylvania5, University of Oxford6, Johns Hopkins University7, University of British Columbia8, Cornell University9, National Institute of Standards and Technology10, University of Michigan11, University of Toronto12, University of Chile13, University of Chicago14, Stanford University15, University of KwaZulu-Natal16, University of California, Berkeley17, University of Cambridge18, Goddard Space Flight Center19, Lawrence Berkeley National Laboratory20, Florida State University21, University of Southern California22, University of Arizona23, University of Pittsburgh24, Stony Brook University25, Pennsylvania State University26, Columbia University27, Rutgers University28, Yale University29, Perimeter Institute for Theoretical Physics30, University of Illinois at Urbana–Champaign31, University of Milan32, Haverford College33, California Institute of Technology34, McGill University35, Pontifical Catholic University of Valparaíso36, West Chester University of Pennsylvania37, Carnegie Mellon University38, Arizona State University39
TL;DR: In this article, the Atacama Cosmology Telescope (ACT) data were used to estimate the temperature and polarization anisotropy from the cosmic microwave background (CMB) at 98 and 150 GHz.
Abstract: We present new arcminute-resolution maps of the Cosmic Microwave Background temperature and polarization anisotropy from the Atacama Cosmology Telescope, using data taken from 2013–2016 at 98 and 150 GHz. The maps cover more than 17,000 deg2, the deepest 600 deg2 with noise levels below 10μK-arcmin. We use the power spectrum derived from almost 6,000 deg2 of these maps to constrain cosmology. The ACT data enable a measurement of the angular scale of features in both the divergence-like polarization and the temperature anisotropy, tracing both the velocity and density at last-scattering. From these one can derive the distance to the last-scattering surface and thus infer the local expansion rate, H0. By combining ACT data with large-scale information from WMAP we measure H0=67.6± 1.1 km/s/Mpc, at 68% confidence, in excellent agreement with the independently-measured Planck satellite estimate (from ACT alone we find H0=67.9± 1.5 km/s/Mpc). The ΛCDM model provides a good fit to the ACT data, and we find no evidence for deviations: both the spatial curvature, and the departure from the standard lensing signal in the spectrum, are zero to within 1σ; the number of relativistic species, the primordial Helium fraction, and the running of the spectral index are consistent with ΛCDM predictions to within 1.5–2.2σ. We compare ACT, WMAP, and Planck at the parameter level and find good consistency; we investigate how the constraints on the correlated spectral index and baryon density parameters readjust when adding CMB large-scale information that ACT does not measure. The DR4 products presented here will be publicly released on the NASA Legacy Archive for Microwave Background Data Analysis.
298 citations
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National Radio Astronomy Observatory1, University of Manitoba2, Cornell University3, United States Naval Research Laboratory4, Space Telescope Science Institute5, University of Toronto6, Saint Anselm College7, California Institute of Technology8, University of California, Berkeley9, Max Planck Society10, Drexel University11, University of Alberta12, University of Minnesota13, University of Cape Town14, University of the Western Cape15, Universidad de Guanajuato16, Harvard University17, University of Bristol18, Academia Sinica Institute of Astronomy and Astrophysics19, Pennsylvania State University20, University of Iowa21, West Virginia University22, University of Colorado Boulder23, Newcastle University24, Leiden University25, Hebrew University of Jerusalem26, University of Washington27, University of Oxford28, Smithsonian Institution29, University of Illinois at Urbana–Champaign30, National Autonomous University of Mexico31, Spanish National Research Council32, European Southern Observatory33, University of Hamburg34, INAF35
TL;DR: The Very Large Array Sky Survey (VLASS) as discussed by the authors is a synoptic, all-sky radio sky survey with a unique combination of high angular resolution (≈2.5"), sensitivity (a 1σ goal of 70 μJy/beam in the coadded data), full linear Stokes polarimetry, time domain coverage, and wide bandwidth (2-4 GHz).
Abstract: The Very Large Array Sky Survey (VLASS) is a synoptic, all-sky radio sky survey with a unique combination of high angular resolution (≈2.5\"), sensitivity (a 1σ goal of 70 μJy/beam in the coadded data), full linear Stokes polarimetry, time domain coverage, and wide bandwidth (2-4 GHz). The first observations began in September 2017, and observing for the survey will finish in 2024. VLASS will use approximately 5500 hours of time on the Karl G. Jansky Very Large Array (VLA) to cover the whole sky visible to the VLA (Declination > −40∘), a total of 33,885 deg^2. The data will be taken in three epochs to allow the discovery of variable and transient radio sources. The survey is designed to engage radio astronomy experts, multi-wavelength astronomers, and citizen scientists alike. By utilizing an \"on the fly\" interferometry mode, the observing overheads are much reduced compared to a conventional pointed survey. In this paper, we present the science case and observational strategy for the survey, and also results from early survey observations.
288 citations