Dark Energy Survey Year 3 results: calibration of lens sample redshift distributions using clustering redshifts with BOSS/eBOSS

被引：27

作者：

Cawthon, R. ^{[1
,2
]}

Elvin-Poole, J. ^{[3
,4
]}

Porredon, A. ^{[3
,4
,5
]}

Crocce, M. ^{[5
,6
]}

Giannini, G. ^{[7
]}

Gatti, M. ^{[7
]}

Ross, A. J. ^{[3
]}

Rykoff, E. S. ^{[8
,9
]}

Carnero Rosell, A. ^{[10
,11
]}

DeRose, J. ^{[12
,13
]}

Lee, S. ^{[14
]}

Rodriguez-Monroy, M. ^{[15
]}

Amon, A. ^{[8
]}

Bechtol, K. ^{[1
]}

De Vicente, J. ^{[15
]}

Gruen, D. ^{[8
,9
,16
]}

Morgan, R. ^{[1
]}

Sanchez, E. ^{[15
]}

Sanchez, J. ^{[17
]}

Sevilla-Noarbe, I ^{[15
]}

Abbott, T. M. C. ^{[18
]}

Aguena, M. ^{[19
]}

Allam, S. ^{[17
]}

Annis, J. ^{[17
]}

Avila, S. ^{[20
]}

Bacon, D. ^{[21
]}

Bertin, E. ^{[22
]}

Brooks, D. ^{[24
]}

Burke, D. L. ^{[8
,9
]}

Carrasco Kind, M. ^{[24
,25
]}

Carretero, J. ^{[7
]}

Castander, F. J. ^{[5
,6
]}

Choi, A. ^{[3
]}

Costanzi, M. ^{[26
,27
]}

da Costa, L. N. ^{[28
]}

Pereira, M. E. S. ^{[29
]}

Dawson, K. ^{[30
]}

Desai, S. ^{[31
]}

Diehl, H. T. ^{[17
]}

Eckert, K. ^{[32
]}

Everett, S. ^{[13
]}

Ferrero, I ^{[33
]}

Fosalba, P. ^{[5
,6
]}

Frieman, J. ^{[17
,34
]}

Garcia-Bellido, J. ^{[20
]}

Gaztanaga, E. ^{[5
,6
]}

Gruendl, R. A. ^{[24
,25
]}

Gschwend, J. ^{[28
]}

Gutierrez, G. ^{[17
]}

Hinton, S. R. ^{[35
]}

机构：

[1] Univ Wisconsin, Phys Dept, 2320 Chamberlin Hall, Madison, WI 53706 USA

[2] William Jewell Coll, Phys Dept, Liberty, MO 64068 USA

[3] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[4] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

[5] Inst Estudis Espacials Catalunya IEEC, Barcelona 08034, Spain

[6] Campus UAB, CSIC, Inst Space Sci, ICE, Carrer Can Magrans S-N, Barcelona 08193, Spain

[7] Campus UAB, Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Bellaterra, Barcelona, Spain

[8] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA

[9] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[10] Inst Astrofis Canarias, E-38205 Tenerife, Spain

[11] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain

[12] Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA

[13] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

[14] Duke Univ, Dept Phys, Durham, NC 27708 USA

[15] CIEMAT, Ctr Invest Energet Medioambientales & Tecnol, Madrid, Spain

[16] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA

[17] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[18] Cerro Tololo Interamer Observ, NSFs Natl Opt Infrared Astron Res Lab, La Serena, Chile

[19] Univ S ao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil

[20] Univ Autonoma Madrid, CSIC, UAM, Inst Fis Teor, Madrid 28049, Spain

[21] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[22] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France

[23] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[24] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[25] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA

[26] Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-34143 Trieste, Italy

[27] Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste, Italy

[28] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[29] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[30] Univ Utah, Dept Phys & Astron, 115 S 1400 E, Salt Lake City, UT 84112 USA

[31] IIT Hyderabad, Dept Phys, Kandi 502285, Telangana, India

[32] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[33] Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway

[34] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[35] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia

[36] Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA

[37] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA

[38] Ecole Polytech Fed Lausanne EPFL, Astrophys Lab, Inst Phys, Observ Sauverny, CH-1290 Versoix, Switzerland

[39] Macquarie Univ, Australian Astron Opt, N Ryde, NSW 2113, Australia

[40] Lowell Observ, 1400 Mars Hill Rd, Flagstaff, AZ 86001 USA

[41] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA

[42] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany

[43] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany

[44] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[45] Univ Waterloo, Dept Phys & Astron, Waterloo Ctr Astrophys, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada

[46] Sejong Univ, Dept Phys & Astron, Seoul 143747, South Korea

[47] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[48] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA

[49] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2022年 / 513卷 / 04期

基金：

欧洲研究理事会; 美国国家科学基金会; 英国科学技术设施理事会; 美国安德鲁·梅隆基金会;

关键词：

surveys; galaxies: distances and redshifts; large-scale structure of Universe; cosmology: observations; CROSS-CORRELATION REDSHIFTS; SCALE STRUCTURE CATALOGS; SDSS; GALAXIES; DES;

D O I：

10.1093/mnras/stac1160

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present clustering redshift measurements for Dark Energy Survey (DES) lens sample galaxies used in weak gravitational lensing and galaxy clustering studies. To perform these measurements, we cross-correlate with spectroscopic galaxies from the Baryon Acoustic Oscillation Survey (BOSS) and its extension, eBOSS. We validate our methodology in simulations, including a new technique to calibrate systematic errors that result from the galaxy clustering bias, and we find that our method is generally unbiased in calibrating the mean redshift. We apply our method to the data, and estimate the redshift distribution for 11 different photometrically selected bins. We find general agreement between clustering redshift and photometric redshift estimates, with differences on the inferred mean redshift found to be below |Delta z| = 0.01 in most of the bins. We also test a method to calibrate a width parameter for redshift distributions, which we found necessary to use for some of our samples. Our typical uncertainties on the mean redshift ranged from 0.003 to 0.008, while our uncertainties on the width ranged from 4 to 9 per cent. We discuss how these results calibrate the photometric redshift distributions used in companion papers for DES Year 3 results.

引用

页码：5517 / 5539

页数：23

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Evrard, A. E.
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Ferte, A.
Flaugher, B.
Fosalba, P.
Frieman, J.
Garcia-Bellido, J.
Gaztanaga, E.
Gerdes, D. W.
Giannantonio, T.
Gruen, D.
Gruendl, R. A.
Gschwend, J.
Gutierrez, G.
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