Dark Energy Survey Year 1 results: cross-correlation redshifts - methods and systematics characterization

被引：60

作者：

Gatti, M. ^{[1
]}

Vielzeuf, P. ^{[1
]}

Davis, C. ^{[2
]}

Cawthon, R. ^{[3
]}

Rau, M. M. ^{[4
]}

DeRose, J. ^{[2
,5
]}

De Vicente, J. ^{[6
]}

Alarcon, A. ^{[7
]}

Rozo, E. ^{[8
]}

Gaztanaga, E. ^{[7
]}

Hoyle, B. ^{[4
]}

Miquel, R. ^{[1
,9
]}

Bernstein, G. M. ^{[10
]}

Bonnett, C. ^{[1
]}

Rosell, A. Carnero ^{[11
,12
]}

Castander, F. J. ^{[14
,15
]}

Chang, C. ^{[16
]}

da Costa, L. N. ^{[17
,18
]}

Gruen, D. ^{[11
,12
]}

Gschwend, J. ^{[11
,12
]}

Hartley, W. G. ^{[14
,15
]}

Lin, H. ^{[16
]}

MacCrann, N. ^{[17
,18
]}

Maia, M. A. G. ^{[11
,12
]}

Ogando, R. L. C. ^{[11
,12
]}

Roodman, A. ^{[2
,13
]}

Sevilla-Noarbe, I. ^{[6
]}

Troxel, M. A. ^{[17
,18
]}

Wechsler, R. H. ^{[2
,5
,13
]}

Asorey, J. ^{[19
,20
]}

Davis, T. M. ^{[19
,20
]}

Glazebrook, K. ^{[21
]}

Hinton, S. R. ^{[20
]}

Lewis, G. ^{[19
,22
]}

Lidman, C. ^{[19
,23
]}

Macaulay, E. ^{[20
]}

Moeller, A. ^{[19
,24
]}

O'Neill, C. R. ^{[19
]}

Sommer, N. E. ^{[19
,24
]}

Uddin, S. A. ^{[19
,25
]}

Yuan, F. ^{[19
,24
]}

Zhang, B. ^{[19
,24
]}

Abbott, T. M. C. ^{[26
]}

Allam, S. ^{[16
]}

Annis, J. ^{[16
]}

Bechtol, K. ^{[27
]}

Brooks, D. ^{[14
]}

Burke, D. L. ^{[2
,13
]}

Carollo, D. ^{[19
,28
]}

Kind, M. Carrasco ^{[29
,30
]}

机构：

[1] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain

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

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

[4] Ludwig Maximilians Univ Munchen, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany

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

[6] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain

[7] CSIC, IEEC, Inst Space Sci, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

[8] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA

[9] Ist Cataluna Recerca & Estudis Avancats, E-08010 Barcelona, Spain

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

[11] Lab Interinst e Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

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

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

[14] UCL, Dept Phys & Astron, Gower Sheet, London WC1E 6B1, England

[15] Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland

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

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

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

[19] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia

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

[21] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia

[22] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia

[23] Australian Astron Observ, N Ryde, NSW 2113, Australia

[24] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2601, Australia

[25] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China

[26] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

[27] LSST, 933 North Cherry Ave, Tucson, AZ 85721 USA

[28] Osserv Astron Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, Italy

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

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

[31] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA

[32] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

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

[34] CALTECH, Dept Phys, Pasadena, CA 91125 USA

[35] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[36] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

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

[38] Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain

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

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

[41] Univ Washington, Astron Dept, Box 351580, Seattle, WA 98195 USA

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

[43] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA

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

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

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

[47] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA

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

[49] Univ Estadual Campinas, Inst Fis Gleb Wataghin, BR-13083859 Campinas, SP, Brazil

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

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2018年 / 477卷 / 02期

基金：

澳大利亚研究理事会; 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;

关键词：

galaxies: distances and redshifts; cosmology: observations; DIGITAL SKY SURVEY; COSMIC SHEAR; DATA RELEASE; GALAXY BIAS; DISTRIBUTIONS; MAGNIFICATION; LUMINOSITY; SAMPLES; ERROR; TESTS;

D O I：

10.1093/mnras/sty466

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We use numerical simulations to characterize the performance of a clustering-based method to calibrate photometric redshift biases. In particular, we cross-correlate the weak lensing source galaxies from the Dark Energy Survey Year 1 sample with redMaGiC galaxies (luminous red galaxies with secure photometric redshifts) to estimate the redshift distribution of the former sample. The recovered redshift distributions are used to calibrate the photometric redshift bias of standard photo-z methods applied to the same source galaxy sample. We apply the method to two photo-z codes run in our simulated data: Bayesian Photometric Redshift and Directional Neighbourhood Fitting. We characterize the systematic uncertainties of our calibration procedure, and find that these systematic uncertainties dominate our error budget. The dominant systematics are due to our assumption of unevolving bias and clustering across each redshift bin, and to differences between the shapes of the redshift distributions derived by clustering versus photo-zs. The systematic uncertainty in the mean redshift bias of the source galaxy sample is Delta z less than or similar to 0.02, though the precise value depends on the redshift bin under consideration. We discuss possible ways to mitigate the impact of our dominant systematics in future analyses.

引用

页码：1651 / 1669

页数：19

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