Dark Energy Survey Year 1 results: measurement of the baryon acoustic oscillation scale in the distribution of galaxies to redshift 1

被引：119

作者：

Abbott, T. M. C. ^{[1
]}

Abdalla, F. B. ^{[2
,3
]}

Alarcon, A. ^{[4
,5
]}

Allam, S. ^{[6
]}

Andrade-Oliveira, F. ^{[7
,8
]}

Annis, J. ^{[6
]}

Avila, S. ^{[9
,10
]}

Banerji, M. ^{[11
,12
]}

Banik, N. ^{[6
,13
,14
,15
]}

Bechtol, K. ^{[16
]}

Bernstein, A. ^{[17
]}

Bernstein, G. M. ^{[18
]}

Bertin, E. ^{[19
,20
]}

Brooks, D. ^{[2
]}

Buckley-Geer, E. ^{[6
]}

Burke, D. L. ^{[21
,22
]}

Camacho, H. ^{[7
,23
]}

Carnero Rosell, A. ^{[7
,24
]}

Kind, M. Carrasco ^{[25
,26
]}

Carretero, J. ^{[27
]}

Castander, F. J. ^{[4
,5
]}

Cawthon, R. ^{[28
]}

Chan, K. C. ^{[4
,5
,29
]}

Crocce, M. ^{[4
,5
]}

Cunha, C. E. ^{[22
]}

D'Andrea, C. B. ^{[18
]}

da Costa, L. N. ^{[7
,24
]}

Davis, C. ^{[22
]}

De Vicente, J. ^{[30
]}

DePoy, L. ^{[31
,32
]}

Desai, S. ^{[33
]}

Diehl, H. T. ^{[6
]}

Doel, P. ^{[2
]}

Drlica-Wagner, A. ^{[6
]}

Eifler, T. F. ^{[34
,35
]}

Elvin-Poole, J. ^{[36
]}

Estrada, J. ^{[6
]}

Evrard, A. E. ^{[37
,38
]}

Flaugher, B. ^{[6
]}

Fosalba, P. ^{[4
,5
]}

Frieman, J. ^{[6
,28
]}

Garcia-Bellido, J. ^{[10
]}

Gaztanaga, E. ^{[4
,5
]}

Gerdes, D. W. ^{[37
,38
]}

Giannantonio, T. ^{[11
,12
,39
]}

Gruen, D. ^{[21
,22
]}

Gruendl, R. A. ^{[25
,26
]}

Gschwend, J. ^{[7
,24
]}

Gutierrez, G. ^{[6
]}

Hartley, W. G. ^{[2
,40
]}

机构：

[1] Natl Optic Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

[2] Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[3] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa

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

[5] IEEC, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain

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

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

[8] Univ Estadual Paulista, Inst Fis Teor, Sao Paulo, Brazil

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

[10] UAM, CSIC, Inst Fis Teor, E-28049 Madrid, Spain

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

[12] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

[13] Univ Florida, Dept Phys, Gainesville, FL 32611 USA

[14] Univ Amsterdam, Inst Theoret Phys, GRAPPA, Sci Pk 904, NL-1090 GL Amsterdam, Netherlands

[15] Leiden Univ, Lorentz Inst, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands

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

[17] Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA

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

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

[20] UPMC Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, F-75014 Paris, France

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

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

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

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

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

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

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

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

[29] Sun Yat Sen Univ, Sch Phys & Astron, Guangzhou 510275, Guangdong, Peoples R China

[30] Ctr Invest Energet Med Medioambient & Tecnol CIEM, Madrid, Spain

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

[35] Steward Observ, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA

[36] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England

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

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

[39] Ludwig Maximilians Uni Munchen, Univ Sternwarte, Fac Phys, D-81679 Munich, Germany

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

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

[42] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA

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

[44] Max Planck Inst Extraterrestrial Phys, Giessenbachstr, D-85748 Garching, Germany

[45] Harvard Smithsonian Ctr Astrophys, Event Horizon Telescope, MS-42,60 Garden St, Cambridge, MA 02138 USA

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

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

[48] Univ Geneva, Dept Phys Theor, 24 Quai Ernest Ansermet, CH-1211 Geneva, Switzerland

[49] Univ Geneva, Ctr Astroparticle Phys, 24 Quai Ernest Ansermet, CH-1211 Geneva, Switzerland

[50] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2019年 / 483卷 / 04期

基金：

美国国家科学基金会; 欧洲研究理事会; 英国科学技术设施理事会; 巴西圣保罗研究基金会; 澳大利亚研究理事会;

关键词：

cosmology: observations; large-scale structure of Universe; CHALLENGE LIGHTCONE SIMULATION; LUMINOUS RED GALAXIES; POWER-SPECTRUM; CENT DISTANCE; SAMPLE; COSMOLOGY; MODEL; HALO; BAO; I;

D O I：

10.1093/mnras/sty3351

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present angular diameter distance measurements obtained by locating the baryon acoustic oscillations (BAO) scale in the distribution of galaxies selected from the first year of Dark Energy Survey data. We consider a sample of over 1.3 million galaxies distributed over a footprint of 1336 deg(2) with 0.6 < z(photo) < 1 and a typical redshift uncertainty of 0.03(1 + z). This sample was selected, as fully described in a companion paper, using a colour/magnitude selection that optimizes trade-offs between number density and redshift uncertainty. We investigate the BAO signal in the projected clustering using three conventions, the angular separation, the comoving transverse separation, and spherical harmonics. Further, we compare results obtained from template-based and machine-learning photometric redshift determinations. We use 1800 simulations that approximate our sample in order to produce covariance matrices and allow us to validate our distance scale measurement methodology. We measure the angular diameter distance, D-A, at the effective redshift of our sample divided by the true physical scale of the BAO feature, r(d). We obtain close to a 4 per cent distance measurement of D-A (z(eff )= 0.81)/r(d) = 10.75 +/- 0.43. These results are consistent with the flat A cold dark matter concordance cosmological model supported by numerous other recent experimental results.

引用

页码：4866 / 4883

页数：18

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