HOD-dependent systematics in Emission Line Galaxies for the DESI 2024 BAO analysis

被引:1
|
作者
Garcia-Quintero, C. [1 ]
Mena-Fernandez, J. [2 ]
Rocher, A. [3 ,4 ]
Yuan, S. [5 ]
Hadzhiyska, B. [6 ,7 ]
Alves, O. [8 ]
Rashkovetskyi, M. [9 ]
Seo, H. [10 ]
Padmanabhan, N. [11 ]
Nadathur, S. [12 ]
Howlett, C. [13 ]
Ishak, M. [1 ]
Medina-Varela, L. [1 ]
McDonald, P. [6 ]
Ross, A. J. [14 ,15 ,16 ]
Xie, Y. [1 ]
Chen, X. [11 ]
Bera, A. [1 ]
Aguilar, J. [6 ]
Ahlen, S. [17 ]
Andrade, U. [8 ,18 ]
BenZvi, S. [19 ]
Brooks, D. [20 ]
Burtin, E. [4 ]
Chen, S. [21 ]
Claybaugh, T. [6 ]
Cole, S. [22 ]
de la Macorra, A. [23 ]
de Mattia, A. [4 ]
Dey, A. [24 ]
Dey, B. [25 ,26 ]
Ding, Z. [27 ]
Doel, P. [20 ]
Fanning, K. [5 ,28 ]
Forero-Romero, J. E. [29 ,30 ]
Gaztanaga, E. [12 ,31 ,32 ]
Gil-Marin, H. [31 ,33 ,34 ]
Gontcho, S. Gontcho A. [6 ]
Gutierrez, G. [35 ]
Guy, J. [6 ]
Hahn, C. [36 ]
Honscheid, K. [14 ,16 ,37 ]
Kremin, A. [6 ]
Landriau, M. [6 ]
Le Guillou, L. [38 ]
Levi, M. E. [6 ]
Manera, M. [39 ,40 ]
Martini, P. [14 ,15 ,16 ]
Meisner, A. [24 ]
Miquel, R. [40 ,41 ]
机构
[1] Univ Texas Dallas, Dept Phys, Richardson, TX 75080 USA
[2] Lab Phys Subatom & Cosmol, 53 Ave Martyrs, F-38000 Grenoble, France
[3] Ecole Polytech Fed Lausanne, CH-1015 Lausanne, Switzerland
[4] Univ Paris Saclay, IRFU, CEA, F-91191 Gif Sur Yvette, France
[5] SLAC Natl Accelerator Lab, Menlo Pk, CA 94305 USA
[6] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA
[7] Univ Calif Berkeley, 110 Sproul Hall 5800, Berkeley, CA 94720 USA
[8] Univ Michigan, Ann Arbor, MI 48109 USA
[9] Ctr Astrophys Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138 USA
[10] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA
[11] Yale Univ, Dept Phys, POB 208120, New Haven, CT 06511 USA
[12] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England
[13] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia
[14] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA
[15] Ohio State Univ, Dept Astron, 4055 McPherson Lab,140 W 18th Ave, Columbus, OH 43210 USA
[16] Ohio State Univ, Columbus, OH 43210 USA
[17] Boston Univ, Dept Phys, 590 Commonwealth Ave, Boston, MA 02215 USA
[18] Univ Michigan, Leinweber Ctr Theoret Phys, 450 Church St, Ann Arbor, MI 48109 USA
[19] Univ Rochester, Dept Phys & Astron, 206 Bausch & Lomb Hall,POB 270171, Rochester, NY 14627 USA
[20] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England
[21] Inst Adv Study, 1 Einstein Dr, Princeton, NJ 08540 USA
[22] Univ Durham, Inst Computat Cosmol, Dept Phys, South Rd, Durham DH1 3LE, England
[23] Univ Nacl Autonoma Mexico, Inst Fis, Mexico City 04510, DF, Mexico
[24] NSF NOIRLab, 950 N Cherry Ave, Tucson, AZ 85719 USA
[25] Univ Pittsburgh, Dept Phys & Astron, 3941 OHara St, Pittsburgh, PA 15260 USA
[26] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, 3941 OHara St, Pittsburgh, PA 15260 USA
[27] Shanghai Jiao Tong Univ, Sch Phys & Astron, Dept Astron, Shanghai 200240, Peoples R China
[28] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94305 USA
[29] Univ Los Andes, Dept Fis, Cra 1 18A-10,Edificio Ip, Bogota 111711, Colombia
[30] Univ Los Andes, Observ Astron, Cra 1 18A-10,Edificio H, Bogota 111711, Colombia
[31] Inst Estudis Espacials Catalunya IEEC, Barcelona 08034, Spain
[32] CSIC, ICE, Inst Space Sci, Campus UAB,Carrer Can Magrans S-N, Barcelona 08913, Spain
[33] Univ Barcelona, Dept Fis Quant & Astrofis, Marti & Franques 1, E-08028 Barcelona, Spain
[34] Univ Barcelona UB, Inst Ciencies Cosmos ICCUB, C Marti & Franques 1, Barcelona 08028, Spain
[35] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA
[36] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA
[37] Ohio State Univ, Dept Phys, 191 West Woodruff Ave, Columbus, OH 43210 USA
[38] Sorbonne Univ, Lab Phys Nucl & Hautes Energies LPNHE, CNRS, IN2P3, FR-75005 Paris, France
[39] Univ Autonoma Barcelona, Dept Fis, Serra Hunter, Bellaterra 08193, Barcelona, Spain
[40] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, Barcelona 08193, Spain
[41] Inst Catalana Recerca & Estudis Avancats, Passeig Lluis Companys 23, Barcelona 08010, Spain
[42] Siena Coll, Dept Phys & Astron, 515 Loudon Rd, Loudonville, NY 12211 USA
[43] Univ Sussex, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England
[44] Univ Wyoming, Dept Phys & Astron, 1000 E Univ,Dept 3905, Laramie, WY 82071 USA
[45] Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China
[46] Univ Guanajuato, Dept Fis, DCI, Guanajuato 37150, Mexico
[47] Inst Avanzado Cosmol AC, San Marcos 11 Atenas 202 Magdalena Contreras, Mexico City 10720, DF, Mexico
[48] Univ Waterloo, Dept Phys & Astron, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada
[49] Univ Waterloo, Waterloo Ctr Astrophys, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada
[50] Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada
基金
美国国家科学基金会; 英国科学技术设施理事会;
关键词
baryon acoustic oscillations; galaxy clustering; HALO OCCUPATION DISTRIBUTION; BARYON ACOUSTIC-OSCILLATIONS; MILLENNIUMTNG PROJECT; RED; MODEL; EVOLUTION; SPACE; CONNECTION; CONFORMITY; DISTANCE;
D O I
10.1088/1475-7516/2025/01/132
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The Dark Energy Spectroscopic Instrument (DESI) will provide precise measurements of Baryon Acoustic Oscillations (BAO) to constrain the expansion history of the Universe and set stringent constraints on dark energy. Therefore, precise control of the global error budget due to various systematic effects is required for the DESI 2024 BAO analysis. In this work, we estimate the level of systematics induced in the DESI BAO analysis due the assumed Halo Occupation Distribution (HOD) model for the Emission Line Galaxy (ELG) tracer. We make use of mock galaxy catalogs constructed by fitting various HOD models to early DESI data, namely the One-Percent survey data. Our analysis includes typical HOD models for the ELG tracer used in the literature as well as extensions to the baseline models. Among the extensions, we consider various recipes for galactic conformity and assembly bias. We use 25 AbacusSummit simulations under the Lambda CDM cosmology for each HOD model and perform independent analyses in Fourier space and in configuration space. To recover the BAO signal from our mocks we perform BAO reconstruction and apply the control variates technique to reduce sample variance noise. Our BAO analyses can recover the isotropic BAO parameter alpha(iso) within 0.1% and the Alcock Paczynski parameter alpha(AP) within 0.3%. Overall, we find that the systematic error due to the HOD dependence is below 0.17%, with the Fourier space analysis being more robust against the HOD systematics. We conclude that our analysis pipeline is robust enough against the HOD systematics for the ELG tracer in the DESI 2024 BAO analysis, for the assumptions made.
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页数:59
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