Generating mock galaxy catalogues for flux-limited samples like the DESI Bright Galaxy Survey

Author:

Smith A1ORCID,Grove C1ORCID,Cole S1,Norberg P12,Zarrouk P3,Yuan S4ORCID,Aguilar J5,Ahlen S6,Brooks D7,Claybaugh T5,de la Macorra A8,Doel P7,Forero-Romero J E910,Gaztañaga E111213,Gontcho S Gontcho A5,Hahn C14,Kehoe R15,Kremin A5,Levi M E5,Manera M1617,Meisner A18,Miquel R1719,Moustakas J20,Nie J21,Percival W J222324,Rezaie M25,Rossi G26,Sanchez E27,Seo H28,Tarlé G29,Zhou Z21

Affiliation:

1. Institute for Computational Cosmology, Department of Physics, Durham University , South Road, Durham DH1 3LE , UK

2. Centre for Extragalactic Astronomy, Department of Physics, Durham University , South Road, Durham DH1 3LE , UK

3. Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), CNRS/IN2P3 and Sorbonne Université , 4 place Jussieu, F-75005 Paris , France

4. SLAC National Accelerator Laboratory , Menlo Park, CA 94305 , USA

5. Lawrence Berkeley National Laboratory , 1 Cyclotron Road, Berkeley, CA 94720 , USA

6. Physics Dept., Boston University , 590 Commonwealth Avenue, Boston, MA 02215 , USA

7. Department of Physics and Astronomy, University College London , Gower Street, London WC1E 6BT , UK

8. Instituto de Física, Universidad Nacional Autónoma de México , Cd. de México C.P. 04510 , México

9. Departamento de Física, Universidad de los Andes , Cra. 1 No. 18A-10, Edificio Ip, CP 111711 Bogotá , Colombia

10. Observatorio Astronómico, Universidad de los Andes , Cra. 1 No. 18A-10, Edificio H, CP 111711 Bogotá , Colombia

11. Institut d’Estudis Espacials de Catalunya (IEEC) , E-08034 Barcelona , Spain

12. Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building , Portsmouth PO1 3FX , UK

13. Institute of Space Sciences, ICE-CSIC, Campus UAB , Carrer de Can Magrans s/n, E-08913 Bellaterra, Barcelona , Spain

14. Department of Astrophysical Sciences, Princeton University , Princeton, NJ 08544 , USA

15. Department of Physics, Southern Methodist University , 3215 Daniel Avenue, Dallas, TX 75275 , USA

16. Departament de Física, Serra Húnter, Universitat Autònoma de Barcelona , E-08193 Bellaterra, Barcelona , Spain

17. Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology , Campus UAB, E-08193 Bellaterra, Barcelona , Spain

18. NSF’s NOIRLab , 950 N. Cherry Ave., Tucson, AZ 85719 , USA

19. Institució Catalana de Recerca i Estudis Avançats, Passeig de Lluís Companys , 23, E-08010 Barcelona , Spain

20. Department of Physics and Astronomy, Siena College , 515 Loudon Road, Loudonville, NY 12211 , USA

21. National Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Rd., Chaoyang District, Beijing 100012 , P. R. China

22. Department of Physics and Astronomy, University of Waterloo , 200 University Ave W, Waterloo, ON N2L 3G1 , Canada

23. Perimeter Institute for Theoretical Physics , 31 Caroline St. North, Waterloo, ON N2L 2Y5 , Canada

24. Waterloo Centre for Astrophysics, University of Waterloo , 200 University Ave W, Waterloo, ON N2L 3G1 , Canada

25. Department of Physics, Kansas State University , 116 Cardwell Hall, Manhattan, KS 66506 , USA

26. Department of Physics and Astronomy, Sejong University , Seoul 143-747 , Korea

27. CIEMAT , Avenida Complutense 40, E-28040 Madrid , Spain

28. Department of Physics and Astronomy, Ohio University , Athens, OH 45701 , USA

29. Department of Physics, University of Michigan , Ann Arbor, MI 48109 , USA

Abstract

ABSTRACT Accurate mock galaxy catalogues are crucial to validate analysis pipelines used to constrain dark energy models. We present a fast HOD-fitting method which we apply to the AbacusSummit simulations to create a set of mock catalogues for the DESI Bright Galaxy Survey, which contain r-band magnitudes and $(g-r)$ colours. The halo tabulation method fits HODs for different absolute magnitude threshold samples simultaneously, preventing unphysical HOD crossing between samples. We validate the HOD fitting procedure by fitting to real-space clustering measurements and galaxy number densities from the MXXL BGS mock, which was tuned to the SDSS and GAMA surveys. The best-fitting clustering measurements and number densities are mostly within the assumed errors, but the clustering for the faint samples is low on large scales. The best-fitting HOD parameters are robust when fitting to simulations with different realizations of the initial conditions. When varying the cosmology, trends are seen as a function of each cosmological parameter. We use the best-fitting HOD parameters to create cubic box and cut sky mocks from the AbacusSummit simulations, in a range of cosmologies. As an illustration, we compare the ${}^{0.1}M_r\lt -20$ sample of galaxies in the mock with BGS measurements from the DESI one-percent survey. We find good agreement in the number densities, and the projected correlation function is reasonable, with differences that can be improved in the future by fitting directly to BGS clustering measurements. The cubic box and cut-sky mocks in different cosmologies are made publicly available.

Funder

Science and Technology Facilities Council

Publisher

Oxford University Press (OUP)

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