Preparing for low surface brightness science with the Vera C. Rubin Observatory: a comparison of observable and simulated intracluster light fractions

Author:

Brough Sarah1ORCID,Ahad Syeda Lammim2ORCID,Bahé Yannick M234ORCID,Ellien Amaël5,Gonzalez Anthony H6ORCID,Jiménez-Teja Yolanda78,Kimmig Lucas C9,Martin Garreth1011ORCID,Martínez-Lombilla Cristina1ORCID,Montes Mireia121314ORCID,Pillepich Annalisa15ORCID,Ragusa Rossella1617,Remus Rhea-Silvia9,Collins Chris A18,Knapen Johan H1213,Mihos J Christopher19

Affiliation:

1. School of Physics, University of New South Wales , NSW 2052 , Australia

2. Leiden Observatory, Leiden University , PO Box 9513, NL-2300 RA Leiden , the Netherlands

3. Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny , CH-1290 Versoix , Switzerland

4. Institute for Computational Cosmology, Durham University , South Road, Durham DH1 3LE , UK

5. Anton Pannekoek Institute for Astronomy & GRAPPA, University of Amsterdam , Science Park 904, NL-1098 XH, Amsterdam , the Netherlands

6. Department of Astronomy, University of Florida , Gainesville, FL 32611 , USA

7. Instituto de Astrofísica de Andalucía–CSIC, Glorieta de la Astronomía s/n , E-18008 Granada , Spain

8. Observatório Nacional - MCTI (ON) , Rua Gal. José Cristino 77, São Cristóvão, 20921-400, Rio de Janeiro , Brazil

9. Universitäts-Sternwarte München , Scheinerstr 1, D-81679 München , Germany

10. Korea Astronomy and Space Science Institute , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055 , Korea

11. Steward Observatory, University of Arizona , 933 N. Cherry Ave, Tucson, AZ 85719 , USA

12. Instituto de Astrofísica de Canarias , c/ Vía Láctea s/n, E-38205 - La Laguna, Tenerife , Spain

13. Departamento de Astrofísica, Universidad de La Laguna , E-38205 - La Laguna, Tenerife , Spain

14. Space Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218 , USA

15. Max-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg , Germany

16. INAF-Astronomical Observatory of Capodimonte , Salita Moiariello 16, I-80131 Naples , Italy

17. University of Naples ‘Federico II’ , Via Cinthia 21, Naples I-80126 , Italy

18. Astrophysics Research Institute, Liverpool John Moores University , IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF , UK

19. Department of Astronomy, Case Western Reserve University , 10900 Euclid Avenue, Cleveland, OH 44106 , USA

Abstract

ABSTRACT Intracluster light (ICL) provides an important record of the interactions galaxy clusters have undergone. However, we are limited in our understanding by our measurement methods. To address this, we measure the fraction of cluster light that is held in the Brightest Cluster Galaxy and ICL (BCG+ICL fraction) and the ICL alone (ICL fraction) using observational methods (surface brightness threshold-SB, non-parametric measure-NP, composite models-CM, and multi-galaxy fitting-MGF) and new approaches under development (wavelet decomposition-WD) applied to mock images of 61 galaxy clusters (14 <log10M200c/M⊙ < 14.5) from four cosmological hydrodynamical simulations. We compare the BCG+ICL and ICL fractions from observational measures with those using simulated measures (aperture and kinematic separations). The ICL fractions measured by kinematic separation are significantly larger than observed fractions. We find the measurements are related and provide equations to estimate kinematic ICL fractions from observed fractions. The different observational techniques give consistent BCG+ICL and ICL fractions but are biased to underestimating the BCG+ICL and ICL fractions when compared with aperture simulation measures. Comparing the different methods and algorithms, we find that the MGF algorithm is most consistent with the simulations, and CM and SB methods show the smallest projection effects for the BCG+ICL and ICL fractions, respectively. The Ahad (CM), MGF, and WD algorithms are best set up to process larger samples; however, the WD algorithm in its current form is susceptible to projection effects. We recommend that new algorithms using these methods are explored to analyse the massive samples that Rubin Observatory’s Legacy Survey of Space and Time will provide.

Funder

Australian Research Council

NWO

Swiss National Science Foundation

Horizon 2020

Spanish National Research Council

Instituto de Astrofísica de Andalucía

STFC

European Research Council

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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