Quantifying substructures in Hubble Frontier Field clusters: comparison with ΛCDM simulations
Abstract
The Hubble Frontier Fields (HFF) are six clusters of galaxies, all showing indications of recent mergers, which have recently been observed for lensed images. As such they are the natural laboratories to study the merging history of galaxy clusters. In this work, we explore the 2D power spectrum of the mass distribution $$P_{\rm M}(k)$$ as a measure of substructure. We compare $$P_{\rm M}(k)$$ of these clusters (obtained using strong gravitational lensing) to that of $$\Lambda$$CDM simulated clusters of similar mass. In order to compute lensing $$P_{\rm M}(k)$$, we produced free-form lensing mass reconstructions of HFF clusters, without any light traces mass (LTM) assumption. Moreover, the inferred power at small scales tends to be larger if (i)~the cluster is at lower redshift, and/or (ii)~there are deeper observations and hence more lensed images. In contrast, lens reconstructions assuming LTM show higher power at small scales even with fewer lensed images; it appears the small scale power in the LTM reconstructions is dominated by light information, rather than the lensing data. The average lensing derived $$P_{\rm M}(k)$$ shows lower power at small scales as compared to that of simulated clusters at redshift zero, both dark-matter only and hydrodynamical. The possible reasons are: (i)~the available strong lensing data are limited in their effective spatial resolution on the mass distribution, (ii)~HFF clusters have yet to build the small scale power they would have at $$z\sim 0$$, or (iii)~simulations are somehow overestimating the small scale power.
- Authors:
-
- Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); Univ. of Zurich (Switzerland)
- Univ. of Zurich (Switzerland)
- Univ. of Minnesota, Minneapolis, MN (United States)
- Univ. of Hasselt (Belgium)
- Publication Date:
- Research Org.:
- Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), High Energy Physics (HEP)
- OSTI Identifier:
- 1260265
- Report Number(s):
- FERMILAB-PUB-16-083-A; arXiv:1507.01532
Journal ID: ISSN 0035-8711; 1381500
- Grant/Contract Number:
- AC02-07CH11359
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Volume: 459; Journal Issue: 2; Journal ID: ISSN 0035-8711
- Publisher:
- Royal Astronomical Society
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; galaxies: clusters: individual: Abell 2744; galaxies: clusters: individual: Abell 370; galaxies: clusters: individual: Abell S1063; galaxies: clusters: individual: MACS J0416.1+2403; galaxies: clusters: individual: MACS J0717.5+3745; galaxies: clusters: individual: MACS J1149.5+2223
Citation Formats
Mohammed, Irshad, Saha, Prasenjit, Williams, Liliya L. R., Liesenborgs, Jori, and Sebesta, Kevin. Quantifying substructures in Hubble Frontier Field clusters: comparison with ΛCDM simulations. United States: N. p., 2016.
Web. doi:10.1093/mnras/stw727.
Mohammed, Irshad, Saha, Prasenjit, Williams, Liliya L. R., Liesenborgs, Jori, & Sebesta, Kevin. Quantifying substructures in Hubble Frontier Field clusters: comparison with ΛCDM simulations. United States. https://doi.org/10.1093/mnras/stw727
Mohammed, Irshad, Saha, Prasenjit, Williams, Liliya L. R., Liesenborgs, Jori, and Sebesta, Kevin. Wed .
"Quantifying substructures in Hubble Frontier Field clusters: comparison with ΛCDM simulations". United States. https://doi.org/10.1093/mnras/stw727. https://www.osti.gov/servlets/purl/1260265.
@article{osti_1260265,
title = {Quantifying substructures in Hubble Frontier Field clusters: comparison with ΛCDM simulations},
author = {Mohammed, Irshad and Saha, Prasenjit and Williams, Liliya L. R. and Liesenborgs, Jori and Sebesta, Kevin},
abstractNote = {The Hubble Frontier Fields (HFF) are six clusters of galaxies, all showing indications of recent mergers, which have recently been observed for lensed images. As such they are the natural laboratories to study the merging history of galaxy clusters. In this work, we explore the 2D power spectrum of the mass distribution $P_{\rm M}(k)$ as a measure of substructure. We compare $P_{\rm M}(k)$ of these clusters (obtained using strong gravitational lensing) to that of $\Lambda$CDM simulated clusters of similar mass. In order to compute lensing $P_{\rm M}(k)$, we produced free-form lensing mass reconstructions of HFF clusters, without any light traces mass (LTM) assumption. Moreover, the inferred power at small scales tends to be larger if (i)~the cluster is at lower redshift, and/or (ii)~there are deeper observations and hence more lensed images. In contrast, lens reconstructions assuming LTM show higher power at small scales even with fewer lensed images; it appears the small scale power in the LTM reconstructions is dominated by light information, rather than the lensing data. The average lensing derived $P_{\rm M}(k)$ shows lower power at small scales as compared to that of simulated clusters at redshift zero, both dark-matter only and hydrodynamical. The possible reasons are: (i)~the available strong lensing data are limited in their effective spatial resolution on the mass distribution, (ii)~HFF clusters have yet to build the small scale power they would have at $z\sim 0$, or (iii)~simulations are somehow overestimating the small scale power.},
doi = {10.1093/mnras/stw727},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 459,
place = {United States},
year = {Wed Apr 13 00:00:00 EDT 2016},
month = {Wed Apr 13 00:00:00 EDT 2016}
}
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