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Galaxy formation with BECDM – II. Cosmic filaments and first galaxies

Mocz, Philip and Fialkov, Anastasia and Vogelsberger, Mark and Becerra, Fernando and Shen, Xuejian and Robles, Victor H. and Amin, Mustafa A. and Zavala, Jesús and Boylan-Kolchin, Michael and Bose, Sownak and Marinacci, Federico and Chavanis, Pierre-Henri and Lancaster, Lachlan and Hernquist, Lars (2020) Galaxy formation with BECDM – II. Cosmic filaments and first galaxies. Monthly Notices of the Royal Astronomical Society, 494 (2). pp. 2027-2044. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20200611-122301205

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Abstract

Bose–Einstein condensate dark matter (BECDM, also known as fuzzy dark matter) is motivated by fundamental physics and has recently received significant attention as a serious alternative to the established cold dark matter (CDM) model. We perform cosmological simulations of BECDM gravitationally coupled to baryons and investigate structure formation at high redshifts (z ≳ 5) for a boson mass m = 2.5 × 10⁻²² eV, exploring the dynamical effects of its wavelike nature on the cosmic web and the formation of first galaxies. Our BECDM simulations are directly compared to CDM as well as to simulations where the dynamical quantum potential is ignored and only the initial suppression of the power spectrum is considered – a warm dark matter-like (‘WDM’) model often used as a proxy for BECDM. Our simulations confirm that ‘WDM’ is a good approximation to BECDM on large cosmological scales even in the presence of the baryonic feedback. Similarities also exist on small scales, with primordial star formation happening both in isolated haloes and continuously along cosmic filaments; the latter effect is not present in CDM. Global star formation and metal enrichment in these first galaxies are delayed in BECDM/‘WDM’ compared to the CDM case: in BECDM/‘WDM’ first stars form at z ∼ 13/13.5, while in CDM star formation starts at z ∼ 35. The signature of BECDM interference, not present in ‘WDM’, is seen in the evolved dark matter power spectrum: although the small-scale structure is initially suppressed, power on kpc scales is added at lower redshifts. Our simulations lay the groundwork for realistic simulations of galaxy formation in BECDM.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/staa738DOIArticle
https://arxiv.org/abs/1911.05746arXivDiscussion Paper
ORCID:
AuthorORCID
Mocz, Philip0000-0001-6631-2566
Vogelsberger, Mark0000-0001-8593-7692
Becerra, Fernando0000-0002-8282-4024
Robles, Victor H.0000-0002-9497-9963
Zavala, Jesús0000-0002-7051-1100
Boylan-Kolchin, Michael0000-0002-9604-343X
Bose, Sownak0000-0002-0974-5266
Marinacci, Federico0000-0003-3816-7028
Lancaster, Lachlan0000-0002-0041-4356
Hernquist, Lars0000-0001-6950-1629
Additional Information:© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2020 March 13. Received 2020 February 20; in original form 2019 November 13. Published: 14 April 2020. We thank Jerry Ostriker, Mariangela Lisanti, David Spergel, Scott Tremaine, James Bullock, and Frenk van den Bosch for valuable discussions, and the anonymous referee for helpful comments. Support (PM) for this work was provided by NASA through Einstein Postdoctoral Fellowship grant number PF7-180164 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. AF is supported by the Royal Society University Research Fellowship. MBK acknowledges support from NSF grants AST-1517226, AST-1910346, and CAREER grant AST-1752913 and from NASA grants NNX17AG29G and HST-AR-14282, HST-AR-14554, HST-AR-15006, HST-GO-14191, and HST-GO-15658 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555. JZ acknowledges support by a Grant of Excellence from the Icelandic Research fund (grant number 173929). FM is supported by the Program ‘Rita Levi Montalcini’ of the Italian MIUR. The authors acknowledge the Texas Advanced Computing Center (TACC) at The University of Texas at Austin for providing HPC resources that have contributed to the research results reported within this paper. URL: http://www.tacc.utexas.edu. XSEDE Allocation TG-AST170020. Some of the computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University.
Group:TAPIR
Funders:
Funding AgencyGrant Number
NASA Einstein FellowshipPF7-180164
NASANAS8-03060
Royal SocietyUNSPECIFIED
NSFAST-1517226
NSFAST-1910346
NSFAST-1752913
NASANNX17AG29G
NASAHST-AR-14282
NASAHST-AR-14554
NASAHST-AR-15006
NASAHST-GO-14191
NASAHST-GO-15658
Space Telescope Science InstituteUNSPECIFIED
NASANAS5-26555
Icelandic Research Fund173929
Ministero dell'Istruzione, dell'Universita e della Ricerca (MIUR)UNSPECIFIED
NSFTG-AST170020
Subject Keywords:galaxies: formation – galaxies: high-redshift – dark matter – cosmology: theory
Issue or Number:2
Record Number:CaltechAUTHORS:20200611-122301205
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200611-122301205
Official Citation:Philip Mocz, Anastasia Fialkov, Mark Vogelsberger, Fernando Becerra, Xuejian Shen, Victor H Robles, Mustafa A Amin, Jesús Zavala, Michael Boylan-Kolchin, Sownak Bose, Federico Marinacci, Pierre-Henri Chavanis, Lachlan Lancaster, Lars Hernquist, Galaxy formation with BECDM – II. Cosmic filaments and first galaxies, Monthly Notices of the Royal Astronomical Society, Volume 494, Issue 2, May 2020, Pages 2027–2044, https://doi.org/10.1093/mnras/staa738
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:103854
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:11 Jun 2020 20:24
Last Modified:11 Jun 2020 20:24

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