Galaxy formation with BECDM – II. Cosmic filaments and first galaxies
© 2020 Oxford University Press. All rights reserved. Bose-Einstein condensate darkmatter (BECDM,also known as fuzzy darkmatter) 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 cos...
| Main Authors: | , , , , , , , , , , , , , |
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| Other Authors: | |
| Format: | Article |
| Language: | English |
| Published: |
Oxford University Press (OUP)
2021
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| Online Access: | https://hdl.handle.net/1721.1/132565 |
| _version_ | 1826217482935861248 |
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| author | Mocz, Philip Fialkov, Anastasia Vogelsberger, Mark Becerra, Fernando Shen, Xuejian Robles, Victor H Amin, Mustafa A Zavala, Jesús Boylan-Kolchin, Michael Bose, Sownak Marinacci, Federico Chavanis, Pierre-Henri Lancaster, Lachlan Hernquist, Lars |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Mocz, Philip Fialkov, Anastasia Vogelsberger, Mark Becerra, Fernando Shen, Xuejian Robles, Victor H Amin, Mustafa A Zavala, Jesús Boylan-Kolchin, Michael Bose, Sownak Marinacci, Federico Chavanis, Pierre-Henri Lancaster, Lachlan Hernquist, Lars |
| author_sort | Mocz, Philip |
| collection | MIT |
| description | © 2020 Oxford University Press. All rights reserved. Bose-Einstein condensate darkmatter (BECDM,also known as fuzzy darkmatter) 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 ×10-22eV, exploring the dynamical effects of its wavelike nature on the cosmicweb and the formation of first galaxies.OurBECDMsimulations are directly compared toCDMaswell 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. |
| first_indexed | 2024-09-23T17:04:22Z |
| format | Article |
| id | mit-1721.1/132565 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T17:04:22Z |
| publishDate | 2021 |
| publisher | Oxford University Press (OUP) |
| record_format | dspace |
| spelling | mit-1721.1/1325652023-01-27T21:12:31Z Galaxy formation with BECDM – II. Cosmic filaments and first galaxies Mocz, Philip Fialkov, Anastasia Vogelsberger, Mark Becerra, Fernando Shen, Xuejian Robles, Victor H Amin, Mustafa A Zavala, Jesús Boylan-Kolchin, Michael Bose, Sownak Marinacci, Federico Chavanis, Pierre-Henri Lancaster, Lachlan Hernquist, Lars Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research © 2020 Oxford University Press. All rights reserved. Bose-Einstein condensate darkmatter (BECDM,also known as fuzzy darkmatter) 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 ×10-22eV, exploring the dynamical effects of its wavelike nature on the cosmicweb and the formation of first galaxies.OurBECDMsimulations are directly compared toCDMaswell 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. 2021-09-20T18:23:04Z 2021-09-20T18:23:04Z 2020 2020-11-17T15:35:11Z Article http://purl.org/eprint/type/JournalArticle https://hdl.handle.net/1721.1/132565 en 10.1093/MNRAS/STAA738 Monthly Notices of the Royal Astronomical Society Creative Commons Attribution-Noncommercial-Share Alike http://creativecommons.org/licenses/by-nc-sa/4.0/ application/pdf Oxford University Press (OUP) arXiv |
| spellingShingle | Mocz, Philip Fialkov, Anastasia Vogelsberger, Mark Becerra, Fernando Shen, Xuejian Robles, Victor H Amin, Mustafa A Zavala, Jesús Boylan-Kolchin, Michael Bose, Sownak Marinacci, Federico Chavanis, Pierre-Henri Lancaster, Lachlan Hernquist, Lars Galaxy formation with BECDM – II. Cosmic filaments and first galaxies |
| title | Galaxy formation with BECDM – II. Cosmic filaments and first galaxies |
| title_full | Galaxy formation with BECDM – II. Cosmic filaments and first galaxies |
| title_fullStr | Galaxy formation with BECDM – II. Cosmic filaments and first galaxies |
| title_full_unstemmed | Galaxy formation with BECDM – II. Cosmic filaments and first galaxies |
| title_short | Galaxy formation with BECDM – II. Cosmic filaments and first galaxies |
| title_sort | galaxy formation with becdm ii cosmic filaments and first galaxies |
| url | https://hdl.handle.net/1721.1/132565 |
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