How to quench a dwarf galaxy: The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments

Harley Katz; Marius Ramsoy; Joakim Rosdahl; Taysun Kimm; Blaizot Jérémy Blaizot; Martin G. Haehnelt; Michel-Dansac Léo Michel-Dansac; Thibault Garel; Clotilde Laigle; Julien Devriendt; Adrianne Slyz

doi:10.1093/MNRAS/STAA639

How to quench a dwarf galaxy: The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments

Harley Katz, Marius Ramsoy, Joakim Rosdahl, Taysun Kimm, Blaizot Jérémy Blaizot, Martin G. Haehnelt, Michel-Dansac Léo Michel-Dansac, Thibault Garel, Clotilde Laigle, Julien Devriendt, Adrianne Slyz

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34 Citations (Scopus)

Abstract

We use the SPHINX suite of high-resolution cosmological radiation hydrodynamics simulations to study how spatially and temporally inhomogeneous reionization impacts the baryonic content of dwarf galaxies and cosmic filaments. We compare simulations with and without stellar radiation to isolate the effects of radiation feedback from that of supernova, cosmic expansion, and numerical resolution. We find that the gas content of cosmic filaments can be reduced by more than 80 per cent following reionization. The gas inflow rates into haloes with Mvir ≲ 108 M⊙ are strongly affected and are reduced by more than an order of magnitude compared to the simulation without reionization. A significant increase in gas outflow rates is found for halo masses Mvir ≲ 7 × 107 M⊙. Our simulations show that inflow suppression (i.e. starvation), rather than photoevaporation, is the dominant mechanism by which the baryonic content of high-redshift dwarf galaxies is regulated. At fixed redshift and halo mass, there is a large scatter in the halo baryon fractions that is entirely dictated by the timing of reionization in the local region surrounding a halo which can change by Δz ≳ 3 at fixed mass. Finally, although the gas content of high-redshift dwarf galaxies is significantly impacted by reionization, we find that most haloes with Mvir ≲ 108M⊙ can remain self-shielded and form stars long after reionization, until their local gas reservoir is depleted, suggesting that Local Group dwarf galaxies do not necessarily exhibit star formation histories that peak prior to z = 6. Significantly larger simulation boxes will be required to capture the full process of reionization and understand how our results translate to environments not probed by our current work.

Original language	English
Pages (from-to)	2200-2220
Number of pages	21
Journal	Monthly Notices of the Royal Astronomical Society
Volume	494
Issue number	2
DOIs	https://doi.org/10.1093/MNRAS/STAA639
Publication status	Published - 2020

Bibliographical note

Funding Information:
We thank the referee for their detailed and constructive reviewof the manuscript. HK thanks Brasenose College and the support of the NicholasKurti Junior Fellowship and the Beecroft Fellowship. Support by ERC Advanced Grant 320596 'The Emergence of Structure during the Epoch of reionization' is gratefully acknowledged. TK was supported in part by the Yonsei University Future-leading Research Initiative (RMS2-2019-22-0216) and in part by the National Research Foundation of Korea (NRF-2017R1A5A1070354 and NRF-2018R1C1B5036146). JR and JB acknowledge support from the ORAGE project from the Agence Nationale de la Recherche under grand ANR-14-CE33-0016-03. TG acknowledges support from the European Research Council under grant agreement ERCstg- 757258 (TRIPLE). The research of AS and JD is supported by Adrian Beecroft and STFC. The results of this research have been achieved using the PRACE Research Infrastructure resource SuperMUC based in Garching, Germany.

Funding Information:
We thank the referee for their detailed and constructive review of the manuscript. HK thanks Brasenose College and the support of the Nicholas Kurti Junior Fellowship and the Beecroft Fellowship. Support by ERC Advanced Grant 320596 ‘The Emergence of Structure during the Epoch of reionization’ is gratefully acknowledged. TK was supported in part by the Yonsei University Future-leading Research Initiative (RMS2-2019-22-0216) and in part by the National Research Foundation of Korea (NRF-2017R1A5A1070354 and NRF-2018R1C1B5036146). JR and JB acknowledge support from the ORAGE project from the Agence Nationale de la Recherche under grand ANR-14-CE33-0016-03. TG acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE). The research of AS and JD is supported by Adrian Beecroft and STFC. The results of this research have been achieved using the PRACE Research Infrastructure resource SuperMUC based in Garching, Germany.

Publisher Copyright:
© 2020 The Author(s).

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/MNRAS/STAA639

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Katz, H., Ramsoy, M., Rosdahl, J., Kimm, T., Jérémy Blaizot, B., Haehnelt, M. G., Léo Michel-Dansac, M-D., Garel, T., Laigle, C., Devriendt, J., & Slyz, A. (2020). How to quench a dwarf galaxy: The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments. Monthly Notices of the Royal Astronomical Society, 494(2), 2200-2220. https://doi.org/10.1093/MNRAS/STAA639

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title = "How to quench a dwarf galaxy: The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments",

abstract = "We use the SPHINX suite of high-resolution cosmological radiation hydrodynamics simulations to study how spatially and temporally inhomogeneous reionization impacts the baryonic content of dwarf galaxies and cosmic filaments. We compare simulations with and without stellar radiation to isolate the effects of radiation feedback from that of supernova, cosmic expansion, and numerical resolution. We find that the gas content of cosmic filaments can be reduced by more than 80 per cent following reionization. The gas inflow rates into haloes with Mvir ≲ 108 M⊙ are strongly affected and are reduced by more than an order of magnitude compared to the simulation without reionization. A significant increase in gas outflow rates is found for halo masses Mvir ≲ 7 × 107 M⊙. Our simulations show that inflow suppression (i.e. starvation), rather than photoevaporation, is the dominant mechanism by which the baryonic content of high-redshift dwarf galaxies is regulated. At fixed redshift and halo mass, there is a large scatter in the halo baryon fractions that is entirely dictated by the timing of reionization in the local region surrounding a halo which can change by Δz ≳ 3 at fixed mass. Finally, although the gas content of high-redshift dwarf galaxies is significantly impacted by reionization, we find that most haloes with Mvir ≲ 108M⊙ can remain self-shielded and form stars long after reionization, until their local gas reservoir is depleted, suggesting that Local Group dwarf galaxies do not necessarily exhibit star formation histories that peak prior to z = 6. Significantly larger simulation boxes will be required to capture the full process of reionization and understand how our results translate to environments not probed by our current work.",

author = "Harley Katz and Marius Ramsoy and Joakim Rosdahl and Taysun Kimm and {J{\'e}r{\'e}my Blaizot}, Blaizot and Haehnelt, {Martin G.} and {L{\'e}o Michel-Dansac}, Michel-Dansac and Thibault Garel and Clotilde Laigle and Julien Devriendt and Adrianne Slyz",

note = "Funding Information: We thank the referee for their detailed and constructive reviewof the manuscript. HK thanks Brasenose College and the support of the NicholasKurti Junior Fellowship and the Beecroft Fellowship. Support by ERC Advanced Grant 320596 'The Emergence of Structure during the Epoch of reionization' is gratefully acknowledged. TK was supported in part by the Yonsei University Future-leading Research Initiative (RMS2-2019-22-0216) and in part by the National Research Foundation of Korea (NRF-2017R1A5A1070354 and NRF-2018R1C1B5036146). JR and JB acknowledge support from the ORAGE project from the Agence Nationale de la Recherche under grand ANR-14-CE33-0016-03. TG acknowledges support from the European Research Council under grant agreement ERCstg- 757258 (TRIPLE). The research of AS and JD is supported by Adrian Beecroft and STFC. The results of this research have been achieved using the PRACE Research Infrastructure resource SuperMUC based in Garching, Germany. Funding Information: We thank the referee for their detailed and constructive review of the manuscript. HK thanks Brasenose College and the support of the Nicholas Kurti Junior Fellowship and the Beecroft Fellowship. Support by ERC Advanced Grant 320596 {\textquoteleft}The Emergence of Structure during the Epoch of reionization{\textquoteright} is gratefully acknowledged. TK was supported in part by the Yonsei University Future-leading Research Initiative (RMS2-2019-22-0216) and in part by the National Research Foundation of Korea (NRF-2017R1A5A1070354 and NRF-2018R1C1B5036146). JR and JB acknowledge support from the ORAGE project from the Agence Nationale de la Recherche under grand ANR-14-CE33-0016-03. TG acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE). The research of AS and JD is supported by Adrian Beecroft and STFC. The results of this research have been achieved using the PRACE Research Infrastructure resource SuperMUC based in Garching, Germany. Publisher Copyright: {\textcopyright} 2020 The Author(s).",

year = "2020",

doi = "10.1093/MNRAS/STAA639",

language = "English",

volume = "494",

pages = "2200--2220",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "2",

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Katz, H, Ramsoy, M, Rosdahl, J, Kimm, T, Jérémy Blaizot, B, Haehnelt, MG, Léo Michel-Dansac, M-D, Garel, T, Laigle, C, Devriendt, J & Slyz, A 2020, 'How to quench a dwarf galaxy: The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments', Monthly Notices of the Royal Astronomical Society, vol. 494, no. 2, pp. 2200-2220. https://doi.org/10.1093/MNRAS/STAA639

TY - JOUR

T1 - How to quench a dwarf galaxy

T2 - The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments

AU - Katz, Harley

AU - Ramsoy, Marius

AU - Rosdahl, Joakim

AU - Kimm, Taysun

AU - Jérémy Blaizot, Blaizot

AU - Haehnelt, Martin G.

AU - Léo Michel-Dansac, Michel-Dansac

AU - Garel, Thibault

AU - Laigle, Clotilde

AU - Devriendt, Julien

AU - Slyz, Adrianne

N1 - Funding Information: We thank the referee for their detailed and constructive reviewof the manuscript. HK thanks Brasenose College and the support of the NicholasKurti Junior Fellowship and the Beecroft Fellowship. Support by ERC Advanced Grant 320596 'The Emergence of Structure during the Epoch of reionization' is gratefully acknowledged. TK was supported in part by the Yonsei University Future-leading Research Initiative (RMS2-2019-22-0216) and in part by the National Research Foundation of Korea (NRF-2017R1A5A1070354 and NRF-2018R1C1B5036146). JR and JB acknowledge support from the ORAGE project from the Agence Nationale de la Recherche under grand ANR-14-CE33-0016-03. TG acknowledges support from the European Research Council under grant agreement ERCstg- 757258 (TRIPLE). The research of AS and JD is supported by Adrian Beecroft and STFC. The results of this research have been achieved using the PRACE Research Infrastructure resource SuperMUC based in Garching, Germany. Funding Information: We thank the referee for their detailed and constructive review of the manuscript. HK thanks Brasenose College and the support of the Nicholas Kurti Junior Fellowship and the Beecroft Fellowship. Support by ERC Advanced Grant 320596 ‘The Emergence of Structure during the Epoch of reionization’ is gratefully acknowledged. TK was supported in part by the Yonsei University Future-leading Research Initiative (RMS2-2019-22-0216) and in part by the National Research Foundation of Korea (NRF-2017R1A5A1070354 and NRF-2018R1C1B5036146). JR and JB acknowledge support from the ORAGE project from the Agence Nationale de la Recherche under grand ANR-14-CE33-0016-03. TG acknowledges support from the European Research Council under grant agreement ERC-stg-757258 (TRIPLE). The research of AS and JD is supported by Adrian Beecroft and STFC. The results of this research have been achieved using the PRACE Research Infrastructure resource SuperMUC based in Garching, Germany. Publisher Copyright: © 2020 The Author(s).

PY - 2020

Y1 - 2020

N2 - We use the SPHINX suite of high-resolution cosmological radiation hydrodynamics simulations to study how spatially and temporally inhomogeneous reionization impacts the baryonic content of dwarf galaxies and cosmic filaments. We compare simulations with and without stellar radiation to isolate the effects of radiation feedback from that of supernova, cosmic expansion, and numerical resolution. We find that the gas content of cosmic filaments can be reduced by more than 80 per cent following reionization. The gas inflow rates into haloes with Mvir ≲ 108 M⊙ are strongly affected and are reduced by more than an order of magnitude compared to the simulation without reionization. A significant increase in gas outflow rates is found for halo masses Mvir ≲ 7 × 107 M⊙. Our simulations show that inflow suppression (i.e. starvation), rather than photoevaporation, is the dominant mechanism by which the baryonic content of high-redshift dwarf galaxies is regulated. At fixed redshift and halo mass, there is a large scatter in the halo baryon fractions that is entirely dictated by the timing of reionization in the local region surrounding a halo which can change by Δz ≳ 3 at fixed mass. Finally, although the gas content of high-redshift dwarf galaxies is significantly impacted by reionization, we find that most haloes with Mvir ≲ 108M⊙ can remain self-shielded and form stars long after reionization, until their local gas reservoir is depleted, suggesting that Local Group dwarf galaxies do not necessarily exhibit star formation histories that peak prior to z = 6. Significantly larger simulation boxes will be required to capture the full process of reionization and understand how our results translate to environments not probed by our current work.

AB - We use the SPHINX suite of high-resolution cosmological radiation hydrodynamics simulations to study how spatially and temporally inhomogeneous reionization impacts the baryonic content of dwarf galaxies and cosmic filaments. We compare simulations with and without stellar radiation to isolate the effects of radiation feedback from that of supernova, cosmic expansion, and numerical resolution. We find that the gas content of cosmic filaments can be reduced by more than 80 per cent following reionization. The gas inflow rates into haloes with Mvir ≲ 108 M⊙ are strongly affected and are reduced by more than an order of magnitude compared to the simulation without reionization. A significant increase in gas outflow rates is found for halo masses Mvir ≲ 7 × 107 M⊙. Our simulations show that inflow suppression (i.e. starvation), rather than photoevaporation, is the dominant mechanism by which the baryonic content of high-redshift dwarf galaxies is regulated. At fixed redshift and halo mass, there is a large scatter in the halo baryon fractions that is entirely dictated by the timing of reionization in the local region surrounding a halo which can change by Δz ≳ 3 at fixed mass. Finally, although the gas content of high-redshift dwarf galaxies is significantly impacted by reionization, we find that most haloes with Mvir ≲ 108M⊙ can remain self-shielded and form stars long after reionization, until their local gas reservoir is depleted, suggesting that Local Group dwarf galaxies do not necessarily exhibit star formation histories that peak prior to z = 6. Significantly larger simulation boxes will be required to capture the full process of reionization and understand how our results translate to environments not probed by our current work.

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How to quench a dwarf galaxy: The impact of inhomogeneous reionization on dwarf galaxies and cosmic filaments

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