Clues to the nature of dark matter from first galaxies

Stoychev, Boyan; Dixon, Keri L.; Macciò, Andrea V.; Blank, Marvin; Dutton, Aaron A.

doi:10.1093/mnras/stz1924

Cited by 4 publications

(6 citation statements)

References 87 publications

(101 reference statements)

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“…13. Setting X = 0.76, Y = 0.24, η = 1 (Faucher-Giguère et al 2008), C HII = 3 (Kaurov & Gnedin 2015), χ ion = 10 53 photons (M /yr) −1 s −1 (Stoychev et al 2019) and using a fiducial IGM temperature of 2•10 4 K (Hui & Haiman 2003), data are nicely fitted by our unperturbed full box model, if the escape fraction is set to 12%. Keeping this same parameters for all models, the evolution of the neutral hydrogen fraction 1 − Q HII is displayed in Fig.…”

Section: Evolution Of the Hydrogen Ionized Fractionmentioning

confidence: 87%

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Constraining the primordial magnetic field with dwarf galaxy simulations

Sanati,

Revaz,

Schober

et al. 2020

Preprint

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Using a set of cosmological hydro-dynamical simulations, we constrained the properties of primordial magnetic fields by studying their impact on the formation and evolution of dwarf galaxies. We performed a large set of simulations (8 dark matter only and 72 chemo-hydrodynamical) including primordial magnetic fields through the extra density fluctuations they induce at small length scales (k ≥ 10 h Mpc −1 ) in the matter power spectrum. Our sample of dwarfs include 9 systems selected out of the initial (3.4 Mpc/h) 3 parent box, re-simulated from z = 200 to z = 0 using a zoom-in technique and including the physics of baryons. We explored a large variety of primordial magnetic fields with strength B λ ranging from 0.05 to 0.50 nG and magnetic energy spectrum slopes n B from −2.9 to −2.1. Strong magnetic fields characterized by a high amplitude (B λ = 0.50, 0.20 nG with n B = −2.9) or by a steep initial power spectrum slope (n B = −2.1, −2.4, with B λ = 0.05 nG) induce perturbations in the mass scales from 10 7 to 10 9 M . In this context emerging galaxies see their star formation rate strongly boosted. They become more luminous and metal rich than their counterparts without primordial magnetic fields. Such strong fields are ruled out by their inability to reproduce the observed scaling relations of dwarf galaxies. They predict dwarf galaxies to be at the origin of an unrealistically early reionization of the Universe and also overproduce luminous satellites in the Local Group. Weaker magnetic fields impacting the primordial density field at corresponding masses 10 6 M , produce a large number of mini dark halos orbiting the dwarfs, however out of reach for current lensing observations. This study allows for the first time to constrain the properties of primordial magnetic fields based on realistic cosmological simulations of dwarf galaxies.

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Section: Evolution Of the Hydrogen Ionized Fractionmentioning

confidence: 87%

“…The time evolution of the ionized fraction of hydrogen Q HII may be estimated using a simple differential equation (Madau et al 1999;Springel & Hernquist 2003;Kuhlen & Faucher-Giguère 2012;Stoychev et al 2019):…”

Section: Evolution Of the Hydrogen Ionized Fractionmentioning

confidence: 99%

Constraining the primordial magnetic field with dwarf galaxy simulations

Sanati,

Revaz,

Schober

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…( 13). Setting X = 0.76, Y = 0.24, η = 1 (Faucher-Giguère et al 2008), C HII = 3 (Kaurov & Gnedin 2015), and χ ion = 10 53 photons (M yr −1 ) −1 s −1 (Stoychev et al 2019), and using a fiducial IGM temperature of 2 × 10 4 K (Hui & Haiman 2003), the data are nicely fitted by our unperturbed full box model, if the escape fraction is set to 12%. Keeping this same parameters for all models, the evolution of the neutral hydrogen fraction 1 − Q HII is displayed in Figs.…”

Section: Qhiimentioning

confidence: 88%

“…The time evolution of the ionized fraction of hydrogen Q HII can be estimated using a simple differential equation (Madau et al 1999;Springel & Hernquist 2003;Kuhlen & Faucher-Giguère 2012;Stoychev et al 2019): 11, but for a constant magnetic index n B = −2.9 and a variety of magnetic amplitudes, from B λ = 0.05 to B λ = 0.5 nG.…”

Section: Evolution Of the Hydrogen Ionized Fractionmentioning

confidence: 99%

Constraining the primordial magnetic field with dwarf galaxy simulations

Sanati

Revaz

Schober

et al. 2020

A&A

View full text Add to dashboard Cite

Using a set of cosmological hydro-dynamical simulations, we constrained the properties of primordial magnetic fields by studying their impact on the formation and evolution of dwarf galaxies. We performed a large set of simulations (8 dark matter only and 72 chemo-hydrodynamical) including primordial magnetic fields through the extra density fluctuations they induce at small length scales (k ≥ 10 h Mpc−1) in the matter power spectrum. Our sample of dwarfs includes nine systems selected out of the initial (3.4 Mpc h−1)3 parent box, resimulated from z = 200 to z = 0 using a zoom-in technique and including the physics of baryons. We explored a wide variety of primordial magnetic fields with strength Bλ ranging from 0.05 to 0.50 nG and magnetic energy spectrum slopes nB from −2.9 to −2.1. Strong magnetic fields characterized by a high amplitude (Bλ = 0.50, 0.20 nG with nB = −2.9) or by a steep initial power spectrum slope (nB = −2.1, −2.4, with Bλ = 0.05 nG) induce perturbations on mass scales from 107 to 109 M⊙. In this context emerging galaxies see their star formation rates strongly boosted. They become more luminous and metal rich than their counterparts without primordial magnetic fields. Such strong fields are ruled out by their inability to reproduce the observed scaling relations of dwarf galaxies. They predict that dwarf galaxies are at the origin of an unrealistically early reionization of the Universe and that they also overproduce luminous satellites in the Local Group. Weaker magnetic fields impacting the primordial density field at corresponding masses ≲106 M⊙, produce a large number of mini dark matter halos orbiting the dwarfs, however out of reach for current lensing observations. This study allows us, for the first time, to constrain the properties of primordial magnetic fields based on realistic cosmological simulations of dwarf galaxies.

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“…A growing body of work is focusing on extending constraints on mx into the first billion years at z > 7: analytic models, based on the halo mass function, have been compared to high-redshift observations to obtain constraints of mx > 1.3 − 2.9 keV (Schultz et al 2014;Menci et al 2016;Corasaniti et al 2017;Rudakovskyi et al 2021) with others making predictions of the ultra-violet luminosity function (UV LF) and redshift evolution of the stellar mass density (SMD) that can be tested with the James Webb Space Telescope (JWST; e.g. Dayal et al 2015;Stoychev et al 2019;Lapi et al 2022 Maio & Viel 2015;Villanueva-Domingo et al 2018) and zoom-in simulations (e.g. Stoychev et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Warm dark matter constraints from high-z direct collapse black holes using the JWST

Dayal

Choudhury

Pacucci

2017

Monthly Notices of the Royal Astronomical Society

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We use a semi-analytic model, Delphi, that jointly tracks the dark matter and baryonic assembly of high-redshift (z 4−20) galaxies to gain insight on the number density of Direct Collapse Black Hole (DCBH) hosts in three different cosmologies: the standard Cold Dark Matter (CDM) model and two Warm Dark Matter (WDM) models with particle masses of 3.5 and 1.5 keV. Using the Lyman-Werner (LW) luminosity of each galaxy from Delphi we use a clustering bias analysis to identify all, pristine halos with a virial temperature T vir > ∼ 10 4 K that are irradiated by a LW background above a critical value as, DCBH hosts. In good agreement with previous studies, we find the DCBH number density rises from ∼ 10 −6.1 to ∼ 10 −3.5 cMpc −3 from z 17.5 to 8 in the CDM model using a critical LW background value of 30J 21 (where J 21 = 10 −21 erg s −1 Hz −1 cm −2 sr −1 ). We find that a combination of delayed structure formation and an accelerated assembly of galaxies results in a later metalenrichment and an accelerated build-up of the LW background in the 1.5 keV WDM model, resulting in DCBH hosts persisting down to much lower redshifts (z 5) as compared to CDM where DCBH hosts only exist down to z 8. We end by showing how the expected colours in three different bands of the Near Infrared Camera (NIRCam) onboard the forthcoming James Webb Space Telescope can be used to hunt for potential z 5 − 9 DCBHs, allowing hints on the WDM particle mass.

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Clues to the nature of dark matter from first galaxies

Cited by 4 publications

References 87 publications

Constraining the primordial magnetic field with dwarf galaxy simulations

Constraining the primordial magnetic field with dwarf galaxy simulations

Constraining the primordial magnetic field with dwarf galaxy simulations

Warm dark matter constraints from high-z direct collapse black holes using the JWST

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