The impact of cored density profiles on the observable quantities of dwarf spheroidal galaxies

Harvey, David; Revaz, Yves; Robertson, Andrew; Hausammann, Loïc

doi:10.1093/mnrasl/sly159

Cited by 27 publications

(22 citation statements)

References 34 publications

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“…In general, it is non-trivial to infer the DM distribution from observations (e.g. Kowalczyk et al 2013;Harvey et al 2018;Oman et al 2019;Genina et al 2020;He et al 2020) and it is important to test how these difficulties impact the inferred SIDM cross-section when isothermal Jeans modelling is applied to observations. This was recently done in the context of galaxy cluster observations by Sagunski et al (2020), who found that the inferred cross-section from isothermal Jeans modelling using mock observations of simulated clusters was in agreement with the crosssection used in the simulations.…”

Section: Discussion a N D O U T L O O Kmentioning

confidence: 99%

The surprising accuracy of isothermal Jeans modelling of self-interacting dark matter density profiles

Robertson

Massey

Eke

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Recent claims of observational evidence for self-interacting dark matter (SIDM) have relied on a semi-analytic method for predicting the density profiles of galaxies and galaxy clusters containing SIDM. We present a thorough description of this method, known as isothermal Jeans modelling, and then test it with a large ensemble of haloes taken from cosmological simulations. Our simulations were run with cold and collisionless dark matter (CDM) as well as two different SIDM models, all with dark matter only variants as well as versions including baryons and relevant galaxy formation physics. Using a mix of different box sizes and resolutions, we study haloes with masses ranging from 3 × 1010 to $3 \times 10^{15} \mathrm{\, M_\odot }$. Overall, we find that the isothermal Jeans model provides as accurate a description of simulated SIDM density profiles as the Navarro–Frenk–White profile does of CDM haloes. We can use the model predictions, compared with the simulated density profiles, to determine the input DM–DM scattering cross-sections used to run the simulations. This works especially well for large cross-sections, while with CDM our results tend to favour non-zero (albeit fairly small) cross-sections, driven by a bias against small cross-sections inherent to our adopted method of sampling the model parameter space. The model works across the whole halo mass range we study, although including baryons leads to DM profiles of intermediate-mass ($10^{12} - 10^{13} \mathrm{\, M_\odot }$) haloes that do not depend strongly on the SIDM cross-section. The tightest constraints will therefore come from lower and higher mass haloes: dwarf galaxies and galaxy clusters.

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Section: Discussion a N D O U T L O O Kmentioning

confidence: 99%

The surprising accuracy of isothermal Jeans modelling of self-interacting dark matter density profiles

Robertson

Massey

Eke

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…This could lead to gravothermal collapse in dwarf galaxies or low surface brightness galaxies (LSBs) resulting in cuspy DM profiles [42] contrary to perceptions that these systems have cored profiles [26][27][28][29][30][31][32]. On the other hand there is evidence suggesting that not all dwarf spheroidals are cored [35,51,52]. In the present work we are primarily concerned with much more massive galaxies where SMBHs have been observed, so we confine our investigation to the range 200 km/s v c 500 km/s.…”

Section: Dissipative Dark Matter Modelsmentioning

confidence: 98%

Early formation of supermassive black holes via dark matter self-interactions

Choquette

Cline

Cornell

2019

J. Cosmol. Astropart. Phys.

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The existence of supermassive black holes at high redshifts (z ∼ 7) is difficult to accommodate in standard astrophysical scenarios. It has been shown that dark matter models with a subdominant self-interacting component are able to produce early seeds for supermassive black holes through the gravothermal catastrophe. Previous studies used a fluid equation approach, requiring some limiting assumptions. Here we reconsider the problem using N -body gravitational simulations starting from the formation of the initial dark matter halo. We consider both elastic and dissipative scattering, and elucidate the interplay between the dark matter microphysics and subsequent accretion of the black hole needed to match the properties of observed high redshift supermassive black holes. We find a region of parameter space in which a small component of self-interacting dark matter can produce the observed high redshift supermassive black holes.

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“…DMO simulations predict the dark halos to follow an universal cuspy profile (Navarro et al 1996(Navarro et al , 1997, while observations favour cored ones (Moore (1994); Flores & Primack (1994), see Read et al (2018) for a short review.) While improvements in the baryonic treatment of cosmological simulations allowed for a reduction of those tensions (Chan et al 2015;Sawala et al 2016;Wetzel et al 2016;Verbeke et al 2017;Revaz & Jablonka 2018;Pontzen & Governato 2014;Oñorbe et al 2015;Chan et al 2015;Fitts et al 2017;Hausammann et al 2019), modification or alternative to the ΛCDM have been proposed too, like warm dark matter (Lovell et al 2012;Governato et al 2015;Fitts et al 2019), selfinteracting dark matter (Vogelsberger et al 2014;Harvey et al 2018;Fitts et al 2019) or wave dark matter (Chan et al 2018).…”

Section: Introductionmentioning

confidence: 99%

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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The impact of cored density profiles on the observable quantities of dwarf spheroidal galaxies

Cited by 27 publications

References 34 publications

The surprising accuracy of isothermal Jeans modelling of self-interacting dark matter density profiles

The surprising accuracy of isothermal Jeans modelling of self-interacting dark matter density profiles

Early formation of supermassive black holes via dark matter self-interactions

Constraining the primordial magnetic field with dwarf galaxy simulations

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