Fundamental Physics with the Hubble Frontier Fields: Constraining Dark Matter Models with the Abundance of Extremely Faint and Distant Galaxies

Menci, Nicola; Merle, Alexander; Totzauer, Maximilian; Schneider, Aurel; Grazian, A.; Castellano, M.; Sánchez, Norma G.

doi:10.3847/1538-4357/836/1/61

Cited by 76 publications

(68 citation statements)

References 124 publications

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“…To create sizeable cores in halos of dwarf galaxies without involving baryonic processes, one requires rather light dark matter particles (m fd < 300 eV; see Table 1). Such dark matter is in tension with a number of constraints from observations of large-scale structure; see, e.g., recent works [74][75][76][77][78][79][80][81][82][83][84][85]. However, due to the smallness of their potential wells, dwarf galaxies are very sensitive to baryonic feedback processes; see, e.g., [86][87][88][89][90][91][92][93][94][95].…”

Section: Discussionmentioning

confidence: 99%

New Model of Density Distribution for Fermionic Dark Matter Halos

Rudakovskyi

Savchenko

2018

Ukr. J. Phys.

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PACSIn this paper, we formulate a new model of density distribution for halos made of warm dark matter (WDM) particles. The model is described by a single microphysics parameter the mass (or, equivalently, the maximal value of the initial phase-space density distribution) of dark matter particles. Given the WDM particle mass and the parameters of a dark matter density profile at the halo periphery, this model predicts the inner density profile. In case of initial Fermi-Dirac distribution, we successfully reproduce cored dark matter profiles from N -body simulations. Also, we calculate the core radii of warm dark matter halos of dwarf spheroidal galaxies for particle masses mfd = 100, 200, 300 and 400 eV. K e y w o r d s: Dark matter: warm, cold; dark matter halo profile; cores; Navarro-Frenk-White profileThe nature of dark matter the largest gravitating substance in the Universe is not yet identified. Usual (left-handed) neutrinos the only natural dark matter candidate within the Standard Model of particle physics are too light to form the observed large-scale structure of the Universe [1] and the densest dark matter-dominated objects, dwarf spheroidals (dSphs) [2]. So far, many extensions of the Standard Model containing a viable dark matter candidate have been proposed; see, e.g., reviews [3][4][5][6]. In terms of their initial velocities, valid dark matter candidates can be split in two groups 1 (see, e.g., [9]):• cold dark matter (CDM), composed of particles with small (non-relativistic) initial velocities [10,11]; c A.V. RUDAKOVSKYI, D.O. SAVCHENKO, 2018 1 Note that, for some specific dark matter particle candidates, their initial velocity spectrum can be approximated by a mixture of 'cold ' and 'warm' components [7, 8].• warm dark matter (WDM), composed of particles with large (relativistic) initial velocities [12,13].Density distribution of CDM haloes is often described by the Navarro-Frenk-White (NFW) profile [14,15] ρ nfw (r) = ρ s r s r 1 + r rs 2 . (1) Its parameters ρ s and r s are connected with the halo mass M 200 (the mass within the sphere of radius R 200 , within which the average density is 200 times larger than the critical density ρ crit of the Universe) and halo concentration parameter c 200 = R 200 /r s .The phase-space density for CDM haloes becomes infinite towards the halo centre; see, e.g., [16]. For WDM, this is not true: its maximal phase-space density f max is finite at early times and does not increase during halo formation [17]. Usually, density distri-

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Section: Discussionmentioning

confidence: 99%

New Model of Density Distribution for Fermionic Dark Matter Halos

Rudakovskyi

Savchenko

2018

Ukr. J. Phys.

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“…Current limits based on observations of the number counts of high redshift galaxies in the Hubble Frontier Fields places a limit of m > 2.4 keV at the 2σ level, competitive with the Local Volume constraints (e.g. Menci et al 2017;Castellano et al 2019;Sameie et al 2019).…”

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confidence: 98%

Double dark matter vision: twice the number of compact-source lenses with narrow-line lensing and the WFC3 grism

Nierenberg

Gilman²,

Treu³

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The magnifications of compact-source lenses are extremely sensitive to the presence of low mass dark matter halos along the entire sight line from the source to the observer. Traditionally, the study of dark matter structure in compact-source strong gravitational lenses has been limited to radio-loud systems, as the radio emission is extended and thus unaffected by microlensing which can mimic the signal of dark matter structure. An alternate approach is to measure quasar nuclear-narrow line emission, which is free from microlensing and present in virtually all quasar lenses. In this paper, we double the number of systems which can be used for gravitational lensing analyses by presenting measurements of narrow-line emission from a sample of 8 quadruply imaged quasar lens systems, WGD J0405-3308, HS 0810+2554, RX J0911+0551, SDSS J1330+1810, PS J1606-2333, WFI 2026-4536, WFI 2033-4723 and WGD J2038-4008. We describe our updated grism spectral modelling pipeline, which we use to measure narrow-line fluxes with uncertainties of 2-10%, presented here. We fit the lensed image positions with smooth mass models and demonstrate that these models fail to produce the observed distribution of image fluxes, and have typical deviations larger than those expected from macromodel uncertainties. This discrepancy indicates the presence of perturbations caused by small-scale dark matter structure. The interpretation of this result in terms of dark matter models will be presented in a companion paper.

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“…We now wish to quantify more precisely the level of discrepancy between the model and observational measurements. To do so we adopt a procedure similar to Menci et al (2017). In particular, we calculate the expected cumulative number density n obs from data within the stellar mass range of M * = 10 7 − 10 9 M and compare it with the abundance predicted from the simulations for each DM model.…”

Section: Galaxy Stellar Mass Functionmentioning

confidence: 99%

“…A number of works (e.g. Bozek et al 2015;Schive et al 2016;Menci et al 2017;Carucci & Corasaniti 2018) have already discussed how the faint-end LFs can be sensitive to small-scale structure formations and provide a powerful tool to constrain FDM models. In particular, semi-analytic models or DM-only cosmological simulations have been performed to quantify the suppression of the small halo abundance in FDM scenario and then been used to predict the high-redshift galaxy UV LF (using empirical relations between galaxy luminosity and halo mass).…”

Section: Introductionmentioning

confidence: 99%

Predictions for the abundance of high-redshift galaxies in a fuzzy dark matter universe

Feng

Matteo

2019

Monthly Notices of the Royal Astronomical Society

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During the last decades, rapid progress has been made in measurements of the rest-frame ultraviolet (UV) luminosity function (LF) for high-redshift galaxies (z ≥ 6). The faint-end of the galaxy LF at these redshifts provides powerful constraints on different dark matter models that suppress small-scale structure formation. In this work we perform full hydrodynamical cosmological simulations of galaxy formation using an alternative DM model composed of extremely light bosonic particles (m ∼ 10 −22 eV), also known as fuzzy dark matter (FDM), and examine the predictions for the galaxy stellar mass function and luminosity function at z ≥ 6 for a range of FDM masses. We find that for FDM models with bosonic mass m = 5 × 10 −22 eV, the number density of galaxies with stellar mass M * ∼ 10 7 M is suppressed by ∼ 40% at z = 9, ∼ 20% at z = 5, and the UV LFs within magnitude range of -16 < M UV < -14 is suppressed by ∼ 60% at z = 9, ∼ 20% at z = 5 comparing to the CDM counterpart simulation. Comparing our predictions with current measurements of the faint-end LFs (−18 M UV −14), we find that FDM models with m 22 < 5 × 10 −22 are ruled out at 3σ confidence level. We expect that future LF measurements by James Webb Space Telescope (JWST), which will extend down to M UV ∼ −13 for z 10, with a survey volume that is comparable to the Hubble Ultra Deep Field (HUDF) would have the capability to constrain FDM models to m 10 −21 eV.

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Fundamental Physics with the Hubble Frontier Fields: Constraining Dark Matter Models with the Abundance of Extremely Faint and Distant Galaxies

Cited by 76 publications

References 124 publications

New Model of Density Distribution for Fermionic Dark Matter Halos

New Model of Density Distribution for Fermionic Dark Matter Halos

Double dark matter vision: twice the number of compact-source lenses with narrow-line lensing and the WFC3 grism

Predictions for the abundance of high-redshift galaxies in a fuzzy dark matter universe

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