Milky Way Satellite Census. IV. Constraints on Decaying Dark Matter from Observations of Milky Way Satellite Galaxies

Mau, S.; Nadler, Ethan O.; Drlica-Wagner, A.; Bechtol, K.; Green, Gregory; Huterer, Dragan; Li, T. S.; Mao, Yao-Yuan; Martı́nez-Vázquez, C. E.; McNanna, M.; Mutlu-Pakdil, Burçin; Pace, Andrew B.; Peter, Annika H. G.; Riley, A. H.; Strigari, Louis E.; Wang, M. -Y.; Aguena, M.; Allam, S.; Annis, J.; Bacon, David; Bertin, E.; Bocquet, S.; Burke, D. L.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Costanzi, M.; Crocce, M.; Pereira, M. E. S.; Davis, Tamara M.; Vicente, J. De; Desai, S.; Doel, P.; Ferrero, I.; Flaugher, B.; Frieman, Joshua A.; García-Bellido, J.; Gatti, M.; Giannini, G.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gutiérrez, G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; James, D. J.; Kuêhn, K.; Lahav, O.; Maia, M. A. G.; Marshall, J. L.; Miquel, R.; Mohr, J. J.; Morgan, R.; Ogando, R. L. C.; Paz-Chinchón, F.; Pieres, A.; Rodríguez-Monroy, M.; Sánchez, E.; Scarpine, V.; Serrano, S.; Sevilla-Noarbe, I.; Suchyta, E.; Tarlè, G.; To, C.; Tucker, D. L.; Weller, J.

doi:10.3847/1538-4357/ac6e65

Cited by 24 publications

(10 citation statements)

References 118 publications

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“…We perform a cosmological zoom-in simulation of an MWlike system using the SIDM model described above, and we compare our results to a corresponding CDM simulation with identical initial conditions. A lower-resolution version of this MW-like simulation was originally presented in Mao et al (2015), used in Nadler et al (2020bNadler et al ( , 2021b, Mau et al (2022) to model the MW satellite galaxy population, and resimulated in a velocity-independent SIDM model to study the effects of self-interactions on subhalos associated with the LMC in Nadler et al (2021a). The higher-resolution CDM simulation that we use here was first presented in Nadler et al (2020b), and our high-resolution SIDM simulation with a velocitydependent cross section is presented here for the first time.…”

Section: Cosmological Zoom-in Simulationsmentioning

confidence: 99%

“…Importantly, our MW host halo stands out from those used in many previous SIDM simulations, including those described above (Zavala et al 2019;Turner et al 2021;, because (1) its early merger history resembles that of the MW, and (2) it hosts a massive LMC analog on recent infall (Nadler et al 2020b). This host has been used to fit the MW satellite galaxy population in CDM and alternative models (Nadler et al 2020b(Nadler et al , 2021bMau et al 2022), and it has been resimulated in velocity-independent SIDM models (Nadler et al 2021a). These properties add to the realism of our MW subhalo population predictions, and allow us to study the LMC-associated subhalo population in a scenario that includes gravothermal core collapse for the first time.…”

Section: Comparison To Previous Simulationsmentioning

confidence: 99%

“…This choice of n s yields an LMC analog that falls into the MW at the correct lookback time (see the discussion in Appendix A ofMau et al 2022). 5 In particular, greater than 90% of the particles within ∼3 Mpc of the MW host halo center are high-resolution particles(Wang et al 2021).…”

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confidence: 99%

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Strong Dark Matter Self-interactions Diversify Halo Populations within and surrounding the Milky Way

Yang

Nadler

2023

ApJ

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We perform a high-resolution cosmological zoom-in simulation of a Milky Way (MW)–like system, which includes a realistic Large Magellanic Cloud analog, using a large differential elastic dark matter self-interaction cross section that reaches ≈100 cm2 g−1 at relative velocities of ≈10 km s−1, motivated by the diverse and orbitally dependent central densities of dwarf galaxies within and surrounding the MW. We explore the effects of dark matter self-interactions on satellite, splashback, and isolated halos through their abundance, central densities, maximum circular velocities, orbital parameters, and correlations between these variables. We use an effective constant cross section model to analytically predict the stages of our simulated halos’ gravothermal evolution, demonstrating that deviations from the collisionless R max – V max relation can be used to select deeply core-collapsed halos, where V max is a halo’s maximum circular velocity, and R max is the radius at which it occurs. We predict that a sizable fraction (≈20%) of subhalos with masses down to ≈108 M ⊙ is deeply core collapsed in our SIDM model. Core-collapsed systems form ≈10% of the isolated halo population down to the same mass; these isolated, core-collapsed halos would host faint dwarf field galaxies with extremely steep central density profiles. Finally, most halos with masses above ≈109 M ⊙ are core-forming in our simulation. Our study thus demonstrates how self-interactions diversify halo populations in an environmentally dependent fashion within and surrounding MW-mass hosts, providing a compelling avenue to address the diverse dark matter distributions of observed dwarf galaxies.

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Section: Cosmological Zoom-in Simulationsmentioning

confidence: 99%

Section: Comparison To Previous Simulationsmentioning

confidence: 99%

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Strong Dark Matter Self-interactions Diversify Halo Populations within and surrounding the Milky Way

Yang

Nadler

2023

ApJ

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“…[15,[18][19][20][21][22][23][24] and references therein), its de Broglie wavelength or mass in ultralight dark-matter models (see, e.g., refs. [25][26][27][28][29][30]), its late-decay lifetime [31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46][47], and the free-streaming scale from non-negligible velocities [48][49][50][51][52][53][54][55][56][57][58][59][60] or even the detailed shape of its distribution function [61][62][63][64][65][66]…”

Section: Jcap01(2024)023mentioning

confidence: 99%

Distinguishing thermal histories of dark matter from structure formation

Huang,

Li,

2024

J. Cosmol. Astropart. Phys.

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It is important to understand the implications of current observational constraints and potential signatures on the thermal history of dark matter. In this paper, we build the connection between the present-day velocities and the production mechanism of dark matter and find that the current observation on structure formation can be imposed to constrain the decoupling temperatures and the phase-space distribution of dark matter. We further explore the potential of distinguishing different possible thermal histories of dark matter with hypothetical future observational data. Using the freeze-in/-out scenarios as templates, we find that future precision data may uniquely identify the allowed parameter spaces for freeze-in and freeze-out, or even completely rule out one of the scenarios. This method can be more generally applied to other scenarios.

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“…Recent systematic searches for ultrafaint Milky Way (MW) satellite galaxies over ∼80% of the sky have allowed for robust inferences about the population of such galaxies within the virial radius of the MW (Koposov et al 2008;Drlica-Wagner et al 2020). This census has allowed for the first constraints on the galaxy-halo connection for dark matter halos below 10 8 M e , including evidence for the statistical impact of the Large Magellanic Cloud (LMC) on the MW satellite population (Nadler et al 2020), and limits on the properties of several alternative dark matter models (Kim et al 2018;Newton et al 2018Newton et al , 2021Nadler et al 2021;Mau et al 2022).…”

Section: Introductionmentioning

confidence: 99%

A Search for Faint Resolved Galaxies Beyond the Milky Way in DES Year 6: A New Faint, Diffuse Dwarf Satellite of NGC 55

McNanna,

Bechtol,

Mau

et al. 2024

ApJ

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We report results from a systematic wide-area search for faint dwarf galaxies at heliocentric distances from 0.3 to 2 Mpc using the full 6 yr of data from the Dark Energy Survey (DES). Unlike previous searches over the DES data, this search specifically targeted a field population of faint galaxies located beyond the Milky Way virial radius. We derive our detection efficiency for faint, resolved dwarf galaxies in the Local Volume with a set of synthetic galaxies and expect our search to be complete to M V ∼ (−7, −10) mag for galaxies at D = (0.3, 2.0) Mpc. We find no new field dwarfs in the DES footprint, but we report the discovery of one high-significance candidate dwarf galaxy at a distance of 2.2 − 0.12 + 0.05 Mpc , a potential satellite of the Local Volume galaxy NGC 55, separated by 47′ (physical separation as small as 30 kpc). We estimate this dwarf galaxy to have an absolute V-band magnitude of − 8.0 − 0.3 + 0.5 mag and an azimuthally averaged physical half-light radius of 2.2 − 0.4 + 0.5 kpc , making this one of the lowest surface brightness galaxies ever found with μ = 32.3 mag arcsec − 2 . This is the largest, most diffuse galaxy known at this luminosity, suggesting possible tidal interactions with its host.

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Milky Way Satellite Census. IV. Constraints on Decaying Dark Matter from Observations of Milky Way Satellite Galaxies

Cited by 24 publications

References 118 publications

Strong Dark Matter Self-interactions Diversify Halo Populations within and surrounding the Milky Way

Strong Dark Matter Self-interactions Diversify Halo Populations within and surrounding the Milky Way

Distinguishing thermal histories of dark matter from structure formation

A Search for Faint Resolved Galaxies Beyond the Milky Way in DES Year 6: A New Faint, Diffuse Dwarf Satellite of NGC 55

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