Magnification Bias of Distant Galaxies in the Hubble Frontier Fields: Testing Wave Versus Particle Dark Matter Predictions

Leung, Enoch; Broadhurst, Tom; Lim, Jeremy; Diego, J. M.; Chiueh, Tzihong; Schive, Hsi-Yu; Windhorst, Rogier A.

doi:10.3847/1538-4357/aacdad

Cited by 23 publications

(27 citation statements)

References 88 publications

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“…[46]) are largely consistent with monotonicity (however, see Ref. [48]), which is consistent with all sources being in halos with mass above 𝑀 0 . In this case, all the halos we observe are formed on scales far from the Jeans scale, and so the relationship between UV magnitude, 𝑀 𝐴𝐵 , and halo mass, 𝑀 ℎ (𝑀 𝐴𝐵 ) is as in Fig.…”

Section: Galaxies and Nonlinear Structuresupporting

confidence: 68%

Astrophysical Searches and Constraints on Ultralight Bosonic Dark Matter

Marsh¹,

Hoof²

2021

Preprint

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Starting from the evidence that dark matter (DM) indeed exists and permeates the entire cosmos, various bounds on its properties can be estimated. Beginning with the cosmic microwave background and large scale structure, we summarize bounds on the ultralight bosonic dark matter (UBDM) mass and cosmic density. These bounds are extended to larger masses by considering galaxy formation and evolution, and the phenomenon of black hole superradiance. We then discuss the formation of different classes of UBDM compact objects including solitons/axion stars and miniclusters. Next, we consider astrophysical constraints on the couplings of UBDM to Standard Model particles, from stellar cooling (production of UBDM) and indirect searches (decays or conversion of UBDM). Throughout, there are short discussions of "hints and opportunities" in searching for UBDM in each area. Astrophysical search channelsAstrophysics and cosmology, as outlined in Chapter 1, give convincing evidence that dark matter (DM) exists in the form of new particles beyond the Standard Model of particle physics. The space of possible theories in Chapter 2, even for the subclass of ultralight bosonic DM (UBDM) models considered in this book, is vast. Beyond the basic fact of the existence of DM, astrophysics can be used to reign in this vast theoretical parameter space, with a view to direct detection and measurement of model parameters.The most basic astrophysical route to constrain UBDM is via the relic density. There are three channels for UBDM production:1. Coherent field oscillations. a. Vacuum realigment. b. Topological defect decay.2. Thermal production. 3. Non-thermal production by direct decay.

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Section: Galaxies and Nonlinear Structuresupporting

confidence: 68%

Astrophysical Searches and Constraints on Ultralight Bosonic Dark Matter

Marsh¹,

Hoof²

2021

Preprint

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“…With that they are able to place a very strong constraint in the mass of the FDM, which must be m 8 × 10 −22 eV to be compatible with this data. A similar study (Leung et al 2018) using HFF finds that m 10 −22 eV.…”

Section: Uv Luminosity Functionmentioning

confidence: 70%

Ultra-light dark matter

Ferreira

2021

Astron Astrophys Rev

232

126

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Ultra-light dark matter is a class of dark matter models (DM), where DM is composed by bosons with masses ranging from $$10^{-24}\, \mathrm {eV}< m < \mathrm {eV}$$ 10 - 24 eV < m < eV . These models have been receiving a lot of attention in the past few years given their interesting property of forming a Bose–Einstein condensate (BEC) or a superfluid on galactic scales. BEC and superfluidity are some of the most striking quantum mechanical phenomena that manifest on macroscopic scales, and upon condensation, the particles behave as a single coherent state, described by the wavefunction of the condensate. The idea is that condensation takes place inside galaxies while outside, on large scales, it recovers the successes of $$\varLambda $$ Λ CDM. This wave nature of DM on galactic scales that arise upon condensation can address some of the curiosities of the behaviour of DM on small-scales. There are many models in the literature that describe a DM component that condenses in galaxies. In this review, we are going to describe those models, and classify them into three classes, according to the different non-linear evolution and structures they form in galaxies: the fuzzy dark matter (FDM), the self-interacting fuzzy dark matter (SIFDM), and the DM superfluid. Each of these classes comprises many models, each presenting a similar phenomenology in galaxies. They also include some microscopic models like the axions and axion-like particles. To understand and describe this phenomenology in galaxies, we are going to review the phenomena of BEC and superfluidity that arise in condensed matter physics, and apply this knowledge to DM. We describe how ULDM can potentially reconcile the cold DM picture with the small-scale behaviour. These models present a rich phenomenology that is manifest in different astrophysical consequences. We review here the astrophysical and cosmological tests used to constrain those models, together with new and future observations that promise to test these models in different regimes. For the case of the FDM class, the mass where this model has an interesting phenomenology on small-scales $$ \sim 10^{-22}\, \mathrm {eV}$$ ∼ 10 - 22 eV , is strongly challenged by current observations. The parameter space for the other two classes remains weakly constrained. We finalize by showing some predictions that are a consequence of the wave nature of this component, like the creation of vortices and interference patterns, that could represent a smoking gun in the search of these rich and interesting alternative class of DM models.

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“…In particular, we consider also the alternative model of wave dark matter (ψDM, Schive et al 2014), which produces a suppression of small-scale structure. The UV LF of this model can be described as a modified Schechter function (see Leung et al 2018, for more details).…”

Section: Predicted Number Of Lensed High-redshift Galaxiesmentioning

confidence: 99%

Probability of magnification in the $\textit{Hubble Frontier Fields}$ clusters

Vega-Ferrero,

Diego,

Bernstein

2019

Preprint

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We present free-form gravitational lensing models derived with the wslap+ code for the six Hubble Frontier Fields clusters using the latest data available from the Frontier Fields Lensing Models v.4 collaboration. We present magnifications maps in the lens plane and caustic maps in the source plane. From these maps, we derive the probability of magnification using two different, but related, methods. We confirm MACS 0717 as the cluster with the most complex structure, and having the largest lensing efficiency and Einstein radius. When comparing these results with the ones obtained by previous observations of these clusters, we obtain an increase in the lensing efficiency between 1.4 and 2.3. We also find a good correlation with a relatively small dispersion between the lensing efficiency and Einstein radius as a function of the source redshift (z s ). Finally, we estimate the lensing effects produced by the six Hubble Frontier Fields clusters on the luminosity function of galaxies at high redshift (z = 9) for standard luminosity functions and an alternative luminosity function based on predictions from wave dark matter (ψDM) models.

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Magnification Bias of Distant Galaxies in the Hubble Frontier Fields: Testing Wave Versus Particle Dark Matter Predictions

Cited by 23 publications

References 88 publications

Astrophysical Searches and Constraints on Ultralight Bosonic Dark Matter

Astrophysical Searches and Constraints on Ultralight Bosonic Dark Matter

Ultra-light dark matter

Probability of magnification in the $\textit{Hubble Frontier Fields}$ clusters

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