Self-interactions of ULDM to the rescue?

Dave, Bihag; Goswami, Gaurav

doi:10.1088/1475-7516/2023/07/015

Cited by 12 publications

(3 citation statements)

References 72 publications

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“…It is also worth noting that for the case of attractive self-interactions, we do not look at solutions for λini < −0.4. This is because in the absence of tidal effects, λini < −0.4 corresponds to the unstable branch of solutions (or the so-called non-gravitational regime) [17,62]. We see that just like the case of no interactions, a larger ωini leads to a larger decay rate and a smaller lifetime.…”

Section: The Impact Of Self-interactions Of Dm: a First Lookmentioning

confidence: 79%

“…(3.45) in section 3.2.3 in [13], section 5.1.2 in [11] as well as [54,55]). Indeed, there has been a growing interest in recent years to study and constrain self-interactions of scalar field dark matter [14,15,[56][57][58][59][60][61][62][63][64][65][66][67].…”

Section: Jcap02(2024)044mentioning

confidence: 99%

“…In [62], we had found that (a) repulsive self-interactions with λ ≳ 10 −91 can explain observed rotation curves for dark matter dominated galaxies as well as satisfy an appropriate soliton-halo relation, and, (b) including attractive self-interactions did not have the same interesting effect. On the contrary, in the present work, we found that consideration of lifetimes of satellite galaxies prefers attractive self-couplings of comparable strengths.…”

Section: Jcap02(2024)044mentioning

confidence: 99%

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ULDM self-interactions, tidal effects and tunnelling out of satellite galaxies

Dave,

Goswami

2024

J. Cosmol. Astropart. Phys.

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It is well-known that Dark Matter (DM) inside a satellite galaxy orbiting a host halo experiences a tidal potential. If DM is ultra-light, given its wave-like nature, one expects it to tunnel out of the satellite — if this happens sufficiently quickly, then the satellite will not survive over cosmological timescales, severely constraining this dark matter model. In this paper, we study the effects of the inevitable quartic self-interaction of scalar Ultra-Light Dark Matter (ULDM) on the lifetimes of satellite galaxies by looking for quasi-stationary solutions with outgoing wave boundary conditions. For a satellite with some known core mass and orbital period, we find that, attractive (repulsive) self-interactions decrease (increase) the rate of tunnelling of DM out of it. In particular, for satellite galaxies with core mass ∼𝒪(107–108) M⊙ and orbital period ∼𝒪(1) Gyr, one can impose constraints on the strength of self-interactions as small as λ∼𝒪(10-92). For instance, for ULDM mass m = 10-22 eV, the existence of the Fornax dwarf galaxy necessitates attractive self-interactions with λ≲ -2.12 × 10-91.

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Section: The Impact Of Self-interactions Of Dm: a First Lookmentioning

confidence: 79%

Section: Jcap02(2024)044mentioning

confidence: 99%

Section: Jcap02(2024)044mentioning

confidence: 99%

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ULDM self-interactions, tidal effects and tunnelling out of satellite galaxies

Dave,

Goswami

2024

J. Cosmol. Astropart. Phys.

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Confronting fuzzy dark matter with the rotation curves of nearby dwarf irregular galaxies

Banares-Hernandez¹,

Castillo²,

Camalich³

et al. 2023

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Aims. In this paper, we carry out a phenomenological investigation of the viability of fuzzy dark matter, which is composed of coherent waves of non-interacting ultralight axions with a mass of ma ≈ 10−22 eV. We did so by confronting the predictions of the model, in particular, the formation of a solitonic core at the center of dark matter halos, with a homogeneous and robust sample of high-resolution rotation curves from the LITTLE THINGS in 3D catalog. This comprises a collection of isolated, dark matter-dominated dwarf-irregular galaxies that provides an optimal benchmark for cosmological studies. Our aim is to find evidence of fuzzy dark matter in the observations; alternatively, we seek to set exclusion ranges for its mass. Methods. We used a statistical framework based on a χ2 analysis of the rotation curves of the LITTLE THINGS in 3D catalog using a fuzzy dark matter profile as the theoretical model. This allows us to extract relevant parameters such as the axion mass and mass of the solitonic core, as well as the mass of the dark matter halo and its concentration parameter. We fit the data using current Markov chain Monte Carlo techniques with a rather loose set of priors, except for the implementation of a core-halo relation predicted by simulations. The results of the fits were then used to perform various diagnostics on the predictions of the model. Results. Fuzzy dark matter provides an excellent fit to the rotation curves of the LITTLE THINGS in 3D catalog, with axion masses determined from different galaxies clustering around ma ≈ 2 × 10−23 eV. However, we find two major problems from our analysis. First, the data follow scaling relations of the properties of the core, which are not consistent with the predictions of the soliton. This problem is particularly acute in the core radius-mass relation with a tension that (at face value) has a significance of ≳5σ. The second problem is related to the strong suppression of the linear power spectrum that is predicted by fuzzy dark matter for the axion mass preferred by the data. This can be constrained very conservatively by the galaxy counts in our sample, which leads to a tension that exceeds 5σ. We estimate the effects of baryons in our analysis and discuss whether they could alleviate the tensions of the model with observations.

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Novel structures and collapse of solitons in nonminimally gravitating dark matter halos

Chen,

Zhang

2024

J. Cosmol. Astropart. Phys.

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Ultralight dark matter simulations predict condensates with short-range correlation, known as solitons or boson stars, at the centers of dark matter halos. This paper investigates the formation and collapse of dark matter solitons influenced by nonminimal gravitational effects, characterized by gradient-dependent self-interactions of dark matter and an additional source in Poisson's equation for gravity. Our simulations suggest that the initial evolution of dark matter resembles that without nonminimal gravitational effects. However, regions with negative potential curvature may develop, and solitons will collapse when their densities reach certain critical values for both positive and negative coupling constants. With strong nonminimal gravitational effects, we verify that linear density perturbations could grow on both large and small scales, potentially enhancing structure formation.

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Self-interactions of ULDM to the rescue?

Cited by 12 publications

References 72 publications

ULDM self-interactions, tidal effects and tunnelling out of satellite galaxies

ULDM self-interactions, tidal effects and tunnelling out of satellite galaxies

Confronting fuzzy dark matter with the rotation curves of nearby dwarf irregular galaxies

Novel structures and collapse of solitons in nonminimally gravitating dark matter halos

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