First Simulations of Axion Minicluster Halos

Eggemeier, Benedikt; Redondo, Javier; Dolag, K.; Niemeyer, J. C.; Vaquero, Alejandro

doi:10.1103/physrevlett.125.041301

Cited by 94 publications

(172 citation statements)

References 47 publications

(46 reference statements)

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“…But whether it is still a good approximation for models that, on small scales, differ vastly from ΛCDM has yet to be studied in detail. We plan to study this question in future work, but for the moment we limit our discussion to PS predictions and compare them to numerical results available for the case of axion miniclusters [34]. The results of this comparison, shown in appendix B, suggest that -at least for axion miniclusters -PS still provides a good estimate of the HMF.…”

Section: Halo Mass Functionmentioning

confidence: 96%

“…(3.10) against N -body simulations. For ΛCDM halos (for which z col 10) we use the results in [35] and find C ρ ∼ 600, for axion miniclusters (for which z col 10 3 ) we use the results of [34] and find C ρ ∼ 9 × 10 4 . In the following we use a z col -dependent C ρ which smoothly interpolates between these two values.…”

Section: Jhep06(2021)028mentioning

confidence: 99%

“…In this appendix we compare the numerically derived HMF for axion models where the PQ symmetry is broken after inflation [34], against some commonly used analytic prescriptions. Specifically, we compare the numerical result against the analytic predictions of the Press-Schechter [19], and Sheth-Tormen [50] formalisms.…”

Section: A Signal Generation Monte Carlomentioning

confidence: 99%

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Probing small-scale power spectra with pulsar timing arrays

Lee

Mitridate

Trickle

et al. 2021

J. High Energ. Phys.

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Models of Dark Matter (DM) can leave unique imprints on the Universe’s small scale structure by boosting density perturbations on small scales. We study the capability of Pulsar Timing Arrays to search for, and constrain, subhalos from such models. The models of DM we consider are ordinary adiabatic perturbations in ΛCDM, QCD axion miniclusters, models with early matter domination, and vector DM produced during inflation. We show that ΛCDM, largely due to tidal stripping effects in the Milky Way, is out of reach for PTAs. Axion miniclusters may be within reach, although this depends crucially on whether the axion relic density is dominated by the misalignment or string contribution. Models where there is matter domination with a reheat temperature below 1 GeV may be observed with future PTAs. Lastly, vector DM produced during inflation can be detected if it is lighter than 10−16 GeV. We also make publicly available a Python Monte Carlo tool for generating the PTA time delay signal from any model of DM substructure.

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Section: Halo Mass Functionmentioning

confidence: 96%

Section: Jhep06(2021)028mentioning

confidence: 99%

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Probing small-scale power spectra with pulsar timing arrays

Lee

Mitridate

Trickle

et al. 2021

J. High Energ. Phys.

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“…Thus, the initial distribution is not predicted by e.g., Boltzmann codes but has to be followed by QCD lattice simulations (Vaquero et al 2019;Buschmann et al 2019). Because of these complications, only recently the first selfconsistent cosmological simulation of the formation of structure in an axion dark matter field was carried out (Eggemeier et al 2020; see Fig. 14).…”

Section: Axionsmentioning

confidence: 99%

Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

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We review the field of collisionless numerical simulations for the large-scale structure of the Universe. We start by providing the main set of equations solved by these simulations and their connection with General Relativity. We then recap the relevant numerical approaches: discretization of the phase-space distribution (focusing on N-body but including alternatives, e.g., Lagrangian submanifold and Schrödinger–Poisson) and the respective techniques for their time evolution and force calculation (direct summation, mesh techniques, and hierarchical tree methods). We pay attention to the creation of initial conditions and the connection with Lagrangian Perturbation Theory. We then discuss the possible alternatives in terms of the micro-physical properties of dark matter (e.g., neutralinos, warm dark matter, QCD axions, Bose–Einstein condensates, and primordial black holes), and extensions to account for multiple fluids (baryons and neutrinos), primordial non-Gaussianity and modified gravity. We continue by discussing challenges involved in achieving highly accurate predictions. A key aspect of cosmological simulations is the connection to cosmological observables, we discuss various techniques in this regard: structure finding, galaxy formation and baryonic modelling, the creation of emulators and light-cones, and the role of machine learning. We finalise with a recount of state-of-the-art large-scale simulations and conclude with an outlook for the next decade.

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“…In addition, localized clumps can also be produced if dark matter features strong self-interactions [54][55][56][57]. Another important potential source are initial conditions featuring large inhomogeneities, a prominent example of which are axion miniclusters [58][59][60][61] (see also [62][63][64][65][66] for some more recent work). More recently, such large fluctuations have also been discussed in the context of inflationary production mechanisms [67,68] or as a consequence of a fragmentation of homogeneous fields due to their (self-)interactions [69,70].…”

Section: Introductionmentioning

confidence: 99%

Probing dark matter clumps, strings and domain walls with gravitational wave detectors

Jaeckel¹,

Schenk

Spannowsky

2021

Eur. Phys. J. C

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Gravitational wave astronomy has recently emerged as a new way to study our Universe. In this work, we survey the potential of gravitational wave interferometers to detect macroscopic astrophysical objects comprising the dark matter. Starting from the well-known case of clumps we expand to cosmic strings and domain walls. We also consider the sensitivity to measure the dark matter power spectrum on small scales. Our analysis is based on the fact that these objects, when traversing the vicinity of the detector, will exert a gravitational pull on each node of the interferometer, in turn leading to a differential acceleration and corresponding Doppler signal, that can be measured. As a prototypical example of a gravitational wave interferometer, we consider signals induced at LISA. We further extrapolate our results to gravitational wave experiments sensitive in other frequency bands, including ground-based interferometers, such as LIGO, and pulsar timing arrays, e.g. ones based on the Square Kilometer Array. Assuming moderate sensitivity improvements beyond the current designs, clumps, strings and domain walls may be within reach of these experiments.

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First Simulations of Axion Minicluster Halos

Cited by 94 publications

References 47 publications

Probing small-scale power spectra with pulsar timing arrays

Probing small-scale power spectra with pulsar timing arrays

Large-scale dark matter simulations

Probing dark matter clumps, strings and domain walls with gravitational wave detectors

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