15 research outputs found
The viability of low-mass subhaloes as targets for gamma-ray dark matter searches
In this work, we investigate the discovery potential of low-mass Galactic
dark matter (DM) subhaloes for indirect searches of DM. We use data from the
Via Lactea II (VL-II) N-body cosmological simulation, which resolves subhaloes
down to solar masses and it is thus ideal for this purpose.
First, we characterize the abundance, distribution and structural properties of
the VL-II subhalo population in terms of both subhalo masses and maximum
circular velocities. Then, we repopulate the original simulation with millions
of subhaloes of masses down to about five orders of magnitude below the minimum
VL-II subhalo mass (more than one order of magnitude in velocities). We compute
subhalo DM annihilation astrophysical "J-factors" and angular sizes for the
entire subhalo population, by placing the Earth at a random position but at the
right galactocentric distance in the simulation. Thousands of these
realizations are generated in order to obtain statistically meaningful results.
We find that some nearby low-mass Galactic subhaloes, not massive enough to
retain stars or gas, may indeed yield DM annihilation fluxes comparable to
those expected from other, more massive and acknowledgeable DM targets like
dwarf satellite galaxies. Typical angular sizes are of the order of the degree,
thus subhaloes potentially appearing as extended sources in gamma-ray
telescopes, depending on instrument angular resolution and sensitivity. Our
work shows that low-mass Galactic subhaloes with no visible counterparts are
expected to play a relevant role in current and future indirect DM search
searches and should indeed be considered as excellent DM targets.Comment: 15 pages, 15 figures. Submitted to MNRAS. Comments welcome
Spatial extension of dark subhalos as seen by Fermi-LAT and the implications for WIMP constraints
Spatial extension has been hailed as a "smoking gun"in the gamma-ray search of dark galactic subhalos, which would appear as unidentified sources for gamma-ray telescopes. In this work, we study the sensitivity of the Fermi-LAT to extended subhalos using simulated data based on a realistic sky model. We simulate spatial templates for a set of representative subhalos, whose parameters were derived from our previous work with N-body cosmological simulation data. We find that detecting an extended subhalo and finding an unequivocal signal of angular extension requires, respectively, a flux 2 to 10 times larger than in the case of a pointlike source. By studying a large grid of models, where parameters such as the WIMP mass, annihilation channel, or subhalo model are varied significantly, we obtain the response of the LAT as a function of the product of annihilation cross-section times the J factor. Indeed, we show that spatial extension can be used as an additional "filter"to reject subhalos candidates among the pool of unidentified LAT sources, as well as a smoking gun for positive identification. For instance, typical angular extensions of a few tenths of a degree are expected for the considered scenarios. Finally, we also study the impact of the obtained LAT sensitivity to such extended subhalos on the achievable dark matter constraints, which are a few times less constraining than comparable point-source limit
Shedding light on low-mass subhalo survival and annihilation luminosity with numerical simulations
In this work, we carry out a suite of specially designed numerical simulations to shed light on dark matter (DM) subhalo
survival at mass scales relevant for gamma-ray DM searches, a topic subject to intense debate nowadays. We have employed
an improved version of DASH, a GPU N-body code, to study the evolution of low-mass subhaloes inside a Milky-Way-like
halo with unprecedented accuracy, reaching solar-mass and sub-parsec resolution. We simulate subhaloes with varying mass,
concentration, and orbital properties, and consider the effect of baryons in the host. We analyse the evolution of the bound
mass fraction and annihilation luminosity, finding that most subhaloes survive until present, yet losing in some cases more than
99 per cent of their initial mass. Baryons induce a much greater mass-loss, especially when the subhalo orbit is more parallel
to the Galactic disc. Many of these subhaloes cross the solar Galactocentric radius, making it easier to detect their annihilation
fluxes from Earth. We find subhaloes orbiting a DM-only halo with a pericentre in the solar vicinity to lose 70–90 per cent
of their initial annihilation luminosity at present, which increases up to 99 per cent when including baryons. We find a strong
relation between subhalo’s mass-loss and the effective tidal field at pericentre. Indeed, much of the dependence on all considered
parameters can be explained through this single parameter. In addition to shedding light on the survival of low-mass Galactic
subhaloes, our results can provide detailed predictions that will aid current and future quests for the nature of D
Properties of subhalos in the interacting dark matter scenario
One possible and natural derivation fromthe collisionless cold dark matter (CDM) standard cosmological framework is the assumption of the existence of interactions between dark matter (DM) and photons or neutrinos. Such a possible interacting dark matter (IDM) model would imply a suppression of small-scale structures due to a large collisional damping effect, even though the weakly-interacting massive particle (WIMP) can still be the DM candidate. Because of this, IDM models can help alleviate alleged tensions between standard CDM predictions and observations at small mass scales. In this work, we investigate the properties of the DM halo substructure or subhalos formed in a high-resolution cosmological N-body simulation specifically run within these alternative models. We also run its CDM counterpart, which allowed us to compare subhalo properties in both cosmologies. We show that, in the lower mass range covered by our simulation runs, both subhalo concentrations and abundances are systematically lower in IDM compared to the CDM scenario. Yet, as in CDM, we find that median IDM subhalo concentration values increase towards the innermost regions of their hosts for the same mass subhalos. Similarly to CDM, we find IDM subhalos to be more concentrated than field halos of the same mass. Our work has a direct application to studies aimed at the indirect detection of DM where subhalos are expected to boost the DM signal of their host halos significantly. From our results, we conclude that the role of the halo substructure in DM searches will be less important in interacting scenarios than in CDM, but is nevertheless far from being negligible.Fil: Moliné, Ángeles. Universidad Autónoma de Madrid; España. Consejo Superior de Investigaciones Científicas; EspañaFil: Schewtschenko, Jascha A.. University of Portsmouth; Reino UnidoFil: Sánchez Conde, Miguel A.. Universidad Autónoma de Madrid; EspañaFil: Aguirre Santaella, Alejandra. Universidad Autónoma de Madrid; EspañaFil: Cora, Sofia Alejandra. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Abadi, Mario Gabriel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentin
Properties of subhalos in the interacting dark matter scenario
One possible and natural derivation from the collisionless cold dark matter (CDM) standard cosmological framework is the assumption of the existence of interactions between dark matter (DM) and photons or neutrinos. Such possible interacting dark matter (IDM) model would imply a suppression of small-scale structures due to a large collisional damping effect, even though the weakly interacting massive particle (WIMP) can still be the DM candidate. Because of this, IDM models can help alleviate alleged tensions between standard CDM predictions and observations at small mass scales. In this work, we investigate the properties of DM halo substructure or subhalos formed in a high-resolution cosmological N-body simulation specifically run within these alternative models. We also run its CDM counterpart, which allowed us to compare subhalo properties in both cosmologies. We show that, in the lower mass range covered by our simulation runs, both subhalo concentrations and abundances are systematically lower in IDM compared to the CDM scenario. Yet, as in CDM, we find that median IDM subhalo concentration values increase towards the innermost regions of their hosts for same mass subhalos. Also similarly to CDM, we find IDM subhalos to be more concentrated than field halos of the same mass. Our work has a direct application on studies aimed at the indirect detection of DM where subhalos are expected to boost the DM signal of their host halos significantly. From our results, we conclude that the role of halo substructure in DM searches will be less important in interacting scenarios than in CDM, but is nevertheless far from being negligible.Facultad de Ciencias Astronómicas y Geofísica
Spectral and spatial analysis of the dark matter subhalo candidates among Fermi Large Area Telescope unidentified sources
Fermi-LAT unidentified sources (unIDs) have proven to be compelling targets
for performing indirect dark matter (DM) searches. In a previous work, we found
that among the 1235 unIDs in Fermi-LAT catalogs (3FGL, 2FHL and 3FHL) only 44
of those are DM subhalos candidates. We now implement a spectral analysis to
test whether these remaining sources are compatible or not with DM origin. This
analysis is executed using almost 10 years of Pass 8 Fermi-LAT data. None of
the unIDs are found to significantly prefer DM-induced emission compared to
other, more conventional, astrophysical sources. In order to discriminate
between pulsar and DM sources, we developed a new method which is based on the
source's spectral curvature, peak energy, and its detection significance. We
also look for spatial extension, which may be a hint for a DM origin according
to our N-body simulation studies of the subhalo population. In addition, we
used Gaia DR2 data to search for a potential stellar counterpart to our best DM
subhalo candidates and, although no firm associations could be found, one of
them coincides with the Sagittarius stream. Finally, previous constraints on
the DM annihilation cross section are updated with the new number of remaining
DM subhalo candidates among unIDs. Our limits now rule out canonical thermal
WIMPs up to masses of 10 GeV for and 20 GeV for
annihilation channels, in this way being as sensitive and complementary to
those obtained from other targets and probes.Comment: 27 pages, 10 figures, JCAP accepted. Matches the accepted versio
LCDM halo substructure properties revealed with high resolution and large volume cosmological simulations
We investigate the structural properties, distribution and abundance of LCDM
dark matter subhaloes using the Phi-4096 and Uchuu suite of N-body cosmological
simulations. Thanks to the combination of their large volume, high mass
resolution and superb statistics, we are able to quantify -- for the first time
consistently over more than seven decades in ratio of subhalo-to-host-halo mass
-- dependencies of subhalo properties with mass, maximum circular velocity,
Vmax, host halo mass and distance to host halo centre. We also dissect the
evolution of these dependencies over cosmic time. We provide accurate fits for
the subhalo mass and velocity functions, both exhibiting decreasing power-law
slopes in the expected range of values and with no significant dependence on
redshift. We also find subhalo abundance to depend weakly on host halo mass. We
explore the distribution of subhaloes within their hosts and its evolution over
cosmic time for subhaloes located as deep as ~0.1 per cent of the host virial
radius. Subhalo structural properties are codified via a concentration
parameter, cV, that does not depend on any specific, pre-defined density
profile and relies only on Vmax. We derive the cV-Vmax relation in the range
7-1500 km/s and find an important dependence on distance of the subhalo to the
host halo centre, as already described in Molin\'e et al. (2017).
Interestingly, we also find subhaloes of the same mass to be significantly more
concentrated into more massive hosts. Finally, we investigate the redshift
evolution of cV, and provide accurate fits that take into account all mentioned
dependencies. Our results offer an unprecedented detailed characterization of
the subhalo population, consistent over a wide range of subhalo and host halo
masses, as well as cosmic times. Our work enables precision work in any future
research involving dark matter halo substructure.Comment: 17 pages, 15 figures, 5 tables. Submitted to the journal. Comments
welcome
Tidal Stripping in the Adiabatic Limit
We present a model for the remnants of haloes that have gone through an
adiabatic tidal stripping process. We show that this model exactly reproduces
the remnant of an NFW halo that is exposed to a slowly increasing isotropic
tidal field and approximately for an anisotropic tidal field. The model can be
used to predict the asymptotic mass loss limit for orbiting subhaloes, solely
as a function of the initial structure of the subhalo and the value of the
tidal field at pericentre. Predictions can easily be made for differently
concentrated host-haloes with and without baryonic components, which differ
most notably in their relation between pericentre radius and tidal field. The
model correctly predicts several empirically measured relations such as the
`tidal track' and the `orbital frequency relation' that was reported by Errani
& Navarro (2021) for the case of an isothermal sphere. Further, we discover the
`structure-tide' degeneracy which implies that increasing the concentration of
a subhalo has exactly the same impact on tidal stripping as reducing the
amplitude of the tidal field. Beyond this, we find that simple relations hold
for the bound mass, truncation radius, WIMP annihilation luminosity and tidal
ratio of tidally stripped NFW haloes in relation to quantities measured at the
radius of maximum circular velocity. Finally, we note that NFW haloes cannot be
completely disrupted when exposed adiabatically to tidal fields of arbitrary
magnitudes. We provide an open-source implementation of our model and suggest
that it can be used to improve predictions of dark matter annihilation.Comment: 30 pages, 19 figures, submitted to MNRAS, comments welcome, code
publicly available under https://github.com/jstuecker/adiabatic-tide
Unidentified gamma-ray sources as targets for indirect dark matter detection with the Fermi-Large Area Telescope
One of the predictions of the ΛCDM cosmological framework is the hierarchical formation of structure, giving rise to dark matter (DM) halos and subhalos. When the latter are massive enough they retain gas (i.e., baryons) and become visible. This is the case of the dwarf satellite galaxies in the Milky Way (MW). Below a certain mass, halos may not accumulate significant amounts of baryons and remain completely dark. However, if DM particles are Weakly Interacting Massive Particles (WIMPs), we expect them to annihilate in subhalos, producing gamma rays which can be detected with the Fermi satellite. Using the three most recent point-source Fermi Large Area Telescope (LAT) catalogs (3FGL, 2FHL and 3FHL), we search for DM subhalo candidates among the unidentified sources, i.e., sources with no firm association to a known astrophysical object. We apply several selection criterio based on the expected properties of the DM-induced emission from subhalos, which allow us to significantly reduce the list of potential candidates. Then, by characterizing the mínimum detection flux of the instrument and comparing our sample to predictions from the Via Lactea II (VL-II) N-body cosmological simulation, we place conservative and robust constraints on the hσvi – m_(DM) parameter space. For annihilation via the τ ^(+)τ^(−) channel, we put an upper limit of 4 × 10^(26) (5 × 10^(25)) cm^(3)s^(−1) for a mass of 10 (100) GeV. A critical improvement over previous treatments is the repopulation we made to include low-mass subhalos below the VL-II mass resolution. With more advanced subhalo candidate filtering the sensitivity reach of our method can potentially improve these constraints by a factor 3 (2) for τ^( +)τ^(−) (b ̄b) channel.Comunidad de MadridCentros de Excelencia Severo OchoaNASA Fermi Guest Investigator ProgramMinisterio de Economía y Empresa (España)Agencia Estatal de Investigación (España)United States Department of Energy (DOE)Depto. de Estructura de la Materia, Física Térmica y ElectrónicaFac. de Ciencias FísicasInstituto de Física de Partículas y del Cosmos (IPARCOS)TRUEpu
CDM halo substructure properties revealed with high resolution and large volume cosmological simulations
We investigate the structural properties, distribution and abundance of LCDM dark matter subhaloes using the Phi-4096 and Uchuu suite of N-body cosmological simulations. Thanks to the combination of their large volume, high mass resolution and superb statistics, we are able to quantify -- for the first time consistently over more than seven decades in ratio of subhalo-to-host-halo mass -- dependencies of subhalo properties with mass, maximum circular velocity, Vmax, host halo mass and distance to host halo centre. We also dissect the evolution of these dependencies over cosmic time. We provide accurate fits for the subhalo mass and velocity functions, both exhibiting decreasing power-law slopes in the expected range of values and with no significant dependence on redshift. We also find subhalo abundance to depend weakly on host halo mass. We explore the distribution of subhaloes within their hosts and its evolution over cosmic time for subhaloes located as deep as ~0.1 per cent of the host virial radius. Subhalo structural properties are codified via a concentration parameter, cV, that does not depend on any specific, pre-defined density profile and relies only on Vmax. We derive the cV-Vmax relation in the range 7-1500 km/s and find an important dependence on distance of the subhalo to the host halo centre, as already described in Moliné et al. (2017). Interestingly, we also find subhaloes of the same mass to be significantly more concentrated into more massive hosts. Finally, we investigate the redshift evolution of cV, and provide accurate fits that take into account all mentioned dependencies. Our results offer an unprecedented detailed characterization of the subhalo population, consistent over a wide range of subhalo and host halo masses, as well as cosmic times. Our work enables precision work in any future research involving dark matter halo substructure