43 research outputs found
Cosmic reionization history and dark matter scenarios
Summary plot is Fig. 8: constraints on escape fraction and UV limiting magnitude for cold and non-cold dark matter. This version matches the published oneInternational audienceWe perform an analysis of the cosmic reionization in the standard cold dark matter (CDM) paradigm and in alternative dark matter scenarios. Building upon the work of Corasaniti et al. (2017), we predict the reionization history for CDM, for warm dark matter (WDM), late-forming dark matter (LFDM) and ultra-light axion dark matter (ADM) models which reproduce state-of-art measurements of the galaxy luminosity function at very high-redshifts . To this purpose we adopt a reionization model parametrized in terms of the limiting UV-magnitude of galaxies contributing to the reionization and the average effective escape fraction of UV photons reaching the intergalactic medium . For each DM model we compute the redshift evolution of the Thomson scattering optical depth and the comoving ionization fraction . We find the different DM models to have similar reionization histories. Differences with respect to the CDM case increase at fainter limiting UV-magnitudes and are degenerate with the effect of varying the reionization model parameters. Using Planck's determination of the integrated optical depth in combination with measurements of the neutral hydrogen fraction at different redshifts, we infer constraints on and . The results are largely independent of the assumed DM scenario, in particular for we obtain that the effective escape fraction lies in the range at
Matter around Kerr black holes in scalar-tensor theories: scalarization and superradiant instability
In electrovacuum stationary, asymptotically flat black holes in scalar-tensor
theories of gravity are described by the Kerr-Newman family of solutions, just
as in general relativity. We show that there exist two mechanisms which can
render Kerr black holes unstable when matter is present in the vicinity of the
black hole, as this induces an effective mass for the scalar. The first
mechanism is a tachyonic instability that appears when the effective mass
squared is negative, triggering the development of scalar hair --- a black hole
version of "spontaneous scalarization". The second instability is associated
with superradiance and is present when the effective mass squared is positive
and when the black hole spin exceeds a certain threshold. The second mechanism
is also responsible for a resonant effect in the superradiant scattering of
scalar waves, with amplification factors as large as 10^5 or more.Comment: 11 pages, 3 figures. v2: published versio
Black holes with surrounding matter in scalar-tensor theories
We uncover two mechanisms that can render Kerr black holes unstable in
scalar-tensor gravity, both associated to the presence of matter in the
vicinity of the black hole and the fact that this introduces an effective mass
for the scalar. Our results highlight the importance of understanding the
structure of spacetime in realistic, astrophysical black holes in scalar-tensor
theories.Comment: 5 pages. Published version. arXiv admin note: substantial text
overlap with arXiv:1305.693
Particle ejection during mergers of dark matter halos
Dark matter halos are built from accretion and merging. During merging some
of the dark matter particles may be ejected with velocities higher than the
escape velocity. We use both N-body simulations and single-particle
smooth-field simulations to demonstrate that rapid changes to the mean field
potential are responsible for such ejection, and in particular that dynamical
friction plays no significant role in it. Studying a range of minor mergers, we
find that typically between 5-15% of the particles from the smaller of the two
merging structures are ejected. We also find that the ejected particles
originate essentially from the small halo, and more specifically are particles
in the small halo which pass later through the region in which the merging
occurs.Comment: 18 pages, 12 figures. Accepted for publication in JCA
The foreground transfer function for HI intensity mapping signal reconstruction: MeerKLASS and precision cosmology applications
Blind cleaning methods are currently the preferred strategy for handling
foreground contamination in single-dish HI intensity mapping surveys. Despite
the increasing sophistication of blind techniques, some signal loss will be
inevitable across all scales. Constructing a corrective transfer function using
mock signal injection into the contaminated data has been a practice relied on
for HI intensity mapping experiments. However, assessing whether this approach
is viable for future intensity mapping surveys where precision cosmology is the
aim, remains unexplored. In this work, using simulations, we validate for the
first time the use of a foreground transfer function to reconstruct power
spectra of foreground-cleaned low-redshift intensity maps and look to expose
any limitations. We reveal that even when aggressive foreground cleaning is
required, which causes negative bias on the largest scales, the
power spectrum can be reconstructed using a transfer function to within
sub-percent accuracy. We specifically outline the recipe for constructing an
unbiased transfer function, highlighting the pitfalls if one deviates from this
recipe, and also correctly identify how a transfer function should be applied
in an auto-correlation power spectrum. We validate a method that utilises the
transfer function variance for error estimation in foreground-cleaned power
spectra. Finally, we demonstrate how incorrect fiducial parameter assumptions
(up to bias) in the generation of mocks, used in the construction
of the transfer function, do not significantly bias signal reconstruction or
parameter inference (inducing bias in recovered values).Comment: 25 pages, 20 figures. See Figure 4 for the main demonstration of the
transfer function's performance for reconstructing signal loss from
foreground cleaning. Submitted to MNRAS for publicatio
SKAO HI intensity mapping: blind foreground subtraction challenge
Neutral Hydrogen Intensity Mapping (H I IM) surveys will be a powerful new probe of cosmology. However, strong astrophysical
foregrounds contaminate the signal and their coupling with instrumental systematics further increases the data cleaning
complexity. In this work, we simulate a realistic single-dish HI IM survey of a 5000 deg2 patch in the 950–1400 MHz
range, with both the MID telescope of the SKA Observatory (SKAO) and MeerKAT, its precursor. We include a state-of-the-art
HI simulation and explore different foreground models and instrumental effects such as non-homogeneous thermal noise and
beam side lobes. We perform the first Blind Foreground Subtraction Challenge for HI IM on these synthetic data cubes, aiming
to characterize the performance of available foreground cleaning methods with no prior knowledge of the sky components and
noise level. Nine foreground cleaning pipelines joined the challenge, based on statistical source separation algorithms, blind
polynomial fitting, and an astrophysical-informed parametric fit to foregrounds. We devise metrics to compare the pipeline
performances quantitatively. In general, they can recover the input maps’ two-point statistics within 20 per cent in the range of
scales least affected by the telescope beam. However, spurious artefacts appear in the cleaned maps due to interactions between
the foreground structure and the beam side lobes. We conclude that it is fundamental to develop accurate beam deconvolution
algorithms and test data post-processing steps carefully before cleaning. This study was performed as part of SKAO preparatory
work by the HI IM Focus Group of the SKA Cosmology Science Working Group
Cosmology with the Highly Redshifted 21cm Line
In addition to being a probe of Cosmic Dawn and Epoch of Reionization
astrophysics, the 21cm line at is also a powerful way to constrain
cosmology. Its power derives from several unique capabilities. First, the 21cm
line is sensitive to energy injections into the intergalactic medium at high
redshifts. It also increases the number of measurable modes compared to
existing cosmological probes by orders of magnitude. Many of these modes are on
smaller scales than are accessible via the CMB, and moreover have the advantage
of being firmly in the linear regime (making them easy to model theoretically).
Finally, the 21cm line provides access to redshifts prior to the formation of
luminous objects. Together, these features of 21cm cosmology at provide
multiple pathways toward precise cosmological constraints. These include the
"marginalizing out" of astrophysical effects, the utilization of redshift space
distortions, the breaking of CMB degeneracies, the identification of signatures
of relative velocities between baryons and dark matter, and the discovery of
unexpected signs of physics beyond the CDM paradigm at high redshifts.Comment: Science white paper submitted to Decadal 2020 surve