This document discusses using Milky Way white dwarfs as detectors for dark matter (DM) in the sub-GeV to multi-TeV mass range. It presents an improved calculation of DM capture rates in white dwarfs that accounts for the low-temperature velocity distribution of ions as the white dwarf approaches crystallization. This yields DM capture rates that are smaller than previous calculations by a factor of a few up to two orders of magnitude, depending on the white dwarf size and astrophysical system. The document also investigates using gamma rays from DM annihilation within white dwarfs in the inner Milky Way as a new search strategy. It models the distribution of white dwarfs in the Galactic center and considers a range of white dwarf properties. Sensit
Black-hole-regulated star formation in massive galaxiesSérgio Sacani
Supermassive black holes, with masses more than a million
times that of the Sun, seem to inhabit the centres of all massive
galaxies1,2
. Cosmologically motivated theories of galaxy formation
require feedback from these supermassive black holes to regulate
star formation3
. In the absence of such feedback, state-of-the-art
numerical simulations fail to reproduce the number density and
properties of massive galaxies in the local Universe4–6. There
is, however, no observational evidence of this strongly coupled
coevolution between supermassive black holes and star formation,
impeding our understanding of baryonic processes within galaxies.
Here we report that the star formation histories of nearby massive
galaxies, as measured from their integrated optical spectra, depend
on the mass of the central supermassive black hole. Our results
indicate that the black-hole mass scales with the gas cooling rate
in the early Universe. The subsequent quenching of star formation
takes place earlier and more efficiently in galaxies that host highermass
central black holes. The observed relation between black-hole
mass and star formation efficiency applies to all generations of
stars formed throughout the life of a galaxy, revealing a continuous
interplay between black-hole activity and baryon cooling.
The document discusses dark matter and provides evidence for its existence from various astronomical observations. It notes that while ordinary matter makes up only about 4% of the universe, dark matter accounts for about 23%. Various properties of dark matter are described, including that it interacts gravitationally but does not emit or absorb light. Possible candidates for dark matter are discussed, including WIMPs (Weakly Interacting Massive Particles), which are favored from both astronomical data and particle physics models. The document outlines how WIMPs could have been thermally produced in the early universe to account for the observed dark matter abundance.
The characterization of_the_gamma_ray_signal_from_the_central_milk_way_a_comp...Sérgio Sacani
This document analyzes the gamma-ray signal from the central Milky Way that is consistent with emission from annihilating dark matter particles. The authors re-examine Fermi data using cuts on an event parameter to improve gamma-ray maps and more easily separate components. They find the GeV excess is robust and well-fit by a 36-51 GeV dark matter particle annihilating to bottom quarks with a cross section of 1-3×10−26 cm3/s. The signal extends over 10 degrees from the Galactic Center and is spherically symmetric, disfavoring explanations from millisecond pulsars or gas interactions.
This document summarizes a study that estimates the dynamical surface mass density between 1.5 and 4 kpc from the Galactic plane using kinematics of thick disk stars. The authors derive an exact analytical expression for the surface density based on assumptions about the stellar population and Galactic potential. Their expression matches expectations of visible mass alone, with no evidence for additional dark matter required. They extrapolate a local dark matter density of 0±1 mM⊙ pc−3, excluding all current spherical dark matter halo models at over 4σ confidence. Only a highly prolate dark matter halo could potentially reconcile the observations with models, but this is unlikely according to ΛCDM.
EMU M.Sc. Thesis Presentation
Thesis Title: "Dark Matter; Modification of f(R) or WIMPS Miracle"
Student: Ali Övgün
Supervisor: Prof. Dr. Mustafa Halilsoy
Dark Matter Annihilation inside Large-Volume Neutrino DetectorsSérgio Sacani
New particles in theories beyond the standard model can manifest as stable relics that interact strongly with visible matter and make up a small fraction of the total dark matter abundance. Such particles represent an interesting physics target since they can evade existing bounds from direct detection due to their rapid thermalization in high-density environments. In this work we point out that their annihilation to visible matter inside large-volume neutrino telescopes can provide a new way to constrain or discover such particles. The signal is the most pronounced for relic masses in the GeV range, and can be efficiently constrained by existing Super-Kamiokande searches for dinucleon annihilation. We also provide an explicit realization of this scenario in the form of secluded dark matter coupled to a dark photon, and we show that the present method implies novel and stringent bounds on the model that are complementary to direct constraints from beam dumps, colliders, and direct detection experiments.
1) The observable universe has a mass of approximately 24x10^53 kg.
2) Normal matter, including atoms, stars and galaxies, constitute only about 4% of the observable universe. The rest is dark matter (27%) and dark energy (71%).
3) Dark matter interacts gravitationally but is unseen, and helps hold galaxies together. Dark energy is causing the accelerating expansion of the universe against the force of gravity.
A spectroscopic sample_of_massive_galaxiesSérgio Sacani
This document describes a study of 16 massive galaxies at z ~ 2 selected from the 3D-HST spectroscopic survey based on the detection of a strong 4000 Angstrom break in their spectra. Spectroscopy and imaging from HST/WFC3 are used to determine accurate redshifts, stellar population properties, and structural parameters. The sample significantly increases the number of spectroscopically confirmed evolved galaxies at z ~ 2 with robust size measurements. The analysis populates the mass-size relation and finds it is consistent with local relations but with smaller sizes by a factor of 2-3. A model is presented where the observed size evolution is explained by quenching of increasingly larger star-forming galaxies at a rate set by
Black-hole-regulated star formation in massive galaxiesSérgio Sacani
Supermassive black holes, with masses more than a million
times that of the Sun, seem to inhabit the centres of all massive
galaxies1,2
. Cosmologically motivated theories of galaxy formation
require feedback from these supermassive black holes to regulate
star formation3
. In the absence of such feedback, state-of-the-art
numerical simulations fail to reproduce the number density and
properties of massive galaxies in the local Universe4–6. There
is, however, no observational evidence of this strongly coupled
coevolution between supermassive black holes and star formation,
impeding our understanding of baryonic processes within galaxies.
Here we report that the star formation histories of nearby massive
galaxies, as measured from their integrated optical spectra, depend
on the mass of the central supermassive black hole. Our results
indicate that the black-hole mass scales with the gas cooling rate
in the early Universe. The subsequent quenching of star formation
takes place earlier and more efficiently in galaxies that host highermass
central black holes. The observed relation between black-hole
mass and star formation efficiency applies to all generations of
stars formed throughout the life of a galaxy, revealing a continuous
interplay between black-hole activity and baryon cooling.
The document discusses dark matter and provides evidence for its existence from various astronomical observations. It notes that while ordinary matter makes up only about 4% of the universe, dark matter accounts for about 23%. Various properties of dark matter are described, including that it interacts gravitationally but does not emit or absorb light. Possible candidates for dark matter are discussed, including WIMPs (Weakly Interacting Massive Particles), which are favored from both astronomical data and particle physics models. The document outlines how WIMPs could have been thermally produced in the early universe to account for the observed dark matter abundance.
The characterization of_the_gamma_ray_signal_from_the_central_milk_way_a_comp...Sérgio Sacani
This document analyzes the gamma-ray signal from the central Milky Way that is consistent with emission from annihilating dark matter particles. The authors re-examine Fermi data using cuts on an event parameter to improve gamma-ray maps and more easily separate components. They find the GeV excess is robust and well-fit by a 36-51 GeV dark matter particle annihilating to bottom quarks with a cross section of 1-3×10−26 cm3/s. The signal extends over 10 degrees from the Galactic Center and is spherically symmetric, disfavoring explanations from millisecond pulsars or gas interactions.
This document summarizes a study that estimates the dynamical surface mass density between 1.5 and 4 kpc from the Galactic plane using kinematics of thick disk stars. The authors derive an exact analytical expression for the surface density based on assumptions about the stellar population and Galactic potential. Their expression matches expectations of visible mass alone, with no evidence for additional dark matter required. They extrapolate a local dark matter density of 0±1 mM⊙ pc−3, excluding all current spherical dark matter halo models at over 4σ confidence. Only a highly prolate dark matter halo could potentially reconcile the observations with models, but this is unlikely according to ΛCDM.
EMU M.Sc. Thesis Presentation
Thesis Title: "Dark Matter; Modification of f(R) or WIMPS Miracle"
Student: Ali Övgün
Supervisor: Prof. Dr. Mustafa Halilsoy
Dark Matter Annihilation inside Large-Volume Neutrino DetectorsSérgio Sacani
New particles in theories beyond the standard model can manifest as stable relics that interact strongly with visible matter and make up a small fraction of the total dark matter abundance. Such particles represent an interesting physics target since they can evade existing bounds from direct detection due to their rapid thermalization in high-density environments. In this work we point out that their annihilation to visible matter inside large-volume neutrino telescopes can provide a new way to constrain or discover such particles. The signal is the most pronounced for relic masses in the GeV range, and can be efficiently constrained by existing Super-Kamiokande searches for dinucleon annihilation. We also provide an explicit realization of this scenario in the form of secluded dark matter coupled to a dark photon, and we show that the present method implies novel and stringent bounds on the model that are complementary to direct constraints from beam dumps, colliders, and direct detection experiments.
1) The observable universe has a mass of approximately 24x10^53 kg.
2) Normal matter, including atoms, stars and galaxies, constitute only about 4% of the observable universe. The rest is dark matter (27%) and dark energy (71%).
3) Dark matter interacts gravitationally but is unseen, and helps hold galaxies together. Dark energy is causing the accelerating expansion of the universe against the force of gravity.
A spectroscopic sample_of_massive_galaxiesSérgio Sacani
This document describes a study of 16 massive galaxies at z ~ 2 selected from the 3D-HST spectroscopic survey based on the detection of a strong 4000 Angstrom break in their spectra. Spectroscopy and imaging from HST/WFC3 are used to determine accurate redshifts, stellar population properties, and structural parameters. The sample significantly increases the number of spectroscopically confirmed evolved galaxies at z ~ 2 with robust size measurements. The analysis populates the mass-size relation and finds it is consistent with local relations but with smaller sizes by a factor of 2-3. A model is presented where the observed size evolution is explained by quenching of increasingly larger star-forming galaxies at a rate set by
A population of faint low surface brightness galaxies in the Perseus cluster ...Sérgio Sacani
We present the detection of 89 low surface brightness (LSB), and thus low stellar
density galaxy candidates in the Perseus cluster core, of the kind named ‘ultra-diffuse
galaxies’, with mean effective V-band surface brightnesses 24.8–27.1 mag arcsec−2
, total
V-band magnitudes −11.8 to −15.5 mag, and half-light radii 0.7–4.1 kpc. The candidates
have been identified in a deep mosaic covering 0.3 deg2
, based on wide-field
imaging data obtained with the William Herschel Telescope. We find that the LSB
galaxy population is depleted in the cluster centre and only very few LSB candidates
have half-light radii larger than 3 kpc. This appears consistent with an estimate of
their tidal radius, which does not reach beyond the stellar extent even if we assume
a high dark matter content (M/L = 100). In fact, three of our candidates seem to
be associated with tidal streams, which points to their current disruption. Given that
published data on faint LSB candidates in the Coma cluster – with its comparable central
density to Perseus – show the same dearth of large objects in the core region, we
conclude that these cannot survive the strong tides in the centres of massive clusters.
An almost dark galaxy with the mass of the Small Magellanic CloudSérgio Sacani
This document describes the discovery and characterization of an almost dark galaxy named Nube. Deep imaging with GTC revealed Nube has an extremely low surface brightness of 26.7 mag/arcsec^2 and a stellar mass of 4x10^8 solar masses. Follow-up observations with GBT detected HI emission from Nube, suggesting it is located 107 Mpc away. At this distance, Nube has a large half-mass radius of 6.9 kpc and low effective stellar density, making it the most extended low-surface brightness galaxy found. Its properties are difficult to reproduce in CDM simulations but are consistent with an ultra-light dark matter particle model.
Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroid...Sérgio Sacani
The Milky Way dwarf spheroidal satellite galaxies (dSphs) are particularly intriguing targets to search for gamma rays from Weakly Interacting Massive Particle (WIMP) dark matter (DM) annihilation or decay. They are nearby, DM-dominated, and lack significant emission from standard astrophysical processes. Previous studies using the Fermi-Large Area Telescope (LAT) of DMinduced emission from dSphs have provided the most robust and stringent constraints on the DM annihilation cross section and mass. We report here an analysis of the Milky Way dSphs using over 14 years of LAT data along with an updated census of dSphs and J-factor estimates. While no individual dSphs are significantly detected, we do find slight excesses with respect to background at the ≳ 2σ local significance level in both tested annihilation channels (b¯ b, τ+τ−) for seven of the dSphs. We do not find a significant DM signal from the combined likelihood analysis of the dSphs (sglobal ∼ 0.5σ), yet a marginal local excess relative to background at a 2−3σ level is observed at a DMmass of Mχ = 150−230 GeV (Mχ = 30−50 GeV) for DM annihilation into b¯ b (τ+τ−). Given the lack of a significant detection, we place updated constraints on the b¯ b and τ+τ− annihilation channels that are generally consistent with previous recent results. As in past studies, tension is found with some WIMP DM interpretations of the Galactic Center Excess (GCE), though the limits are consistent with other interpretations given the uncertainties of the Galactic DM density profile and GCE systematics. Based on conservative assumptions of improved sensitivity with increased Fermi-LAT exposure time and moderate increases in the sample of Milky Way dSphs, we project that the local ∼ 2σ signal, if real, could approach the ∼ 4σ local confidence level with additional ∼10 years of observation.
Multi wavelenth observations and surveys of galaxy clustersJoana Santos
This document provides an overview of galaxy clusters, focusing on their baryonic components (intracluster medium and galaxies) and how they relate to the cluster's physical properties like mass. It discusses that galaxy clusters form hierarchically through gravitational collapse. The intracluster medium, which makes up most of the baryonic mass, emits X-rays and has been heated to temperatures of millions of degrees. The document reviews properties of the intracluster medium like density, temperature, metallicity, and how they can be measured from X-ray spectra. It also discusses upcoming surveys that will advance the study of galaxy clusters.
On some structural_features_of_the_metagalaxySérgio Sacani
Progress in a group of investigations designed
to discover some of the structural details in individual galaxies and in the
Metagalaxy is reported in the following pages.
(a) The first section is concerned with the distribution of cluster-type
Cepheids in high galactic latitude. To the 169 already known in latitudes,
greater than or equal to ± 20o
, the systematic variable star programme carried
on at Harvard has added 312, mostly fainter than magnitude 13-0. With
allowance for absorption and for uncertainties yet remaining in the mean
absolute magnitude of these stars, the thickness of the Milky Way, so far
as this type of star is concerned, is not less than twenty-five kiloparsecs ;
he extent of the Milky Way in its own plane, by the same criterion, is more
than thirty kiloparsecs, perhaps much more.
(b) The extent of the Milky Way in the anti-centre quadrant is considered
on the basis of classical and cluster-type Cepheids ; provisionally
it is found that the galactic system reaches to a distance of at least ten
kiloparsecs in longitude 150o
.
(r) More than six hundred new variables have been found in the Large
Magellanic Cloud and measured for position, ranges and median magnitudes ;
the frequency of periods is not unlike that for the classical Cepheids in the
galactic system ; the light curves also are comparable in all details. The
Magellanic Cepheids, like the galactic classical Cepheids, are concentrated
in regions of high star-density.
(d) Further study of the period-luminosity relation in the Large Magellanic
Cloud permits its revision and strengthening for the Cepheids of
highest absolute magnitude. An observed deviation from the relation
that had previously been found for the Small Cloud is probably to be
attributed to scale error in the magnitude system. No seriously disturbing
This document discusses the nature of dark matter, whether it is warm or cold. It provides evidence from simulations and observations that both support and cast doubt on the standard cold dark matter (CDM) model. On small scales, CDM simulations predict more substructure than observed, and cuspy dark matter density profiles rather than cored profiles as suggested by some observations of dwarf galaxies. Warm dark matter is proposed as an alternative to address these issues, but current constraints from Lyman-alpha forests limit the mass of warm dark matter particles. Future weak lensing surveys like Euclid may help constrain the nature of dark matter.
The distribution and_annihilation_of_dark_matter_around_black_holesSérgio Sacani
Uma nova simulação computacional feita pela NASA mostra que as partículas da matéria escura colidindo na extrema gravidade de um buraco negro pode produzir uma luz de raios-gamma forte e potencialmente observável. Detectando essa emissão forneceria aos astrônomos com uma nova ferramenta para entender tanto os buracos negros como a natureza da matéria escura, uma elusiva substância responsável pela maior parte da massa do universo que nem reflete, absorve ou emite luz.
Galaxy dynamics and the mass density of the universeSérgio Sacani
Dynamical evidence accumulated over the
past 20 years has convinced astronomers that luminous matter
in a spiral galaxy constitutes no more than 10% of the mass of
a galaxy. An additional 90% is inferred by its gravitational
effect on luminous material. Here I review recent observations
concerning the distribution of luminous and nonluminous
matter in the Milky Way, in galaxies, and in galaxy clusters.
Observations of neutral hydrogen disks, some extending in
radius several times the optical disk, confirm that a massive
dark halo is a major component of virtually every spiral. A
recent surprise has been the discovery that stellar and gas
motions in ellipticals are enormously complex. To date, only for
a few spheroidal galaxies do the velocities extend far enough to
probe the outer mass distribution. But the diverse kinematics
of inner cores, peripheral to deducing the overall mass distribution,
offer additional evidence that ellipticals have acquired
gas-rich systems after initial formation. Dynamical results are
consistent with a low-density universe, in which the required
dark matter could be baryonic. On smallest scales of galaxies
[10 kiloparsec (kpc); H. = 50 kmsec'lmegaparsec'11 the
luminous matter constitutes only 1% of the closure density. On
scales greater than binary galaxies (i.e., .100 kpc) all systems
indicate a density -10% of the closure density, a density
consistent with the low baryon density in the universe. If
large-scale motions in the universe require a higher mass
density, these motions would constitute the first dynamical
evidence for nonbaryonic matter in a universe of higher
density.
This document is a dissertation by Joakim Carlsen submitted in 2014/2015 for a Bsc(Honours) in Applied Physics. It investigates detecting massive galaxies at high redshift (z > 4) using photometric data from the Dark Energy Survey (DES). The dissertation aims to identify massive galaxy candidates at z > 4 based on their colors and fit their spectral energy distributions using photometric redshift modeling software. Several high redshift massive galaxy candidates were identified and their properties were analyzed, with the most promising candidates to be proposed for follow-up spectroscopy to confirm their redshifts.
This document presents evidence that massive galaxies at redshift 2.2 (~3 billion years after the Big Bang) undergo an "inside-out quenching" process, where star formation is quenched first in the inner regions and later in the outer disks. High-resolution observations of 22 star-forming galaxies show that the most massive galaxies already have dense bulges similar to local spheroids, while still actively forming stars in their outer disks. The data suggests star formation is suppressed from the inside out on timescales of less than 1 Gyr in the centers and up to a few Gyr in the outer disks, as an "inside-out quenching wave" propagates through the galaxies. This provides insights into how
Too much pasta_for_pulsars_to_spin_downSérgio Sacani
This document summarizes a study investigating why no isolated X-ray pulsars have been observed with spin periods longer than 12 seconds. The researchers suggest this is due to a highly resistive layer in the inner crust of neutron stars, which is expected to be in a state called "nuclear pasta". Nuclear pasta has an irregular structure that increases electrical resistivity, limiting the spin-down of pulsars. Modeling the long-term magnetic field evolution incorporating a resistive nuclear pasta layer successfully reproduced the observed 12 second period limit. The results provide the first potential observational evidence for the existence of nuclear pasta in neutron star crusts.
The current ability to test theories of gravity with black hole shadowsSérgio Sacani
Our Galactic Centre, Sagittarius A*, is believed to harbour a
supermassive black hole, as suggested by observations tracking
individual orbiting stars1,2
. Upcoming submillimetre verylong
baseline interferometry images of Sagittarius A* carried
out by the Event Horizon Telescope collaboration (EHTC)3,4
are expected to provide critical evidence for the existence of
this supermassive black hole5,6. We assess our present ability
to use EHTC images to determine whether they correspond
to a Kerr black hole as predicted by Einstein’s theory
of general relativity or to a black hole in alternative theories
of gravity. To this end, we perform general-relativistic magnetohydrodynamical
simulations and use general-relativistic
radiative-transfer calculations to generate synthetic shadow
images of a magnetized accretion flow onto a Kerr black hole.
In addition, we perform these simulations and calculations for
a dilaton black hole, which we take as a representative solution
of an alternative theory of gravity. Adopting the very-long
baseline interferometry configuration from the 2017 EHTC
campaign, we find that it could be extremely difficult to distinguish
between black holes from different theories of gravity,
thus highlighting that great caution is needed when interpreting
black hole images as tests of general relativity.
This document is a dissertation investigating recent findings from direct dark matter detection experiments, specifically performing an analysis of XENON100's 100 Live-Days data. It begins with an introduction to the evidence and theory of dark matter, possible candidates, and detection methods. It then discusses the theory of direct detection and relevant astrophysical parameters. The document reviews the principles of xenon-based time projection chambers and backgrounds. It discusses various direct detection experiments and their claims of discovery. Through Bayesian statistics, it sets an exclusion limit based on XENON100's parameters and compares to their results. Finally, it considers an alternative velocity distribution to investigate uncertainties for WIMP masses below 30GeV.
This document summarizes research on determining temperatures, luminosities, and masses of the coldest known brown dwarfs. The key findings are:
1) Precise distances were measured for a sample of late-T and Y dwarfs using Spitzer Space Telescope astrometry, allowing accurate calculation of absolute fluxes, luminosities, and temperatures.
2) Y0 dwarfs were found to have temperatures of 400-450 K, significantly warmer than previous estimates, and masses of 5-20 times Jupiter's mass.
3) While having similar temperatures, Y dwarfs showed diverse spectral energy distributions, suggesting temperature alone does not determine spectra. Physical properties like gravity, clouds and chemistry also influence spectra.
Using the Milky Way satellites to study interactions between cold dark matter...GOASA
The document discusses using simulations of cold dark matter (CDM) interacting with radiation (photons or neutrinos) to study its impact on the number of satellite galaxies around the Milky Way. It finds that including such interactions leads to a dramatic reduction in satellite galaxies that could help alleviate tensions between the CDM model and observations. The methodology allows stronger constraints on dark matter interactions than from cosmic microwave background data alone. Simulations of CDM interacting with photons show a reduced number of subhalos around Milky Way-sized halos for interaction cross sections allowed by CMB data, demonstrating this physics may be important for small-scale structure formation predictions.
1) The document provides a summary of a course on high-energy astrophysics that the author took. It discusses various topics covered in the course including accretion disks, pulsars, black holes, supernovae, and more.
2) The author argues that high-energy astrophysics is important for understanding the universe and requests that the provost offer a similar course at their university.
3) Key concepts in high-energy astrophysics discussed include accretion and its relation to luminosity, binary star systems, properties of neutron stars and black holes, and x-ray emissions from astrophysical phenomena like supernovae.
1. The document estimates the maximum intensity of dark matter glow based on Dr. Hewett's Time Symmetric Cosmology theory, which predicts dark matter is a boson resulting from Hawking evaporation of primordial black holes.
2. Using classical approximations, the author estimates the total photon intensity of the Andromeda galaxy's dark matter halo would be 4.67x1024, far greater than its visible light intensity of 3.19x109.
3. However, the author acknowledges the model's assumptions and approximations likely overestimate the intensity by many orders of magnitude, and more rigorous modeling is needed to test if dark matter glow could be detectable.
The colision between_the_milky_way_and_andromedaSérgio Sacani
The document summarizes a simulation of the future collision between the Milky Way and Andromeda galaxies. It finds that given current observational constraints on their distance, velocity, and masses:
1) The Milky Way and Andromeda are likely to collide in a few billion years, within the lifetime of the Sun.
2) During the interaction, there is a chance the Sun could be pulled into an extended tidal tail between the galaxies.
3) Eventually, after the merger is complete, the Sun would most likely be scattered to the outer halo of the merged galaxy at a distance over 30 kpc.
A density cusp of quiescent X-ray binaries in the central parsec of the GalaxySérgio Sacani
The existence of a ‘density cusp’1,2—a localized increase in
number—of stellar-mass black holes near a supermassive black
hole is a fundamental prediction of galactic stellar dynamics3
. The
best place to detect such a cusp is in the Galactic Centre, where
the nearest supermassive black hole, Sagittarius A*, resides. As
many as 20,000 black holes are predicted to settle into the central
parsec of the Galaxy as a result of dynamical friction3–5; however,
so far no density cusp of black holes has been detected. Low-mass
X-ray binary systems that contain a stellar-mass black hole are
natural tracers of isolated black holes. Here we report observations
of a dozen quiescent X-ray binaries in a density cusp within one
parsec of Sagittarius A*. The lower-energy emission spectra that
we observed in these binaries is distinct from the higher-energy
spectra associated with the population of accreting white dwarfs that
dominates the central eight parsecs of the Galaxy6
. The properties
of these X-ray binaries, in particular their spatial distribution and
luminosity function, suggest the existence of hundreds of binary
systems in the central parsec of the Galaxy and many more isolated
black holes. We cannot rule out a contribution to the observed
emission from a population (of up to about one-half the number of
X-ray binaries) of rotationally powered, millisecond pulsars. The
spatial distribution of the binary systems is a relic of their formation
history, either in the stellar disk around Sagittarius A* (ref. 7) or
through in-fall from globular clusters, and constrains the number
density of sources in the modelling of gravitational waves from
massive stellar remnants8,9
, such as neutron stars and black holes.
Compositions of iron-meteorite parent bodies constrainthe structure of the pr...Sérgio Sacani
Magmatic iron-meteorite parent bodies are the earliest planetesimals in the Solar System,and they preserve information about conditions and planet-forming processes in thesolar nebula. In this study, we include comprehensive elemental compositions andfractional-crystallization modeling for iron meteorites from the cores of five differenti-ated asteroids from the inner Solar System. Together with previous results of metalliccores from the outer Solar System, we conclude that asteroidal cores from the outerSolar System have smaller sizes, elevated siderophile-element abundances, and simplercrystallization processes than those from the inner Solar System. These differences arerelated to the formation locations of the parent asteroids because the solar protoplane-tary disk varied in redox conditions, elemental distributions, and dynamics at differentheliocentric distances. Using highly siderophile-element data from iron meteorites, wereconstruct the distribution of calcium-aluminum-rich inclusions (CAIs) across theprotoplanetary disk within the first million years of Solar-System history. CAIs, the firstsolids to condense in the Solar System, formed close to the Sun. They were, however,concentrated within the outer disk and depleted within the inner disk. Future modelsof the structure and evolution of the protoplanetary disk should account for this dis-tribution pattern of CAIs.
Signatures of wave erosion in Titan’s coastsSérgio Sacani
The shorelines of Titan’s hydrocarbon seas trace flooded erosional landforms such as river valleys; however, it isunclear whether coastal erosion has subsequently altered these shorelines. Spacecraft observations and theo-retical models suggest that wind may cause waves to form on Titan’s seas, potentially driving coastal erosion,but the observational evidence of waves is indirect, and the processes affecting shoreline evolution on Titanremain unknown. No widely accepted framework exists for using shoreline morphology to quantitatively dis-cern coastal erosion mechanisms, even on Earth, where the dominant mechanisms are known. We combinelandscape evolution models with measurements of shoreline shape on Earth to characterize how differentcoastal erosion mechanisms affect shoreline morphology. Applying this framework to Titan, we find that theshorelines of Titan’s seas are most consistent with flooded landscapes that subsequently have been eroded bywaves, rather than a uniform erosional process or no coastal erosion, particularly if wave growth saturates atfetch lengths of tens of kilometers.
More Related Content
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A population of faint low surface brightness galaxies in the Perseus cluster ...Sérgio Sacani
We present the detection of 89 low surface brightness (LSB), and thus low stellar
density galaxy candidates in the Perseus cluster core, of the kind named ‘ultra-diffuse
galaxies’, with mean effective V-band surface brightnesses 24.8–27.1 mag arcsec−2
, total
V-band magnitudes −11.8 to −15.5 mag, and half-light radii 0.7–4.1 kpc. The candidates
have been identified in a deep mosaic covering 0.3 deg2
, based on wide-field
imaging data obtained with the William Herschel Telescope. We find that the LSB
galaxy population is depleted in the cluster centre and only very few LSB candidates
have half-light radii larger than 3 kpc. This appears consistent with an estimate of
their tidal radius, which does not reach beyond the stellar extent even if we assume
a high dark matter content (M/L = 100). In fact, three of our candidates seem to
be associated with tidal streams, which points to their current disruption. Given that
published data on faint LSB candidates in the Coma cluster – with its comparable central
density to Perseus – show the same dearth of large objects in the core region, we
conclude that these cannot survive the strong tides in the centres of massive clusters.
An almost dark galaxy with the mass of the Small Magellanic CloudSérgio Sacani
This document describes the discovery and characterization of an almost dark galaxy named Nube. Deep imaging with GTC revealed Nube has an extremely low surface brightness of 26.7 mag/arcsec^2 and a stellar mass of 4x10^8 solar masses. Follow-up observations with GBT detected HI emission from Nube, suggesting it is located 107 Mpc away. At this distance, Nube has a large half-mass radius of 6.9 kpc and low effective stellar density, making it the most extended low-surface brightness galaxy found. Its properties are difficult to reproduce in CDM simulations but are consistent with an ultra-light dark matter particle model.
Legacy Analysis of Dark Matter Annihilation from the Milky Way Dwarf Spheroid...Sérgio Sacani
The Milky Way dwarf spheroidal satellite galaxies (dSphs) are particularly intriguing targets to search for gamma rays from Weakly Interacting Massive Particle (WIMP) dark matter (DM) annihilation or decay. They are nearby, DM-dominated, and lack significant emission from standard astrophysical processes. Previous studies using the Fermi-Large Area Telescope (LAT) of DMinduced emission from dSphs have provided the most robust and stringent constraints on the DM annihilation cross section and mass. We report here an analysis of the Milky Way dSphs using over 14 years of LAT data along with an updated census of dSphs and J-factor estimates. While no individual dSphs are significantly detected, we do find slight excesses with respect to background at the ≳ 2σ local significance level in both tested annihilation channels (b¯ b, τ+τ−) for seven of the dSphs. We do not find a significant DM signal from the combined likelihood analysis of the dSphs (sglobal ∼ 0.5σ), yet a marginal local excess relative to background at a 2−3σ level is observed at a DMmass of Mχ = 150−230 GeV (Mχ = 30−50 GeV) for DM annihilation into b¯ b (τ+τ−). Given the lack of a significant detection, we place updated constraints on the b¯ b and τ+τ− annihilation channels that are generally consistent with previous recent results. As in past studies, tension is found with some WIMP DM interpretations of the Galactic Center Excess (GCE), though the limits are consistent with other interpretations given the uncertainties of the Galactic DM density profile and GCE systematics. Based on conservative assumptions of improved sensitivity with increased Fermi-LAT exposure time and moderate increases in the sample of Milky Way dSphs, we project that the local ∼ 2σ signal, if real, could approach the ∼ 4σ local confidence level with additional ∼10 years of observation.
Multi wavelenth observations and surveys of galaxy clustersJoana Santos
This document provides an overview of galaxy clusters, focusing on their baryonic components (intracluster medium and galaxies) and how they relate to the cluster's physical properties like mass. It discusses that galaxy clusters form hierarchically through gravitational collapse. The intracluster medium, which makes up most of the baryonic mass, emits X-rays and has been heated to temperatures of millions of degrees. The document reviews properties of the intracluster medium like density, temperature, metallicity, and how they can be measured from X-ray spectra. It also discusses upcoming surveys that will advance the study of galaxy clusters.
On some structural_features_of_the_metagalaxySérgio Sacani
Progress in a group of investigations designed
to discover some of the structural details in individual galaxies and in the
Metagalaxy is reported in the following pages.
(a) The first section is concerned with the distribution of cluster-type
Cepheids in high galactic latitude. To the 169 already known in latitudes,
greater than or equal to ± 20o
, the systematic variable star programme carried
on at Harvard has added 312, mostly fainter than magnitude 13-0. With
allowance for absorption and for uncertainties yet remaining in the mean
absolute magnitude of these stars, the thickness of the Milky Way, so far
as this type of star is concerned, is not less than twenty-five kiloparsecs ;
he extent of the Milky Way in its own plane, by the same criterion, is more
than thirty kiloparsecs, perhaps much more.
(b) The extent of the Milky Way in the anti-centre quadrant is considered
on the basis of classical and cluster-type Cepheids ; provisionally
it is found that the galactic system reaches to a distance of at least ten
kiloparsecs in longitude 150o
.
(r) More than six hundred new variables have been found in the Large
Magellanic Cloud and measured for position, ranges and median magnitudes ;
the frequency of periods is not unlike that for the classical Cepheids in the
galactic system ; the light curves also are comparable in all details. The
Magellanic Cepheids, like the galactic classical Cepheids, are concentrated
in regions of high star-density.
(d) Further study of the period-luminosity relation in the Large Magellanic
Cloud permits its revision and strengthening for the Cepheids of
highest absolute magnitude. An observed deviation from the relation
that had previously been found for the Small Cloud is probably to be
attributed to scale error in the magnitude system. No seriously disturbing
This document discusses the nature of dark matter, whether it is warm or cold. It provides evidence from simulations and observations that both support and cast doubt on the standard cold dark matter (CDM) model. On small scales, CDM simulations predict more substructure than observed, and cuspy dark matter density profiles rather than cored profiles as suggested by some observations of dwarf galaxies. Warm dark matter is proposed as an alternative to address these issues, but current constraints from Lyman-alpha forests limit the mass of warm dark matter particles. Future weak lensing surveys like Euclid may help constrain the nature of dark matter.
The distribution and_annihilation_of_dark_matter_around_black_holesSérgio Sacani
Uma nova simulação computacional feita pela NASA mostra que as partículas da matéria escura colidindo na extrema gravidade de um buraco negro pode produzir uma luz de raios-gamma forte e potencialmente observável. Detectando essa emissão forneceria aos astrônomos com uma nova ferramenta para entender tanto os buracos negros como a natureza da matéria escura, uma elusiva substância responsável pela maior parte da massa do universo que nem reflete, absorve ou emite luz.
Galaxy dynamics and the mass density of the universeSérgio Sacani
Dynamical evidence accumulated over the
past 20 years has convinced astronomers that luminous matter
in a spiral galaxy constitutes no more than 10% of the mass of
a galaxy. An additional 90% is inferred by its gravitational
effect on luminous material. Here I review recent observations
concerning the distribution of luminous and nonluminous
matter in the Milky Way, in galaxies, and in galaxy clusters.
Observations of neutral hydrogen disks, some extending in
radius several times the optical disk, confirm that a massive
dark halo is a major component of virtually every spiral. A
recent surprise has been the discovery that stellar and gas
motions in ellipticals are enormously complex. To date, only for
a few spheroidal galaxies do the velocities extend far enough to
probe the outer mass distribution. But the diverse kinematics
of inner cores, peripheral to deducing the overall mass distribution,
offer additional evidence that ellipticals have acquired
gas-rich systems after initial formation. Dynamical results are
consistent with a low-density universe, in which the required
dark matter could be baryonic. On smallest scales of galaxies
[10 kiloparsec (kpc); H. = 50 kmsec'lmegaparsec'11 the
luminous matter constitutes only 1% of the closure density. On
scales greater than binary galaxies (i.e., .100 kpc) all systems
indicate a density -10% of the closure density, a density
consistent with the low baryon density in the universe. If
large-scale motions in the universe require a higher mass
density, these motions would constitute the first dynamical
evidence for nonbaryonic matter in a universe of higher
density.
This document is a dissertation by Joakim Carlsen submitted in 2014/2015 for a Bsc(Honours) in Applied Physics. It investigates detecting massive galaxies at high redshift (z > 4) using photometric data from the Dark Energy Survey (DES). The dissertation aims to identify massive galaxy candidates at z > 4 based on their colors and fit their spectral energy distributions using photometric redshift modeling software. Several high redshift massive galaxy candidates were identified and their properties were analyzed, with the most promising candidates to be proposed for follow-up spectroscopy to confirm their redshifts.
This document presents evidence that massive galaxies at redshift 2.2 (~3 billion years after the Big Bang) undergo an "inside-out quenching" process, where star formation is quenched first in the inner regions and later in the outer disks. High-resolution observations of 22 star-forming galaxies show that the most massive galaxies already have dense bulges similar to local spheroids, while still actively forming stars in their outer disks. The data suggests star formation is suppressed from the inside out on timescales of less than 1 Gyr in the centers and up to a few Gyr in the outer disks, as an "inside-out quenching wave" propagates through the galaxies. This provides insights into how
Too much pasta_for_pulsars_to_spin_downSérgio Sacani
This document summarizes a study investigating why no isolated X-ray pulsars have been observed with spin periods longer than 12 seconds. The researchers suggest this is due to a highly resistive layer in the inner crust of neutron stars, which is expected to be in a state called "nuclear pasta". Nuclear pasta has an irregular structure that increases electrical resistivity, limiting the spin-down of pulsars. Modeling the long-term magnetic field evolution incorporating a resistive nuclear pasta layer successfully reproduced the observed 12 second period limit. The results provide the first potential observational evidence for the existence of nuclear pasta in neutron star crusts.
The current ability to test theories of gravity with black hole shadowsSérgio Sacani
Our Galactic Centre, Sagittarius A*, is believed to harbour a
supermassive black hole, as suggested by observations tracking
individual orbiting stars1,2
. Upcoming submillimetre verylong
baseline interferometry images of Sagittarius A* carried
out by the Event Horizon Telescope collaboration (EHTC)3,4
are expected to provide critical evidence for the existence of
this supermassive black hole5,6. We assess our present ability
to use EHTC images to determine whether they correspond
to a Kerr black hole as predicted by Einstein’s theory
of general relativity or to a black hole in alternative theories
of gravity. To this end, we perform general-relativistic magnetohydrodynamical
simulations and use general-relativistic
radiative-transfer calculations to generate synthetic shadow
images of a magnetized accretion flow onto a Kerr black hole.
In addition, we perform these simulations and calculations for
a dilaton black hole, which we take as a representative solution
of an alternative theory of gravity. Adopting the very-long
baseline interferometry configuration from the 2017 EHTC
campaign, we find that it could be extremely difficult to distinguish
between black holes from different theories of gravity,
thus highlighting that great caution is needed when interpreting
black hole images as tests of general relativity.
This document is a dissertation investigating recent findings from direct dark matter detection experiments, specifically performing an analysis of XENON100's 100 Live-Days data. It begins with an introduction to the evidence and theory of dark matter, possible candidates, and detection methods. It then discusses the theory of direct detection and relevant astrophysical parameters. The document reviews the principles of xenon-based time projection chambers and backgrounds. It discusses various direct detection experiments and their claims of discovery. Through Bayesian statistics, it sets an exclusion limit based on XENON100's parameters and compares to their results. Finally, it considers an alternative velocity distribution to investigate uncertainties for WIMP masses below 30GeV.
This document summarizes research on determining temperatures, luminosities, and masses of the coldest known brown dwarfs. The key findings are:
1) Precise distances were measured for a sample of late-T and Y dwarfs using Spitzer Space Telescope astrometry, allowing accurate calculation of absolute fluxes, luminosities, and temperatures.
2) Y0 dwarfs were found to have temperatures of 400-450 K, significantly warmer than previous estimates, and masses of 5-20 times Jupiter's mass.
3) While having similar temperatures, Y dwarfs showed diverse spectral energy distributions, suggesting temperature alone does not determine spectra. Physical properties like gravity, clouds and chemistry also influence spectra.
Using the Milky Way satellites to study interactions between cold dark matter...GOASA
The document discusses using simulations of cold dark matter (CDM) interacting with radiation (photons or neutrinos) to study its impact on the number of satellite galaxies around the Milky Way. It finds that including such interactions leads to a dramatic reduction in satellite galaxies that could help alleviate tensions between the CDM model and observations. The methodology allows stronger constraints on dark matter interactions than from cosmic microwave background data alone. Simulations of CDM interacting with photons show a reduced number of subhalos around Milky Way-sized halos for interaction cross sections allowed by CMB data, demonstrating this physics may be important for small-scale structure formation predictions.
1) The document provides a summary of a course on high-energy astrophysics that the author took. It discusses various topics covered in the course including accretion disks, pulsars, black holes, supernovae, and more.
2) The author argues that high-energy astrophysics is important for understanding the universe and requests that the provost offer a similar course at their university.
3) Key concepts in high-energy astrophysics discussed include accretion and its relation to luminosity, binary star systems, properties of neutron stars and black holes, and x-ray emissions from astrophysical phenomena like supernovae.
1. The document estimates the maximum intensity of dark matter glow based on Dr. Hewett's Time Symmetric Cosmology theory, which predicts dark matter is a boson resulting from Hawking evaporation of primordial black holes.
2. Using classical approximations, the author estimates the total photon intensity of the Andromeda galaxy's dark matter halo would be 4.67x1024, far greater than its visible light intensity of 3.19x109.
3. However, the author acknowledges the model's assumptions and approximations likely overestimate the intensity by many orders of magnitude, and more rigorous modeling is needed to test if dark matter glow could be detectable.
The colision between_the_milky_way_and_andromedaSérgio Sacani
The document summarizes a simulation of the future collision between the Milky Way and Andromeda galaxies. It finds that given current observational constraints on their distance, velocity, and masses:
1) The Milky Way and Andromeda are likely to collide in a few billion years, within the lifetime of the Sun.
2) During the interaction, there is a chance the Sun could be pulled into an extended tidal tail between the galaxies.
3) Eventually, after the merger is complete, the Sun would most likely be scattered to the outer halo of the merged galaxy at a distance over 30 kpc.
A density cusp of quiescent X-ray binaries in the central parsec of the GalaxySérgio Sacani
The existence of a ‘density cusp’1,2—a localized increase in
number—of stellar-mass black holes near a supermassive black
hole is a fundamental prediction of galactic stellar dynamics3
. The
best place to detect such a cusp is in the Galactic Centre, where
the nearest supermassive black hole, Sagittarius A*, resides. As
many as 20,000 black holes are predicted to settle into the central
parsec of the Galaxy as a result of dynamical friction3–5; however,
so far no density cusp of black holes has been detected. Low-mass
X-ray binary systems that contain a stellar-mass black hole are
natural tracers of isolated black holes. Here we report observations
of a dozen quiescent X-ray binaries in a density cusp within one
parsec of Sagittarius A*. The lower-energy emission spectra that
we observed in these binaries is distinct from the higher-energy
spectra associated with the population of accreting white dwarfs that
dominates the central eight parsecs of the Galaxy6
. The properties
of these X-ray binaries, in particular their spatial distribution and
luminosity function, suggest the existence of hundreds of binary
systems in the central parsec of the Galaxy and many more isolated
black holes. We cannot rule out a contribution to the observed
emission from a population (of up to about one-half the number of
X-ray binaries) of rotationally powered, millisecond pulsars. The
spatial distribution of the binary systems is a relic of their formation
history, either in the stellar disk around Sagittarius A* (ref. 7) or
through in-fall from globular clusters, and constrains the number
density of sources in the modelling of gravitational waves from
massive stellar remnants8,9
, such as neutron stars and black holes.
Similar to Milky Way White Dwarfs as Sub-GeV to Multi-TeV Dark Matter Detectors (20)
Compositions of iron-meteorite parent bodies constrainthe structure of the pr...Sérgio Sacani
Magmatic iron-meteorite parent bodies are the earliest planetesimals in the Solar System,and they preserve information about conditions and planet-forming processes in thesolar nebula. In this study, we include comprehensive elemental compositions andfractional-crystallization modeling for iron meteorites from the cores of five differenti-ated asteroids from the inner Solar System. Together with previous results of metalliccores from the outer Solar System, we conclude that asteroidal cores from the outerSolar System have smaller sizes, elevated siderophile-element abundances, and simplercrystallization processes than those from the inner Solar System. These differences arerelated to the formation locations of the parent asteroids because the solar protoplane-tary disk varied in redox conditions, elemental distributions, and dynamics at differentheliocentric distances. Using highly siderophile-element data from iron meteorites, wereconstruct the distribution of calcium-aluminum-rich inclusions (CAIs) across theprotoplanetary disk within the first million years of Solar-System history. CAIs, the firstsolids to condense in the Solar System, formed close to the Sun. They were, however,concentrated within the outer disk and depleted within the inner disk. Future modelsof the structure and evolution of the protoplanetary disk should account for this dis-tribution pattern of CAIs.
Signatures of wave erosion in Titan’s coastsSérgio Sacani
The shorelines of Titan’s hydrocarbon seas trace flooded erosional landforms such as river valleys; however, it isunclear whether coastal erosion has subsequently altered these shorelines. Spacecraft observations and theo-retical models suggest that wind may cause waves to form on Titan’s seas, potentially driving coastal erosion,but the observational evidence of waves is indirect, and the processes affecting shoreline evolution on Titanremain unknown. No widely accepted framework exists for using shoreline morphology to quantitatively dis-cern coastal erosion mechanisms, even on Earth, where the dominant mechanisms are known. We combinelandscape evolution models with measurements of shoreline shape on Earth to characterize how differentcoastal erosion mechanisms affect shoreline morphology. Applying this framework to Titan, we find that theshorelines of Titan’s seas are most consistent with flooded landscapes that subsequently have been eroded bywaves, rather than a uniform erosional process or no coastal erosion, particularly if wave growth saturates atfetch lengths of tens of kilometers.
SDSS1335+0728: The awakening of a ∼ 106M⊙ black hole⋆Sérgio Sacani
Context. The early-type galaxy SDSS J133519.91+072807.4 (hereafter SDSS1335+0728), which had exhibited no prior optical variations during the preceding two decades, began showing significant nuclear variability in the Zwicky Transient Facility (ZTF) alert stream from December 2019 (as ZTF19acnskyy). This variability behaviour, coupled with the host-galaxy properties, suggests that SDSS1335+0728 hosts a ∼ 106M⊙ black hole (BH) that is currently in the process of ‘turning on’. Aims. We present a multi-wavelength photometric analysis and spectroscopic follow-up performed with the aim of better understanding the origin of the nuclear variations detected in SDSS1335+0728. Methods. We used archival photometry (from WISE, 2MASS, SDSS, GALEX, eROSITA) and spectroscopic data (from SDSS and LAMOST) to study the state of SDSS1335+0728 prior to December 2019, and new observations from Swift, SOAR/Goodman, VLT/X-shooter, and Keck/LRIS taken after its turn-on to characterise its current state. We analysed the variability of SDSS1335+0728 in the X-ray/UV/optical/mid-infrared range, modelled its spectral energy distribution prior to and after December 2019, and studied the evolution of its UV/optical spectra. Results. From our multi-wavelength photometric analysis, we find that: (a) since 2021, the UV flux (from Swift/UVOT observations) is four times brighter than the flux reported by GALEX in 2004; (b) since June 2022, the mid-infrared flux has risen more than two times, and the W1−W2 WISE colour has become redder; and (c) since February 2024, the source has begun showing X-ray emission. From our spectroscopic follow-up, we see that (i) the narrow emission line ratios are now consistent with a more energetic ionising continuum; (ii) broad emission lines are not detected; and (iii) the [OIII] line increased its flux ∼ 3.6 years after the first ZTF alert, which implies a relatively compact narrow-line-emitting region. Conclusions. We conclude that the variations observed in SDSS1335+0728 could be either explained by a ∼ 106M⊙ AGN that is just turning on or by an exotic tidal disruption event (TDE). If the former is true, SDSS1335+0728 is one of the strongest cases of an AGNobserved in the process of activating. If the latter were found to be the case, it would correspond to the longest and faintest TDE ever observed (or another class of still unknown nuclear transient). Future observations of SDSS1335+0728 are crucial to further understand its behaviour. Key words. galaxies: active– accretion, accretion discs– galaxies: individual: SDSS J133519.91+072807.4
Discovery of An Apparent Red, High-Velocity Type Ia Supernova at 𝐳 = 2.9 wi...Sérgio Sacani
We present the JWST discovery of SN 2023adsy, a transient object located in a host galaxy JADES-GS
+
53.13485
−
27.82088
with a host spectroscopic redshift of
2.903
±
0.007
. The transient was identified in deep James Webb Space Telescope (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) program. Photometric and spectroscopic followup with NIRCam and NIRSpec, respectively, confirm the redshift and yield UV-NIR light-curve, NIR color, and spectroscopic information all consistent with a Type Ia classification. Despite its classification as a likely SN Ia, SN 2023adsy is both fairly red (
�
(
�
−
�
)
∼
0.9
) despite a host galaxy with low-extinction and has a high Ca II velocity (
19
,
000
±
2
,
000
km/s) compared to the general population of SNe Ia. While these characteristics are consistent with some Ca-rich SNe Ia, particularly SN 2016hnk, SN 2023adsy is intrinsically brighter than the low-
�
Ca-rich population. Although such an object is too red for any low-
�
cosmological sample, we apply a fiducial standardization approach to SN 2023adsy and find that the SN 2023adsy luminosity distance measurement is in excellent agreement (
≲
1
�
) with
Λ
CDM. Therefore unlike low-
�
Ca-rich SNe Ia, SN 2023adsy is standardizable and gives no indication that SN Ia standardized luminosities change significantly with redshift. A larger sample of distant SNe Ia is required to determine if SN Ia population characteristics at high-
�
truly diverge from their low-
�
counterparts, and to confirm that standardized luminosities nevertheless remain constant with redshift.
Evidence of Jet Activity from the Secondary Black Hole in the OJ 287 Binary S...Sérgio Sacani
Wereport the study of a huge optical intraday flare on 2021 November 12 at 2 a.m. UT in the blazar OJ287. In the binary black hole model, it is associated with an impact of the secondary black hole on the accretion disk of the primary. Our multifrequency observing campaign was set up to search for such a signature of the impact based on a prediction made 8 yr earlier. The first I-band results of the flare have already been reported by Kishore et al. (2024). Here we combine these data with our monitoring in the R-band. There is a big change in the R–I spectral index by 1.0 ±0.1 between the normal background and the flare, suggesting a new component of radiation. The polarization variation during the rise of the flare suggests the same. The limits on the source size place it most reasonably in the jet of the secondary BH. We then ask why we have not seen this phenomenon before. We show that OJ287 was never before observed with sufficient sensitivity on the night when the flare should have happened according to the binary model. We also study the probability that this flare is just an oversized example of intraday variability using the Krakow data set of intense monitoring between 2015 and 2023. We find that the occurrence of a flare of this size and rapidity is unlikely. In machine-readable Tables 1 and 2, we give the full orbit-linked historical light curve of OJ287 as well as the dense monitoring sample of Krakow.
Candidate young stellar objects in the S-cluster: Kinematic analysis of a sub...Sérgio Sacani
Context. The observation of several L-band emission sources in the S cluster has led to a rich discussion of their nature. However, a definitive answer to the classification of the dusty objects requires an explanation for the detection of compact Doppler-shifted Brγ emission. The ionized hydrogen in combination with the observation of mid-infrared L-band continuum emission suggests that most of these sources are embedded in a dusty envelope. These embedded sources are part of the S-cluster, and their relationship to the S-stars is still under debate. To date, the question of the origin of these two populations has been vague, although all explanations favor migration processes for the individual cluster members. Aims. This work revisits the S-cluster and its dusty members orbiting the supermassive black hole SgrA* on bound Keplerian orbits from a kinematic perspective. The aim is to explore the Keplerian parameters for patterns that might imply a nonrandom distribution of the sample. Additionally, various analytical aspects are considered to address the nature of the dusty sources. Methods. Based on the photometric analysis, we estimated the individual H−K and K−L colors for the source sample and compared the results to known cluster members. The classification revealed a noticeable contrast between the S-stars and the dusty sources. To fit the flux-density distribution, we utilized the radiative transfer code HYPERION and implemented a young stellar object Class I model. We obtained the position angle from the Keplerian fit results; additionally, we analyzed the distribution of the inclinations and the longitudes of the ascending node. Results. The colors of the dusty sources suggest a stellar nature consistent with the spectral energy distribution in the near and midinfrared domains. Furthermore, the evaporation timescales of dusty and gaseous clumps in the vicinity of SgrA* are much shorter ( 2yr) than the epochs covered by the observations (≈15yr). In addition to the strong evidence for the stellar classification of the D-sources, we also find a clear disk-like pattern following the arrangements of S-stars proposed in the literature. Furthermore, we find a global intrinsic inclination for all dusty sources of 60 ± 20◦, implying a common formation process. Conclusions. The pattern of the dusty sources manifested in the distribution of the position angles, inclinations, and longitudes of the ascending node strongly suggests two different scenarios: the main-sequence stars and the dusty stellar S-cluster sources share a common formation history or migrated with a similar formation channel in the vicinity of SgrA*. Alternatively, the gravitational influence of SgrA* in combination with a massive perturber, such as a putative intermediate mass black hole in the IRS 13 cluster, forces the dusty objects and S-stars to follow a particular orbital arrangement. Key words. stars: black holes– stars: formation– Galaxy: center– galaxies: star formation
JAMES WEBB STUDY THE MASSIVE BLACK HOLE SEEDSSérgio Sacani
The pathway(s) to seeding the massive black holes (MBHs) that exist at the heart of galaxies in the present and distant Universe remains an unsolved problem. Here we categorise, describe and quantitatively discuss the formation pathways of both light and heavy seeds. We emphasise that the most recent computational models suggest that rather than a bimodal-like mass spectrum between light and heavy seeds with light at one end and heavy at the other that instead a continuum exists. Light seeds being more ubiquitous and the heavier seeds becoming less and less abundant due the rarer environmental conditions required for their formation. We therefore examine the different mechanisms that give rise to different seed mass spectrums. We show how and why the mechanisms that produce the heaviest seeds are also among the rarest events in the Universe and are hence extremely unlikely to be the seeds for the vast majority of the MBH population. We quantify, within the limits of the current large uncertainties in the seeding processes, the expected number densities of the seed mass spectrum. We argue that light seeds must be at least 103 to 105 times more numerous than heavy seeds to explain the MBH population as a whole. Based on our current understanding of the seed population this makes heavy seeds (Mseed > 103 M⊙) a significantly more likely pathway given that heavy seeds have an abundance pattern than is close to and likely in excess of 10−4 compared to light seeds. Finally, we examine the current state-of-the-art in numerical calculations and recent observations and plot a path forward for near-future advances in both domains.
Anti-Universe And Emergent Gravity and the Dark UniverseSérgio Sacani
Recent theoretical progress indicates that spacetime and gravity emerge together from the entanglement structure of an underlying microscopic theory. These ideas are best understood in Anti-de Sitter space, where they rely on the area law for entanglement entropy. The extension to de Sitter space requires taking into account the entropy and temperature associated with the cosmological horizon. Using insights from string theory, black hole physics and quantum information theory we argue that the positive dark energy leads to a thermal volume law contribution to the entropy that overtakes the area law precisely at the cosmological horizon. Due to the competition between area and volume law entanglement the microscopic de Sitter states do not thermalise at sub-Hubble scales: they exhibit memory effects in the form of an entropy displacement caused by matter. The emergent laws of gravity contain an additional ‘dark’ gravitational force describing the ‘elastic’ response due to the entropy displacement. We derive an estimate of the strength of this extra force in terms of the baryonic mass, Newton’s constant and the Hubble acceleration scale a0 = cH0, and provide evidence for the fact that this additional ‘dark gravity force’ explains the observed phenomena in galaxies and clusters currently attributed to dark matter.
The binding of cosmological structures by massless topological defectsSérgio Sacani
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...Sérgio Sacani
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
The debris of the ‘last major merger’ is dynamically youngSérgio Sacani
The Milky Way’s (MW) inner stellar halo contains an [Fe/H]-rich component with highly eccentric orbits, often referred to as the
‘last major merger.’ Hypotheses for the origin of this component include Gaia-Sausage/Enceladus (GSE), where the progenitor
collided with the MW proto-disc 8–11 Gyr ago, and the Virgo Radial Merger (VRM), where the progenitor collided with the
MW disc within the last 3 Gyr. These two scenarios make different predictions about observable structure in local phase space,
because the morphology of debris depends on how long it has had to phase mix. The recently identified phase-space folds in Gaia
DR3 have positive caustic velocities, making them fundamentally different than the phase-mixed chevrons found in simulations
at late times. Roughly 20 per cent of the stars in the prograde local stellar halo are associated with the observed caustics. Based
on a simple phase-mixing model, the observed number of caustics are consistent with a merger that occurred 1–2 Gyr ago.
We also compare the observed phase-space distribution to FIRE-2 Latte simulations of GSE-like mergers, using a quantitative
measurement of phase mixing (2D causticality). The observed local phase-space distribution best matches the simulated data
1–2 Gyr after collision, and certainly not later than 3 Gyr. This is further evidence that the progenitor of the ‘last major merger’
did not collide with the MW proto-disc at early times, as is thought for the GSE, but instead collided with the MW disc within
the last few Gyr, consistent with the body of work surrounding the VRM.
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Multi-source connectivity as the driver of solar wind variability in the heli...Sérgio Sacani
The ambient solar wind that flls the heliosphere originates from multiple
sources in the solar corona and is highly structured. It is often described
as high-speed, relatively homogeneous, plasma streams from coronal
holes and slow-speed, highly variable, streams whose source regions are
under debate. A key goal of ESA/NASA’s Solar Orbiter mission is to identify
solar wind sources and understand what drives the complexity seen in the
heliosphere. By combining magnetic feld modelling and spectroscopic
techniques with high-resolution observations and measurements, we show
that the solar wind variability detected in situ by Solar Orbiter in March
2022 is driven by spatio-temporal changes in the magnetic connectivity to
multiple sources in the solar atmosphere. The magnetic feld footpoints
connected to the spacecraft moved from the boundaries of a coronal hole
to one active region (12961) and then across to another region (12957). This
is refected in the in situ measurements, which show the transition from fast
to highly Alfvénic then to slow solar wind that is disrupted by the arrival of
a coronal mass ejection. Our results describe solar wind variability at 0.5 au
but are applicable to near-Earth observatories.
Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Tr...Sérgio Sacani
Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the
atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets
receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric
composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet
transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days.
The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We
confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and
validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as
well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope
and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host
star is inactive, with an X-ray-to-bolometric luminosity ratio of log 5.7 L L X bol » - . Joint analysis of the light
curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕,a3σ mass upper limit of
3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric
(TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small
list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.
Gliese 12 b, a temperate Earth-sized planet at 12 parsecs discovered with TES...Sérgio Sacani
We report on the discovery of Gliese 12 b, the nearest transiting temperate, Earth-sized planet found to date. Gliese 12 is a
bright (V = 12.6 mag, K = 7.8 mag) metal-poor M4V star only 12.162 ± 0.005 pc away from the Solar system with one of the
lowest stellar activity levels known for M-dwarfs. A planet candidate was detected by TESS based on only 3 transits in sectors
42, 43, and 57, with an ambiguity in the orbital period due to observational gaps. We performed follow-up transit observations
with CHEOPS and ground-based photometry with MINERVA-Australis, SPECULOOS, and Purple Mountain Observatory,
as well as further TESS observations in sector 70. We statistically validate Gliese 12 b as a planet with an orbital period of
12.76144 ± 0.00006 d and a radius of 1.0 ± 0.1 R⊕, resulting in an equilibrium temperature of ∼315 K. Gliese 12 b has excellent
future prospects for precise mass measurement, which may inform how planetary internal structure is affected by the stellar
compositional environment. Gliese 12 b also represents one of the best targets to study whether Earth-like planets orbiting cool
stars can retain their atmospheres, a crucial step to advance our understanding of habitability on Earth and across the galaxy.
The importance of continents, oceans and plate tectonics for the evolution of...Sérgio Sacani
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
A Giant Impact Origin for the First Subduction on EarthSérgio Sacani
Hadean zircons provide a potential record of Earth's earliest subduction 4.3 billion years ago. Itremains enigmatic how subduction could be initiated so soon after the presumably Moon‐forming giant impact(MGI). Earlier studies found an increase in Earth's core‐mantle boundary (CMB) temperature due to theaccumulation of the impactor's core, and our recent work shows Earth's lower mantle remains largely solid, withsome of the impactor's mantle potentially surviving as the large low‐shear velocity provinces (LLSVPs). Here,we show that a hot post‐impact CMB drives the initiation of strong mantle plumes that can induce subductioninitiation ∼200 Myr after the MGI. 2D and 3D thermomechanical computations show that a high CMBtemperature is the primary factor triggering early subduction, with enrichment of heat‐producing elements inLLSVPs as another potential factor. The models link the earliest subduction to the MGI with implications forunderstanding the diverse tectonic regimes of rocky planets.
Climate extremes likely to drive land mammal extinction during next supercont...Sérgio Sacani
Mammals have dominated Earth for approximately 55 Myr thanks to their
adaptations and resilience to warming and cooling during the Cenozoic. All
life will eventually perish in a runaway greenhouse once absorbed solar
radiation exceeds the emission of thermal radiation in several billions of
years. However, conditions rendering the Earth naturally inhospitable to
mammals may develop sooner because of long-term processes linked to
plate tectonics (short-term perturbations are not considered here). In
~250 Myr, all continents will converge to form Earth’s next supercontinent,
Pangea Ultima. A natural consequence of the creation and decay of Pangea
Ultima will be extremes in pCO2 due to changes in volcanic rifting and
outgassing. Here we show that increased pCO2, solar energy (F⨀;
approximately +2.5% W m−2 greater than today) and continentality (larger
range in temperatures away from the ocean) lead to increasing warming
hostile to mammalian life. We assess their impact on mammalian
physiological limits (dry bulb, wet bulb and Humidex heat stress indicators)
as well as a planetary habitability index. Given mammals’ continued survival,
predicted background pCO2 levels of 410–816 ppm combined with increased
F⨀ will probably lead to a climate tipping point and their mass extinction.
The results also highlight how global landmass configuration, pCO2 and F⨀
play a critical role in planetary habitability.
PPT on Alternate Wetting and Drying presented at the three-day 'Training and Validation Workshop on Modules of Climate Smart Agriculture (CSA) Technologies in South Asia' workshop on April 22, 2024.
Describing and Interpreting an Immersive Learning Case with the Immersion Cub...Leonel Morgado
Current descriptions of immersive learning cases are often difficult or impossible to compare. This is due to a myriad of different options on what details to include, which aspects are relevant, and on the descriptive approaches employed. Also, these aspects often combine very specific details with more general guidelines or indicate intents and rationales without clarifying their implementation. In this paper we provide a method to describe immersive learning cases that is structured to enable comparisons, yet flexible enough to allow researchers and practitioners to decide which aspects to include. This method leverages a taxonomy that classifies educational aspects at three levels (uses, practices, and strategies) and then utilizes two frameworks, the Immersive Learning Brain and the Immersion Cube, to enable a structured description and interpretation of immersive learning cases. The method is then demonstrated on a published immersive learning case on training for wind turbine maintenance using virtual reality. Applying the method results in a structured artifact, the Immersive Learning Case Sheet, that tags the case with its proximal uses, practices, and strategies, and refines the free text case description to ensure that matching details are included. This contribution is thus a case description method in support of future comparative research of immersive learning cases. We then discuss how the resulting description and interpretation can be leveraged to change immersion learning cases, by enriching them (considering low-effort changes or additions) or innovating (exploring more challenging avenues of transformation). The method holds significant promise to support better-grounded research in immersive learning.
TOPIC OF DISCUSSION: CENTRIFUGATION SLIDESHARE.pptxshubhijain836
Centrifugation is a powerful technique used in laboratories to separate components of a heterogeneous mixture based on their density. This process utilizes centrifugal force to rapidly spin samples, causing denser particles to migrate outward more quickly than lighter ones. As a result, distinct layers form within the sample tube, allowing for easy isolation and purification of target substances.
CLASS 12th CHEMISTRY SOLID STATE ppt (Animated)eitps1506
Description:
Dive into the fascinating realm of solid-state physics with our meticulously crafted online PowerPoint presentation. This immersive educational resource offers a comprehensive exploration of the fundamental concepts, theories, and applications within the realm of solid-state physics.
From crystalline structures to semiconductor devices, this presentation delves into the intricate principles governing the behavior of solids, providing clear explanations and illustrative examples to enhance understanding. Whether you're a student delving into the subject for the first time or a seasoned researcher seeking to deepen your knowledge, our presentation offers valuable insights and in-depth analyses to cater to various levels of expertise.
Key topics covered include:
Crystal Structures: Unravel the mysteries of crystalline arrangements and their significance in determining material properties.
Band Theory: Explore the electronic band structure of solids and understand how it influences their conductive properties.
Semiconductor Physics: Delve into the behavior of semiconductors, including doping, carrier transport, and device applications.
Magnetic Properties: Investigate the magnetic behavior of solids, including ferromagnetism, antiferromagnetism, and ferrimagnetism.
Optical Properties: Examine the interaction of light with solids, including absorption, reflection, and transmission phenomena.
With visually engaging slides, informative content, and interactive elements, our online PowerPoint presentation serves as a valuable resource for students, educators, and enthusiasts alike, facilitating a deeper understanding of the captivating world of solid-state physics. Explore the intricacies of solid-state materials and unlock the secrets behind their remarkable properties with our comprehensive presentation.
PPT on Direct Seeded Rice presented at the three-day 'Training and Validation Workshop on Modules of Climate Smart Agriculture (CSA) Technologies in South Asia' workshop on April 22, 2024.
Sexuality - Issues, Attitude and Behaviour - Applied Social Psychology - Psyc...PsychoTech Services
A proprietary approach developed by bringing together the best of learning theories from Psychology, design principles from the world of visualization, and pedagogical methods from over a decade of training experience, that enables you to: Learn better, faster!
Authoring a personal GPT for your research and practice: How we created the Q...Leonel Morgado
Thematic analysis in qualitative research is a time-consuming and systematic task, typically done using teams. Team members must ground their activities on common understandings of the major concepts underlying the thematic analysis, and define criteria for its development. However, conceptual misunderstandings, equivocations, and lack of adherence to criteria are challenges to the quality and speed of this process. Given the distributed and uncertain nature of this process, we wondered if the tasks in thematic analysis could be supported by readily available artificial intelligence chatbots. Our early efforts point to potential benefits: not just saving time in the coding process but better adherence to criteria and grounding, by increasing triangulation between humans and artificial intelligence. This tutorial will provide a description and demonstration of the process we followed, as two academic researchers, to develop a custom ChatGPT to assist with qualitative coding in the thematic data analysis process of immersive learning accounts in a survey of the academic literature: QUAL-E Immersive Learning Thematic Analysis Helper. In the hands-on time, participants will try out QUAL-E and develop their ideas for their own qualitative coding ChatGPT. Participants that have the paid ChatGPT Plus subscription can create a draft of their assistants. The organizers will provide course materials and slide deck that participants will be able to utilize to continue development of their custom GPT. The paid subscription to ChatGPT Plus is not required to participate in this workshop, just for trying out personal GPTs during it.
BIRDS DIVERSITY OF SOOTEA BISWANATH ASSAM.ppt.pptxgoluk9330
Ahota Beel, nestled in Sootea Biswanath Assam , is celebrated for its extraordinary diversity of bird species. This wetland sanctuary supports a myriad of avian residents and migrants alike. Visitors can admire the elegant flights of migratory species such as the Northern Pintail and Eurasian Wigeon, alongside resident birds including the Asian Openbill and Pheasant-tailed Jacana. With its tranquil scenery and varied habitats, Ahota Beel offers a perfect haven for birdwatchers to appreciate and study the vibrant birdlife that thrives in this natural refuge.
Microbial interaction
Microorganisms interacts with each other and can be physically associated with another organisms in a variety of ways.
One organism can be located on the surface of another organism as an ectobiont or located within another organism as endobiont.
Microbial interaction may be positive such as mutualism, proto-cooperation, commensalism or may be negative such as parasitism, predation or competition
Types of microbial interaction
Positive interaction: mutualism, proto-cooperation, commensalism
Negative interaction: Ammensalism (antagonism), parasitism, predation, competition
I. Mutualism:
It is defined as the relationship in which each organism in interaction gets benefits from association. It is an obligatory relationship in which mutualist and host are metabolically dependent on each other.
Mutualistic relationship is very specific where one member of association cannot be replaced by another species.
Mutualism require close physical contact between interacting organisms.
Relationship of mutualism allows organisms to exist in habitat that could not occupied by either species alone.
Mutualistic relationship between organisms allows them to act as a single organism.
Examples of mutualism:
i. Lichens:
Lichens are excellent example of mutualism.
They are the association of specific fungi and certain genus of algae. In lichen, fungal partner is called mycobiont and algal partner is called
II. Syntrophism:
It is an association in which the growth of one organism either depends on or improved by the substrate provided by another organism.
In syntrophism both organism in association gets benefits.
Compound A
Utilized by population 1
Compound B
Utilized by population 2
Compound C
utilized by both Population 1+2
Products
In this theoretical example of syntrophism, population 1 is able to utilize and metabolize compound A, forming compound B but cannot metabolize beyond compound B without co-operation of population 2. Population 2is unable to utilize compound A but it can metabolize compound B forming compound C. Then both population 1 and 2 are able to carry out metabolic reaction which leads to formation of end product that neither population could produce alone.
Examples of syntrophism:
i. Methanogenic ecosystem in sludge digester
Methane produced by methanogenic bacteria depends upon interspecies hydrogen transfer by other fermentative bacteria.
Anaerobic fermentative bacteria generate CO2 and H2 utilizing carbohydrates which is then utilized by methanogenic bacteria (Methanobacter) to produce methane.
ii. Lactobacillus arobinosus and Enterococcus faecalis:
In the minimal media, Lactobacillus arobinosus and Enterococcus faecalis are able to grow together but not alone.
The synergistic relationship between E. faecalis and L. arobinosus occurs in which E. faecalis require folic acid
Immersive Learning That Works: Research Grounding and Paths ForwardLeonel Morgado
We will metaverse into the essence of immersive learning, into its three dimensions and conceptual models. This approach encompasses elements from teaching methodologies to social involvement, through organizational concerns and technologies. Challenging the perception of learning as knowledge transfer, we introduce a 'Uses, Practices & Strategies' model operationalized by the 'Immersive Learning Brain' and ‘Immersion Cube’ frameworks. This approach offers a comprehensive guide through the intricacies of immersive educational experiences and spotlighting research frontiers, along the immersion dimensions of system, narrative, and agency. Our discourse extends to stakeholders beyond the academic sphere, addressing the interests of technologists, instructional designers, and policymakers. We span various contexts, from formal education to organizational transformation to the new horizon of an AI-pervasive society. This keynote aims to unite the iLRN community in a collaborative journey towards a future where immersive learning research and practice coalesce, paving the way for innovative educational research and practice landscapes.
Immersive Learning That Works: Research Grounding and Paths Forward
Milky Way White Dwarfs as Sub-GeV to Multi-TeV Dark Matter Detectors
1. SLAC-PUB-17741
Milky Way White Dwarfs as Sub-GeV to Multi-TeV
Dark Matter Detectors
Javier F. Acevedo,a Rebecca K. Leane,a,b Lillian Santos-Olmsted,a
a
Particle Theory Group, SLAC National Accelerator Laboratory, Stanford, CA 94035, USA
b
Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94035,
USA
E-mail: jfacev@slac.stanford.edu, rleane@slac.stanford.edu,
solmsted@stanford.edu
Abstract: We show that Milky Way white dwarfs are excellent targets for dark matter
(DM) detection. Using Fermi and H.E.S.S. Galactic center gamma-ray data, we investigate
sensitivity to DM annihilating within white dwarfs into long-lived or boosted mediators and
producing detectable gamma rays. Depending on the Galactic DM distribution, we set new
constraints on the spin-independent scattering cross section down to 10−45 − 10−41 cm2 in
the sub-GeV DM mass range, which is multiple orders of magnitude stronger than existing
limits. For a generalized NFW DM profile, we find that our white dwarf constraints exceed
spin-independent direct detection limits across most of the sub-GeV to multi-TeV DM mass
range, achieving sensitivities as low as about 10−46 cm2. In addition, we improve earlier
versions of the DM capture calculation in white dwarfs, by including the low-temperature
distribution of nuclei when the white dwarf approaches crystallization. This yields smaller
capture rates than previously calculated by a factor of a few up to two orders of magnitude,
depending on white dwarf size and the astrophysical system.
arXiv:2309.10843v1
[hep-ph]
19
Sep
2023
2. Contents
1 Introduction 2
2 White Dwarf Properties and Galactic Distribution 3
2.1 Distribution in the Inner Milky Way 3
2.2 Age, Temperature, and Composition 4
3 Refined Treatment of Dark Matter Capture in White Dwarfs 5
3.1 Velocity Distributions 6
3.2 Capture Rate for a Single White Dwarf 8
3.2.1 Formalism 8
3.2.2 Comparison with Previous Treatment of the Capture Rate 10
3.3 Maximum Capture Rate for a Single White Dwarf 12
4 Annihilation Flux and Gamma-Ray Detection 13
4.1 Dark Matter Thermalization and Annihilation Rate 13
4.2 Gamma-Ray Energy Flux 15
4.3 Gamma-Ray Detection 16
5 Dark Matter Parameter Space Constraints 17
5.1 Results 17
5.2 Discussion of Astrophysical Uncertainties 19
5.2.1 Dark Matter Uncertainties 19
5.2.2 White Dwarf Uncertainties 20
6 Summary and Conclusions 21
A Velocity Distribution for Ions in Cold White Dwarfs 22
– 1 –
3. 1 Introduction
O
ur milky way galaxy is host to hundreds of billions of stars. Unfortunately, these
stars can not shine brightly forever, and they must eventually meet their demise.
The final evolutionary state for over 97 percent of stars is called a white dwarf. As a
star enters its red giant phase, it fuses helium to carbon and oxygen in its core, but if it does
not have sufficient mass to generate the temperatures required for carbon fusion, an inert
mass of carbon and oxygen will accumulate at its center. White dwarfs are the remnants of
low to medium mass stars that have exhausted their nuclear fuel, and shed their outer layers,
revealing the remaining core, typically composed of a crystalline lattice of carbon and oxygen
atoms.
White dwarfs are incredibly dense, packing the mass of our Sun into a sphere the size
of the Earth. It is exactly these two properties – density and radius – which make it an
ideal target for new dark matter (DM) searches. Its density renders it one of the most dense
celestial objects in the Universe, only coming second to neutron stars. But compared to
neutron stars, white dwarfs are much larger, such that the surface area available for DM
capture is much larger. This aids DM detection, as larger maximal capture rates mean more
potential consequent particles arising from DM annihilation in white dwarfs. Furthermore,
the sheer number of white dwarfs present in our Milky Way Galaxy is about one order of
magnitude higher than the number of neutron stars, due to the prevalence of low to medium
mass stars and their final evolutionary fate.
White dwarfs have been considered as DM detectors in the past [1–23]. The most com-
monly considered scenario for sub-GeV DM, is DM capture and consequent annihilation to
short-lived or not very boosted mediators, which in turn leads to the DM rest mass energy
being absorbed by the white dwarf. In this case, the temperature of the white dwarf can in-
crease proportionally to the density of DM available in its local environment. As white dwarfs
are generally quite hot, a large local DM density is required to achieve an appreciable DM
heating signal. Therefore, previous work has dominantly focused on white dwarf DM heating
in globular clusters such as Messier 4 (M4) [3, 4, 9, 11, 13, 17, 18, 20–22], where sufficiently
cool white dwarfs have been observed, and the DM density has been speculated to potentially
be as high as about O(100) GeV/cm3 [3, 4]; about 1,000 times higher than the local Solar
position. However, as was already emphasized in the bulk of these studies, the DM density in
globular clusters such as M4 is not well understood, and the current systematic error bar on
the DM density is substantial, with some astrophysical studies long stating consistency with
little to no DM at all [24, 25]. Therefore, while the commonly-studied white dwarf heating
signal offers substantial potential sensitivity, it is not yet a robust search.
In this work, we investigate a new search for DM in white dwarfs. We target white
dwarfs in the inner region of the Milky Way Galaxy, where they are numerous, and where
the DM content is still high and yet much better understood (i.e., the DM density is not
expected to be zero in the Galactic center). While the inner slope of the DM distribution
in our Galaxy is not yet known, we consider a range of variations to somewhat bracket the
– 2 –
4. expected systematics, which still give substantial amounts of DM to power a signal in white
dwarfs. The scenario we investigate is also complementary to DM heating searches, which
require mediators to not escape the white dwarf; we investigate the scenario where mediators
decay outside the white dwarf and produce gamma rays. As an important component of this
work, we also present and use an improved calculation for DM capture in white dwarfs, which
takes into account the velocity distribution of low-temperature nuclei in the white dwarf as it
approaches crystallization. Depending on the white dwarf size and the astrophysical system
of interest, this produces white dwarf capture rates between a factor of a few up to about two
orders of magnitude smaller than previously calculated.
This paper is organized as follows. In Section 2, we discuss the white dwarf properties
relevant for our capture calculation, including our modeling of the Galactic white dwarf radial
number distribution, as well as their physical properties such as temperature and composition.
In Section 3, we discuss our improved treatment for DM capture in white dwarfs, building on
the existing literature. In Section 4, we discuss the detection prospects for DM annihilation
to gamma rays in these white dwarfs with Fermi and H.E.S.S.. We show our new limits on the
spin-independent DM-SM scattering cross section in Section 5, and include some additional
discussion on the relevant astrophysical uncertainties for our search. We summarize our
findings and conclude in Section 6. Appendix A contains additional discussion on the low-
temperature ion velocity in white dwarfs.
2 White Dwarf Properties and Galactic Distribution
2.1 Distribution in the Inner Milky Way
To determine the size of our white dwarf population DM signal, we first need to know how
many white dwarfs reside in the inner Galaxy, as well as how they are distributed. Our signal
is dominated by the central region of the Galaxy, as it is where the density of white dwarfs
and the density of DM are at their highest. Stars in the inner parsec of our Galaxy are a part
of what is called the nuclear star cluster, which surrounds the central supermassive black hole
of the Milky Way, Sagittarius A∗ (Sgr A∗), and contains a significant stellar density.
We parameterize the white dwarf number density distribution nWD in this central region
as a power-law with slope α,
nWD(r) = nWD(r0)
r
r0
−α
, (2.1)
where r is the radial distance to the Galactic center, and r0 and nWD(r0) define the normal-
ization as we will discuss shortly. Power-law density profiles for the stellar components of
nuclear star clusters are predicted by N-body simulations [26–29], as well as analytical mass
segregation solutions assuming a steady state is reached through gravitational interactions
between the stars [30–32]. Cuspy distributions of the stellar objects in the inner parsec sur-
rounding Sgr A∗ are also favoured by recent spectroscopic and photometric surveys [33–35]
and X-ray observations [36]. The index depends on several modeling assumptions including
– 3 –
5. the star formation history, initial mass function, and initial-to-final mass relation for stellar
remnants. The latter in particular can be sensitive to the exact metallicity value; we detail
this further below. These assumptions determine the distribution of masses and abundance of
each star type, which in turn influences how the energy is distributed among the components
of the stellar population through gravitational scattering, and therefore their number density
at a given radius. We adopt α = 1.4 following the analytic estimates of Ref. [32].
To determine the normalization of Eq. (2.1), we use the state-of-the-art predictions for
the number of white dwarfs as per Ref. [37]. There, a number of star formation scenarios in
the Galactic center were analyzed, leading to a prediction of ∼ 8.7 × 106 white dwarfs within
the central 1.5 pc. Thus, with the exponent choice above, fixing r0 = 1.5 pc gives nWD(r0) ≃
5.79×105 pc−3. This normalization assumes the power-law is only valid between 10−4 pc and
1.5 pc, which matches the approximate range of Ref. [32]. This estimate is a factor of ∼ 4−10
larger than previous white dwarf counts in the Galactic center, see e.g. Refs. [31, 32]. This is
because Ref. [37] incorporated for the first time metallicity measurements from spectroscopic
surveys [38–40], which revealed a large population of stars with super-solar metallicity in
this region. Higher metallicity leads to enhanced mass loss rates during the progenitor phase
through stellar winds, and as a result more of these compact objects are produced compared
to lower metallicity regions.
2.2 Age, Temperature, and Composition
As well as knowing how the white dwarf population is distributed, we need to consider the
range of properties expected for the individual white dwarfs. We model the dense white dwarf
plasma using the Feynman-Metropolis-Teller equation of state [41], which in its most recent
iteration incorporates a number of corrections ranging from weak and nuclear interactions to
general relativistic effects [42, 43]. This equation of state is commonly used in previous works
on DM capture in white dwarfs, and therefore also facilitates direct comparison. For a given
central density and composition, the resulting white dwarf configuration is obtained by cou-
pling the equation of state to the Tolman-Volkoff-Oppenheimer equation (see e.g. Ref. [44]).
The exact composition of white dwarfs can depend on a number of its progenitor’s prop-
erties, including its mass, rotation, metallicity, and binarity. Both observations and simula-
tions of the white dwarf mass distribution indicate that most of these objects have masses
0.3 M⊙ ≲ MWD ≲ 1.0 M⊙ (where M⊙ is the Solar mass), for which they are expected to
be predominantly made of carbon-12 and oxygen-16 [45, 46]. For white dwarfs with masses
MWD ≲ 0.3 M⊙, their composition is predominantly helium-4. However, it is well known
these low-mass remnants cannot be the result of single star evolution and are thus rare, see
e.g. Ref. [47]. In the case of ultra-massive white dwarfs with MWD ≳ 1.0 M⊙, a fraction of this
population will also be composed of carbon-12 and oxygen-16 as a result of mergers of binary
white dwarfs [48–50] or the specific evolution of its progenitor [51–53], with the remaining
white dwarfs having oxygen-16 cores with traces of neon-20 and heavier elements. In fact,
N-body simulations predict carbon-oxygen white dwarfs to be more prevalent in our central
Galactic region of interest [28]. To be conservative, we assume our white dwarfs are only
– 4 –
6. Benchmark Mass [M⊙] Radius [km] Central Density [g/cm3]
Light Mass 0.49 9390 1.98 × 106
Intermediate Mass 1.00 5380 3.46 × 107
Heavy Mass 1.38 1250 1.14 × 1010
Table 1. Properties of our benchmark white dwarfs. We assume all the benchmarks to be pure
carbon-12; see text for details.
made of carbon-12. This is conservative because, while the equation of state used predicts
extremely similar density profiles and mass-radius relations for both pure carbon and pure
oxygen compositions [42], DM-oxygen scattering has a larger coherent enhancement factor
compared to carbon, which would produce larger capture rates. Furthermore, we emphasize
that the equation of state considered here predicts very similar profiles to other existing equa-
tions of state such as Ref. [54], except near the stability threshold where it actually predicts
smaller masses compared to other treatments. Thus, the limits we derive from the white
dwarfs in the high mass end are also conservative.
Table 1 details the three benchmark white dwarfs we consider: one light mass, one
intermediate mass, and one heavy mass white dwarf. These are chosen to span the range
of realizations of white dwarfs expected in galaxies and globular clusters, and to facilitate
comparison with the results in Ref. [20]. We also assume that the white dwarfs powering
the gamma-ray signal from DM annihilation have ages greater than about 3 Gyr. Recent
star formation history analyses of the Milky Way’s nuclear star cluster show preference for a
double-starburst model, with the initial star formation episode occurring between 5 − 13 Gyr
ago and producing over ∼ 90% of the stars observed today [37, 55]. Thus, the majority of
white dwarfs around or above a solar mass must have formed by now, since their progenitors
only last less than about 100 Myr. For our light mass benchmark, on the other hand, their
existence is contingent upon the precise time at which the first starburst occurred, since these
white dwarfs are formed from roughly solar mass progenitors which can last for about 10 Gyr.
If an early starburst occurred ∼ 13 Gyr ago [55], then these stars must have ages greater than
about 3 Gyr. The most advanced white dwarf cooling models predict white dwarfs in this
age range will have a luminosity of order ≲ 10−4 L⊙ [56], where L⊙ is the solar luminosity.
This corresponds to white dwarf core temperatures TWD ≲ 106 K, with some slight variation
depending on the atmospheric composition [44].
3 Refined Treatment of Dark Matter Capture in White Dwarfs
Equipped with the properties and number distribution of white dwarfs in the inner Galaxy,
we now discuss the rates in which white dwarfs capture DM. We will focus on DM capture
– 5 –
7. through scattering against white dwarf ions, and make some improvements on the previous
treatments of DM capture in white dwarfs.
3.1 Velocity Distributions
We first consider the distribution of the relative velocity between the DM and the target ions,
which is an important quantity for DM capture. This is given by
Frel(uχ) =
uχ
vWD
3
2π(v2
d + ⟨v2
N ⟩)
1/2
exp
−
3(uχ − vWD)2
2(v2
d + ⟨v2
N ⟩)
− exp
−
3(uχ + vWD)2
2(v2
d + ⟨v2
N ⟩)
,
(3.1)
where uχ is the DM-ion relative velocity before the DM is accelerated by the white dwarf,
vd is the local velocity dispersion of the DM halo, vWD is the white dwarf speed in the
Galactic rest frame, and ⟨v2
N ⟩ is the mean squared white dwarf ion velocity. We assume
a constant DM velocity dispersion throughout the Galaxy equal to vd = v⊙
d ≃ 270 km/s;
the dispersion towards the Galactic center is not precisely known and varies in the range
∼ 100 − 500 km/s [57], but this only translates into a factor of less than two in variation in
the capture rates we derive in this region. For the white dwarf speed vWD, we adopt a value
of vWD =
p
8/π σ∗ ≃ 285 km/s, where σ∗ = 179 km/s is the inferred velocity dispersion for
old stars in the Milky Way’s nuclear stellar cluster [58, 59]. In practice, the specific choice
of these parameters does not have a significant impact on our results due to the magnitude
of ⟨v2
N ⟩, which is the dominant scale in the above distribution for most white dwarfs in the
mass range we analyze. Note that Eq. (3.1) does not explicitly include a velocity cutoff at the
Galactic escape velocity, which is expected to be of order ∼ 1000 km/s in the central inner
parsec [60]. We have checked that our capture rates are fairly insensitive to the inclusion
of such cutoff, changing only by a few percent in the regime where most of the distribution
above is relevant for capture.
To estimate the mean squared ion velocity ⟨v2
N ⟩, we must first discuss the velocity distri-
bution that results from the microscopic structure of a white dwarf. Most of a white dwarf
volume is fully ionized due to the extreme pressure, with the state of such a dense plasma
depending on the ratio between the Coulomb energy of the ions and the temperature. When
the white dwarf is formed, the ions are hot enough to form a dense Boltzmann gas. This
phase smoothly transitions into a strongly coupled liquid as the object cools down. This
liquid plasma phase eventually solidifies into a lattice, in a first-order phase transition known
as white dwarf crystallization. The transition point for a single component plasma was first
numerically estimated in Ref. [61]. More detailed and accurate numerical calculations (see
e.g. Ref. [62]) are in reasonable agreement with this estimate, and empirical confirmation of
this first-order phase transition has been obtained from Gaia data in Ref. [63].
Even prior to the onset of crystallization, at sufficiently low temperatures each ion feels a
restoring force from the neighboring ions which can be approximated as a harmonic oscillator
– 6 –
8. 0 1 2 3 4 5
0
40
80
120
160
200
240
280
320
360
400
vN [ 10-3
c ]
v
N
2
ℱ
ion
(
v
N
)
[
c
-1
]
�������-���������
ρ�� = ���
� ��-�
ρ�� = ���
� ��-�
ρ�� = ���
� ��-�
ρ�� = ���
� ��-�
ρ�� = ���
� ��-�
Figure 1. Speed probability density of the white dwarf ions in the stellar rest frame using the
classical Maxwell-Boltzmann distribution (dashed), and the more accurate distribution accounting
for quantum effects which produce higher ion velocities at the specified densities (solid). For this plot,
we assume a temperature TWD = 105
K and a pure carbon-12 composition.
potential, with a natural constant given by the ion plasma frequency,
ωp =
4πZ2e2nN
mN
1/2
≃ 1.68 keV
ρWD
1.98 × 106 g/cm3
1/2
Z
6
A
12
−1
, (3.2)
where nN is the white dwarf ion number density, mN = A mn is the ion mass with mn =
0.93 GeV, A is the atomic mass, and Z is the atomic number. On the right of Eq. (3.2) we
have normalized to the central value of our light benchmark white dwarf. This approximation
will be valid for temperatures that satisfy TWD ≲ ωp. In this regime, ion quantum effects also
become relevant, as the thermal de Broglie wavelength of the ions is much shorter than their
average separation. As we show in Appendix A, the velocity distribution of the ions in this
regime is well approximated by
Fion(vN ) =
mN
πωp coth (ωp/2TWD)
3/2
exp
−
mN v2
N
ωp coth (ωp/2TWD)
, (3.3)
– 7 –
9. which gives a mean squared velocity
⟨v2
N ⟩ =
3ωp
2mN
coth
ωp
2TWD
. (3.4)
In what follows, we will assume that white dwarfs have a uniform temperature TWD. This is
a good approximation for the volume relevant for capture in the optically thin limit, where
degenerate electrons have high thermal conductivity.
Figure 1 shows our velocity distribution for a temperature TWD = 105 K and density
values, which translates into ion plasma frequencies of order ∼ 0.37 − 40 keV. These are
chosen to approximately cover the range of our white dwarf benchmarks (cf. Table 1). For
comparison, we show as the dashed line the classical Maxwell-Boltzmann distribution at
the same temperature of TWD = 105 K. As the density decreases, as is expected towards the
white dwarf surface, eventually our distribution converges to the Maxwell-Boltzmann because
quantum effects stop being relevant at low ion plasma frequencies. It can therefore be seen that
our approach naturally reproduces the velocity distribution used in Ref. [20], if we consider
the outer regions of the object where TWD ≫ ωp. In this limit, ⟨v2
N ⟩ converges to the expected
limit from classical statistical mechanics, i.e. 3TWD/mN . We further expand on this point in
Appendix A. In practice, however, DM capture in the optically thin limit will occur within the
volume where the mean squared velocity scales as ∼ 3ωp/2mN , which is significantly greater
than the naive thermal value. As we discuss further below, this discrepancy can produce
significant deviations compared to the previous treatment. This ranges from an order one
factor in regions where the DM has a high velocity dispersion, up to about two orders of
magnitude in systems with low velocity dispersion such as globular clusters where v2
d ≪ ⟨v2
N ⟩.
3.2 Capture Rate for a Single White Dwarf
3.2.1 Formalism
We now describe the DM capture rate in a single white dwarf. We follow the treatment of
DM in white dwarfs considered in Ref. [20], which is based on the earlier Refs. [64–66] (which
had been applied to the Earth and Sun), however we improve upon the implementation
of the velocity distribution of the white dwarf ions, accounting for quantum effects at low
temperatures as discussed in the previous section. In the optically thin limit, where the DM
particles scatter on average less than once per white dwarf crossing, the capture rate CWD is
given by
CWD =
ρχ
mχ
Z RWD
0
dr 4πr2
Z ∞
0
duχ
w(r)
uχ
Frel(uχ) Ω−
(w) , (3.5)
where the down-scattering rate is
Ω−
(w) =
Z vesc(r)
0
dv R−
(w → v) , (3.6)
– 8 –
10. and the differential down-scattering rate is
R−
(w → v) =
Z ∞
0
ds
Z ∞
0
dt 32πµ4
+
vt
w
dσNχ
d cos θ
nN (r)Fion(vN )Θ (t + s − w) Θ (v − |t − s|) ,
(3.7)
with the following definitions
w(r)2
= vesc(r)2
+ u2
χ , (3.8)
vN (r)2
= 2µµ+t2
+ 2µ+s2
− µw(r)2
, (3.9)
µ =
mχ
mN
, (3.10)
µ± =
µ ± 1
2
, (3.11)
and the distributions Frel(uχ) and Fion(vN ) are given by Eqs. (3.1) and (3.3) respectively.
Note that our expression also differs from that of Ref. [20] by a factor π3/2 due to the way
we have normalized Fion(vN ). The factors mχ and ρχ respectively are the DM mass and
local DM mass density around the white dwarf. The total DM particle capture rate CWD is
obtained through the integration over shells of the rate at which DM particles scatter and
become gravitationally bound to the white dwarf. The velocities w and v denote the DM
velocity in the white dwarf rest frame before and after scattering, respectively. For capture,
we require v ≲ vesc(r) at the specific shell where the scattering occurred. Lastly, the variables
s and t are the center-of-mass velocity and the velocity of the DM in the center-of-mass frame,
respectively.
We consider an isotropic and constant DM-ion cross section, given by
dσNχ
d cos θ
= A4
mχ + mn
mχ + Amn
2
|Fhelm(ER)|2
σnχ , (3.12)
where σnχ is the DM-nucleon cross section. The function Fhelm(ER) is the Helm form factor,
which accounts for nuclear substructure effects for scattering at large momentum transfers
compared to the inverse nuclear radius. This function can be expressed in terms of the recoil
energy of the target
|Fhelm(ER)|2
= exp
−
ER
EN
, (3.13)
where ER = q2/2mN is the recoil energy, and q is the magnitude of the momentum transfer.
In terms of the center-of-mass velocity s and the velocity of the DM t in this frame, the
average momentum transfer magnitude reads [66]
q(s, t) =
2m2
χt2
1 −
(s2 + t2 − v2)(s2 + t2 − w2)
4s2t2
1/2
. (3.14)
The scale EN = 3/(2mN Λ2
N ) determines the recoil energy at which coherence loss becomes
relevant, where we parameterize ΛN as [67]
ΛN ≃
0.91
mN
GeV
1/3
+ 0.3
fm . (3.15)
– 9 –
11. We integrate the capture rate CWD, as given by Eq. (3.5), using the numerical code Vegas [68].
The capture rate given by Eq. (3.5) is directly proportional to the background DM density
ρχ, which is of course dependent on the position within the Galaxy. We consider the following
DM halo profiles
ρ(Ein)
χ (r) = ρ0
χ exp
−
2
α
r
rs
α
− 1
, (3.16)
ρ(NFW)
χ (r) =
ρ0
χ
r
rs
γ
1 +
r
rs
3−γ , (3.17)
where ρ
(Ein)
χ (r) is the Einasto halo profile, and ρ
(NFW)
χ (r) is the Navarro-Frenk-White (NFW)
halo profile. We will consider the Einasto profile as the core-like DM profile benchmark with
α = 0.17 and rs = 20 kpc, which matches well for Milky Way-like halos in the DM-only
Aquarius simulations [69]. We will also study an NFW profile which fixes γ = 1, as well
as a more cuspy generalized NFW (gNFW) profile with γ = 1.5, motivated by the expected
adiabatic contraction in the inner Galaxy [70, 71]. For both of the NFW-like profiles we set
rs = 12 kpc. For all DM density profiles, the normalization constant ρ0
χ is adjusted so that
the profile evaluates to ρ⊙
χ ≃ 0.42 GeV/cm3 in the Solar neighborhood.
3.2.2 Comparison with Previous Treatment of the Capture Rate
Figure 2 illustrates the difference between our improved treatment of DM capture in white
dwarfs compared to previous works, in the context of two astrophysical systems: the inner
Milky Way Galaxy (which we use in this work), and the globular cluster M4 (used dominantly
in other works for white dwarf heating searches). In both cases, the capture rates are com-
puted for all three benchmark white dwarfs in Tab. 1, assuming a DM-nucleon cross section
σnχ = 10−45 cm2, and a temperature of TWD = 105 K. For the inner Galaxy case, we chose
a DM density ρχ ≃ 9322.7 GeV/cm3 corresponding to an NFW profile at r = 1 pc from the
Galactic center, and used the velocity parameters outlined in Sec. 3.1. For M4, we use the
following parameters as per Ref. [20]: ρχ = 798 GeV/cm3, vWD = 20 km/s and vd = 8 km/s.
Note that the density for M4 is subject to substantial systematics, and these are not robust
values [20, 24, 25]. We use these commonly assumed M4 values as an example globular cluster
and to compare directly to their use in the literature; better clusters may be identified in the
future with more precise DM content measurements.
In Fig. 2, the dashed lines are the zero-temperature capture rates computed as per
Ref. [20], which assumes the white dwarf ions to be at rest. This corresponds to replac-
ing Eq. (3.6) with
Ω−
(w) =
4µ2
+
µw
nN (r)
Z vesc
w
|µ−|
µ+
dv v
dσNχ
d cos θ
, (3.18)
and taking ⟨v2
N ⟩ = 0 in Eq. (3.1). However, as white dwarfs are extremely dense plasmas,
the relevant energy scale at low temperatures is the ion plasma frequency, rather than the
– 10 –
12. 10-2 0.1 1 10 102
1025
1026
1027
1028
1029
1030
1031
1032
mχ [ GeV ]
C
WD
[
s
-1
]
��������
������
����� ��
������������ ��
����� ��
10-2 0.1 1 10 102
1025
1026
1027
1028
1029
1030
1031
1032
mχ [ GeV ]
C
WD
[
s
-1
]
�� ��������
�������
����� ��
������������ ��
����� �
�
Figure 2. Left: Capture rates for our three benchmark white dwarfs at 1 pc from the Galactic
center, assuming an NFW profile and a DM-nucleon cross section σnχ = 10−45
cm2
. For each case,
we show our capture rate which includes the white dwarf ions’ zero-point energy (solid), as well as
the previous treatment which assumes the ions are at rest (dashed). Right: Same as left panel, but
for the M4 Globular Cluster under the common assumption of large DM content, see text for details.
temperature of the white dwarf. Compared to taking only the ions at rest, our calculation,
which is shown as the solid lines in Fig. 2, includes the quantum effects due to the dense
white dwarf plasma. Including the zero-point motion is like considering a classical Maxwell-
Boltzmann distribution for a substantially hotter white dwarf, despite the white dwarf actually
being relatively cold; see Appendix A for more details.
In Fig. 2, compared to treating the ions as being at rest, we see there can be a substantial
difference in the predicted DM capture rates. Firstly, in the left panel for the light white dwarf,
we see that including the zero-point motion of the ions can increase the capture rate for the
lightest DM masses plotted. This enhancement arises because the lower average DM kinetic
energy leads to less suppression in the capture rate, and quantum effects increase the range of
velocities contributing to capture (cf. Fig. 1). For other white dwarf masses, this enhancement
also can occur, however this happens at even lighter DM masses than shown. Secondly, as the
DM mass increases, the enhancement disappears and the capture rate becomes suppressed
relative to the treatment that assumes targets at rest. The reason for this decrease is due to
the increasing DM kinetic energy leading to a regime where not all scatters result in a net
energy loss for the DM. Thirdly, at high DM masses, there is a constant offset for all the white
dwarf masses. The offset is constant at high DM masses, but not lower DM masses. This is
because at lower DM masses other competing effects also affect the capture rate; namely for
light DM masses the ion’s kinetic energy dominates the center-of-mass energy. Still, in the
– 11 –
13. heavy DM limit the solid line does not asymptote to the dashed line, because less collisions
result in a net energy loss for the DM with the ion velocity included.
When ⟨v2
N ⟩ ≫ v2
d, the gap between our treatment which includes the zero-point energy
for the ions, and a capture treatment which assumes that the white dwarf ions are at rest,
can be significant. This is why the difference between solid and dashed lines increases from
the light to the heavy benchmark (higher density and therefore higher ⟨v2
N ⟩), as well as why
it becomes more pronounced in the case of M4 (lower DM velocity dispersion compared to
the Galactic center). In this last case, the difference can reach about two orders of magnitude
for the heavy white dwarf benchmark.
While for lower masses we expect the capture rate to be enhanced by the effects we
described above, it is also worth pointing out that we have not included any collective modes,
which can become relevant in white dwarfs for DM masses below about 100 MeV depending
on the DM particle model [21]. For our DM constraints shown shortly, we do not enter the
regime where collective effects are important, as we will focus on DM sensitivities above about
100 MeV.
3.3 Maximum Capture Rate for a Single White Dwarf
The maximum capture rate is obtained in the limit σnχ → ∞, where the white dwarf becomes
optically thick and all incoming DM particles are captured near its surface. Coincidentally,
quantum effects on the ion velocity distribution vanish near the surface because of the low
density, recovering the expression [20]
C
(max)
WD =
πR2
WDρχ
3vWDmχ
3v2
esc(RWD) + 3v2
WD + v2
d
erf
r
3
2
vWD
vd
!
+
r
6
π
vWDvd exp
−
3v2
WD
2v2
d
#
.
(3.19)
Figure 3 shows the maximum capture rate for a single white dwarf as a function of the Galactic
radius in the Milky Way Galaxy, for our three benchmark DM density profiles NFW, gNFW,
and Einasto, as labelled. We show capture rates for our two extremal benchmark white
dwarfs (see Sec. 2.2 for modeling assumptions); the range between the extremal white dwarf
benchmarks will approximately cover the expected variation in the Milky Way. The plot
illustrates the expected variation in the signal size with DM density, which is not well known
in the inner Galaxy. Our capture rates in this maximum scenario are very large, and will lead
to substantial expected fluxes above the sensitivity of existing gamma-ray telescopes, as we
will discuss shortly.
While the maximum capture rate is not technically reached until the cross section is
infinite, we can approximate what cross section corresponds to a capture rate within a few
tens of percent of the maximum. We approximate the maximum capture cross section as the
value for which CWD, as given in the optically thin limit by Eq. (3.5), equals C
(max)
WD for a given
white dwarf benchmark. If the DM capture rate at this cross section is not sufficiently large to
produce a detectable signal, increasing the cross section further will not aid detection, as the
geometric capture rate of all DM passing through has already been approximately reached.
– 12 –
14. 10-4
10-3
10-2
0.1 1 10 102
103
104
1027
1029
1031
1033
1035
1037
1039
r [ pc ]
m
χ
C
WD
(max)
[
GeV
/
s
]
���
����
�������
Figure 3. Maximum DM mass capture rate for white dwarfs as a function of the Galactocentric
radius in the Milky Way Galaxy, for DM density profiles as labelled. The shaded bands cover the
variation across the different white dwarf sizes in our benchmarks.
Because our capture rates including the ion’s zero-point energy are suppressed relative to
the treatment assuming the ions are at rest, but the maximum capture rate is unchanged,
our estimated maximum capture cross section for a given DM mass is higher than the values
computed in Ref. [20], by the inverse of such suppression factor.
4 Annihilation Flux and Gamma-Ray Detection
4.1 Dark Matter Thermalization and Annihilation Rate
The total annihilation rate of captured DM within white dwarfs depends on the annihila-
tion cross section, which determines the likelihood of two DM particles annihilating upon
interaction. It also depends on their spatial distribution inside the star, which determines
the frequency at which DM particles interact. The latter depends on the DM-nucleon cross-
section, as this quantity governs how quickly the DM can lose energy and attain equilibrium
with the object.
In the weak interaction regime we consider, the thermalization of captured DM will occur
in two stages. Initially, the DM particles will be bound to the white dwarf, with wide orbits
– 13 –
15. that intersect the object but have turning points much larger than its radius. Due to the
energy lost in each star crossing, the turning point of such orbits gradually contracts until
the DM particles are fully contained within the white dwarf volume. Even for the large
DM masses and small cross sections we probe, this first thermalization stage is completed
on a short timescale. Following the estimates of Refs. [6, 12], and choosing parameters
mχ ≃ 40 TeV and DM-nucleon cross section σnχ ≃ 7 × 10−47 cm2 which correspond to the
longest timescale in our detectable parameter space, we find the longest time for a captured
DM particle to be fully trapped inside is about 3 × 10−6 Gyr. Once this stage is complete,
further loss of energy proceeds until the DM reaches a distribution with a virial radius that
is much smaller than the white dwarf radius for the DM masses we consider.
The timescale for capture and annihilation to reach equilibrium is
teq =
s
V
⟨σannvrel⟩ CWD
, (4.1)
where V is the volume in which annihilation proceeds and ⟨σannvrel⟩ is the thermal average of
the product of annihilation cross section σann and the relative velocity of the DM particles,
vrel. We expand the annihilation cross section in partial waves ℓ as
⟨σannvrel⟩ = ⟨σannvrel⟩0
∞
X
ℓ=0
aℓ v2ℓ
rel . (4.2)
To individually analyze the contribution of each annihilation mode, we will set the coefficient
aℓ = 1 for each mode of interest while keeping the other modes equal to zero. Furthermore,
we will also conservatively set the annihilation volume equal to the full volume of our light
white dwarf (cf. Table 1), which is the largest in size amongst our benchmark white dwarfs.
The relative velocity is estimated as the average speed over one radial orbit once the DM has
been fully trapped by the white dwarf, and is of order 10−2 c for our light white dwarf. With
these considerations, the timescales for capture-annihilation equilibrium are
teq ≃
7.5 × 10−3 Gyr s-wave
0.75 Gyr
10−2 c
vrel
p-wave
(4.3)
where in all cases we have normalized ⟨σannvrel⟩0 = 3 × 10−26 cm3/s. The capture rate, on
the other hand, has been conservatively set to the lowest value for which we would get an
observable gamma-ray signal. This occurs also for a DM mass mχ ≃ 40 TeV and a DM-
nucleon cross-section σnχ ≃ 7 × 10−47 cm2, for our benchmark light white dwarf situated at
r = 1.5 pc assuming a gNFW profile (see below). For the other DM profiles, we have verified
that they produce shorter equilibration timescales. This is because although the other profiles
have lower DM densities, they correspond to larger cross sections. Therefore, comparing the
– 14 –
16. smallest cross section we reach, which occurs for the gNFW DM density profile, is the most
conservative check.
The capture-annihilation equilibrium timescales we find in Eq. (4.3) indicate that our
setup has ample sensitivity to DM models with both s- and p-wave annihilation channels. In
fact, even the d-wave channel, which is rarely testable in indirect detection searches, can reach
equilibrium for some parameters (though this does not happen at the extremal conservative
parameters). It is also worth reiterating that we have been highly conservative when making
these estimates. In particular, we expect DM annihilation to proceed within a much smaller
volume than the one we have used, leading to a much more efficient equilibration with DM
capture. Therefore, we assume the annihilation rate to be
Γann =
CWD
2
, (4.4)
where the factor 2 reflects the fact that each annihilation event depletes two DM particles.
4.2 Gamma-Ray Energy Flux
The gamma-ray energy flux from a single white dwarf is calculated as [72]
E2 dΦ
dE
WD
=
Γann
4πD2
× E2 dN
dE
× Br(ϕ → SM) × Psurv , (4.5)
where we fix D = 8 kpc as the approximate distance between the white dwarfs in the central
parsec of the Milky Way and the Earth, E2 dN
dE is the gamma-ray spectrum per DM annihila-
tion, and Br(ϕ → SM) is the branching ratio of the mediator to SM particles. The probability
of the mediator surviving to be detectable at Earth’s position, Psurv, is related to the decay
length L of the mediator by [72]
Psurv = exp
−
RWD
L
− exp
−
D
L
, (4.6)
where RWD is the radius of the white dwarf. Eq. (4.6) implies that Psurv is approximately one
for RWD ≲ L ≲ D, which spans an extreme 14 orders of magnitude range of mediator decay
lengths, so we take Psurv = 1. Other decay lengths may be probed, but will lead to decreased
sensitivity and smaller values of Psurv. We assume that the mediators escape the white dwarf
without attenuation. This is a reasonable assumption for weakly coupled mediators, which is
our scenario of interest.
To not specify a particle model, the branching ratio into photons is set to one, but other
values can still provide strong sensitivity and can be simply rescaled accordingly. For DM
annihilation into mediators that decay directly into photons, the spectrum is box shaped and
given by [73]
dN
dE
=
4
∆E
Θ(E − E−)Θ(E+ − E) , (4.7)
– 15 –
17. where Θ is the Heaviside function, ∆E = E+ − E− =
q
m2
χ − m2
ϕ and
E± =
mχ
2
1 ±
s
1 −
m2
ϕ
m2
χ
, (4.8)
where mϕ is the mass of the mediator. While our search will yield results for a wide range of
mediator masses, for demonstration purposes in our results below we will take mϕ = 10−3 mχ.
Any mediator mass leading to a decay length RWD ≲ L ≲ D will also produce Psurv ≃ 1 and so
will provide essentially identical bounds. The lower end of the box spectra does change more
notably with mediator mass, however it will still not affect the constraints if the mediator
mass corresponds to Psurv ≃ 1, as it is only the peak of the gamma-ray box spectra that sets
the bound, which is approximately the same for all boosted mediators.
Following Ref. [74], the resulting signal from the white dwarf population in the inner
Galaxy is obtained from the volume integral
E2 dΦ
dE
tot
=
Z rmax
rmin
nWD(r)
E2 dΦ
dE
WD
4πr2
dr , (4.9)
where nWD(r) is the number density of the white dwarf population at Galactic radius r as
per Eq. (2.1). We integrate from rmin = 10−4 pc to rmax = 1.5 pc. These values are chosen to
approximately match the range of the power-law number density of Ref. [32]. We emphasize
that greater sensitivity can be obtained by extrapolating the power law to Galactocentric
distances larger than 1.5 pc. In particular, our limits assuming a cored Einasto profile would
extend into the sub-GeV range in this case. To remain conservative however, we will only
integrate up to the maximum projected distance of 1.5 pc considered in Ref. [37].
4.3 Gamma-Ray Detection
The Fermi Gamma-Ray Space Telescope (Fermi), and the High Energy Stereoscopic System
(H.E.S.S.), have high-quality measurements of Galactic center gamma rays. Fermi, through
its Large Area Telescope (LAT) instrument, has good sensitivity to gamma rays up to O(100)
GeV, and so will be relevant for annihilation of DM with masses up to this energy. H.E.S.S.
is a system of imaging atmospheric Cherenkov telescopes and has sensitivity to gamma rays
with energies of a few tens of GeV up to 100 TeV, and so will be used to obtain our TeV-
scale DM sensitivity. While other gamma-ray telescopes operate in the TeV energy range,
H.E.S.S. has the best Galactic center region exposure due to its southern hemisphere location.
Other telescopes such as the High-Altitude Water Cherenkov Observatory (HAWC) and the
Very Energetic Radiation Imaging Telescope Array System (VERITAS) lie in the northern
hemisphere, and have poor exposures of the Galactic center region. Note that there are also
complementary celestial-body searches using gamma rays from the Sun, and in that case TeV
gamma rays require use of the HAWC Observatory, as atmospheric Cherenkov telescopes (like
H.E.S.S. and VERITAS) would be fried if pointed at the Sun. Fermi can be used for both
– 16 –
18. the Sun and the Galactic center region, as it has all-sky exposure, and detects gamma rays
through pair conversion.
Throughout the DM mass range we explore, the flux calculated from Eq. (4.9) is compared
to the gamma-ray flux data from Fermi and H.E.S.S observations [75]. We then exclude DM-
nucleon cross sections for which the resulting flux would be greater than the observed flux in
any energy bin, which is a very conservative limit. Modeling the astrophysical backgrounds
would provide stronger DM limits than what we present here.
5 Dark Matter Parameter Space Constraints
5.1 Results
Figure 4 shows our calculated spin-independent cross-section sensitivity as a function of DM
mass, for three Galactic DM distributions (gNFW, NFW, and Einasto). The bands for each
case illustrate the variation of these limits with the white dwarf’s physical properties, and are
detailed further below along with other uncertainties in the white dwarf modeling. We also
show current leading limits from direct detection experiments, which are LZ [76], PandaX-
4T [77], DarkSide-50 [78], and a low-mass search in Xenon-1T accounting for the Migdal
effect [79]. Depending on the DM density profile, our white dwarf bounds can outperform
these searches below 10 GeV masses as well as above a few hundred GeV. The improvement
in sensitivity is especially stark in the sub-GeV region, where direct detection sensitivity is
suppressed due to limited recoil thresholds.
In Fig. 4, the shape of the cross section limits is driven by both the capture rate scaling
with DM mass and the Galactic center gamma-ray data from Fermi and H.E.S.S.. At around
230 GeV DM mass, the kink in the curve is due to the H.E.S.S. sensitivity taking over from the
Fermi sensitivity. The dips near a few tens of TeV DM mass are due to the H.E.S.S. measured
background gamma-ray flux being particularly low at these corresponding energies, leading to
the strongest bounds. Approaching 100 TeV DM mass, the bounds weaken rapidly due to the
peak of the gamma-ray spectrum moving out of the H.E.S.S. energy detection range. The edge
of the gamma ray spectrum is still detectable, but leads to smaller fluxes and therefore weaker
constraints. Above about 10 TeV DM mass, multiscatter capture also becomes important.
However, we have conservatively only considered a single scatter formalism even in this mass
range, and so the limits rise faster than they would in a more complete treatment.
Other than white dwarfs, another celestial body population that is able to probe sub-
GeV DM through gamma-rays are brown dwarfs [74]. Our sub-GeV limits are stronger than
those derived from brown dwarfs in Ref. [74] by a few orders of magnitude in the case of
spin-independent scattering. These improvements occur due to the higher number density
of white dwarfs at the Galactic center, and the higher white dwarf capture efficiency at
lower cross sections. Note that Ref. [74] focuses on the spin-dependent scattering parameter
space. While our white dwarf limits are stronger than the spin-independent limits expected
for brown dwarfs, in the case of spin-dependent scattering the brown dwarf search in Ref. [74]
is superior. This is because spin-dependent scattering only occurs with elements which have
– 17 –
19. 0.1 1 10 102 103 104 105
10-47
10-46
10-45
10-44
10-43
10-42
10-41
10-40
10-39
10-38
10-37
mχ [ GeV ]
σ
χ
N
(
SI
)
[
cm
2
]
���
�����+��������
(���� ����)
�������
���
����
�
�
�
�
�
�
�
�
�
�
�
�
�
�
�
Figure 4. Spin-independent DM-nucleon cross-section limits derived from Fermi-LAT and H.E.S.S.
gamma-ray data using white dwarfs in the inner Milky Way, for NFW, gNFW and Einasto DM profiles
as labelled. The darker and lighter shaded regions for a given DM profile correspond to the conservative
or optimistic result respectively across our white dwarf benchmarks. Complementary constraints from
direct detection are also shown, see text for details.
non-zero nuclear spin. White dwarfs contain dominantly carbon and oxygen, which have
zero nuclear spin, leading to a negligible spin-dependent scattering rate. Therefore, whether
the white dwarf or brown dwarf population gamma-ray search provides the stronger limits
will depend on the particle physics model in question, that is whether DM exhibits spin-
independent or spin-dependent scattering. The Galactic center neutron star population was
also proposed in Ref. [74] as DM gamma-ray emitters. However, as neutron stars are much
smaller, their maximal capture rate is smaller, and they therefore only produce a sufficiently
large signal in a limited part of the DM parameter space [74].
Limits on the DM-nucleon scattering parameter space have also been calculated using
gamma rays from the Sun [72, 80–82] and Jupiter [83], and depending on the DM model
may be competitive with our limits in Fig. 4. The main benefit in using a Galactic center
population search (be it with brown dwarfs, white dwarfs, or neutron stars) compared to
a local position search is the larger range of mediator decay lengths that can be detected.
For many of the extreme decay lengths which can be probed with our search with strong
– 18 –
20. sensitivity, the corresponding Sun or Jupiter bounds do not exist. We therefore do not show
these limits in Fig. 4, as they are not directly comparable, but they should be kept in mind
as an alternative search strategy.
Compared to existing searches, our white dwarf search has other additional advantages.
These include the fact that capture-annihilation equilibrium is possible for very small cross
sections, even for highly suppressed annihilation modes such as p-wave or d-wave annihila-
tion. Another benefit of using white dwarfs over the Sun or Jupiter is the low white dwarf
evaporation mass. However, while white dwarfs can access much lower DM masses, the exact
evaporation mass is highly model dependent. For example, attractive long-range forces can
substantially decrease the DM evaporation mass [84], making Jupiter and the Sun poten-
tially competitive at even sub-MeV masses, depending on the DM model parameters. Local
position searches are also not subject to the same astrophysical uncertainties as a Galactic
center population search, however conservative choices can be made to still reveal substantial
complementary sensitivity.
It is worth reiterating that here we have assumed that the dark mediator decays directly
into gamma rays. While this is the most optimistic scenario, it is not the only possible one.
Other final states with varied branching ratios generally decrease the sensitivity. However,
given the extreme increase in cross section sensitivity we find compared to existing searches,
less optimistic scenarios will also be detectable with our search. Indeed, while we have
not specified a specific particle model for our bounds, there are a wide range that can be
applicable to this white dwarf scenario. One example is a scalar-pseudoscalar model, similar
to the one considered for the Sun in Ref. [80]. Several other applicable model examples are
also considered in the context of the Sun in Ref. [85].
5.2 Discussion of Astrophysical Uncertainties
5.2.1 Dark Matter Uncertainties
In Fig. 4, our DM density profiles cover a range of what is considered in the literature, and
illustrate that the DM density is a substantial systematic for this inner Galaxy search (as
per effectively all Milky Way indirect DM detection searches). In any case, even taking up
to about 8 orders of magnitude uncertainty in the DM density in the inner Galaxy (see
Fig. 3), across cored and cuspy profiles, we show that DM can still be probed with this
search. As expected, the cuspier profiles (gNFW and NFW) provide stronger limits than the
cored profile (Einasto), due to the greater DM density at the Galactic center predicted by
the cuspier profiles. The most conservative case is therefore given by the Einasto profile. The
bounds for this profile are shown only for DM masses above about 6 GeV, because these are
the only DM masses for which any cross section corresponds to a capture rate large enough to
be detected. However, sub-GeV sensitivity could be attained with an Einasto DM profile by
taking a less conservative approach than we do here, and integrating the white dwarf density
out to larger Galactic radii than 1.5 pc.
– 19 –
21. The most optimistic case is provided by the gNFW profile with γ = 1.5, and such cuspy
distributions are well motivated as they are commonly predicted when including baryonic
effects, i.e. adiabatic contraction. In this case, our sub-GeV limits are stronger than leading
direct detection experiments by at least ∼ 4 − 9 orders of magnitude. Even in a more
conservative case, considering the NFW profile with γ = 1, our sub-GeV bounds are stronger
than direct detection by ∼ 2 − 7 orders of magnitude. Note that while we have shown a
range of DM density profile benchmarks, these do not necessarily cover all possibilities. It is
plausible that the DM density profile is somewhat different to the cases we show here, as it
is still not robustly known or measured. However, the cases we show do cover a substantial
variation in the DM density profiles considered in the literature, and do still produce strong
sensitivity.
5.2.2 White Dwarf Uncertainties
The sensitivity bands for a given DM profile in Fig. 4 show the range of our results spanned by
the three benchmark white dwarfs we consider. These are constructed by taking the minimum
and maximum from the cross-section limits generated by each individual benchmark, where
each extreme case was obtained assuming all Galactic white dwarfs have the same physical
properties (i.e. mass, radius, central density). Our light white dwarf benchmark drives the
upper limit of the band (the most conservative case) from the sub-GeV regime up until
mχ ≃ 230 GeV. Past this value, the most conservative limits are actually drawn from our
heavy benchmark. This is because heavier white dwarfs have denser cores with larger plasma
frequencies, leading to a suppression such that the heavy benchmark is more inefficient at
capturing DM in this high mass end despite having more target nuclei. For the lower limit
of the band (the most optimistic case), constraints in the sub-GeV regime are driven by
our heavy benchmark white dwarf for masses up to mχ ≃ 3 GeV. Beyond this value, the
lower limit is determined by our intermediate benchmark, as this white dwarf configuration
is overall more effective at capturing dark matter than both the light and heavy cases (cf.
Fig. 2). This is due to the increased number of targets compared to the light benchmark,
combined with having a milder suppression compared to the heavy benchmark. More detailed
modeling and observations of the white dwarf mass distribution in the Galactic center will
lead to a reduction in the band width.
We also comment on our assumptions about the white dwarf number density distribution
in the central parsec of the Milky Way, cf. Eq. (2.1). Reported values for the power law index
α range from about 1.0 [28], to about 1.4 [32]. Within this range, our results only vary from a
few percent in the case of our Einasto profile, to about sixty percent for the gNFW profile. On
the other hand, to fix the normalization of Eq. (2.1), we used used state-of-the-art predictions
for the white dwarf abundance from Ref. [37], which incorporated recent observations of super-
solar metallicity in this region. It is worth pointing out that this estimate depends on the
initial-to-final mass relation utilized to model the star formation history. At present, only one
is available for high metallicity stars [86]. Advancements in the modeling of star formation
– 20 –
22. and evolution in this high metallicity regime will lead to more accurate determinations of the
number of stellar remnants in the future.
Finally, we discuss the impact of dark matter kinetic heating on our estimates. Depending
on the cross section and DM halo profile, we find white dwarfs in the Milky Way’s inner parsec
can be kinetically heated up to TWD ≃ 107 K. We verified that this temperature increase does
not lead to more than a few percent variation in our capture rate and thus the cross-section
limits we show in Fig. 4. We also note that this temperature increase is not significant enough
for corrections to the equation of state to become relevant for the range of white dwarf masses
and composition we consider [87].
6 Summary and Conclusions
White dwarfs are excellent DM detectors. They are incredibly dense, leading to efficient
capture for small cross sections, while also having large surface areas, leading to large capture
rates. Previous studies of DM in white dwarfs have largely focused on DM heating of white
dwarfs in globular clusters such as Messier 4, where the DM content is not well understood.
We instead targeted the Milky Way Galactic center white dwarf population, where even for
a range of DM density distributions, a substantial DM signal could arise. We explored the
scenario where DM is captured and annihilates into boosted or long-lived mediators, which can
escape the Galactic white dwarf population and decay into detectable gamma rays. We used
Fermi and H.E.S.S. Galactic center gamma-ray data to place strong limits on the resulting
gamma-ray signal, and constrained the DM-SM scattering cross section for DM masses as
low as 80 MeV. We have shown that for a cuspy halo profile, spin-independent cross section
limits from DM capture by white dwarfs can outperform direct detection limits by up to nine
orders of magnitude for sub-GeV DM masses. Above a few hundred GeV, our white dwarf
limits for that same halo profile are also stronger than world-leading direct detection limits.
We also presented an improved treatment of the DM capture rate in white dwarfs, which
accounts for quantum effects of the ions when the white dwarf temperature falls below the ion
plasma frequency. The zero-point motion of the ions in this regime results in a significantly
higher velocity compared to the usual thermal estimate used in previous works. We then
showed that this effect produces lower capture rates in the Galactic center by a factor of up
to about five in our DM mass range, depending on the white dwarf mass. While the focus of
our work was on DM in Galactic center white dwarfs, DM in globular cluster white dwarfs
have been often considered in the literature. The capture framework we discussed in this work
is also applicable to those results – for globular clusters, the difference between our treatment
and neglecting the ion thermal velocity is even larger, due to the DM velocity dispersion often
being very low in globular clusters, and therefore the ion velocity being potentially larger than
the DM velocity. For the example case of the commonly considered M4 globular cluster, we
found that our improved ion velocity treatment leads to DM capture rates up to two orders
of magnitude smaller than was previously considered.
– 21 –
23. In the future, sensitivities for DM searches in white dwarfs will be improved with advances
in our understanding of the DM content both in our galaxy and in globular clusters. Our
strongest constraints assume that the center of the Milky Way is very DM rich, but the
systematic uncertainty is high given the extensive range of possible DM density profiles.
Although our sensitivity is strong for a range of DM profiles, an improved understanding
of the DM density in our galaxy could reduce the uncertainty in our cross section limits by
several orders of magnitude. It is also possible that better understanding the DM content in
globular clusters could lead to improved sensitivity of both white dwarf heating and gamma-
ray signals. In particular, a positive DM detection is possible if new clusters with high DM
densities are discovered nearby, and any anomalous signals from gamma rays or heating were
found. Another possibility for future work is to take advantage of nearby individual white
dwarfs, which could lead to strong DM sensitivity.
Acknowledgments
We thank Joseph Bramante, Christopher Cappiello, Zhuo Chen, Bernhard Mistlberger, Juri
Smirnov, and Aaron Vincent for helpful discussions. JFA, RKL, and LSO are supported
in part by the U.S. Department of Energy under Contract DE-AC02-76SF00515. LSO is
supported by a Stanford Physics Department Fellowship.
A Velocity Distribution for Ions in Cold White Dwarfs
We derive the momentum distribution of the white dwarf ions at finite temperature, Eq. (A.5),
starting from the expression (see e.g. Ref. [88])
Fion(vN ) = Z−1
X
n
|⟨vN |n⟩|2
exp (−En/TWD) , (A.1)
where TWD is the white dwarf temperature, and the sum is over all energy eigenstates En. We
approximate the latter by those of a harmonic oscillator potential with a natural frequency
equal to the ion plasma frequency ωp of the medium, whereby |n⟩ = |nx, ny, nz⟩. This
approximation is valid for white dwarfs sufficiently cold that their temperature is below ωp.
In this thermodynamic state, the velocity dispersion of nuclei is determined by the energy
scale ωp rather than the temperature, as we show shortly. Note that Fion(vN ) will be only a
function of vN = |vN |. The partition function Z is
Z =
X
n
exp (−En/TWD) =
exp (−3ωp/2TWD)
(1 − exp(−ωp/TWD))3 . (A.2)
The squared matrix elements read
|⟨vN |n⟩|2
=
mN
πωp
3/2 Y
j=x,y,z
1
2nj nj!
H2
nj
r
mN
ωp
vj
exp
−
mN
ωp
v2
j
, (A.3)
– 22 –
24. 0 1 2 3 4 5
0
40
80
120
160
200
vN [ 10-3
c ]
v
N
2
ℱ
ion
(
v
N
)
[
c
-1
]
�������
���������
��� = ���
�
��� = ���
�
��� = � � ���
�
��� = ��� � ���
�
0 1 2 3 4 5
0
40
80
120
160
200
vN [ 10-3
c ]
v
N
2
ℱ
ion
(
v
N
)
[
c
-1
]
����� �����
������
��� ≲ ���
�
��� = � � ���
�
��� = ��� � ���
�
Figure 5. Left: Speed probability density of the white dwarf ions in the stellar rest frame using the
classical Maxwell-Boltzmann distribution, assuming a pure carbon composition for temperatures as
specified. This is the classical picture. Right: Same as left panel, but including the ion’s zero-point
motion (as per Eq. (A.5)) for an ion density of order 107
g/cm3
. This is the quantum picture.
where the functions Hn(x) are Hermite polynomials of order n. The sum in Eq. (A.1) can be
computed exactly by making use of the following completeness relation for Hermite polyno-
mials (see p. 194 of Ref. [89])
∞
X
n=0
Hn(x)Hn(y)
2n n!
zn
= 1 − z2
−1/2
exp
2z
1 + z
xy −
z2
1 − z2
(x − y)2
, (A.4)
with the identifications z = exp(−ωp/TWD) and x = y =
p
mN /ωp vj for each separate
component j. Factorizing the sum into each cartesian component and using the above identity
we obtain the distribution
Fion(vN ) =
mN
πωp coth (ωp/2TWD)
3/2
exp
−
mN v2
N
ωp coth (ωp/2TWD)
, (A.5)
with a mean squared velocity
⟨v2
N ⟩ = 4π
Z ∞
0
dvN v4
N Fion(vN ) =
3ωp
2mN
coth
ωp
2TWD
. (A.6)
Note that the ion plasma frequency depends on the local ion density, cf. Eq. (3.2). Thus,
for old white dwarfs in the inner Galaxy, most of their volume will satisfy TWD ≪ ωp except
very near the surface. In the regions where the plasma frequency dominates over temperature,
– 23 –
25. only the ground state contributes to the sum in Eq. (A.1), yielding
Fion(vN ) −
−
−
−
−
−
→
TWD ≪ ωp
mN
πωp
3/2
exp
−
mN v2
N
ωp
, (A.7)
with a mean squared velocity
⟨v2
N ⟩ −
−
−
−
−
−
→
TWD ≪ ωp
3ωp
2mN
. (A.8)
Thus, the ion velocity distribution for old white dwarfs can be thought of being like a Maxwell-
Boltzmann, but the plasma frequency replaces the temperature as the energy scale.
As a final consistency check, note that in the limit that quantum effects are irrelevant,
which will occur near the surface of the white dwarf, the above distribution asymptotes to a
classical Maxwell-Boltzmann distribution
Fion(vN ) −
−
−
−
−
−
→
TWD ≫ ωp
mN
2πTWD
3/2
exp
−
mN v2
N
2TWD
, (A.9)
with the mean squared velocity matching that of Ref. [20],
⟨v2
N ⟩ −
−
−
−
−
−
→
TWD ≫ ωp
3TWD
mN
. (A.10)
Figure 5 illustrates how our distribution, Eq. (A.5), converges to the classical Maxwell-
Boltzmann distribution given by Eq. (A.9) as the temperature increases, for a fiducial density
ρWD = 107 g/cm3. In consistency with the above, at high temperatures both distributions
align closely. However, as the temperature decreases, Eq. (3.3) exhibits a significantly broader
spread compared to the classical Maxwell-Boltzmann distribution. This is because the plasma
frequency serves as a lower bound on the energy scale of the white dwarf ions.
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