This document summarizes an analysis of X-ray spectra from the Andromeda galaxy and Perseus galaxy cluster observed with the XMM-Newton X-ray observatory. The analysis identified a weak unidentified line at an energy of approximately 3.5 keV in the spectra of both objects. The line strength increases towards the centers of the objects and is stronger in Perseus than in Andromeda. The line properties are consistent with originating from the decay of dark matter particles, though an instrumental or astrophysical source cannot be ruled out based on individual objects. Future detections or non-detections in additional targets could help reveal the nature of this line.
Detection of an_unindentified_emission_line_in_the_stacked_x_ray_spectrum_of_...Sérgio Sacani
1. Researchers detected a previously unknown emission line in the stacked X-ray spectrum of 73 galaxy clusters observed by XMM-Newton. 2. The line was detected at an energy of 3.55-3.57 keV and was seen independently in subsamples of clusters. 3. The line was also detected in Chandra observations of the Perseus cluster but not in observations of the Virgo cluster. 4. The nature of this line is unclear - it could be a thermal line from an undetected element, or potentially the decay line of a hypothesized dark matter particle called a sterile neutrino. Further observations are needed to determine the origin of the line.
Detection of an_unidentified_emission_line_in_the_stacked_xray_spectrum_of_ga...Sérgio Sacani
This document describes the detection of an unidentified emission line in the stacked X-ray spectrum of 73 galaxy clusters observed by XMM-Newton. The line was detected at an energy of 3.55-3.57 keV in independent analyses of the MOS and PN instruments. The line was also seen in Chandra observations of the Perseus cluster. Possible explanations discussed include an atomic transition in thermal plasma, or the decay of sterile neutrino dark matter particles. However, the origin is unclear and requires further observation.
1) Researchers observed 15 transits of the exoplanet GJ 1214b using the Hubble Space Telescope to measure its transmission spectrum from 1.1 to 1.7 microns.
2) The transmission spectrum was featureless, inconsistent with cloud-free atmospheres dominated by water, methane, carbon monoxide, nitrogen, or carbon dioxide.
3) The most likely explanation for the featureless spectrum is the presence of high-altitude clouds in the planet's atmosphere, which block the transmission of stellar light through the lower atmosphere.
This document summarizes a research article that develops a theoretical model to describe how decoherence effects rubidium vapor in an electromagnetically induced transparency (EIT) experiment. The model accounts for decoherence from both dephasing and population relaxation. It quantifies the impact of decoherence on various experimental measurements, including Faraday rotation, susceptibility, transmission, and coherence relationships. The model is in good agreement with previous experimental results. It also discusses how the model could be applied to other EIT-based experiments and how Faraday rotation could be used to detect single atoms.
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.
Supermassive black holes in galaxy centres can grow by the accretion
of gas, liberating enormous amounts of energy that might
regulate star formation on galaxy-wide scales1–3
. The nature of
gaseous fuel reservoirs that power black hole growth is nevertheless
largely unconstrained by observations, and is instead routinely
simplified as a smooth, spherical inflow of very hot gas
in accordance with the Bondi solution4
. Recent theory5–7 and
simulations8–10 instead predict that accretion can be dominated by
a stochastic, clumpy distribution of very cold molecular clouds,
though unambiguous observational support for this prediction remains
elusive. Here we show observational evidence for a cold,
clumpy accretion flow toward a supermassive black hole fuel reservoir
in the nucleus of the Abell 2597 Brightest Cluster Galaxy
(BCG), a nearby (z = 0.0821) giant elliptical galaxy surrounded
by a dense halo of hot plasma11–13. Under the right conditions,
thermal instabilities can precipitate from this hot gas, producing a
rain of cold clouds that fall toward the galaxy’s centre14, sustaining
star formation amid a kiloparsec-scale molecular nebula that inhabits
its core15. New interferometric sub-millimetre observations
show that these cold clouds also fuel black hole accretion, revealing
“shadows” cast by molecular clouds as they move inward at ∼ 300
km s−1
toward the active supermassive black hole in the galaxy
centre, which serves as a bright backlight. Corroborating evidence
from prior observations16 of warmer atomic gas at extremely high
spatial resolution17, along with simple arguments based on geometry
and probability, indicates that these clouds are within the innermost
hundred parsecs of the black hole, and falling closer toward
it
Laser Pulsing in Linear Compton ScatteringTodd Hodges
This document summarizes a method for calculating the energy spectrum of radiation produced in linear Compton scattering, accounting for the pulsed structure of the incident laser beam. The method involves performing a Lorentz transformation of the Klein-Nishina scattering cross section to calculate the emission from individual electrons in an electron beam, and then summing over all electrons to obtain the total energy spectrum. This approach allows for accurate modeling of effects of electron beam energy spread and emittance. The method is then applied to predict the photon spectrum from a proposed compact inverse Compton scattering x-ray source at Old Dominion University.
Detection of an_unindentified_emission_line_in_the_stacked_x_ray_spectrum_of_...Sérgio Sacani
1. Researchers detected a previously unknown emission line in the stacked X-ray spectrum of 73 galaxy clusters observed by XMM-Newton. 2. The line was detected at an energy of 3.55-3.57 keV and was seen independently in subsamples of clusters. 3. The line was also detected in Chandra observations of the Perseus cluster but not in observations of the Virgo cluster. 4. The nature of this line is unclear - it could be a thermal line from an undetected element, or potentially the decay line of a hypothesized dark matter particle called a sterile neutrino. Further observations are needed to determine the origin of the line.
Detection of an_unidentified_emission_line_in_the_stacked_xray_spectrum_of_ga...Sérgio Sacani
This document describes the detection of an unidentified emission line in the stacked X-ray spectrum of 73 galaxy clusters observed by XMM-Newton. The line was detected at an energy of 3.55-3.57 keV in independent analyses of the MOS and PN instruments. The line was also seen in Chandra observations of the Perseus cluster. Possible explanations discussed include an atomic transition in thermal plasma, or the decay of sterile neutrino dark matter particles. However, the origin is unclear and requires further observation.
1) Researchers observed 15 transits of the exoplanet GJ 1214b using the Hubble Space Telescope to measure its transmission spectrum from 1.1 to 1.7 microns.
2) The transmission spectrum was featureless, inconsistent with cloud-free atmospheres dominated by water, methane, carbon monoxide, nitrogen, or carbon dioxide.
3) The most likely explanation for the featureless spectrum is the presence of high-altitude clouds in the planet's atmosphere, which block the transmission of stellar light through the lower atmosphere.
This document summarizes a research article that develops a theoretical model to describe how decoherence effects rubidium vapor in an electromagnetically induced transparency (EIT) experiment. The model accounts for decoherence from both dephasing and population relaxation. It quantifies the impact of decoherence on various experimental measurements, including Faraday rotation, susceptibility, transmission, and coherence relationships. The model is in good agreement with previous experimental results. It also discusses how the model could be applied to other EIT-based experiments and how Faraday rotation could be used to detect single atoms.
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.
Supermassive black holes in galaxy centres can grow by the accretion
of gas, liberating enormous amounts of energy that might
regulate star formation on galaxy-wide scales1–3
. The nature of
gaseous fuel reservoirs that power black hole growth is nevertheless
largely unconstrained by observations, and is instead routinely
simplified as a smooth, spherical inflow of very hot gas
in accordance with the Bondi solution4
. Recent theory5–7 and
simulations8–10 instead predict that accretion can be dominated by
a stochastic, clumpy distribution of very cold molecular clouds,
though unambiguous observational support for this prediction remains
elusive. Here we show observational evidence for a cold,
clumpy accretion flow toward a supermassive black hole fuel reservoir
in the nucleus of the Abell 2597 Brightest Cluster Galaxy
(BCG), a nearby (z = 0.0821) giant elliptical galaxy surrounded
by a dense halo of hot plasma11–13. Under the right conditions,
thermal instabilities can precipitate from this hot gas, producing a
rain of cold clouds that fall toward the galaxy’s centre14, sustaining
star formation amid a kiloparsec-scale molecular nebula that inhabits
its core15. New interferometric sub-millimetre observations
show that these cold clouds also fuel black hole accretion, revealing
“shadows” cast by molecular clouds as they move inward at ∼ 300
km s−1
toward the active supermassive black hole in the galaxy
centre, which serves as a bright backlight. Corroborating evidence
from prior observations16 of warmer atomic gas at extremely high
spatial resolution17, along with simple arguments based on geometry
and probability, indicates that these clouds are within the innermost
hundred parsecs of the black hole, and falling closer toward
it
Laser Pulsing in Linear Compton ScatteringTodd Hodges
This document summarizes a method for calculating the energy spectrum of radiation produced in linear Compton scattering, accounting for the pulsed structure of the incident laser beam. The method involves performing a Lorentz transformation of the Klein-Nishina scattering cross section to calculate the emission from individual electrons in an electron beam, and then summing over all electrons to obtain the total energy spectrum. This approach allows for accurate modeling of effects of electron beam energy spread and emittance. The method is then applied to predict the photon spectrum from a proposed compact inverse Compton scattering x-ray source at Old Dominion University.
The open cluster_ngc6520_and_the_nearby_dark_molecular_cloud_barnard_86Sérgio Sacani
This document presents optical photometry and CO observations of the open cluster NGC 6520 and nearby dark molecular cloud Barnard 86. Analysis of the optical data finds the cluster radius is 1.0±0.5 arcmin, smaller than previous estimates. The cluster age is estimated to be 150±50 Myr with reddening of EB−V =0.42±0.10. The distance from the Sun is estimated to be 1900±100 pc, larger than previous estimates. CO observations are used to derive basic properties of Barnard 86 under the assumption it lies at the same distance as the cluster.
1. This document describes a multiwavelength campaign on the Seyfert 1 galaxy Mrk 509 using five satellites and two ground-based facilities.
2. The campaign aims to study several open questions about active galactic nuclei (AGN), including the location and physics of outflows from AGN, the nature of continuum emission, the geometry and physical state of the X-ray broad emission line region, and the Fe-K line complex.
3. The observations cover more than five decades in frequency, from 2 μm to 200 keV, and include a simultaneous set of deep XMM-Newton and INTEGRAL observations over seven weeks. This allows the authors to disentangle different components and study time variability
The Internal Structure of Asteroid (25143) Itokawa as Revealed by Detection o...WellingtonRodrigues2014
- The authors detected an acceleration in the rotation rate of asteroid (25143) Itokawa through photometric observations spanning 2001 to 2013.
- By measuring rotational phase offsets between observed and modeled lightcurves, they found a YORP acceleration of 3.54 ± 0.38 × 10−8 rad day−2, equivalent to a decrease in the asteroid's rotation period of about 45 ms per year.
- Thermophysical modeling of the detailed shape model from the Hayabusa spacecraft could not reconcile the observed YORP strength unless the asteroid's center of mass is shifted by about 21 m along its long axis. This suggests Itokawa has two components with different densities that merged, either from a
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.
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.
Topology of charge density from pseudopotential density functional theory cal...Alexander Decker
nl
2(2l + 1)Rnl2 (r )
(6)
n,l
The document discusses the challenges of determining the topology of charge density from pseudopotential density functional theory calculations due to the absence of core electrons. Specifically, it notes that pseudopotential calculations lack critical points at nuclear positions defined by core electrons. To address this, the document examines methods to reconstruct the correct topology, such as adding an isolated atomic core density or using orthogonalized core orbitals. It also provides background on the quantum theory of atoms in molecules and defines key concepts like critical points, atomic basins, and charge density topology. Results are reported for several molecules to analyze
Structural, electronic, elastic, optical and thermodynamical properties of zi...Alexander Decker
nl
2(2l + 1)Rnl2 (r )
(6)
n,l
The document discusses the challenges of determining the topology of charge density from pseudopotential density functional theory calculations due to the absence of core electrons. Specifically, it notes that pseudopotential calculations lack critical points at nuclear positions where core electrons have been removed. To address this, the document examines methods to reconstruct the correct topology, such as adding back core densities or using orthogonalized densities. It also explores analyzing charge density topology using Bader's Quantum Theory of Atoms in Molecules and discusses applications to molecules like alanine.
An advanced DFT based methodology applied to
(VASP, Quantum Espresso, WIEN2K)
1) higher atomic number containing complex oxides to understand metal to insulator transition.
2) when we add d electron containing atoms (e.g. iron, cobalt etc.) on oxide surfaces they exhibit surprises
In both the cases, this work shows how to complement experiment by theory
The ASTRODEEP Frontier Fields catalogues II. Photometric redshifts and rest f...Sérgio Sacani
This document describes a public release of photometric redshifts and galaxy properties from multi-wavelength data in the Abell-2744 and MACS-J0416 galaxy cluster fields observed as part of the Frontier Fields program. Photometric redshifts were estimated using six different methods and have an accuracy of 3-5%. Accounting for gravitational lensing magnification, the H-band number counts agree with CANDELS at bright magnitudes but extend to intrinsically fainter galaxies of H=32-33. The Frontier Fields data allow probing galaxy stellar masses 0.5-1.5 dex lower than in wide fields, including sources with masses of 107-108 solar masses at z>5. Star formation rates can be detected 1
Science with small telescopes - exoplanetsguest8aa6ebb
The search for extrasolar planets has become one of the most attractive problems in modern astrophysics. The biggest observatories in the world are involved in this task as well as little amateur instruments. There is also a huge variety of astronomical methods used for their investigation. Here I present the projects for searching for exoplanets by transit method and our observations of the planet WASP-2b. We observed a transit on 3/4 August 2008 with a 354 mm Schmidt-Cassegrain Celestron telescope and CCD SBIG STL 11000M camera. By precise photometry made using MaximDL software we obtained the light curve of the star system. Decrease of brightness by 0.02m is detected. Analyzing our data we estimate the radius of the planet and inclination of its orbit. Our results are in good correlation with the published information in literature.
1. This paper presents results from a 600 ks XMM-Newton observation of Mrk 509 as part of a large multiwavelength campaign.
2. The high quality spectrum allows an unprecedented investigation of the ionized outflow through the detection of multiple absorption lines.
3. The outflow is found to consist of at least two velocity components that have been observed previously, as well as a tentative high velocity component. Discrete ionization components are detected spanning four orders of magnitude in ionization parameter.
1) The document reports on optical spectroscopic monitoring of the ultraluminous X-ray source M 101 ULX-1.
2) Analysis revealed the companion is a Wolf-Rayet star in an 8.2 day orbit around a black hole with a minimum mass of 5 solar masses.
3) M 101 ULX-1 has an exceptionally soft X-ray spectrum that violates expectations for accretion onto stellar-mass black holes, challenging current models of ultraluminous X-ray sources.
This document presents a study using density functional theory calculations to examine the adsorption of titanium dioxide nanostructures on pure and functionalized single-walled carbon nanotubes. The study finds that TiO2 nanostructures preferentially adsorb to chemical adsorption sites on functionalized SWCNTs, such as epoxy, alcohol, and carboxylate sites, compared to physical adsorption sites on pure SWCNTs, such as top, bridge, and hollow sites. Partial density of states calculations and charge density maps provide insight into the electronic structure and charge transfer between TiO2 nanostructures and SWCNTs. The results provide a theoretical understanding of controlled growth mechanisms of TiO2 nanostructures on carbon nanotube substrates.
Dynamical dark energy in light of the latest observationsSérgio Sacani
A flat Friedmann–Robertson–Walker universe dominated by a cosmological constant (Λ) and cold dark matter (CDM) has been the working model preferred by cosmologists since the discovery of cosmic acceleration1,2. However, tensions of various degrees of significance are known to be present among existing datasets within the ΛCDM framework3–11. In particular, the Lyman-α forest measurement of the baryon acoustic oscillations (BAO) by the Baryon Oscillation Spectroscopic Survey3 prefers a smaller value of the matter density fraction ΩM than that preferred by cosmic microwave background (CMB). Also, the recently measured value of the Hubble constant, H0 = 73.24 ± 1.74 km s−1 Mpc−1 (ref. 12), is 3.4σ higher than the 66.93 ± 0.62 km s−1 Mpc−1 inferred from the Planck CMB data7. In this work, we investigate whether these tensions can be interpreted as evidence for a non-constant dynamical dark energy. Using the Kullback–Leibler divergence13 to quantify the tension between datasets, we find that the tensions are relieved by an evolving dark energy, with the dynamical dark energy model preferred at a 3.5σ significance level based on the improvement in the fit alone. While, at present, the Bayesian evidence for the dynamical dark energy is insufficient to favour it over ΛCDM, we show that, if the current best-fit dark energy happened to be the true model, it would be decisively detected by the upcoming Dark Energy Spectroscopic Instrument survey14.
A massive protocluster of galaxies at a redshift of z<5.3Sérgio Sacani
This document describes the discovery of a massive protocluster of galaxies located approximately 1 billion years after the Big Bang (redshift of z=5.3). The protocluster contains overdense regions of massive galaxies extending over 13 megaparsecs. It contains an extremely luminous starburst galaxy with large molecular gas reserves and a luminous quasar. Together, these objects place a minimum total mass of over 4×1011 solar masses in this early cluster, consistent with cosmological simulations of the earliest galaxy clusters. This discovery provides evidence for the hierarchical formation of massive structures in the early universe.
This document describes a theoretical study of graphene membrane rupture under strong electric fields using molecular dynamics simulations. The study examined pristine and defective graphene membranes of various sizes under electric fields of varying strengths, both with and without ion bombardment, to determine the cause of experimental membrane ruptures. The simulations found that electric fields alone did not rupture membranes. Ion bombardment was shown to be able to rupture membranes if ions possessed kinetic energies of approximately 0.7 electronvolts upon impact. Sequential ion bombardment, mimicking experimental conditions, was also found to potentially rupture membranes through accumulated damage.
Quantum jumps of light recording the birth and death of a photon in a cavityGabriel O'Brien
This document summarizes an experiment that observed quantum jumps in the photon number inside a superconducting cavity. Key points:
- Microwave photons were stored in a superconducting cavity for up to half a second and repeatedly probed by non-absorbing atoms passing through.
- An atom interferometer measured the atomic phase shift induced by the non-resonant cavity field, revealing the presence or absence of a single photon.
- Sequences of hundreds of correlated atom measurements were interrupted by sudden changes, recording the creation and destruction of individual photons over time.
- This realized a quantum non-demolition measurement of the photon number in the cavity in real time, allowing observation of its
This document summarizes research verifying simulations of a novel muon radiography detector system through experimentation. It estimates the detector's spatial resolution as 9.32mm, better than the 1cm reported previously. It also explores the detector's imaging potential through both simulation and initial promising experimental results. The document provides background on muon production, tomography using scattering angles, and radiography using transmission measurements. It describes common detector types and current applications like border security using large-scale muon tomography to detect nuclear materials more effectively than gamma-ray systems.
In search of multipath interference using large moleculesGabriel O'Brien
This document summarizes an experiment that tested the quantum mechanical principle of superposition using large dye molecules. The experiment measured interference patterns when the molecules passed through single, double, and triple slits. It observed less than 1% deviation from the expected interference patterns based on quantum mechanics, providing evidence that the superposition principle applies even to massive particles like these large molecules. The experiment is one of the first to directly observe quantum interference using massive particles rather than light or single particles.
Unknown 2019 - expand “explorations at and beyond the neutron dripline ”LinhBui343479
The EXPAND project aims to investigate the structure of light neutron-rich nuclei near and beyond the neutron dripline using the RIBF facility at RIKEN. It focuses on augmenting the neutron detection capabilities of the existing SAMURAI setup by transforming the two-wall NEBULA array into the NEBULA-Plus four-wall array. This will enable the routine detection of 3 and 4 neutrons and significantly increase single and two-neutron detection efficiencies. The project has faced delays and budget issues but now plans to equip 60-70 of the 90 acquired scintillator modules for NEBULA-Plus within the existing budget to provide significant gains in neutron detection capabilities.
Alma observations of_feeding_and_feedback_in_nearby_seyfert_galaxies_outflow_...Sérgio Sacani
ALMA observations of the Seyfert 2 galaxy NGC 1433 reveal a nuclear gaseous spiral structure within a nuclear ring encircling a nuclear stellar bar. Near the nucleus, there is intense high-velocity CO emission interpreted as an AGN-driven molecular outflow. The outflow involves a molecular mass of 3.6 million solar masses and a flow rate of about 7 solar masses per year. Continuum emission at the center is likely thermal dust emission from a molecular torus expected in this Seyfert 2 galaxy. The observations probe gas dynamics within 24 parsecs of the active galactic nucleus.
This document summarizes a detonating failed deflagration model of Type Ia supernovae. The model involves an off-center deflagration in a massive white dwarf that fails to unbind the star. Disturbances from the failed deflagration pollute the stellar surface and eventually evolve into isolated shock regions, serving as ignition points for detonations that result in supernova explosion. Preliminary results show ejecta composed of silicon and iron group elements, with an inner egg-shaped region surrounded by an incomplete burning shell. Explosion energies are around 1.3-1.5×1051 erg.
The open cluster_ngc6520_and_the_nearby_dark_molecular_cloud_barnard_86Sérgio Sacani
This document presents optical photometry and CO observations of the open cluster NGC 6520 and nearby dark molecular cloud Barnard 86. Analysis of the optical data finds the cluster radius is 1.0±0.5 arcmin, smaller than previous estimates. The cluster age is estimated to be 150±50 Myr with reddening of EB−V =0.42±0.10. The distance from the Sun is estimated to be 1900±100 pc, larger than previous estimates. CO observations are used to derive basic properties of Barnard 86 under the assumption it lies at the same distance as the cluster.
1. This document describes a multiwavelength campaign on the Seyfert 1 galaxy Mrk 509 using five satellites and two ground-based facilities.
2. The campaign aims to study several open questions about active galactic nuclei (AGN), including the location and physics of outflows from AGN, the nature of continuum emission, the geometry and physical state of the X-ray broad emission line region, and the Fe-K line complex.
3. The observations cover more than five decades in frequency, from 2 μm to 200 keV, and include a simultaneous set of deep XMM-Newton and INTEGRAL observations over seven weeks. This allows the authors to disentangle different components and study time variability
The Internal Structure of Asteroid (25143) Itokawa as Revealed by Detection o...WellingtonRodrigues2014
- The authors detected an acceleration in the rotation rate of asteroid (25143) Itokawa through photometric observations spanning 2001 to 2013.
- By measuring rotational phase offsets between observed and modeled lightcurves, they found a YORP acceleration of 3.54 ± 0.38 × 10−8 rad day−2, equivalent to a decrease in the asteroid's rotation period of about 45 ms per year.
- Thermophysical modeling of the detailed shape model from the Hayabusa spacecraft could not reconcile the observed YORP strength unless the asteroid's center of mass is shifted by about 21 m along its long axis. This suggests Itokawa has two components with different densities that merged, either from a
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.
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.
Topology of charge density from pseudopotential density functional theory cal...Alexander Decker
nl
2(2l + 1)Rnl2 (r )
(6)
n,l
The document discusses the challenges of determining the topology of charge density from pseudopotential density functional theory calculations due to the absence of core electrons. Specifically, it notes that pseudopotential calculations lack critical points at nuclear positions defined by core electrons. To address this, the document examines methods to reconstruct the correct topology, such as adding an isolated atomic core density or using orthogonalized core orbitals. It also provides background on the quantum theory of atoms in molecules and defines key concepts like critical points, atomic basins, and charge density topology. Results are reported for several molecules to analyze
Structural, electronic, elastic, optical and thermodynamical properties of zi...Alexander Decker
nl
2(2l + 1)Rnl2 (r )
(6)
n,l
The document discusses the challenges of determining the topology of charge density from pseudopotential density functional theory calculations due to the absence of core electrons. Specifically, it notes that pseudopotential calculations lack critical points at nuclear positions where core electrons have been removed. To address this, the document examines methods to reconstruct the correct topology, such as adding back core densities or using orthogonalized densities. It also explores analyzing charge density topology using Bader's Quantum Theory of Atoms in Molecules and discusses applications to molecules like alanine.
An advanced DFT based methodology applied to
(VASP, Quantum Espresso, WIEN2K)
1) higher atomic number containing complex oxides to understand metal to insulator transition.
2) when we add d electron containing atoms (e.g. iron, cobalt etc.) on oxide surfaces they exhibit surprises
In both the cases, this work shows how to complement experiment by theory
The ASTRODEEP Frontier Fields catalogues II. Photometric redshifts and rest f...Sérgio Sacani
This document describes a public release of photometric redshifts and galaxy properties from multi-wavelength data in the Abell-2744 and MACS-J0416 galaxy cluster fields observed as part of the Frontier Fields program. Photometric redshifts were estimated using six different methods and have an accuracy of 3-5%. Accounting for gravitational lensing magnification, the H-band number counts agree with CANDELS at bright magnitudes but extend to intrinsically fainter galaxies of H=32-33. The Frontier Fields data allow probing galaxy stellar masses 0.5-1.5 dex lower than in wide fields, including sources with masses of 107-108 solar masses at z>5. Star formation rates can be detected 1
Science with small telescopes - exoplanetsguest8aa6ebb
The search for extrasolar planets has become one of the most attractive problems in modern astrophysics. The biggest observatories in the world are involved in this task as well as little amateur instruments. There is also a huge variety of astronomical methods used for their investigation. Here I present the projects for searching for exoplanets by transit method and our observations of the planet WASP-2b. We observed a transit on 3/4 August 2008 with a 354 mm Schmidt-Cassegrain Celestron telescope and CCD SBIG STL 11000M camera. By precise photometry made using MaximDL software we obtained the light curve of the star system. Decrease of brightness by 0.02m is detected. Analyzing our data we estimate the radius of the planet and inclination of its orbit. Our results are in good correlation with the published information in literature.
1. This paper presents results from a 600 ks XMM-Newton observation of Mrk 509 as part of a large multiwavelength campaign.
2. The high quality spectrum allows an unprecedented investigation of the ionized outflow through the detection of multiple absorption lines.
3. The outflow is found to consist of at least two velocity components that have been observed previously, as well as a tentative high velocity component. Discrete ionization components are detected spanning four orders of magnitude in ionization parameter.
1) The document reports on optical spectroscopic monitoring of the ultraluminous X-ray source M 101 ULX-1.
2) Analysis revealed the companion is a Wolf-Rayet star in an 8.2 day orbit around a black hole with a minimum mass of 5 solar masses.
3) M 101 ULX-1 has an exceptionally soft X-ray spectrum that violates expectations for accretion onto stellar-mass black holes, challenging current models of ultraluminous X-ray sources.
This document presents a study using density functional theory calculations to examine the adsorption of titanium dioxide nanostructures on pure and functionalized single-walled carbon nanotubes. The study finds that TiO2 nanostructures preferentially adsorb to chemical adsorption sites on functionalized SWCNTs, such as epoxy, alcohol, and carboxylate sites, compared to physical adsorption sites on pure SWCNTs, such as top, bridge, and hollow sites. Partial density of states calculations and charge density maps provide insight into the electronic structure and charge transfer between TiO2 nanostructures and SWCNTs. The results provide a theoretical understanding of controlled growth mechanisms of TiO2 nanostructures on carbon nanotube substrates.
Dynamical dark energy in light of the latest observationsSérgio Sacani
A flat Friedmann–Robertson–Walker universe dominated by a cosmological constant (Λ) and cold dark matter (CDM) has been the working model preferred by cosmologists since the discovery of cosmic acceleration1,2. However, tensions of various degrees of significance are known to be present among existing datasets within the ΛCDM framework3–11. In particular, the Lyman-α forest measurement of the baryon acoustic oscillations (BAO) by the Baryon Oscillation Spectroscopic Survey3 prefers a smaller value of the matter density fraction ΩM than that preferred by cosmic microwave background (CMB). Also, the recently measured value of the Hubble constant, H0 = 73.24 ± 1.74 km s−1 Mpc−1 (ref. 12), is 3.4σ higher than the 66.93 ± 0.62 km s−1 Mpc−1 inferred from the Planck CMB data7. In this work, we investigate whether these tensions can be interpreted as evidence for a non-constant dynamical dark energy. Using the Kullback–Leibler divergence13 to quantify the tension between datasets, we find that the tensions are relieved by an evolving dark energy, with the dynamical dark energy model preferred at a 3.5σ significance level based on the improvement in the fit alone. While, at present, the Bayesian evidence for the dynamical dark energy is insufficient to favour it over ΛCDM, we show that, if the current best-fit dark energy happened to be the true model, it would be decisively detected by the upcoming Dark Energy Spectroscopic Instrument survey14.
A massive protocluster of galaxies at a redshift of z<5.3Sérgio Sacani
This document describes the discovery of a massive protocluster of galaxies located approximately 1 billion years after the Big Bang (redshift of z=5.3). The protocluster contains overdense regions of massive galaxies extending over 13 megaparsecs. It contains an extremely luminous starburst galaxy with large molecular gas reserves and a luminous quasar. Together, these objects place a minimum total mass of over 4×1011 solar masses in this early cluster, consistent with cosmological simulations of the earliest galaxy clusters. This discovery provides evidence for the hierarchical formation of massive structures in the early universe.
This document describes a theoretical study of graphene membrane rupture under strong electric fields using molecular dynamics simulations. The study examined pristine and defective graphene membranes of various sizes under electric fields of varying strengths, both with and without ion bombardment, to determine the cause of experimental membrane ruptures. The simulations found that electric fields alone did not rupture membranes. Ion bombardment was shown to be able to rupture membranes if ions possessed kinetic energies of approximately 0.7 electronvolts upon impact. Sequential ion bombardment, mimicking experimental conditions, was also found to potentially rupture membranes through accumulated damage.
Quantum jumps of light recording the birth and death of a photon in a cavityGabriel O'Brien
This document summarizes an experiment that observed quantum jumps in the photon number inside a superconducting cavity. Key points:
- Microwave photons were stored in a superconducting cavity for up to half a second and repeatedly probed by non-absorbing atoms passing through.
- An atom interferometer measured the atomic phase shift induced by the non-resonant cavity field, revealing the presence or absence of a single photon.
- Sequences of hundreds of correlated atom measurements were interrupted by sudden changes, recording the creation and destruction of individual photons over time.
- This realized a quantum non-demolition measurement of the photon number in the cavity in real time, allowing observation of its
This document summarizes research verifying simulations of a novel muon radiography detector system through experimentation. It estimates the detector's spatial resolution as 9.32mm, better than the 1cm reported previously. It also explores the detector's imaging potential through both simulation and initial promising experimental results. The document provides background on muon production, tomography using scattering angles, and radiography using transmission measurements. It describes common detector types and current applications like border security using large-scale muon tomography to detect nuclear materials more effectively than gamma-ray systems.
In search of multipath interference using large moleculesGabriel O'Brien
This document summarizes an experiment that tested the quantum mechanical principle of superposition using large dye molecules. The experiment measured interference patterns when the molecules passed through single, double, and triple slits. It observed less than 1% deviation from the expected interference patterns based on quantum mechanics, providing evidence that the superposition principle applies even to massive particles like these large molecules. The experiment is one of the first to directly observe quantum interference using massive particles rather than light or single particles.
Unknown 2019 - expand “explorations at and beyond the neutron dripline ”LinhBui343479
The EXPAND project aims to investigate the structure of light neutron-rich nuclei near and beyond the neutron dripline using the RIBF facility at RIKEN. It focuses on augmenting the neutron detection capabilities of the existing SAMURAI setup by transforming the two-wall NEBULA array into the NEBULA-Plus four-wall array. This will enable the routine detection of 3 and 4 neutrons and significantly increase single and two-neutron detection efficiencies. The project has faced delays and budget issues but now plans to equip 60-70 of the 90 acquired scintillator modules for NEBULA-Plus within the existing budget to provide significant gains in neutron detection capabilities.
Alma observations of_feeding_and_feedback_in_nearby_seyfert_galaxies_outflow_...Sérgio Sacani
ALMA observations of the Seyfert 2 galaxy NGC 1433 reveal a nuclear gaseous spiral structure within a nuclear ring encircling a nuclear stellar bar. Near the nucleus, there is intense high-velocity CO emission interpreted as an AGN-driven molecular outflow. The outflow involves a molecular mass of 3.6 million solar masses and a flow rate of about 7 solar masses per year. Continuum emission at the center is likely thermal dust emission from a molecular torus expected in this Seyfert 2 galaxy. The observations probe gas dynamics within 24 parsecs of the active galactic nucleus.
This document summarizes a detonating failed deflagration model of Type Ia supernovae. The model involves an off-center deflagration in a massive white dwarf that fails to unbind the star. Disturbances from the failed deflagration pollute the stellar surface and eventually evolve into isolated shock regions, serving as ignition points for detonations that result in supernova explosion. Preliminary results show ejecta composed of silicon and iron group elements, with an inner egg-shaped region surrounded by an incomplete burning shell. Explosion energies are around 1.3-1.5×1051 erg.
Non xrays from_the_very_nearby_typeia_sn_2014j_constraints_on_its_environmentSérgio Sacani
Deep X-ray observations of SN 2014J reveal no X-ray emission down to a luminosity limit of Lx < 7 × 1036 ergs−1, constraining the mass-loss rate of the progenitor system to be < 10−9 M☉/yr. Alternatively, the SN shock could be expanding into a uniform medium with density < 3 cm−3. These results rule out single-degenerate systems with steady mass transfer until explosion and constrain unstable hydrogen burning systems to have recurrence times < 300 years. Allowed progenitors include double white dwarf systems or systems where mass transfer ceased before explosion.
Propagation of highly_efficient_star_formation_in_ngc7000Sérgio Sacani
This document summarizes a study of star formation in molecular clouds near the H II region NGC 7000. The authors surveyed NH3 and H2O maser emission toward the molecular cloud L935 located near NGC 7000. They identified five dense molecular clumps based on NH3 emission, which have similar gas temperatures but different levels of star formation activity. One clump located near the boundary of the H II region has a high star formation efficiency of 36-62%, suggesting triggered star formation due to its interaction with the expanding H II region.
Artigo relata como a Terra sofreu com os impactos de ateroides a 4 bilhões de anos atrás, e como a superfície do planeta foi remodelada e os oceanos formados.
Results from telescope_array_experimentSérgio Sacani
The Telescope Array (TA) experiment studies ultrahigh energy cosmic rays using a hybrid detector consisting of a surface detector and three fluorescence detector stations. This paper reports three results from TA:
1) The cosmic ray spectrum measured by the surface detector shows an ankle feature and a 3.5 sigma suppression at the expected GZK cutoff energy, consistent with the HiRes experiment.
2) Measurement of the average shower maximum depth with the fluorescence detectors indicates a light composition, most likely protons.
3) A search for correlations between surface detector events and Active Galactic Nuclei found no significant correlations, consistent with results from HiRes.
Xray and protostars_in_the_trifid_nebulaSérgio Sacani
The document summarizes X-ray observations of the Trifid Nebula using ROSAT and ASCA. ROSAT images revealed around a dozen X-ray sources in the nebula, including the bright O7 star HD 164492 that provides much of the ionization. Ten X-ray sources were correlated with near-infrared sources identified as young stars or protostars. ASCA spectroscopy of the brightest source showed hard X-ray emission up to 10 keV including an iron K line, best fit with a two-temperature thermal model and absorption. The hotter component's temperature is unusually high and may originate from interaction with another object or protostellar flares.
The birth of_a_galaxy_propelling_reionisation_with_the_faintest_galaxiesSérgio Sacani
This document summarizes a study that uses cosmological radiation hydrodynamics simulations to model dwarf galaxy formation and properties at z > 7. The study finds that metal-enriched star formation can occur in halos down to masses of ~106 M, especially in neutral regions, and that these smallest galaxies provide nearly 30% of the ionizing photon budget needed for reionization despite only hosting up to 104 M of stars. The study also finds that the galaxy luminosity function flattens above MUV = -12 at z = 10 and that the fraction of ionizing radiation escaping into the intergalactic medium decreases from 50% to 5% over the halo mass range of log M/M⊙ = 7.0-8.
This document summarizes observations of rapid dust formation in the luminous supernova SN 2010jl over multiple epochs from 26 to 868 days past peak brightness. Analysis of emission line profiles shows increasing extinction over time, indicating continuous dust formation. The extinction curve implies the presence of very large (>1 micron) dust grains. Thermal emission models suggest dust temperatures declining from 2300K to 1100K over time, requiring carbonaceous rather than silicate dust. Combined extinction and emission data indicate a dust mass of ~0.0025 solar masses at 868 days, growing rapidly and expected to reach ~0.5 solar masses by 8000 days if production continues. The rapid formation of large dust grains suggests an efficient mechanism for dust nucle
This pilot survey used modest aperture telescopes to image 8 nearby spiral galaxies in order to search for stellar tidal streams. Ultra-deep imaging revealed 6 previously undetected extensive (up to 30 kpc) stellar structures likely from tidally disrupted satellites. A diversity of tidal feature morphologies was found, including great circle-like streams, remote shells, and jets emerging from disks. Simulations predict tidal debris should be common and match the observed variety, providing evidence minor mergers have shaped disk galaxies since z=1.
Kinematics and simulations_of_the_stellar_stream_in_the_halo_of_the_umbrella_...Sérgio Sacani
This document summarizes a study of the stellar stream and substructures around the Umbrella Galaxy (NGC 4651). Deep imaging and spectroscopy were used to characterize the properties and kinematics of the stream. Tracer objects like globular clusters and planetary nebulae were identified and found to delineate a kinematically cold feature in position-velocity space. Dynamical modeling suggests the stream originated from the tidal disruption of a dwarf galaxy on a highly eccentric orbit about 6-10 billion years ago. This work demonstrates the feasibility of using discrete tracers to recover the kinematics and model the dynamics of low surface brightness stellar streams around distant galaxies.
This document summarizes the detection of a super-Earth planet orbiting the star GJ 832. Radial velocity data from three telescopes revealed a planet, GJ 832c, with an orbital period of 35.68 days and a minimum mass of 5.4 Earth masses. GJ 832c has a low eccentricity orbit of 0.18 near the inner edge of the star's habitable zone. However, given its large mass, the planet likely has a massive atmosphere that could render it uninhabitable. The GJ 832 system resembles a miniature version of our solar system, with an interior potentially rocky planet and a distant gas giant.
Detection of an_unidentified_emission_line_in_the_stacked_xray_spectrum_of_ga...GOASA
This document describes the detection of an unidentified emission line in the stacked X-ray spectrum of 73 galaxy clusters observed by XMM-Newton. The line was detected at an energy of 3.55-3.57 keV in the combined spectrum. It was also seen independently in subsets of the clusters. The line is very weak, with an equivalent width of about 1 eV, and is within 50-110 eV of several known faint lines, making its nature difficult to determine. Possible explanations discussed include an atomic transition in the thermal plasma of the clusters or the decay of sterile neutrino dark matter particles.
Solar abundance ratios of the iron-peak elements in the Perseus clusterSérgio Sacani
The metal abundance of the hot plasma that permeates galaxy
clusters represents the accumulation of heavy elements produced
by billions of supernovae1. Therefore, X-ray spectroscopy of the
intracluster medium provides an opportunity to investigate the
nature of supernova explosions integrated over cosmic time. In
particular, the abundance of the iron-peak elements (chromium,
manganese, iron and nickel) is key to understanding how the
progenitors of typical type Ia supernovae evolve and explode2–6.
Recent X-ray studies of the intracluster medium found that the
abundance ratios of these elements differ substantially from those
seen in the Sun7–11, suggesting differences between the nature of type
Ia supernovae in the clusters and in the Milky Way. However, because
the K-shell transition lines of chromium and manganese are weak
and those of iron and nickel are very close in photon energy, highresolution
spectroscopy is required for an accurate determination
of the abundances of these elements. Here we report observations
of the Perseus cluster, with statistically significant detections of the
resonance emission from chromium, manganese and nickel. Our
measurements, combined with the latest atomic models, reveal that
these elements have near-solar abundance ratios with respect to iron,
in contrast to previous claims. Comparison between our results and
modern nucleosynthesis calculations12–14 disfavours the hypothesis
that type Ia supernova progenitors are exclusively white dwarfs with
masses well below the Chandrasekhar limit (about 1.4 times the
mass of the Sun). The observed abundance pattern of the iron-peak
elements can be explained by taking into account a combination
of near- and sub-Chandrasekhar-mass type Ia supernova systems,
adding to the mounting evidence that both progenitor types make a
substantial contribution to cosmic chemical enrichment5,15,16.
Forming intracluster gas in a galaxy protocluster at a redshift of 2.16Sérgio Sacani
Galaxy clusters are the most massive gravitationally bound structures in the Universe, comprising thousands of galaxies and
pervaded by a diffuse, hot “intracluster medium” (ICM) that dominates the baryonic content of these systems. The formation
and evolution of the ICM across cosmic time1
is thought to be driven by the continuous accretion of matter from the large-scale
filamentary surroundings and dramatic merger events with other clusters or groups. Until now, however, direct observations of
the intracluster gas have been limited only to mature clusters in the latter three-quarters of the history of the Universe, and we
have been lacking a direct view of the hot, thermalized cluster atmosphere at the epoch when the first massive clusters formed.
Here we report the detection (about 6σ) of the thermal Sunyaev-Zeldovich (SZ) effect2
in the direction of a protocluster. In fact,
the SZ signal reveals the ICM thermal energy in a way that is insensitive to cosmological dimming, making it ideal for tracing
the thermal history of cosmic structures3
. This result indicates the presence of a nascent ICM within the Spiderweb protocluster
at redshift z = 2.156, around 10 billion years ago. The amplitude and morphology of the detected signal show that the SZ
effect from the protocluster is lower than expected from dynamical considerations and comparable with that of lower-redshift
group-scale systems, consistent with expectations for a dynamically active progenitor of a local galaxy cluster.
Effect of a_high_opacity_on_the_light_curves_of_radioactively_powered_transie...Sérgio Sacani
This document discusses how higher opacities from lanthanide elements in the ejecta of neutron star mergers could dramatically affect the predicted light curves of electromagnetic counterparts. The key points are:
1) Ab initio calculations show r-process element opacities are orders of magnitude higher than previously assumed iron opacities, particularly from lanthanide elements.
2) With these higher opacities, radiation transport models predict light curves that are longer (lasting about a week), dimmer, and redder, with emission peaked in the infrared rather than optical/ultraviolet.
3) A two-component light curve may result if there is both lanthanide-rich ejecta and a secondary
The first X-ray look at SMSS J114447.77-430859.3: the most luminous quasar in...Sérgio Sacani
SMSS J114447.77-430859.3 (z = 0.83) has been identified in the SkyMapper Southern Survey as the most luminous quasar in
the last ∼ 9 Gyr . In this paper, we report on the eROSITA/Spectrum–Roentgen–Gamma (SRG) observations of the source from
the eROSITA All Sky Survey, along with presenting results from recent monitoring performed using Swift, XMM-Newton, and
NuSTAR. The source shows a clear variability by factors of ∼10 and ∼2.7 overtime-scales of a year and of a few days,respectively.
When fit with an absorbed power law plus high-energy cutoff, the X-ray spectra reveal a = 2.2 ± 0.2 and Ecut = 23+26
−5 keV
. Assuming Comptonization, we estimate a coronal optical depth and electron temperature of τ = 2.5 − 5.3 (5.2 − 8) and
kT = 8 − 18 (7.5 − 14) keV , respectively, for a slab (spherical) geometry. The broadband SED is successfully modelled by
assuming either a standard accretion disc illuminated by a central X-ray source, or a thin disc with a slim disc emissivity profile.
The former model results in a black hole mass estimate of the order of 1010 M , slightly higher than prior optical estimates;
meanwhile, the latter model suggests a lower mass. Both models suggest sub-Eddington accretion when assuming a spinning
black hole, and a compact (∼ 10 rg ) X-ray corona. The measured intrinsic column density and the Eddington ratio strongly
suggest the presence of an outflow driven by radiation pressure. This is also supported by variation of absorption by an order of
magnitude over the period of ∼ 900 d .
Probing the jet_base_of_blazar_pks1830211_from_the_chromatic_variability_of_i...Sérgio Sacani
This document summarizes ALMA observations of the blazar PKS 1830-211 taken over multiple epochs in 2012. The blazar is lensed by a foreground galaxy, producing two resolved images (NE and SW) separated by 1". The observations were taken at frequencies corresponding to 350-1050 GHz in the blazar rest frame. Analysis of the flux ratio between the two images over time and frequency revealed a remarkable frequency-dependent behavior, implying a "chromatic structure" in the blazar jet. This is interpreted as evidence for a "core-shift effect" caused by plasmon ejection very near the base of the jet. The observations provide a unique probe of activity in the region where plasma acceleration occurs in blazar
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.
Water vapour absorption in the clear atmosphere of a Neptune-sized exoplanetGOASA
1) The transmission spectrum of the exoplanet HAT-P-11b was observed using Hubble and Spitzer space telescopes.
2) Water vapor absorption was detected at 1.4 micrometers in the atmosphere, indicating a clear atmosphere down to 1 mbar pressure.
3) The detection of water vapor and relatively large atmospheric scale height places an upper limit on the abundance of heavy elements in the atmosphere of around 700 times the solar value, consistent with core accretion planet formation theories.
A close pair_binary_in_a_distant_triple_supermassive_black_hole_systemSérgio Sacani
This document reports the discovery of a triple supermassive black hole system through radio observations. Very Long Baseline Interferometry observations revealed two flat-spectrum radio cores, labelled J1502SE and J1502SW, within the galaxy J1502S, separated by about 140 parsecs. Analysis of archival data provides further evidence of this close black hole pair through the detection of 'S-shaped' radio emission between the two cores, indicative of jet precession caused by the binary black holes. This is the closest black hole pair yet discovered and demonstrates a new method for finding binary black holes that cannot be spatially resolved with current instruments.
Water vapour absorption_in_the_clear_atmosphere_of_a_neptune_sized_exoplanetSérgio Sacani
This document summarizes research on the transmission spectrum of the exoplanet HAT-P-11b, a Neptune-sized planet. Observations from the Hubble Space Telescope and Spitzer Space Telescope detected water vapor absorption in the planet's atmosphere at a wavelength of 1.4 micrometers. Analysis of the spectrum indicates the atmosphere is predominantly clear down to 1 mbar and has a hydrogen abundance similar to solar values. Atmospheric modeling suggests a metallicity around 190 times that of the Sun's, in agreement with core accretion planet formation theories. This makes HAT-P-11b the smallest exoplanet to date with a detected molecular signature in its atmosphere, providing new insights into the composition and formation of Neptune-sized
Pulsar emission amplified and resolved by plasma lensing in an eclipsing binarySérgio Sacani
Radio pulsars scintillate because their emission travels through the
ionized interstellar medium along multiple paths, which interfere
with each other. It has long been realized that, independent of their
nature, the regions responsible for the scintillation could be used
as ‘interstellar lenses’ to localize pulsar emission regions1,2
. Most
such lenses, however, resolve emission components only marginally,
limiting results to statistical inferences and detections of small
positional shifts3–5
. As lenses situated close to their source offer
better resolution, it should be easier to resolve emission regions of
pulsars located in high-density environments such as supernova
remnants6
or binaries in which the pulsar’s companion has an
ionized outflow. Here we report observations of extreme plasma
lensing in the ‘black widow’ pulsar, B1957+20, near the phase in its
9.2-hour orbit at which its emission is eclipsed by its companion’s
outflow7–9
. During the lensing events, the observed radio flux is
enhanced by factors of up to 70–80 at specific frequencies. The
strongest events clearly resolve the emission regions: they affect the
narrow main pulse and parts of the wider interpulse differently. We
show that the events arise naturally from density fluctuations in
the outer regions of the outflow, and we infer a resolution of our
lenses that is comparable to the pulsar’s radius, about 10 kilometres.
Furthermore, the distinct frequency structures imparted by the
lensing are reminiscent of what is observed for the repeating fast
radio burst FRB 121102, providing observational support for the
idea that this source is observed through, and thus at times strongly
magnified by, plasma lenses10
An eclipsing binary_distance_to_the_large_magellanic_cloud_accurate_to_two_pe...Sérgio Sacani
This document reports on a study that measured the distance to the Large Magellanic Cloud (LMC) using 8 eclipsing binary star systems composed of late-type giant stars. The study obtained high-resolution spectra and photometry of the binary systems. It analyzed the data using modeling techniques to determine physical properties with a few percent accuracy. Distances were then calculated combining angular sizes from surface brightness relations with linear sizes from modeling. This yielded a weighted mean distance to the LMC of 49.97 ± 0.19 (statistical) ± 1.11 (systematic) kiloparsecs, accurate to 2.2%. This provides an improved anchor for determining the Hubble constant.
This document presents observations from the VLT X-shooter instrument of two quasars, SDSS J1106+1939 and SDSS J1512+1119. For SDSS J1106+1939, a broad absorption line (BAL) outflow is detected with a kinetic luminosity of at least 10^46 erg/s, which is 5% of the quasar's bolometric luminosity. This outflow has a velocity of ~8000 km/s and is located ~300 pc from the quasar. For SDSS J1512+1119, two separate outflows are detected using the same technique, with distances ranging from 100-2000 pc from the central source. The distances of the outflows
Dissecting x ray_emitting_gas_around_the_center_of_our_galaxySérgio Sacani
1) The Chandra X-ray Observatory was used to observe the supermassive black hole at the center of the Milky Way, Sgr A*, for a total of 3 megaseconds.
2) The observations revealed extended X-ray emission around Sgr A* that aligns spatially with a surrounding disk of massive stars.
3) Spectral analysis ruled out low-mass stars as the origin of the X-ray emission and instead found evidence that the emission is from a radiatively inefficient accretion flow onto the black hole, with an outflow present.
Inverse Compton cooling limits the brightness temperature of the radiating plasma to a maximum of
1011.5 K. Relativistic boosting can increase its observed value, but apparent brightness temperatures
much in excess of 1013 K are inaccessible using ground-based very long baseline interferometry (VLBI)
at any wavelength. We present observations of the quasar 3C 273, made with the space VLBI mission
RadioAstron on baselines up to 171,000 km, which directly reveal the presence of angular structure as
small as 26 µas (2.7 light months) and brightness temperature in excess of 1013 K. These measurements
challenge our understanding of the non-thermal continuum emission in the vicinity of supermassive
black holes and require a much higher Doppler factor than what is determined from jet apparent
kinematics.
Keywords: galaxies: active — galaxies: jets — radio continuum: galaxies — techniques: interferometric
— quasars: individual (3C 273)
A rapidly spinning_supermassive_black_hole_at_the_centre_of_ngc1365Sérgio Sacani
1) XMM-Newton and NuSTAR observed the galaxy NGC 1365 simultaneously over 130 ks, detecting broadband X-ray emission from 3-79 keV.
2) The observations revealed variable absorption below 10 keV and prominent broad emission features between 5-7 keV and 10-30 keV, indicative of relativistic reflection from an accretion disk near a spinning supermassive black hole.
3) Time-resolved spectral analysis was able to disentangle the variable absorption component from the relativistic reflection component. Absorption-dominated models without reflection could be ruled out statistically and on physical grounds.
MAGNETIZED PLASMA WITH FERROMAGNETIC GRAINS AS A VIABLE NEGATIVE REFRACTIVE I...ijrap
This document discusses magnetized plasma with ferromagnetic grains (MPFG) as a potential negative refractive index medium. It is shown that:
1) MPFG has permittivity and permeability tensors that are controlled by the magnetized plasma and ferromagnetic grains.
2) For extraordinary waves propagating parallel to an external magnetic field, the refractive index of MPFG can be negative, indicating left-handed behavior, in certain frequency domains near resonance.
3) Numerical calculations demonstrate that both the effective permittivity and permeability of MPFG can be simultaneously negative for some frequencies, allowing for negative refractive index and transparent propagation of electromagnetic waves.
Similar to An unindetified line_in_xray_spectra_of_the_adromeda_galaxy_and_perseus_galaxy_cluster (20)
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.
Constraints on Neutrino Natal Kicks from Black-Hole Binary VFTS 243Sérgio Sacani
The recently reported observation of VFTS 243 is the first example of a massive black-hole binary
system with negligible binary interaction following black-hole formation. The black-hole mass (≈10M⊙)
and near-circular orbit (e ≈ 0.02) of VFTS 243 suggest that the progenitor star experienced complete
collapse, with energy-momentum being lost predominantly through neutrinos. VFTS 243 enables us to
constrain the natal kick and neutrino-emission asymmetry during black-hole formation. At 68% confidence
level, the natal kick velocity (mass decrement) is ≲10 km=s (≲1.0M⊙), with a full probability distribution
that peaks when ≈0.3M⊙ were ejected, presumably in neutrinos, and the black hole experienced a natal
kick of 4 km=s. The neutrino-emission asymmetry is ≲4%, with best fit values of ∼0–0.2%. Such a small
neutrino natal kick accompanying black-hole formation is in agreement with theoretical predictions.
Detectability of Solar Panels as a TechnosignatureSérgio Sacani
In this work, we assess the potential detectability of solar panels made of silicon on an Earth-like
exoplanet as a potential technosignature. Silicon-based photovoltaic cells have high reflectance in the
UV-VIS and in the near-IR, within the wavelength range of a space-based flagship mission concept
like the Habitable Worlds Observatory (HWO). Assuming that only solar energy is used to provide
the 2022 human energy needs with a land cover of ∼ 2.4%, and projecting the future energy demand
assuming various growth-rate scenarios, we assess the detectability with an 8 m HWO-like telescope.
Assuming the most favorable viewing orientation, and focusing on the strong absorption edge in the
ultraviolet-to-visible (0.34 − 0.52 µm), we find that several 100s of hours of observation time is needed
to reach a SNR of 5 for an Earth-like planet around a Sun-like star at 10pc, even with a solar panel
coverage of ∼ 23% land coverage of a future Earth. We discuss the necessity of concepts like Kardeshev
Type I/II civilizations and Dyson spheres, which would aim to harness vast amounts of energy. Even
with much larger populations than today, the total energy use of human civilization would be orders of
magnitude below the threshold for causing direct thermal heating or reaching the scale of a Kardashev
Type I civilization. Any extraterrrestrial civilization that likewise achieves sustainable population
levels may also find a limit on its need to expand, which suggests that a galaxy-spanning civilization
as imagined in the Fermi paradox may not exist.
Jet reorientation in central galaxies of clusters and groups: insights from V...Sérgio Sacani
Recent observations of galaxy clusters and groups with misalignments between their central AGN jets
and X-ray cavities, or with multiple misaligned cavities, have raised concerns about the jet – bubble
connection in cooling cores, and the processes responsible for jet realignment. To investigate the
frequency and causes of such misalignments, we construct a sample of 16 cool core galaxy clusters and
groups. Using VLBA radio data we measure the parsec-scale position angle of the jets, and compare
it with the position angle of the X-ray cavities detected in Chandra data. Using the overall sample
and selected subsets, we consistently find that there is a 30% – 38% chance to find a misalignment
larger than ∆Ψ = 45◦ when observing a cluster/group with a detected jet and at least one cavity. We
determine that projection may account for an apparently large ∆Ψ only in a fraction of objects (∼35%),
and given that gas dynamical disturbances (as sloshing) are found in both aligned and misaligned
systems, we exclude environmental perturbation as the main driver of cavity – jet misalignment.
Moreover, we find that large misalignments (up to ∼ 90◦
) are favored over smaller ones (45◦ ≤ ∆Ψ ≤
70◦
), and that the change in jet direction can occur on timescales between one and a few tens of Myr.
We conclude that misalignments are more likely related to actual reorientation of the jet axis, and we
discuss several engine-based mechanisms that may cause these dramatic changes.
The solar dynamo begins near the surfaceSérgio Sacani
The magnetic dynamo cycle of the Sun features a distinct pattern: a propagating
region of sunspot emergence appears around 30° latitude and vanishes near the
equator every 11 years (ref. 1). Moreover, longitudinal flows called torsional oscillations
closely shadow sunspot migration, undoubtedly sharing a common cause2. Contrary
to theories suggesting deep origins of these phenomena, helioseismology pinpoints
low-latitude torsional oscillations to the outer 5–10% of the Sun, the near-surface
shear layer3,4. Within this zone, inwardly increasing differential rotation coupled with
a poloidal magnetic field strongly implicates the magneto-rotational instability5,6,
prominent in accretion-disk theory and observed in laboratory experiments7.
Together, these two facts prompt the general question: whether the solar dynamo is
possibly a near-surface instability. Here we report strong affirmative evidence in stark
contrast to traditional models8 focusing on the deeper tachocline. Simple analytic
estimates show that the near-surface magneto-rotational instability better explains
the spatiotemporal scales of the torsional oscillations and inferred subsurface
magnetic field amplitudes9. State-of-the-art numerical simulations corroborate these
estimates and reproduce hemispherical magnetic current helicity laws10. The dynamo
resulting from a well-understood near-surface phenomenon improves prospects
for accurate predictions of full magnetic cycles and space weather, affecting the
electromagnetic infrastructure of Earth.
Extensive Pollution of Uranus and Neptune’s Atmospheres by Upsweep of Icy Mat...Sérgio Sacani
In the Nice model of solar system formation, Uranus and Neptune undergo an orbital upheaval,
sweeping through a planetesimal disk. The region of the disk from which material is accreted by
the ice giants during this phase of their evolution has not previously been identified. We perform
direct N-body orbital simulations of the four giant planets to determine the amount and origin of solid
accretion during this orbital upheaval. We find that the ice giants undergo an extreme bombardment
event, with collision rates as much as ∼3 per hour assuming km-sized planetesimals, increasing the
total planet mass by up to ∼0.35%. In all cases, the initially outermost ice giant experiences the
largest total enhancement. We determine that for some plausible planetesimal properties, the resulting
atmospheric enrichment could potentially produce sufficient latent heat to alter the planetary cooling
timescale according to existing models. Our findings suggest that substantial accretion during this
phase of planetary evolution may have been sufficient to impact the atmospheric composition and
thermal evolution of the ice giants, motivating future work on the fate of deposited solid material.
A workshop hosted by the South African Journal of Science aimed at postgraduate students and early career researchers with little or no experience in writing and publishing journal articles.
Chapter wise All Notes of First year Basic Civil Engineering.pptxDenish Jangid
Chapter wise All Notes of First year Basic Civil Engineering
Syllabus
Chapter-1
Introduction to objective, scope and outcome the subject
Chapter 2
Introduction: Scope and Specialization of Civil Engineering, Role of civil Engineer in Society, Impact of infrastructural development on economy of country.
Chapter 3
Surveying: Object Principles & Types of Surveying; Site Plans, Plans & Maps; Scales & Unit of different Measurements.
Linear Measurements: Instruments used. Linear Measurement by Tape, Ranging out Survey Lines and overcoming Obstructions; Measurements on sloping ground; Tape corrections, conventional symbols. Angular Measurements: Instruments used; Introduction to Compass Surveying, Bearings and Longitude & Latitude of a Line, Introduction to total station.
Levelling: Instrument used Object of levelling, Methods of levelling in brief, and Contour maps.
Chapter 4
Buildings: Selection of site for Buildings, Layout of Building Plan, Types of buildings, Plinth area, carpet area, floor space index, Introduction to building byelaws, concept of sun light & ventilation. Components of Buildings & their functions, Basic concept of R.C.C., Introduction to types of foundation
Chapter 5
Transportation: Introduction to Transportation Engineering; Traffic and Road Safety: Types and Characteristics of Various Modes of Transportation; Various Road Traffic Signs, Causes of Accidents and Road Safety Measures.
Chapter 6
Environmental Engineering: Environmental Pollution, Environmental Acts and Regulations, Functional Concepts of Ecology, Basics of Species, Biodiversity, Ecosystem, Hydrological Cycle; Chemical Cycles: Carbon, Nitrogen & Phosphorus; Energy Flow in Ecosystems.
Water Pollution: Water Quality standards, Introduction to Treatment & Disposal of Waste Water. Reuse and Saving of Water, Rain Water Harvesting. Solid Waste Management: Classification of Solid Waste, Collection, Transportation and Disposal of Solid. Recycling of Solid Waste: Energy Recovery, Sanitary Landfill, On-Site Sanitation. Air & Noise Pollution: Primary and Secondary air pollutants, Harmful effects of Air Pollution, Control of Air Pollution. . Noise Pollution Harmful Effects of noise pollution, control of noise pollution, Global warming & Climate Change, Ozone depletion, Greenhouse effect
Text Books:
1. Palancharmy, Basic Civil Engineering, McGraw Hill publishers.
2. Satheesh Gopi, Basic Civil Engineering, Pearson Publishers.
3. Ketki Rangwala Dalal, Essentials of Civil Engineering, Charotar Publishing House.
4. BCP, Surveying volume 1
LAND USE LAND COVER AND NDVI OF MIRZAPUR DISTRICT, UPRAHUL
This Dissertation explores the particular circumstances of Mirzapur, a region located in the
core of India. Mirzapur, with its varied terrains and abundant biodiversity, offers an optimal
environment for investigating the changes in vegetation cover dynamics. Our study utilizes
advanced technologies such as GIS (Geographic Information Systems) and Remote sensing to
analyze the transformations that have taken place over the course of a decade.
The complex relationship between human activities and the environment has been the focus
of extensive research and worry. As the global community grapples with swift urbanization,
population expansion, and economic progress, the effects on natural ecosystems are becoming
more evident. A crucial element of this impact is the alteration of vegetation cover, which plays a
significant role in maintaining the ecological equilibrium of our planet.Land serves as the foundation for all human activities and provides the necessary materials for
these activities. As the most crucial natural resource, its utilization by humans results in different
'Land uses,' which are determined by both human activities and the physical characteristics of the
land.
The utilization of land is impacted by human needs and environmental factors. In countries
like India, rapid population growth and the emphasis on extensive resource exploitation can lead
to significant land degradation, adversely affecting the region's land cover.
Therefore, human intervention has significantly influenced land use patterns over many
centuries, evolving its structure over time and space. In the present era, these changes have
accelerated due to factors such as agriculture and urbanization. Information regarding land use and
cover is essential for various planning and management tasks related to the Earth's surface,
providing crucial environmental data for scientific, resource management, policy purposes, and
diverse human activities.
Accurate understanding of land use and cover is imperative for the development planning
of any area. Consequently, a wide range of professionals, including earth system scientists, land
and water managers, and urban planners, are interested in obtaining data on land use and cover
changes, conversion trends, and other related patterns. The spatial dimensions of land use and
cover support policymakers and scientists in making well-informed decisions, as alterations in
these patterns indicate shifts in economic and social conditions. Monitoring such changes with the
help of Advanced technologies like Remote Sensing and Geographic Information Systems is
crucial for coordinated efforts across different administrative levels. Advanced technologies like
Remote Sensing and Geographic Information Systems
9
Changes in vegetation cover refer to variations in the distribution, composition, and overall
structure of plant communities across different temporal and spatial scales. These changes can
occur natural.
Leveraging Generative AI to Drive Nonprofit InnovationTechSoup
In this webinar, participants learned how to utilize Generative AI to streamline operations and elevate member engagement. Amazon Web Service experts provided a customer specific use cases and dived into low/no-code tools that are quick and easy to deploy through Amazon Web Service (AWS.)
Reimagining Your Library Space: How to Increase the Vibes in Your Library No ...Diana Rendina
Librarians are leading the way in creating future-ready citizens – now we need to update our spaces to match. In this session, attendees will get inspiration for transforming their library spaces. You’ll learn how to survey students and patrons, create a focus group, and use design thinking to brainstorm ideas for your space. We’ll discuss budget friendly ways to change your space as well as how to find funding. No matter where you’re at, you’ll find ideas for reimagining your space in this session.
How to Make a Field Mandatory in Odoo 17Celine George
In Odoo, making a field required can be done through both Python code and XML views. When you set the required attribute to True in Python code, it makes the field required across all views where it's used. Conversely, when you set the required attribute in XML views, it makes the field required only in the context of that particular view.
Strategies for Effective Upskilling is a presentation by Chinwendu Peace in a Your Skill Boost Masterclass organisation by the Excellence Foundation for South Sudan on 08th and 09th June 2024 from 1 PM to 3 PM on each day.
How to Fix the Import Error in the Odoo 17Celine George
An import error occurs when a program fails to import a module or library, disrupting its execution. In languages like Python, this issue arises when the specified module cannot be found or accessed, hindering the program's functionality. Resolving import errors is crucial for maintaining smooth software operation and uninterrupted development processes.
A review of the growth of the Israel Genealogy Research Association Database Collection for the last 12 months. Our collection is now passed the 3 million mark and still growing. See which archives have contributed the most. See the different types of records we have, and which years have had records added. You can also see what we have for the future.
This slide is special for master students (MIBS & MIFB) in UUM. Also useful for readers who are interested in the topic of contemporary Islamic banking.
Chapter 4 - Islamic Financial Institutions in Malaysia.pptx
An unindetified line_in_xray_spectra_of_the_adromeda_galaxy_and_perseus_galaxy_cluster
1. arXiv:1402.4119v1[astro-ph.CO]17Feb2014
An unidentified line in X-ray spectra of the Andromeda galaxy and Perseus galaxy cluster
A. Boyarsky1
, O. Ruchayskiy2
, D. Iakubovskyi3,4
and J. Franse1,5
1
Instituut-Lorentz for Theoretical Physics, Universiteit Leiden, Niels Bohrweg 2, Leiden, The Netherlands
2
Ecole Polytechnique F´ed´erale de Lausanne, FSB/ITP/LPPC, BSP, CH-1015, Lausanne, Switzerland
3
Bogolyubov Institute of Theoretical Physics, Metrologichna Str. 14-b, 03680, Kyiv, Ukraine
4
National University “Kyiv-Mohyla Academy”, Skovorody Str. 2, 04070, Kyiv, Ukraine
5
Leiden Observatory, Leiden University, Niels Bohrweg 2, Leiden, The Netherlands
We identify a weak line at E ∼ 3.5 keV in X-ray spectra of the Andromeda galaxy and the Perseus galaxy
cluster – two dark matter-dominated objects, for which there exist deep exposures with the XMM-Newton X-ray
observatory. Such a line was not previously known to be present in the spectra of galaxies or galaxy clusters.
Although the line is weak, it has a clear tendency to become stronger towards the centers of the objects; it is
stronger for the Perseus cluster than for the Andromeda galaxy and is absent in the spectrum of a very deep
“blank sky” dataset. Although for individual objects it is hard to exclude the possibility that the feature is due
to an instrumental effect or an atomic line of anomalous brightness, it is consistent with the behavior of a line
originating from the decay of dark matter particles. Future detections or non-detections of this line in multiple
astrophysical targets may help to reveal its nature.
The nature of dark matter (DM) is a question of crucial im-
portance for both cosmology and for fundamental physics. As
neutrinos – the only known particles that could be dark mat-
ter candidates – are known to be too light to be consistent with
various observations (see e.g. [1] for a review), it is widely an-
ticipated that a new particle should exist to extend the hot Big
Bang cosmology paradigm to dark matter. Although many
candidates have been put forward by particle physicists (see
e.g. [2]), little is known experimentally about the properties
of DM particles: their masses, lifetimes, and interaction types
remain largely unconstrained. A priori, a given DM candidate
can possess a decay channel if its lifetime exceeds the age
of the Universe. Therefore, the search for a DM decay signal
provides an important test to constrain the properties of DM in
a model-independentway. For fermionic particles, one should
search above the Tremaine-Gunn limit [3] ( 300 eV). If the
mass is below 2mec2
, such a fermion can decay to neutrinos
and photons, and we can expect two-body radiative decay with
photon energy Eγ = 1
2 mDM. Such particles can be searched
for in X-rays (see [4] for review of previous searches). For
each particular DM model, the particle’s mass, lifetime and
other parameters are related by the requirement to provide the
correct DM abundance. For example, for one very interesting
DM candidate – the right-handed neutrino – this requirement
restricts the mass range to 0.5 − 100 keV [4, 5]. A large part
of the available parameter space for sterile neutrinos is fully
consistent with all astrophysical and cosmological bounds [6],
and it is important to probe it still further.
The DM decay line is much narrower than the spectral res-
olution of the present day X-ray telescopes and, as previous
searches have shown, should be rather weak. The X-ray spec-
tra of astrophysical objects are crowded with weak atomic and
instrumental lines, not all of which may be known. Therefore,
even if the exposure of available observations continues to in-
crease, it is hard to exclude an astrophysical or instrumental
origin of any weak line found in the spectrum of individual
object. However, if the same feature is present in the spectra
of a number of different objects, and its surface brightness and
relative normalization between objects is consistent with the
expected behavior of the DM signal, this can provide much
more convincing evidence about its nature.
The present paper takes a step in this direction. We present
the results of the combined analysis of many XMM-Newton
observations of two objects at different redshifts – the Perseus
cluster and the Andromeda galaxy (M31) – together with a
long exposure “blank sky” dataset. We study the 2.8–8 keV
energy band and show that the only significant un-modeled
excess that is present in the spectra of both M31 and Perseus
is located at ∼ 3.5 keV energy and the line in Perseus is cor-
rectly redshifted as compared to Andromeda (at 95% CL). The
relative fluxes for the two objects are in agreement with what
is known about their DM distributions. We also study sur-
face brightness profiles of this line and find them consistent
with expectations for a DM decay line. We do not detect such
a line in the very deep “blank sky” dataset, which disfavors
some of the scenarios for its instrumental origin (e.g. features
in the effective area). The upper bound from this dataset is
consistent with expectations for a DM signal that would come
in this case primarily from the Milky Way halo. However, as
the line is weak (∼ 4σ in the combined dataset) and the uncer-
tainties in DM distribution are significant, positive detections
or strong constraints from more objects are clearly needed in
order to determine the nature of this signal.1
Below we summarize the details of our data analysis and then
1 During our work we became aware that a similar analysis has been carried
out by different group for a collection of galaxy clusters. When this paper
was in preparation, the arXiv preprint [7] by this group appeared, claim-
ing a detection of a spectral feature at the same energy from a number of
clusters.
2. 2
discuss the results.
Data analysis. We use the data obtained with the European
Photon Imaging Camera (EPIC) of XMM-Newton (“XMM” in
what follows), which consists of two MOS [8] and one PN [9]
CCD camera. We start with the basic Observation Data Files
and reduce them using the procedures emproc and epproc
for the MOS and PN cameras (SAS v.13.0.0 [10]). Raw event
lists exhibit significant time variability caused by the soft so-
lar protons [11, 12]. To remove the time-variable component
we use the 60 s histogram for the whole camera’s energy range
and reject the intervals where count rates deviate by more than
1.5σ from the mean value (espfilt procedure from SAS).
By this procedure we discard ∼ 40% of total observation time.
However, residual soft proton flares can produce weak line-
like features in the spectra at positions where the effective area
is non-monotonic (see e.g. [13]). To further filter the data, we
apply the procedure described in [14], based on the compar-
ison of high-energy count rates for “in-FoV” (10-15 arcmin
off-center) and out-FoV CCD regions [15]. We selected only
observations where the ratio of Fin − Fout < 1.15.2
Combined observation of M31 center. The Andromeda
galaxy (M31) has been extensively observed with XMM. In
this work we use ∼ 2 Msec of raw exposure observations of
M31 within the central 1.5◦
. For the list of individual obser-
vations see Table III.
The XMM archive contains 35 observations of the center of
M31 (offset less than 1.5′
from (RA,DEC) = (00h42m44.3s
+41d16m09s)). Of these observations we have selected 29
where residual contamination of the background flares is low
(Fin − Fout < 1.15). For the PN camera only 8 observa-
tions had passed this criterion. We have chosen to keep only
the 26 MOS1 observations taken after the CCD6 was dam-
aged [17, 18]. In what follows we work with 26 MOS1 + 29
MOS2 observations combined.
We co-add channel-by-channel all PHA files for all cen-
tral observations of M31, using the addspec routine from
FTOOLS [19]. It also produces ARF- and exposure-weighted
response files .rsp – the product of .rmf and .arf files
of each observation. Finally, we bin the resulting spectra by
60 eV (4 MOS PI channels). This bin size is a factor ∼ 2
smaller than the spectral resolution of the XMM at these ener-
gies, which makes the bins roughly statistically independent.
Background modeling. We model the contribution of the
instrumental (particle induced) background by a combina-
tion of an unfolded power law (described in xspec11 by
powerlaw/b) plus a number of narrow gaussian lines
2 Ref. [14] argued that Fin − Fout < 1.3 is a sufficient criterion for flare
removal. We find that a stricter criterion is needed to reduce artificial line-
like residuals due to small wiggles in the effective area [13, 16].
at the positions of instrumental K-α lines (Cr, Mn, K, Fe, Ni,
Ca, Cu) and Fe Kβ. The astrophysical component is modeled
by a powerlaw and lines around 2.4 keV and 3.0 keV (Ar
and S line complexes). We restrict our modeling to the energy
interval 2–8 keV, see Fig. 1.
Result. The resulting spectrum shows a group of positive
residuals around 3.5 keV (Fig. 1). Adding a thin Gaussian line
at that energy reduces the total χ2
by ∼ 13, see Table I (more
than 3σ significance for extra 2 degrees of freedom). Exam-
ination of MOS1 and MOS2 observations individually shows
that the line is present in both cameras with comparable flux.
M31 off-center observations. Next we select off-center ob-
servations of M31 that pass the criterion Fin − Fout < 1.15
and whose centers are located within 23.7′
− 55.8′
from the
center of M31 (20 observations for both MOS1 and MOS2).
The background was modeled as in the on-center case. None
of the cameras have any detectable residual in the energy
range 3.53 ± 0.03 keV. The 2σ upper bound on the flux is
given in Table I.
Perseus cluster. If the candidate weak signal is of astrophys-
ical (rather than instrumental) origin, we should be able to
detect its redshift. To this end we have chosen the nearby
Perseus cluster (Abell 426). At its redshift, z = 0.0179, the
line’s centroid would be shifted by 63 eV. As the position of
the line is determined with about 30 eV precision, one can
expect to resolve the line’s shift with about 2σ significance.
We have taken 16 observations with the MOS1 and MOS2
cameras of the Perseus cluster (excluding two observations
on-center; see Table II) and processed them in the same way
as for M31. The flare removal procedure left 215 ksec of PN
camera’s exposure, therefore we also used the PN observa-
tions for Perseus.
Background modeling. The resulting spectra were then
added together and fitted to the combination of vmekal
(with free abundances for Fe, Ni, Ar, Ca and S) plus (extra-
galactic) powerlaw. The unfolded background component
powerlaw/b plus the several most prominent instrumental
lines were added to the model (similar to the M31 case).
Results. The fit shows significant positive residuals at en-
ergies around 3.47 keV (in the detector frame). Adding a
zgauss model with the redshift of the cluster improves the
fit by ∆χ2
= 9.1 (for 2 degrees of freedom: position and nor-
malization). The line’s position is fully consistent with that of
M31 (Table I). If we fix the position of the line to that of M31
and allow the redshift to vary, z = 0 provides a worse fit by
∆χ2
= 3.6 and its best-fit value is close to z = 0.0179.
Blank-sky dataset. To further study the origin of the new line
we combine XMM-Newton blank-sky observations from [20,
21] with observations of the Lockman Hole. The data were
reduced similarly to the other datasets. After filtering of soft
proton flares we obtained 382 MOS observations. A dataset
3. 3
Dataset Exposure χ2
/d.o.f. Line position Flux ∆χ2
[ksec] [keV] 10−6
cts/sec/cm2
M31 ON-CENTER 978.9 97.8/74 3.53 ± 0.025 4.9+1.6
−1.3 13.0
M31 OFF-CENTER 1472.8 107.8/75 3.53 ± 0.03 < 1.8 (2σ) . . .
PERSEUS CLUSTER (MOS) 528.5 72.7/68 3.50+0.044
−0.036 7.0+2.6
−2.6 9.1
PERSEUS CLUSTER (PN) 215.5 62.6/62 3.46 ± 0.04 9.2+3.1
−3.1 8.0
PERSEUS (MOS) 1507.4 191.5/142 3.518+0.019
−0.022 8.6+2.2
−2.3 (Perseus) 25.9
+ M31 ON-CENTER 4.6+1.4
−1.4 (M31) (3 dof)
BLANK-SKY 15700.2 33.1/33 3.53 ± 0.03 < 0.7 (2σ) . . .
TABLE I: Basic properties of combined observations used in this paper. Second column denotes the sum of exposures of individual observa-
tions. The last column shows change in ∆χ2
when 2 extra d.o.f. (position and flux of the line) are added. The energies for Perseus are quoted
in the rest frame of the object.
0.01
0.10
1.00
10.00
Normalizedcountrate
[cts/sec/keV]
M31 ON-center
-6⋅10-3
-4⋅10-3
-2⋅10-3
0⋅100
2⋅10-3
4⋅10-3
6⋅10-3
8⋅10-3
1⋅10-2
1.0 2.0 3.0 4.0 5.0 6.0 7.0 8.0
Data-model
[cts/sec/keV]
Energy [keV]
No line at 3.5 keV
0.22
0.24
0.26
0.28
0.30
0.32
0.34
0.36
Normalizedcountrate
[cts/sec/keV]
M31 ON-center
No line at 3.5 keV
-4⋅10-3
-2⋅10-3
0⋅100
2⋅10-3
4⋅10-3
6⋅10-3
8⋅10-3
1⋅10-2
3.0 3.2 3.4 3.6 3.8 4.0
Data-model
[cts/sec/keV]
Energy [keV]
No line at 3.5 keV
Line at 3.5 keV
FIG. 1: Left: Folded count rate (top) and residuals (bottom) for the MOS spectrum of the central region of M31. Statistical Y-errorbars on the
top plot are smaller than the point size. The line around 3.5 keV is not added, hence the group of positive residuals. Right: zoom onto the line
region.
with such a large exposure requires special analysis (as de-
scribed in [16]). This analysis did not reveal any line-like
residuals in the range 3.45−3.58 keV with the 2σ upper bound
on the flux being 7 × 10−7
cts/cm2
/sec. The closest detected
line-like feature (∆χ2
= 4.5) is at 3.67+0.10
−0.05 keV, consistent
with the instrumental Ca Kα line.3
Combined fit of M31 + Perseus. Finally, we have performed
a simultaneous fit of the on-center M31 and Perseus datasets
(MOS), keeping common position of the line (in the rest-
frame) and allowing the line normalizations to be different.
The line improves the fit by ∆χ2
= 25.9 (Table I), which
constitutes a 4.4σ significant detection for 3 d.o.f.
Results and discussion. We identified a spectral feature at
E = 3.518+0.019
−0.022 keV in the combined dataset of M31 and
Perseus that has a statistical significance 4.4σ and does not
coincide with any known line. Next we compare its properties
with the expected behavior of a DM decay line.
3 Previously this line has only been observed in the PN camera [9].
The observed brightness of a decaying DM line should be pro-
portional to the dark matter column density SDM = ρDMdℓ –
integral along the line of sight of the DM density distribution:
FDM ≈ 2.0 × 10−6 cts
cm2 · sec
Ωfov
500 arcmin2 × (1)
SDM
500 M /pc2
1029
s
τDM
keV
mDM
.
M31 and Perseus brightness profiles. Using the line flux
of the center of M31 and the upper limit from the off-center
observations we constrain the spatial profile of the line. The
DM distribution in M31 has been extensively studied (see an
overview in [13]). We take NFW profiles for M31 with con-
centrations c = 11.7 (solid line, [22]) and c = 19 (dash-dotted
line). For each concentration we adjust the normalization so
that it passes through first data point (Fig. 2). The c = 19
profile was chosen to intersect the upper limit, illustrating that
the obtained line fluxes of M31 are fully consistent with the
density profile of M31 (see e.g. [22, 24, 25] for a c = 19 − 22
model of M31).
4. 4
0
2
4
6
8
10
0 0.2 0.4 0.6 0.8 1
Fluxx106
[cts/cm2
/sec]
Radius [deg]
M31 surface brightness profile
on-center
off-center upper limit
NFW, c = 11.7
NFW, c = 19
0
5
10
15
20
0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2
Fluxx106
[cts/cm2
/sec]
Radius [deg]
Perseus cluster surface brigtness profile
R200
NFW DM line, rs = 360 kpc
NFW DM line, rs = 872 kpc
β-model, β = 0.71, rc = 287 kpc
FIG. 2: The line’s brightness profile in M31 (left) and the Perseus cluster (right). An NFW DM distribution is assumed, the scale rs is fixed to
its best-fit values from [22] (M31) or [23] (Perseus) and the overall normalization is adjusted to pass through the left-most point.
For the Perseus cluster the observations can be grouped in
3 radial bins by their off-center angle. For each bin we fix
the line position to its average value across Perseus (3.47 ±
0.07 keV). The obtained line fluxes together with 1σ errors
are shown in Fig. 2. For comparison, we draw the expected
line distribution from dark matter decay using the NFW pro-
file of [23] (best fit value rs = 360 kpc, black solid line; 1σ
upper bound rs = 872 kpc, black dashed line). The isother-
mal β-profile from [26] is shown in magenta. The surface
brightness profile follows the expected DM decay line’s dis-
tribution in Perseus.
Finally, we compare the predictions for the DM lifetime from
the two objects. The estimates of the average column den-
sity within the central part of M31 give S(rs) ∼ 200 −
600 M⊙/pc2
[13]. The column density of clusters follows
from the c − M relation [27–29]. Considering the uncer-
tainty on the profile and that our observations of Perseus go
beyond rs, the average column density in the region of interest
is within ¯S ∼ 100 − 600 M⊙/pc2
. Therefore the signal from
Perseus can be both stronger and weaker than that of M31, by
0.2 − 3.0. This is consistent with the ratio of measured flux
from Perseus to M31 0.7 − 2.7.
If DM is made of right-handed (sterile) neutrinos [30], the
lifetime is related to its interaction strength (mixing angle):
τDM =
1024π4
9αG2
F sin2
(2θ)m5
DM
7.2 × 1029
sec
10−8
sin2
(2θ)
1 keV
mDM
5
.
Using the data from M31 we obtain the mass mDM = 7.06 ±
0.05 keV and the mixing angle in the range sin2
(2θ) = (2.2−
20) × 10−11
. This value is consistent with previous bounds,
Fig. 4. This means that sterile neutrinos should be produced
resonantly [31–33], which requires the presence of significant
lepton asymmetry in primordial plasma at temperatures few
hundreds MeV. This produces restrictions on parameters of
0.10
Normalizedcountrate
[cts/sec/keV]
Blank sky dataset
-2⋅10
-3
-2⋅10
-3
-1⋅10
-3
-5⋅10
-4
0⋅10
0
5⋅10
-4
1⋅10
-3
2⋅10
-3
2⋅10
-3
2.0 3.0 4.0 5.0 6.0 7.0 8.0
Data-model
[cts/sec/keV]
Energy [keV]
FIG. 3: Blank sky spectrum and residuals.
the νMSM.
The position and flux of the discussed weak line are inevitably
subject to systematical uncertainties. There are two weak in-
strumental lines (K Kα at 3.31 keV and Ca Kα at 3.69 keV),
although formally their centroids are separated by more than
4σ. Additionally, the region below 3 keV is difficult to model
precisely, especially at large exposures, due to the presence of
the absorption edge and galactic emission. However, although
the residuals below 3 keV are similar between the M31 dataset
(Fig. 1) and the blank sky dataset (Fig. 3), the line is not de-
tected in the latter. Although the count rate at these energies
is 4 times larger for M31, the exposure for the blank sky is 16
times larger. This disfavors the interpretation of the line as due
to a wiggle in the effective area. The properties of this line are
consistent (within uncertainties) with the DM interpretation.
To reach a conclusion about its nature, one will need to find
more objects that give a detection or where non-observation of
the line will put tight constraints on its properties. The forth-
coming Astro-H mission [34] has sufficient spectral resolution
to spectrally resolve the line against other nearby features and
5. 5
InteractionstrengthSin
2
(2θ)
Dark matter mass MDM [keV]
10-13
10-12
10-11
10-10
10-9
10-8
10-7
2 5 501 10
DM overproduction
Not enough DM
Tremaine-Gunn/Lyman-α
Excluded by X-ray observations
InteractionstrengthSin
2
(2θ)
Dark matter mass MDM [keV]
10-13
10-12
10-11
10-10
10-9
10-8
10-7
2 5 501 10
DM overproduction
Not enough DM
Tremaine-Gunn/Lyman-α
Excluded by X-ray observations
InteractionstrengthSin
2
(2θ)
Dark matter mass MDM [keV]
10-13
10-12
10-11
10-10
10-9
10-8
10-7
2 5 501 10
DM overproduction
Not enough DM
Tremaine-Gunn/Lyman-α
Excluded by X-ray observations
InteractionstrengthSin
2
(2θ)
Dark matter mass MDM [keV]
10-13
10-12
10-11
10-10
10-9
10-8
10-7
2 5 501 10
DM overproduction
Not enough DM
Tremaine-Gunn/Lyman-α
Excluded by X-ray observations
InteractionstrengthSin
2
(2θ)
Dark matter mass MDM [keV]
10-13
10-12
10-11
10-10
10-9
10-8
10-7
2 5 501 10
DM overproduction
Not enough DM
Tremaine-Gunn/Lyman-α
Excluded by X-ray observations
FIG. 4: Constraints on sterile neutrino DM within νMSM [4]. The
blue point would corresponds to the best-fit value from M31 if the
line comes from DM decay. Thick errorbars are ±1σ limits on the
flux. Thin errorbars correspond to the uncertainty in the DM distri-
bution in the center of M31.
to detect the candidate line in the “strong line” regime [35]. In
particular, Astro-H should be able to resolve the Milky Way
halo’s DM decay signal and therefore all its observations can
be used. Failure to detect such a line will rule out the DM
origin of the Andromeda/Perseus signal presented here.
Acknowledgments. We thank D. Malyshev for collaboration;
A. Neronov for useful critical comments; M. Shaposhnikov
and M. Lovell for reading the manuscript and providing com-
ment. The work of D. I. was supported by part by the the
Program of Cosmic Research of the National Academy of Sci-
ences of Ukraine and the State Programme of Implementation
of Grid Technology in Ukraine.
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6. 6
Appendix A: Supplementary material
ObsID Off-axis angle Cleaned exposure FoV [arcmin2
] Fin-Fout
arcmin MOS1/MOS2 [ksec] MOS1/MOS2
1 0305690301 22.80 18.6 / 18.6 473.6 / 574.3 1.266 / 1.340
2 0085590201 25.01 40.1 / 40.5 564.6 / 572.1 1.290 / 1.336
3 0204720101 27.87 14.1 / 14.5 567.7 / 574.5 2.373 / 2.219
4 0673020401 29.48 15.6 / 17.6 479.6 / 574.0 1.318 / 1.331
5 0405410201 29.52 16.1 / 16.6 480.8 / 573.9 1.354 / 1.366
6 0305690101 29.54 25.1 / 25.4 476.0 / 573.5 1.231 / 1.247
7 0405410101 31.17 15.8 / 16.8 481.8 / 572.9 1.235 / 1.195
8 0305720101 31.23 11.5 / 11.8 476.8 / 573.9 1.288 / 1.296
9 0673020301 36.54 13.9 / 15.4 485.4 / 573.8 1.211 / 1.304
10 0305690401 36.75 25.9 / 26.0 479.1 / 573.8 1.158 / 1.156
11 0305720301 41.92 16.7 / 17.5 464.7 / 573.6 1.433 / 1.447
12 0151560101 47.42 23.7 / 23.6 572.1 / 573.6 1.294 / 1.206
13 0673020201 53.31 22.8 / 23.4 479.5 / 573.9 1.262 / 1.228
14 0204720201 54.11 22.4 / 22.9 564.0 / 573.2 1.153 / 1.195
15 0554500801 95.45 15.0 / 15.3 480.8 / 572.7 1.098 / 1.113
16 0306680301 101.88 12.3 / 13.0 468.1 / 574.0 1.177 / 1.089
TABLE II: Parameters of the XMM-Newton spectra of Perseus cluster used in our analysis. The observations are sorted by
off-axis angle from the center of the Perseus cluster. Two observations on-center (ObsIDs 0305780101 and 0085110101)
are not included in the analysis. The difference in FoVs between MOS1 and MOS2 cameras is due to the loss CCD6 in
MOS1 camera. The parameter Fin-Fout (last column) estimates the presence of residual soft protons according to the pro-
cedure of [14] is also shown. Note, however, that for the bright extended sources, such an estimate is not appropriate,
see http://xmm2.esac.esa.int/external/xmm_sw_cal/background/epic_scripts.shtml for details).
p