A Campanha de Linha de Base Longa do ALMA produziu uma imagem muito detalhada de uma galáxia distante afetada por lente gravitacional. A imagem mostra uma vista ampliada das regiões de formação estelar na galáxia, com um nível de detalhe nunca antes alcançado numa galáxia tão remota. As novas observações são muito mais detalhadas do que as obtidas pelo Telescópio Espacial Hubble da NASA/ESA e revelam regiões de formação estelar na galáxia equivalentes a versões gigantes da Nebulosa de Orion.
A Campanha de Linha de Base Longa do ALMA produziu algumas observações extraordinárias e coletou informação com um detalhe sem precedentes dos habitantes do Universo próximo e longínquo. Foram feitas observações no final de 2014 no âmbito de uma campanha que pretendeu estudar uma galáxia distante chamada HATLAS J090311.6+003906, também conhecida pelo nome mais simples de SDP.81. A radiação emitida por esta galáxia é “vítima” de um efeito cósmico chamado lente gravitacional. Uma galáxia enorme que se situa entre SDP.81 e o ALMA [1] atua como lente gravitacional, distorcendo a radiação emitida pela galáxia mais distante e criando um exemplo quase perfeito do fenômeno conhecido por Anel de Einstein [2].
Pelo menos sete grupos de cientistas [3] analisaram de forma independente os dados do ALMA sobre SDP.81. Esta profusão de artigos científicos deu-nos informação sem precedentes sobre esta galáxia, revelando detalhes sobre a sua estrutura, conteúdo, movimento e outras características físicas.
O ALMA funciona como um interferômetro, isto é, a rede múltipla de antenas trabalha em sintonia perfeita coletando radiação como se de um único e enorme telescópio virtual se tratasse [4]. Como resultado, estas novas imagens de SDP.81 possuem uma resolução até 6 vezes melhor [5] que as imagens obtidas no infravermelho com o Telescópio Espacial Hubble da NASA/ESA.
Alignment of quasar_polarizations_with_large_scale_structuresSérgio Sacani
This document summarizes research measuring the optical polarization of quasars belonging to large-scale quasar groups at redshift z~1.3. Of 93 quasars observed, 19 were significantly polarized. The polarization vectors of these quasars were found to be either parallel or perpendicular to the directions of the large-scale structures they belong to, with a statistical probability of this being due to random orientations of only ~1%. Quasars with polarization perpendicular to their structures tended to have broader emission lines, while those parallel had narrower lines, suggesting quasar spin axes are parallel to their host large-scale structures.
Weak Gravitational Lensing and Gauss-Bonnet Theorem discusses using the Gauss-Bonnet theorem to calculate light deflection angles in various spacetime geometries, including:
1. Calculating the deflection angle of light near a Schwarzschild black hole using the optical geometry and Gaussian curvature.
2. Computing the deflection of light by dyonic wormholes in Einstein-Maxwell-Dilaton theory and showing the deflection depends on the electric, magnetic, and dilaton charges.
3. Finding the deflection angle of light is inversely proportional to the Rindler acceleration for a Rindler modified Schwarzschild black hole.
This document discusses several topics related to cosmology and the search for extraterrestrial life, including:
1) Dimensionless numbers and ratios in physics and cosmology like the fine structure constant and ratios involving cosmological and atomic quantities.
2) Estimates of the number of atoms in the observable universe and other cosmological values.
3) The Drake equation and Fermi paradox regarding the search for extraterrestrial intelligence.
4) Coincidences between values that seem finely-tuned to allow for life like nuclear resonance energies.
This document summarizes a study measuring the transverse beam emittance at the Energy Selection System (ESS) of the KIRAMS-430 superconducting cyclotron. The researchers used a quadrupole variation method, where they varied the magnetic strength of a quadrupole magnet and measured the resulting beam size at a beam profile monitor. They analyzed the measurements using both linear matrix formalism and particle tracking simulations. The results from both analysis methods were consistent with emittances calculated from Monte Carlo simulations within the measurement uncertainties. The study demonstrated the feasibility of using the quadrupole variation method to characterize the beam quality at the ESS ion beamline.
This document discusses three key questions in cosmology: dark matter, inflation, and dark energy. It provides evidence for dark matter from early observations of galaxy rotation curves and clusters. It also summarizes modern evidence from Planck for the matter content of the universe. Regarding inflation, it discusses the generic predictions and open questions about the inflaton field. For dark energy, it reviews evidence from supernovae and Planck and discusses theoretical challenges like the fine-tuning and coincidence problems. It also outlines proposed and ongoing experiments to better understand dark matter, inflation, and dark energy.
The document discusses several topics in graph theory including Feynman diagrams in physics, the smallest strongly connected spanning subgraph problem, and algorithms for finding optimal spanning arborescences. It describes how Feynman diagrams represent particle interactions using graphs and outlines Edmonds' algorithm and Karp's proof for finding an optimum spanning arborescence in polynomial time by reducing the original problem to a simpler derived problem. The Chu-Liu algorithm for this problem is also summarized in 3 steps.
Alignment of quasar_polarizations_with_large_scale_structuresSérgio Sacani
This document summarizes research measuring the optical polarization of quasars belonging to large-scale quasar groups at redshift z~1.3. Of 93 quasars observed, 19 were significantly polarized. The polarization vectors of these quasars were found to be either parallel or perpendicular to the directions of the large-scale structures they belong to, with a statistical probability of this being due to random orientations of only ~1%. Quasars with polarization perpendicular to their structures tended to have broader emission lines, while those parallel had narrower lines, suggesting quasar spin axes are parallel to their host large-scale structures.
Weak Gravitational Lensing and Gauss-Bonnet Theorem discusses using the Gauss-Bonnet theorem to calculate light deflection angles in various spacetime geometries, including:
1. Calculating the deflection angle of light near a Schwarzschild black hole using the optical geometry and Gaussian curvature.
2. Computing the deflection of light by dyonic wormholes in Einstein-Maxwell-Dilaton theory and showing the deflection depends on the electric, magnetic, and dilaton charges.
3. Finding the deflection angle of light is inversely proportional to the Rindler acceleration for a Rindler modified Schwarzschild black hole.
This document discusses several topics related to cosmology and the search for extraterrestrial life, including:
1) Dimensionless numbers and ratios in physics and cosmology like the fine structure constant and ratios involving cosmological and atomic quantities.
2) Estimates of the number of atoms in the observable universe and other cosmological values.
3) The Drake equation and Fermi paradox regarding the search for extraterrestrial intelligence.
4) Coincidences between values that seem finely-tuned to allow for life like nuclear resonance energies.
This document summarizes a study measuring the transverse beam emittance at the Energy Selection System (ESS) of the KIRAMS-430 superconducting cyclotron. The researchers used a quadrupole variation method, where they varied the magnetic strength of a quadrupole magnet and measured the resulting beam size at a beam profile monitor. They analyzed the measurements using both linear matrix formalism and particle tracking simulations. The results from both analysis methods were consistent with emittances calculated from Monte Carlo simulations within the measurement uncertainties. The study demonstrated the feasibility of using the quadrupole variation method to characterize the beam quality at the ESS ion beamline.
This document discusses three key questions in cosmology: dark matter, inflation, and dark energy. It provides evidence for dark matter from early observations of galaxy rotation curves and clusters. It also summarizes modern evidence from Planck for the matter content of the universe. Regarding inflation, it discusses the generic predictions and open questions about the inflaton field. For dark energy, it reviews evidence from supernovae and Planck and discusses theoretical challenges like the fine-tuning and coincidence problems. It also outlines proposed and ongoing experiments to better understand dark matter, inflation, and dark energy.
The document discusses several topics in graph theory including Feynman diagrams in physics, the smallest strongly connected spanning subgraph problem, and algorithms for finding optimal spanning arborescences. It describes how Feynman diagrams represent particle interactions using graphs and outlines Edmonds' algorithm and Karp's proof for finding an optimum spanning arborescence in polynomial time by reducing the original problem to a simpler derived problem. The Chu-Liu algorithm for this problem is also summarized in 3 steps.
The document describes two algorithms for enhancing cometary coma morphology in digital images: the radial weighted model and median coma model. The radial weighted model multiplies each pixel value by its distance from the comet's nucleus, removing the typical 1/r intensity gradient. The median coma model calculates the median pixel value on concentric circles from the nucleus to build a synthetic coma model, which can then be subtracted from or divided into the original image. Examples show how these techniques enhance structural details in cometary comae compared to unprocessed images. The source code for implementing these algorithms is freely available online.
This document summarizes the key concepts around harmonic excitation of undamped and damped systems from Chapter 2. It introduces the important concept of resonance that occurs when the driving frequency matches the natural frequency of the system. For an undamped system under harmonic excitation, the response is the sum of the homogeneous and particular solutions. The particular solution assumes the form of the driving force. When the driving frequency approaches the natural frequency, the amplitude of the response increases dramatically. For a damped system, the particular solution includes a phase shift.
The build up_of_the_c_d_halo_of_m87_evidence_for_accretion_in_the_last_gyrSérgio Sacani
Observações recentes obtidas com o Very Large Telescope do ESO mostraram que Messier 87, a galáxia elíptica gigante mais próximo de nós, engoliu uma galáxia inteira de tamanho médio no último bilhão de anos. Uma equipe de astrônomos conseguiu pela primeira vez seguir o movimento de 300 nebulosas planetárias brilhantes, encontrando evidências claras deste evento e encontrando também excesso de radiação emitida pelos restos da vítima completamente desfeita.
Chiral Particle/Photon emission from heavy-light mesonsTakayuki Matsuki
This document presents a relativistic calculation of one-particle decay widths from heavy-light mesons. It first discusses the successful prediction of heavy-light meson mass spectra using a semi-relativistic potential model. It then outlines the fundamental formulation of one-particle decays and develops a relativistic formulation that includes corrections to the wave functions and relation between moving and static wave functions. Numerical results for one pion/photon emission from excited D, B, and Ds mesons are presented, showing sizable decay widths compared to non-relativistic calculations. The paper concludes by taking the non-relativistic limit and recovering previous results.
The document discusses deformation spectra for single-degree-of-freedom (SDF) linear systems subjected to base excitation. It presents the equations of motion for an SDF system with a moving base and defines terms like relative displacement and pseudo-acceleration. Graphs of deformation spectra are shown for half-cycle acceleration and velocity pulses. Key aspects of the spectra under different inputs are described, including asymptotic behavior and sensitivity to displacement, velocity, and acceleration portions of the input.
This document provides an overview of cosmic microwave background radiation and its theoretical framework. It discusses how CMB was discovered and its importance as evidence for the Big Bang model. The document outlines the theoretical concepts behind CMB, including the standard cosmological model, Friedman equations, perturbations in spacetime metric, and using the Boltzmann equation to model changes in particle densities as the universe expands. It also provides background on key observational findings about CMB from missions like COBE, WMAP and Planck.
The document describes a phase field model of droplet coalescence coupled with a chemical reaction. It aims to study the effect of fluid flow on mixing and reaction rate during droplet coalescence. Governing equations for phase field, fluid flow, and reaction-diffusion are presented. Simulations are performed for droplets with equal and unequal radii, varying fluid viscosities. Results show the neck growth rate during coalescence and evolution of reactants and products over time.
Alessandra Buonanno gave a lecture on the analytical and numerical relativity approaches used to model gravitational waveforms from inspiraling binary systems. She discussed how post-Newtonian theory, effective one body theory, and numerical relativity are used to approximately and exactly solve Einstein's field equations. She emphasized the crucial synergy between analytical and numerical relativity approaches to develop accurate gravitational waveform models like EOBNR and Phenom that have been used to infer astrophysics from LIGO/Virgo detections.
Efficient mode-matching analysis of 2-D scattering by periodic array of circu...Yong Heui Cho
This document proposes a new mode-matching method for analyzing periodic arrays of circular cylinders with different materials. It uses a common-area concept and infinitesimal perfect magnetic conductor wires to match boundary conditions between rectangular and cylindrical coordinate systems. This allows derivation of scattering equations for the arrays. The solutions are compared to other results to validate the method. It can be used to study resonance characteristics of nanostructures and scattering behavior at different frequencies.
The document contains multiple physics problems related to rotation, torque, angular acceleration, and moments of inertia. One problem involves calculating the angular speed of a winch drum that is lifting a 2000 kg block at a constant speed of 8 cm/s. It is determined that:
- The tension in the cable equals 19.6 kN, given by the weight of the block
- The torque exerted on the winch drum by the cable is 5.9 mkN
- The angular speed of the winch drum is 0.27 rad/s
- The power required by the motor is 1.6 kW
Overlapping T-block analysis of axially grooved rectangular waveguideYong Heui Cho
This document presents an analysis of the dispersion relations of an axially grooved rectangular waveguide using an overlapping T-block approach. The waveguide structure is divided into three overlapping asymmetric T-blocks. Field representations are derived for each T-block and combined to determine the total field. By enforcing field continuity conditions, the TE and TM dispersion relations are obtained. Numerical results for the cutoff frequencies are presented and show good agreement with other methods.
Higher-Order Squeezing of a Generic Quadratically-Coupled Optomechanical SystemIOSRJAP
Using short-time dynamics and analytical solution of Heisenberg equation of motion for the Hamiltonian of quadratically-coupled optomechanical system for different field modes, we have investigated the existence of higher-order single mode squeezing, sum squeezing and difference squeezing in absence of driving and dissipation. Depth of squeezing increases with order number for higher-order single mode squeezing. Squeezing factor exhibits a series of revival-collapse phenomena for single mode, which becomes more pronounced as order number increases. In case of sum squeezing amounts of squeezing is greater than single mode higher-order squeezing (n = 2). It is also greater than from difference squeezing for same set of interaction parameters. Sum squeezing is prominently better for extracting information regarding squeezing.
This document summarizes a presentation about reconstructing inflationary models in modified f(R) gravity. It discusses the current status of inflation based on Planck data, reviews how inflation works in f(R) gravity, and describes two approaches - the direct approach of comparing models to data and the inverse approach of smoothly reconstructing models from observational quantities like the scalar spectrum index. A key model discussed is the simple R + R^2 model that can match current measurements of the spectral index and tensor-to-scalar ratio.
This document analyzes the dispersion of multiple V-groove waveguides using Fourier transforms and mode matching. It presents a new rigorous dispersion relation in a fast-converging series for efficient numerical calculation. A closed-form dispersion relation based on a dominant mode approximation is shown to be accurate for practical applications involving double and triple V-groove guides. Field distributions are presented that confirm the validity of the dominant mode approximation.
FREQUENCY RESPONSE ANALYSIS OF 3-DOF HUMAN LOWER LIMBSIJCI JOURNAL
Frequent and prolonged expose of human body to vibrations can induce back pain and physical disorder
and degeneration of tissue. The biomechanical model of human lower limbs are modeled as a three degree
of freedom linear spring-mass-damper system to estimate forces and frequencies. Then three degree of
freedom system was analysed using state space method to find natural frequency and mode shape. A
program was develop to solve simplified equations and results were plotted and discussed in detail. The
mass, stiffness and damping coefficient of various segments are taken from references. The optimal values
of the damping ratios of the body segments are estimated, for the three degrees of freedom model. At last
resonance frequencies are found to avoid expose of lower limbs to such environment for optimum comfort.
Primordial gravitational waves from inflation could be detected using the cosmic microwave background. Gravitational waves passing through the last scattering surface would induce B-mode polarization patterns in the CMB. Future experiments aim to detect these B-modes as a signature of primordial gravitational waves, which would provide insights into inflation and the very early universe.
The canarias einstein_ring_a_newly_discovered_optical_einstein_ringSérgio Sacani
This document reports the discovery of a newly discovered optical Einstein ring (ER) called the "Canarias Einstein Ring". It was discovered serendipitously in imaging data from the Dark Energy Camera. Follow-up spectroscopy with the Gran Telescopio CANARIAS confirmed the nature of the system, with the lens being an early-type galaxy at a redshift of z=0.581 and the source being a starburst galaxy at z=1.165. Analysis of the system determined the Einstein radius to be 2.16 arcseconds and the total enclosed mass producing the lensing effect to be 1.86 ± 0.23 × 1012 solar masses.
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.
MUSE sneaks a peek at extreme ram-pressure stripping events. I. A kinematic s...Sérgio Sacani
- MUSE observations of the galaxy ESO137-001 reveal an extended gaseous tail over 30 kpc long traced by H-alpha emission, providing evidence of an extreme ram pressure stripping event as the galaxy falls into the massive Norma galaxy cluster.
- Analysis of the H-alpha kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center, with gravitational interactions not appearing to be the main mechanism of gas removal.
- The stripped gas retains evidence of the disk's rotational velocity out to around 20 kpc downstream, indicating the galaxy is moving radially along the plane of the sky, while
This document describes observations of the galaxy ESO137-001 using the MUSE instrument on the VLT. The key points are:
1) MUSE observations reveal an extended gas tail stretching over 30 kpc from the galaxy, tracing ongoing ram pressure stripping as it falls into the Norma galaxy cluster.
2) Analysis of the gas kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center.
3) The stripped gas retains evidence of the disk's rotational velocity out to 20 kpc downstream, indicating the galaxy is moving radially through the cluster. Beyond this the gas shows greater turbulence,
The document describes two algorithms for enhancing cometary coma morphology in digital images: the radial weighted model and median coma model. The radial weighted model multiplies each pixel value by its distance from the comet's nucleus, removing the typical 1/r intensity gradient. The median coma model calculates the median pixel value on concentric circles from the nucleus to build a synthetic coma model, which can then be subtracted from or divided into the original image. Examples show how these techniques enhance structural details in cometary comae compared to unprocessed images. The source code for implementing these algorithms is freely available online.
This document summarizes the key concepts around harmonic excitation of undamped and damped systems from Chapter 2. It introduces the important concept of resonance that occurs when the driving frequency matches the natural frequency of the system. For an undamped system under harmonic excitation, the response is the sum of the homogeneous and particular solutions. The particular solution assumes the form of the driving force. When the driving frequency approaches the natural frequency, the amplitude of the response increases dramatically. For a damped system, the particular solution includes a phase shift.
The build up_of_the_c_d_halo_of_m87_evidence_for_accretion_in_the_last_gyrSérgio Sacani
Observações recentes obtidas com o Very Large Telescope do ESO mostraram que Messier 87, a galáxia elíptica gigante mais próximo de nós, engoliu uma galáxia inteira de tamanho médio no último bilhão de anos. Uma equipe de astrônomos conseguiu pela primeira vez seguir o movimento de 300 nebulosas planetárias brilhantes, encontrando evidências claras deste evento e encontrando também excesso de radiação emitida pelos restos da vítima completamente desfeita.
Chiral Particle/Photon emission from heavy-light mesonsTakayuki Matsuki
This document presents a relativistic calculation of one-particle decay widths from heavy-light mesons. It first discusses the successful prediction of heavy-light meson mass spectra using a semi-relativistic potential model. It then outlines the fundamental formulation of one-particle decays and develops a relativistic formulation that includes corrections to the wave functions and relation between moving and static wave functions. Numerical results for one pion/photon emission from excited D, B, and Ds mesons are presented, showing sizable decay widths compared to non-relativistic calculations. The paper concludes by taking the non-relativistic limit and recovering previous results.
The document discusses deformation spectra for single-degree-of-freedom (SDF) linear systems subjected to base excitation. It presents the equations of motion for an SDF system with a moving base and defines terms like relative displacement and pseudo-acceleration. Graphs of deformation spectra are shown for half-cycle acceleration and velocity pulses. Key aspects of the spectra under different inputs are described, including asymptotic behavior and sensitivity to displacement, velocity, and acceleration portions of the input.
This document provides an overview of cosmic microwave background radiation and its theoretical framework. It discusses how CMB was discovered and its importance as evidence for the Big Bang model. The document outlines the theoretical concepts behind CMB, including the standard cosmological model, Friedman equations, perturbations in spacetime metric, and using the Boltzmann equation to model changes in particle densities as the universe expands. It also provides background on key observational findings about CMB from missions like COBE, WMAP and Planck.
The document describes a phase field model of droplet coalescence coupled with a chemical reaction. It aims to study the effect of fluid flow on mixing and reaction rate during droplet coalescence. Governing equations for phase field, fluid flow, and reaction-diffusion are presented. Simulations are performed for droplets with equal and unequal radii, varying fluid viscosities. Results show the neck growth rate during coalescence and evolution of reactants and products over time.
Alessandra Buonanno gave a lecture on the analytical and numerical relativity approaches used to model gravitational waveforms from inspiraling binary systems. She discussed how post-Newtonian theory, effective one body theory, and numerical relativity are used to approximately and exactly solve Einstein's field equations. She emphasized the crucial synergy between analytical and numerical relativity approaches to develop accurate gravitational waveform models like EOBNR and Phenom that have been used to infer astrophysics from LIGO/Virgo detections.
Efficient mode-matching analysis of 2-D scattering by periodic array of circu...Yong Heui Cho
This document proposes a new mode-matching method for analyzing periodic arrays of circular cylinders with different materials. It uses a common-area concept and infinitesimal perfect magnetic conductor wires to match boundary conditions between rectangular and cylindrical coordinate systems. This allows derivation of scattering equations for the arrays. The solutions are compared to other results to validate the method. It can be used to study resonance characteristics of nanostructures and scattering behavior at different frequencies.
The document contains multiple physics problems related to rotation, torque, angular acceleration, and moments of inertia. One problem involves calculating the angular speed of a winch drum that is lifting a 2000 kg block at a constant speed of 8 cm/s. It is determined that:
- The tension in the cable equals 19.6 kN, given by the weight of the block
- The torque exerted on the winch drum by the cable is 5.9 mkN
- The angular speed of the winch drum is 0.27 rad/s
- The power required by the motor is 1.6 kW
Overlapping T-block analysis of axially grooved rectangular waveguideYong Heui Cho
This document presents an analysis of the dispersion relations of an axially grooved rectangular waveguide using an overlapping T-block approach. The waveguide structure is divided into three overlapping asymmetric T-blocks. Field representations are derived for each T-block and combined to determine the total field. By enforcing field continuity conditions, the TE and TM dispersion relations are obtained. Numerical results for the cutoff frequencies are presented and show good agreement with other methods.
Higher-Order Squeezing of a Generic Quadratically-Coupled Optomechanical SystemIOSRJAP
Using short-time dynamics and analytical solution of Heisenberg equation of motion for the Hamiltonian of quadratically-coupled optomechanical system for different field modes, we have investigated the existence of higher-order single mode squeezing, sum squeezing and difference squeezing in absence of driving and dissipation. Depth of squeezing increases with order number for higher-order single mode squeezing. Squeezing factor exhibits a series of revival-collapse phenomena for single mode, which becomes more pronounced as order number increases. In case of sum squeezing amounts of squeezing is greater than single mode higher-order squeezing (n = 2). It is also greater than from difference squeezing for same set of interaction parameters. Sum squeezing is prominently better for extracting information regarding squeezing.
This document summarizes a presentation about reconstructing inflationary models in modified f(R) gravity. It discusses the current status of inflation based on Planck data, reviews how inflation works in f(R) gravity, and describes two approaches - the direct approach of comparing models to data and the inverse approach of smoothly reconstructing models from observational quantities like the scalar spectrum index. A key model discussed is the simple R + R^2 model that can match current measurements of the spectral index and tensor-to-scalar ratio.
This document analyzes the dispersion of multiple V-groove waveguides using Fourier transforms and mode matching. It presents a new rigorous dispersion relation in a fast-converging series for efficient numerical calculation. A closed-form dispersion relation based on a dominant mode approximation is shown to be accurate for practical applications involving double and triple V-groove guides. Field distributions are presented that confirm the validity of the dominant mode approximation.
FREQUENCY RESPONSE ANALYSIS OF 3-DOF HUMAN LOWER LIMBSIJCI JOURNAL
Frequent and prolonged expose of human body to vibrations can induce back pain and physical disorder
and degeneration of tissue. The biomechanical model of human lower limbs are modeled as a three degree
of freedom linear spring-mass-damper system to estimate forces and frequencies. Then three degree of
freedom system was analysed using state space method to find natural frequency and mode shape. A
program was develop to solve simplified equations and results were plotted and discussed in detail. The
mass, stiffness and damping coefficient of various segments are taken from references. The optimal values
of the damping ratios of the body segments are estimated, for the three degrees of freedom model. At last
resonance frequencies are found to avoid expose of lower limbs to such environment for optimum comfort.
Primordial gravitational waves from inflation could be detected using the cosmic microwave background. Gravitational waves passing through the last scattering surface would induce B-mode polarization patterns in the CMB. Future experiments aim to detect these B-modes as a signature of primordial gravitational waves, which would provide insights into inflation and the very early universe.
The canarias einstein_ring_a_newly_discovered_optical_einstein_ringSérgio Sacani
This document reports the discovery of a newly discovered optical Einstein ring (ER) called the "Canarias Einstein Ring". It was discovered serendipitously in imaging data from the Dark Energy Camera. Follow-up spectroscopy with the Gran Telescopio CANARIAS confirmed the nature of the system, with the lens being an early-type galaxy at a redshift of z=0.581 and the source being a starburst galaxy at z=1.165. Analysis of the system determined the Einstein radius to be 2.16 arcseconds and the total enclosed mass producing the lensing effect to be 1.86 ± 0.23 × 1012 solar masses.
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.
MUSE sneaks a peek at extreme ram-pressure stripping events. I. A kinematic s...Sérgio Sacani
- MUSE observations of the galaxy ESO137-001 reveal an extended gaseous tail over 30 kpc long traced by H-alpha emission, providing evidence of an extreme ram pressure stripping event as the galaxy falls into the massive Norma galaxy cluster.
- Analysis of the H-alpha kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center, with gravitational interactions not appearing to be the main mechanism of gas removal.
- The stripped gas retains evidence of the disk's rotational velocity out to around 20 kpc downstream, indicating the galaxy is moving radially along the plane of the sky, while
This document describes observations of the galaxy ESO137-001 using the MUSE instrument on the VLT. The key points are:
1) MUSE observations reveal an extended gas tail stretching over 30 kpc from the galaxy, tracing ongoing ram pressure stripping as it falls into the Norma galaxy cluster.
2) Analysis of the gas kinematics and stellar velocity field show that ram pressure has removed the interstellar medium from the outer disk while the primary tail is still fed by gas from the galaxy center.
3) The stripped gas retains evidence of the disk's rotational velocity out to 20 kpc downstream, indicating the galaxy is moving radially through the cluster. Beyond this the gas shows greater turbulence,
A giant galaxy in the young Universe with a massive ringSérgio Sacani
In the local (redshift z ≈ 0) Universe, collisional ring galaxies make up only ~0.01% of galaxies1 and are formed by head-on galactic collisions that trigger radially propagating density waves2–4. These striking systems provide key snapshots for dissecting galactic disks and are studied extensively in the local Universe5–9. However, not much is known about distant (z > 0.1) collisional rings10–14. Here we present a detailed study of a ring galaxy at a look-back time of 10.8 Gyr (z = 2.19). Compared with our Milky Way, this galaxy has a similar stellar mass, but has a stellar half-light radius that is 1.5–2.2 times larger and is forming stars 50 times faster. The extended, dif- fuse stellar light outside the star-forming ring, combined with a radial velocity on the ring and an intruder galaxy nearby, provides evidence for this galaxy hosting a collisional ring. If the ring is secularly evolved15,16, the implied large bar in a giant disk would be inconsistent with the current understand- ing of the earliest formation of barred spirals17–21. Contrary to previous predictions10–12, this work suggests that massive col- lisional rings were as rare 11 Gyr ago as they are today. Our discovery offers a unique pathway for studying density waves in young galaxies, as well as constraining the cosmic evolution of spiral disks and galaxy groups.
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
A dust-enshrouded tidal disruption event with a resolved radio jet in a galax...Sérgio Sacani
Tidal disruption events (TDEs) are transient flares produced when a star is ripped apart by the
gravitational field of a supermassive black hole (SMBH). We have observed a transient source in the
western nucleus of the merging galaxy pair Arp 299 that radiated >1.5 × 1052 erg in the infrared and radio
but was not luminous at optical or x-ray wavelengths. We interpret this as a TDE with much of its emission
reradiated at infrared wavelengths by dust. Efficient reprocessing by dense gas and dust may explain the
difference between theoretical predictions and observed luminosities of TDEs. The radio observations
resolve an expanding and decelerating jet, probing the jet formation and evolution around a SMBH.
Triple Spiral Arms of a Triple Protostar System Imaged in Molecular LinesSérgio Sacani
Most stars form in multiple-star systems. For a better understanding of their formation processes, it is important to
resolve the individual protostellar components and the surrounding envelope and disk material at the earliest
possible formation epoch, because the formation history can be lost in a few orbital timescales. Here we present
Atacama Large Millimeter/submillimeter Array observational results of a young multiple protostellar system,
IRAS 04239+2436, where three well-developed large spiral arms were detected in the shocked SO emission.
Along the most conspicuous arm, the accretion streamer was also detected in the SO2 emission. The observational
results are complemented by numerical magnetohydrodynamic simulations, where those large arms only appear in
magnetically weakened clouds. Numerical simulations also suggest that the large triple spiral arms are the result of
gravitational interactions between compact triple protostars and the turbulent infalling envelope.
X-RAY MEASUREMENTS OF THE PARTICLE ACCELERATION PROPERTIES AT INWARD SHOCKS I...Sérgio Sacani
We present new evidence that the bright non-thermal X-ray emission features in the interior of the Cassiopeia A
supernova remnant (SNR) are caused by inward moving shocks based on Chandra and NuSTAR observations. Several
bright inward-moving filaments were identified using monitoring data taken by Chandra in 2000–2014. These inwardmoving shock locations are nearly coincident with hard X-ray (15–40 keV) hot spots seen by NuSTAR. From proper
motion measurements, the transverse velocities were estimated to be in the range ∼2,100–3,800 km s−1
for a distance of
3.4 kpc. The shock velocities in the frame of the expanding ejecta reach values of ∼5,100–8,700 km s−1
, slightly higher
than the typical speed of the forward shock. Additionally, we find flux variations (both increasing and decreasing) on
timescales of a few years in some of the inward-moving shock filaments. The rapid variability timescales are consistent
with an amplified magnetic field of B ∼ 0.5–1 mG. The high speed and low photon cut-off energy of the inward-moving
shocks are shown to imply a particle diffusion coefficient that departs from the Bohm regime (k0 = D0/D0,Bohm ∼ 3–8)
for the few simple physical configurations we consider in this study. The maximum electron energy at these shocks is
estimated to be ∼8–11 TeV, smaller than the values of ∼15–34 TeV inferred for the forward shock. Cassiopeia A is
dynamically too young for its reverse shock to appear to be moving inward in the observer frame. We propose instead
that the inward-moving shocks are a consequence of the forward shock encountering a density jump of & 5–8 in the
surrounding material.
ALMA Observations of the Extraordinary Carina Pillars: A Complementary SampleSérgio Sacani
We present a study of six dusty and gaseous pillars (containing the HH 1004 and HH 1010 objects)
and globules (that contain the HH 666, HH 900, HH 1006, and HH 1066 objects) localized in the Carina
nebula using sensitive and high angular resolution (∼0.3′′) Atacama Large Millimeter/Sub-millimeter
Array (ALMA) observations. This is a more extensive study that the one presented in Cortes-Rangel
et al. (2020). As in this former study, we also analyzed the 1.3 mm continuum emission and C18O(2−1),
N2D+(3−2) and 12CO(2−1) spectral lines. These new observations revealed the molecular outflows
emanating from the pillars, the dusty envelopes+disks that are exciting them, and the extended HH
objects far from their respective pillars. We reveal that the masses of the disks+envelopes are in a
range of 0.02 to 0.38 M⊙, and those for the molecular outflows are of the order of 10−3 M⊙, which
suggests that their exciting sources might be low- or intermediate-mass protostars as already revealed
in recent studies at infrared and submillimeter bands. In the regions associated with the objects HH
900 and HH 1004, we report multiple millimeter continuum sources, from where several molecular
outflows emanate.
Keck Integral-field Spectroscopy of M87 Reveals an Intrinsically Triaxial Gal...Sérgio Sacani
The three-dimensional intrinsic shape of a galaxy and the mass of the central supermassive black hole provide key
insight into the galaxy’s growth history over cosmic time. Standard assumptions of a spherical or axisymmetric
shape can be simplistic and can bias the black hole mass inferred from the motions of stars within a galaxy. Here,
we present spatially resolved stellar kinematics of M87 over a two-dimensional 250″ × 300″ contiguous field
covering a radial range of 50 pc–12 kpc from integral-field spectroscopic observations at the Keck II Telescope.
From about 5 kpc and outward, we detect a prominent 25 km s−1 rotational pattern, in which the kinematic axis
(connecting the maximal receding and approaching velocities) is 40° misaligned with the photometric major axis of
M87. The rotational amplitude and misalignment angle both decrease in the inner 5 kpc. Such misaligned and
twisted velocity fields are a hallmark of triaxiality, indicating that M87 is not an axisymmetrically shaped galaxy.
Triaxial Schwarzschild orbit modeling with more than 4000 observational constraints enabled us to determine
simultaneously the shape and mass parameters. The models incorporate a radially declining profile for the stellar
mass-to-light ratio suggested by stellar population studies. We find that M87 is strongly triaxial, with ratios of
p = 0.845 for the middle-to-long principal axes and q = 0.722 for the short-to-long principal axes, and determine
the black hole mass to be ( - ´) 5.37 0.22 10 +
0.25
0.37 9M , where the second error indicates the systematic uncertainty
associated with the distance to M87.
SPECTROSCOPIC CONFIRMATION OF THE EXISTENCE OF LARGE, DIFFUSE GALAXIES IN THE...Sérgio Sacani
We recently identified a population of low surface brightness objects in the field of the z = 0.023 Coma cluster,
using the Dragonfly Telephoto Array. Here we present Keck spectroscopy of one of the largest of these “ultradiffuse
galaxies” (UDGs), confirming that it is a member of the cluster. The galaxy has prominent absorption
features, including the Ca II H+K lines and the G-band, and no detected emission lines. Its radial velocity of
cz=6280±120 km s−1 is within the 1σ velocity dispersion of the Coma cluster. The galaxy has an effective
radius of 4.3 ± 0.3 kpc and a Sérsic index of 0.89 ± 0.06, as measured from Keck imaging. We find no indications
of tidal tails or other distortions, at least out to a radius of ∼2re. We show that UDGs are located in a previously
sparsely populated region of the size—magnitude plane of quiescent stellar systems, as they are ∼6 mag fainter
than normal early-type galaxies of the same size. It appears that the luminosity distribution of large quiescent
galaxies is not continuous, although this could largely be due to selection effects. Dynamical measurements are
needed to determine whether the dark matter halos of UDGs are similar to those of galaxies with the same
luminosity or to those of galaxies with the same size.
The atacama cosmology_telescope_measuring_radio_galaxy_bias_through_cross_cor...Sérgio Sacani
A radiação cósmica de micro-ondas aponta para a matéria escura invisível, marcando o ponto onde jatos de material viajam a velocidades próximas da velocidade da luz, de acordo com uma equipe internacional de astrônomos. O principal autor do estudo, Rupert Allison da Universidade de Oxford apresentou os resultados no dia 6 de Julho de 2015 no National Astronomy Meeting em Venue Cymru, em Llandudno em Wales.
Atualmente, ninguém sabe ao certo do que a matéria escura é feita, mas ela é responsável por cerca de 26% do conteúdo de energia do universo, com galáxias massivas se formando em densas regiões de matéria escura. Embora invisível, a matéria escura se mostra através do efeito gravitacional – uma grande bolha de matéria escura puxa a matéria normal (como elétrons, prótons e nêutrons) através de sua própria gravidade, eventualmente se empacotando conjuntamente para criar as estrelas e galáxias inteiras.
Muitas das maiores dessas são galáxias ativas com buracos negros supermassivos em seus centros. Alguma parte do gás caindo diretamente na direção do buraco negro é ejetada como jatos de partículas e radiação. As observações feitas com rádio telescópios mostram que esses jatos as vezes se espalham por milhões de anos-luz desde a galáxia – mais distante até mesmo do que a extensão da própria galáxia.
Os cientistas esperam que os jatos possam viver em regiões onde existe um excesso de concentração da matéria escura, maior do que o da média. Mas como a matéria escura é invisível, testar essa ideia não é algo tão direto.
Dust in the_polar_region_as_a_major_contributor_to_the_infrared_emission_of_a...Sérgio Sacani
The mid-infrared emission of the active galactic nucleus NGC 3783 was observed using interferometry over multiple epochs, providing dense coverage of position angles and baselines. The emission was found to be strongly elongated along a position angle of -52 degrees, closely aligned with the polar axis orientation of -45 degrees. The half-light radii were measured to be 20.0 mas by 6.7 mas, corresponding to an axis ratio of 3:1. This implies that 60-90% of the 8-13 micron emission is from the polar-elongated component. The observations support a scenario where the majority of mid-infrared emission in Seyfert galaxies originates from a dusty wind in the polar region,
The shadow _of_the_flying_saucer_a_very_low_temperature_for_large_dust_grainsSérgio Sacani
Os astrónomos usaram o ALMA e os telescópios do IRAM para fazer a primeira medição direta da temperatura dos grãos de poeira grandes situados nas regiões periféricas de um disco de formação planetária que se encontra em torno de uma estrela jovem. Ao observar de forma inovadora um objeto cujo nome informal é Disco Voador, os astrónomos descobriram que os grãos de poeira são muito mais frios do que o esperado: -266º Celsius. Este resultado surpreendente sugere que os modelos teóricos destes discos precisam de ser revistos.
Uma equipa internacional liderada por Stephane Guilloteau do Laboratoire d´Astrophysique de Bordeaux, França, mediu a temperatura de enormes grãos de poeira que se encontram em torno da jovem estrela 2MASS J16281370-2431391 na região de formação estelar Rho Ophiuchi, a cerca de 400 anos-luz de distância da Terra.
Esta estrela encontra-se rodeada por um disco de gás e poeira — chamado disco protoplanetário, uma vez que se encontra na fase inicial da formação de um sistema planetário. Este disco é visto de perfil quando observado a partir da Terra e a sua aparência em imagens no visível levou a que se lhe desse o nome informal de Disco Voador.
Os astrónomos utilizaram o ALMA para observar o brilho emitido pelas moléculas de monóxido de carbono no disco da 2MASS J16281370-2431391. As imagens revelaram-se extremamente nítidas e descobriu-se algo estranho — em alguns casos o sinal recebido era negativo. Normalmente um sinal negativo é fisicamente impossível, mas neste caso existe uma explicação, que leva a uma conclusão surpreendente.
Spectroscopic confirmation of an ultra-faint galaxy at the epoch of reionizationSérgio Sacani
Within one billion years of the Big Bang, intergalactic hydrogen
was ionized by sources emitting ultraviolet and higher energy
photons. This was the final phenomenon to globally affect all
the baryons (visible matter) in the Universe. It is referred to
as cosmic reionization and is an integral component of cosmology.
It is broadly expected that intrinsically faint galaxies
were the primary ionizing sources due to their abundance
in this epoch1,2. However, at the highest redshifts (z > 7.5;
lookback time 13.1 Gyr), all galaxies with spectroscopic confirmations
to date are intrinsically bright and, therefore, not
necessarily representative of the general population3. Here,
we report the unequivocal spectroscopic detection of a low
luminosity galaxy at z > 7.5. We detected the Lyman-α emission
line at ∼10,504 Å in two separate observations with
MOSFIRE4 on the Keck I Telescope and independently with
the Hubble Space Telescope’s slitless grism spectrograph,
implying a source redshift of z = 7.640 ± 0.001. The galaxy
is gravitationally magnified by the massive galaxy cluster
MACS J1423.8+2404 (z = 0.545), with an estimated intrinsic
luminosity of MAB = −19.6 ± 0.2 mag and a stellar mass of
☆ = × − +
M 3.0 0.8 10
1.5 8 solar masses. Both are an order of magnitude
lower than the four other Lyman-α emitters currently
known at z > 7.5, making it probably the most distant representative
source of reionization found to date.
This document provides a multiwavelength summary of GRB 130427A, one of the brightest gamma-ray bursts ever detected. It was observed across the electromagnetic spectrum from gamma-rays to radio wavelengths. Key points:
1) GRB 130427A had an extremely high luminosity and energy release, similar to the most powerful high-redshift bursts.
2) Follow-up observations detected associated supernova SN 2013cq, showing that very energetic bursts can still be accompanied by supernovae.
3) Light curves at X-ray, optical, and ultraviolet wavelengths show evidence for a jet break approximately 37 kiloseconds after the burst.
4) Standard synchrotron shock models
First results from a prototype for the Fluorescence detector Array of Single-...Toshihiro FUJII
The document describes the Fluorescence detector Array of Single-pixel Telescopes (FAST) concept for observing ultra-high energy cosmic rays. The FAST prototype was tested using the EUSO-TA telescope and detected laser shots and 16 air shower candidates in coincidence with the Telescope Array fluorescence detector. A new FAST prototype is being constructed to establish its sensitivity and detect air shower profiles including the depth of shower maximum. The document outlines future plans to install FAST at the Pierre Auger Observatory and Telescope Array for cross-calibration and to independently measure energy and air shower maximum between the two experiments using a low-cost simplified fluorescence detector design.
PROBING THE SOLAR INTERIOR WITH LENSED GRAVITATIONAL WAVES FROM KNOWN PULSARSSérgio Sacani
When gravitational waves (GWs) from a spinning neutron star arrive from behind the Sun, they are
subjected to gravitational lensing that imprints a frequency-dependent modulation on the waveform.
This modulation traces the projected solar density and gravitational potential along the path as
the Sun passes in front of the neutron star. We calculate how accurately the solar density prole
can be extracted from the lensed GWs using a Fisher analysis. For this purpose, we selected three
promising candidates (the highly spinning pulsars J1022+1001, J1730-2304, and J1745-23) from the
pulsar catalog of the Australia Telescope National Facility. The lensing signature can be measured
with 3 condence when the signal-to-noise ratio (SNR) of the GW detection reaches 100 (f=300Hz)1
over a one-year observation period (where f is the GW frequency). The solar density prole can be
plotted as a function of radius when the SNR improves to & 104.
Detection of lyman_alpha_emission_from_a_triply_imaged_z_6_85_galaxy_behind_m...Sérgio Sacani
We report the detection of Ly emission at 9538A
in the Keck/DEIMOS and HST WFC3
G102 grism data from a triply-imaged galaxy at z = 6:846 0:001 behind galaxy cluster MACS
J2129.4 0741. Combining the emission line wavelength with broadband photometry, line ratio upper
limits, and lens modeling, we rule out the scenario that this emission line is [O II] at z = 1:57. After
accounting for magnication, we calculate the weighted average of the intrinsic Ly luminosity to be
1:31042 erg s 1 and Ly equivalent width to be 7415A. Its intrinsic UV absolute magnitude at
1600A
is 18:60:2 mag and stellar mass (1:50:3)107 M, making it one of the faintest (intrinsic
LUV 0:14 L
UV) galaxies with Ly detection at z 7 to date. Its stellar mass is in the typical range
for the galaxies thought to dominate the reionization photon budget at z & 7; the inferred Ly escape
fraction is high (& 10%), which could be common for sub-L z & 7 galaxies with Ly emission. This
galaxy oers a glimpse of the galaxy population that is thought to drive reionization, and it shows
that gravitational lensing is an important avenue to probe the sub-L galaxy population.
Similar to High resolution alma_observations_of_sdp81_the_innermost_mass_profile_of_the_lensing_elliptical_galaxy_probed_by_30_milli_arcsecond_images (20)
Discovery of An Apparent Red, High-Velocity Type Ia Supernova at 𝐳 = 2.9 wi...Sérgio Sacani
We present the JWST discovery of SN 2023adsy, a transient object located in a host galaxy JADES-GS
+
53.13485
−
27.82088
with a host spectroscopic redshift of
2.903
±
0.007
. The transient was identified in deep James Webb Space Telescope (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) program. Photometric and spectroscopic followup with NIRCam and NIRSpec, respectively, confirm the redshift and yield UV-NIR light-curve, NIR color, and spectroscopic information all consistent with a Type Ia classification. Despite its classification as a likely SN Ia, SN 2023adsy is both fairly red (
�
(
�
−
�
)
∼
0.9
) despite a host galaxy with low-extinction and has a high Ca II velocity (
19
,
000
±
2
,
000
km/s) compared to the general population of SNe Ia. While these characteristics are consistent with some Ca-rich SNe Ia, particularly SN 2016hnk, SN 2023adsy is intrinsically brighter than the low-
�
Ca-rich population. Although such an object is too red for any low-
�
cosmological sample, we apply a fiducial standardization approach to SN 2023adsy and find that the SN 2023adsy luminosity distance measurement is in excellent agreement (
≲
1
�
) with
Λ
CDM. Therefore unlike low-
�
Ca-rich SNe Ia, SN 2023adsy is standardizable and gives no indication that SN Ia standardized luminosities change significantly with redshift. A larger sample of distant SNe Ia is required to determine if SN Ia population characteristics at high-
�
truly diverge from their low-
�
counterparts, and to confirm that standardized luminosities nevertheless remain constant with redshift.
Evidence of Jet Activity from the Secondary Black Hole in the OJ 287 Binary S...Sérgio Sacani
Wereport the study of a huge optical intraday flare on 2021 November 12 at 2 a.m. UT in the blazar OJ287. In the binary black hole model, it is associated with an impact of the secondary black hole on the accretion disk of the primary. Our multifrequency observing campaign was set up to search for such a signature of the impact based on a prediction made 8 yr earlier. The first I-band results of the flare have already been reported by Kishore et al. (2024). Here we combine these data with our monitoring in the R-band. There is a big change in the R–I spectral index by 1.0 ±0.1 between the normal background and the flare, suggesting a new component of radiation. The polarization variation during the rise of the flare suggests the same. The limits on the source size place it most reasonably in the jet of the secondary BH. We then ask why we have not seen this phenomenon before. We show that OJ287 was never before observed with sufficient sensitivity on the night when the flare should have happened according to the binary model. We also study the probability that this flare is just an oversized example of intraday variability using the Krakow data set of intense monitoring between 2015 and 2023. We find that the occurrence of a flare of this size and rapidity is unlikely. In machine-readable Tables 1 and 2, we give the full orbit-linked historical light curve of OJ287 as well as the dense monitoring sample of Krakow.
Candidate young stellar objects in the S-cluster: Kinematic analysis of a sub...Sérgio Sacani
Context. The observation of several L-band emission sources in the S cluster has led to a rich discussion of their nature. However, a definitive answer to the classification of the dusty objects requires an explanation for the detection of compact Doppler-shifted Brγ emission. The ionized hydrogen in combination with the observation of mid-infrared L-band continuum emission suggests that most of these sources are embedded in a dusty envelope. These embedded sources are part of the S-cluster, and their relationship to the S-stars is still under debate. To date, the question of the origin of these two populations has been vague, although all explanations favor migration processes for the individual cluster members. Aims. This work revisits the S-cluster and its dusty members orbiting the supermassive black hole SgrA* on bound Keplerian orbits from a kinematic perspective. The aim is to explore the Keplerian parameters for patterns that might imply a nonrandom distribution of the sample. Additionally, various analytical aspects are considered to address the nature of the dusty sources. Methods. Based on the photometric analysis, we estimated the individual H−K and K−L colors for the source sample and compared the results to known cluster members. The classification revealed a noticeable contrast between the S-stars and the dusty sources. To fit the flux-density distribution, we utilized the radiative transfer code HYPERION and implemented a young stellar object Class I model. We obtained the position angle from the Keplerian fit results; additionally, we analyzed the distribution of the inclinations and the longitudes of the ascending node. Results. The colors of the dusty sources suggest a stellar nature consistent with the spectral energy distribution in the near and midinfrared domains. Furthermore, the evaporation timescales of dusty and gaseous clumps in the vicinity of SgrA* are much shorter ( 2yr) than the epochs covered by the observations (≈15yr). In addition to the strong evidence for the stellar classification of the D-sources, we also find a clear disk-like pattern following the arrangements of S-stars proposed in the literature. Furthermore, we find a global intrinsic inclination for all dusty sources of 60 ± 20◦, implying a common formation process. Conclusions. The pattern of the dusty sources manifested in the distribution of the position angles, inclinations, and longitudes of the ascending node strongly suggests two different scenarios: the main-sequence stars and the dusty stellar S-cluster sources share a common formation history or migrated with a similar formation channel in the vicinity of SgrA*. Alternatively, the gravitational influence of SgrA* in combination with a massive perturber, such as a putative intermediate mass black hole in the IRS 13 cluster, forces the dusty objects and S-stars to follow a particular orbital arrangement. Key words. stars: black holes– stars: formation– Galaxy: center– galaxies: star formation
JAMES WEBB STUDY THE MASSIVE BLACK HOLE SEEDSSérgio Sacani
The pathway(s) to seeding the massive black holes (MBHs) that exist at the heart of galaxies in the present and distant Universe remains an unsolved problem. Here we categorise, describe and quantitatively discuss the formation pathways of both light and heavy seeds. We emphasise that the most recent computational models suggest that rather than a bimodal-like mass spectrum between light and heavy seeds with light at one end and heavy at the other that instead a continuum exists. Light seeds being more ubiquitous and the heavier seeds becoming less and less abundant due the rarer environmental conditions required for their formation. We therefore examine the different mechanisms that give rise to different seed mass spectrums. We show how and why the mechanisms that produce the heaviest seeds are also among the rarest events in the Universe and are hence extremely unlikely to be the seeds for the vast majority of the MBH population. We quantify, within the limits of the current large uncertainties in the seeding processes, the expected number densities of the seed mass spectrum. We argue that light seeds must be at least 103 to 105 times more numerous than heavy seeds to explain the MBH population as a whole. Based on our current understanding of the seed population this makes heavy seeds (Mseed > 103 M⊙) a significantly more likely pathway given that heavy seeds have an abundance pattern than is close to and likely in excess of 10−4 compared to light seeds. Finally, we examine the current state-of-the-art in numerical calculations and recent observations and plot a path forward for near-future advances in both domains.
Anti-Universe And Emergent Gravity and the Dark UniverseSérgio Sacani
Recent theoretical progress indicates that spacetime and gravity emerge together from the entanglement structure of an underlying microscopic theory. These ideas are best understood in Anti-de Sitter space, where they rely on the area law for entanglement entropy. The extension to de Sitter space requires taking into account the entropy and temperature associated with the cosmological horizon. Using insights from string theory, black hole physics and quantum information theory we argue that the positive dark energy leads to a thermal volume law contribution to the entropy that overtakes the area law precisely at the cosmological horizon. Due to the competition between area and volume law entanglement the microscopic de Sitter states do not thermalise at sub-Hubble scales: they exhibit memory effects in the form of an entropy displacement caused by matter. The emergent laws of gravity contain an additional ‘dark’ gravitational force describing the ‘elastic’ response due to the entropy displacement. We derive an estimate of the strength of this extra force in terms of the baryonic mass, Newton’s constant and the Hubble acceleration scale a0 = cH0, and provide evidence for the fact that this additional ‘dark gravity force’ explains the observed phenomena in galaxies and clusters currently attributed to dark matter.
The binding of cosmological structures by massless topological defectsSérgio Sacani
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...Sérgio Sacani
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
The debris of the ‘last major merger’ is dynamically youngSérgio Sacani
The Milky Way’s (MW) inner stellar halo contains an [Fe/H]-rich component with highly eccentric orbits, often referred to as the
‘last major merger.’ Hypotheses for the origin of this component include Gaia-Sausage/Enceladus (GSE), where the progenitor
collided with the MW proto-disc 8–11 Gyr ago, and the Virgo Radial Merger (VRM), where the progenitor collided with the
MW disc within the last 3 Gyr. These two scenarios make different predictions about observable structure in local phase space,
because the morphology of debris depends on how long it has had to phase mix. The recently identified phase-space folds in Gaia
DR3 have positive caustic velocities, making them fundamentally different than the phase-mixed chevrons found in simulations
at late times. Roughly 20 per cent of the stars in the prograde local stellar halo are associated with the observed caustics. Based
on a simple phase-mixing model, the observed number of caustics are consistent with a merger that occurred 1–2 Gyr ago.
We also compare the observed phase-space distribution to FIRE-2 Latte simulations of GSE-like mergers, using a quantitative
measurement of phase mixing (2D causticality). The observed local phase-space distribution best matches the simulated data
1–2 Gyr after collision, and certainly not later than 3 Gyr. This is further evidence that the progenitor of the ‘last major merger’
did not collide with the MW proto-disc at early times, as is thought for the GSE, but instead collided with the MW disc within
the last few Gyr, consistent with the body of work surrounding the VRM.
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Multi-source connectivity as the driver of solar wind variability in the heli...Sérgio Sacani
The ambient solar wind that flls the heliosphere originates from multiple
sources in the solar corona and is highly structured. It is often described
as high-speed, relatively homogeneous, plasma streams from coronal
holes and slow-speed, highly variable, streams whose source regions are
under debate. A key goal of ESA/NASA’s Solar Orbiter mission is to identify
solar wind sources and understand what drives the complexity seen in the
heliosphere. By combining magnetic feld modelling and spectroscopic
techniques with high-resolution observations and measurements, we show
that the solar wind variability detected in situ by Solar Orbiter in March
2022 is driven by spatio-temporal changes in the magnetic connectivity to
multiple sources in the solar atmosphere. The magnetic feld footpoints
connected to the spacecraft moved from the boundaries of a coronal hole
to one active region (12961) and then across to another region (12957). This
is refected in the in situ measurements, which show the transition from fast
to highly Alfvénic then to slow solar wind that is disrupted by the arrival of
a coronal mass ejection. Our results describe solar wind variability at 0.5 au
but are applicable to near-Earth observatories.
Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Tr...Sérgio Sacani
Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the
atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets
receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric
composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet
transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days.
The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We
confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and
validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as
well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope
and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host
star is inactive, with an X-ray-to-bolometric luminosity ratio of log 5.7 L L X bol » - . Joint analysis of the light
curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕,a3σ mass upper limit of
3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric
(TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small
list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.
Gliese 12 b, a temperate Earth-sized planet at 12 parsecs discovered with TES...Sérgio Sacani
We report on the discovery of Gliese 12 b, the nearest transiting temperate, Earth-sized planet found to date. Gliese 12 is a
bright (V = 12.6 mag, K = 7.8 mag) metal-poor M4V star only 12.162 ± 0.005 pc away from the Solar system with one of the
lowest stellar activity levels known for M-dwarfs. A planet candidate was detected by TESS based on only 3 transits in sectors
42, 43, and 57, with an ambiguity in the orbital period due to observational gaps. We performed follow-up transit observations
with CHEOPS and ground-based photometry with MINERVA-Australis, SPECULOOS, and Purple Mountain Observatory,
as well as further TESS observations in sector 70. We statistically validate Gliese 12 b as a planet with an orbital period of
12.76144 ± 0.00006 d and a radius of 1.0 ± 0.1 R⊕, resulting in an equilibrium temperature of ∼315 K. Gliese 12 b has excellent
future prospects for precise mass measurement, which may inform how planetary internal structure is affected by the stellar
compositional environment. Gliese 12 b also represents one of the best targets to study whether Earth-like planets orbiting cool
stars can retain their atmospheres, a crucial step to advance our understanding of habitability on Earth and across the galaxy.
The importance of continents, oceans and plate tectonics for the evolution of...Sérgio Sacani
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
A Giant Impact Origin for the First Subduction on EarthSérgio Sacani
Hadean zircons provide a potential record of Earth's earliest subduction 4.3 billion years ago. Itremains enigmatic how subduction could be initiated so soon after the presumably Moon‐forming giant impact(MGI). Earlier studies found an increase in Earth's core‐mantle boundary (CMB) temperature due to theaccumulation of the impactor's core, and our recent work shows Earth's lower mantle remains largely solid, withsome of the impactor's mantle potentially surviving as the large low‐shear velocity provinces (LLSVPs). Here,we show that a hot post‐impact CMB drives the initiation of strong mantle plumes that can induce subductioninitiation ∼200 Myr after the MGI. 2D and 3D thermomechanical computations show that a high CMBtemperature is the primary factor triggering early subduction, with enrichment of heat‐producing elements inLLSVPs as another potential factor. The models link the earliest subduction to the MGI with implications forunderstanding the diverse tectonic regimes of rocky planets.
Climate extremes likely to drive land mammal extinction during next supercont...Sérgio Sacani
Mammals have dominated Earth for approximately 55 Myr thanks to their
adaptations and resilience to warming and cooling during the Cenozoic. All
life will eventually perish in a runaway greenhouse once absorbed solar
radiation exceeds the emission of thermal radiation in several billions of
years. However, conditions rendering the Earth naturally inhospitable to
mammals may develop sooner because of long-term processes linked to
plate tectonics (short-term perturbations are not considered here). In
~250 Myr, all continents will converge to form Earth’s next supercontinent,
Pangea Ultima. A natural consequence of the creation and decay of Pangea
Ultima will be extremes in pCO2 due to changes in volcanic rifting and
outgassing. Here we show that increased pCO2, solar energy (F⨀;
approximately +2.5% W m−2 greater than today) and continentality (larger
range in temperatures away from the ocean) lead to increasing warming
hostile to mammalian life. We assess their impact on mammalian
physiological limits (dry bulb, wet bulb and Humidex heat stress indicators)
as well as a planetary habitability index. Given mammals’ continued survival,
predicted background pCO2 levels of 410–816 ppm combined with increased
F⨀ will probably lead to a climate tipping point and their mass extinction.
The results also highlight how global landmass configuration, pCO2 and F⨀
play a critical role in planetary habitability.
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.
Sexuality - Issues, Attitude and Behaviour - Applied Social Psychology - Psyc...PsychoTech Services
A proprietary approach developed by bringing together the best of learning theories from Psychology, design principles from the world of visualization, and pedagogical methods from over a decade of training experience, that enables you to: Learn better, faster!
The technology uses reclaimed CO₂ as the dyeing medium in a closed loop process. When pressurized, CO₂ becomes supercritical (SC-CO₂). In this state CO₂ has a very high solvent power, allowing the dye to dissolve easily.
Mending Clothing to Support Sustainable Fashion_CIMaR 2024.pdfSelcen Ozturkcan
Ozturkcan, S., Berndt, A., & Angelakis, A. (2024). Mending clothing to support sustainable fashion. Presented at the 31st Annual Conference by the Consortium for International Marketing Research (CIMaR), 10-13 Jun 2024, University of Gävle, Sweden.
Immersive Learning That Works: Research Grounding and Paths ForwardLeonel Morgado
We will metaverse into the essence of immersive learning, into its three dimensions and conceptual models. This approach encompasses elements from teaching methodologies to social involvement, through organizational concerns and technologies. Challenging the perception of learning as knowledge transfer, we introduce a 'Uses, Practices & Strategies' model operationalized by the 'Immersive Learning Brain' and ‘Immersion Cube’ frameworks. This approach offers a comprehensive guide through the intricacies of immersive educational experiences and spotlighting research frontiers, along the immersion dimensions of system, narrative, and agency. Our discourse extends to stakeholders beyond the academic sphere, addressing the interests of technologists, instructional designers, and policymakers. We span various contexts, from formal education to organizational transformation to the new horizon of an AI-pervasive society. This keynote aims to unite the iLRN community in a collaborative journey towards a future where immersive learning research and practice coalesce, paving the way for innovative educational research and practice landscapes.
Current Ms word generated power point presentation covers major details about the micronuclei test. It's significance and assays to conduct it. It is used to detect the micronuclei formation inside the cells of nearly every multicellular organism. It's formation takes place during chromosomal sepration at metaphase.
Describing and Interpreting an Immersive Learning Case with the Immersion Cub...Leonel Morgado
Current descriptions of immersive learning cases are often difficult or impossible to compare. This is due to a myriad of different options on what details to include, which aspects are relevant, and on the descriptive approaches employed. Also, these aspects often combine very specific details with more general guidelines or indicate intents and rationales without clarifying their implementation. In this paper we provide a method to describe immersive learning cases that is structured to enable comparisons, yet flexible enough to allow researchers and practitioners to decide which aspects to include. This method leverages a taxonomy that classifies educational aspects at three levels (uses, practices, and strategies) and then utilizes two frameworks, the Immersive Learning Brain and the Immersion Cube, to enable a structured description and interpretation of immersive learning cases. The method is then demonstrated on a published immersive learning case on training for wind turbine maintenance using virtual reality. Applying the method results in a structured artifact, the Immersive Learning Case Sheet, that tags the case with its proximal uses, practices, and strategies, and refines the free text case description to ensure that matching details are included. This contribution is thus a case description method in support of future comparative research of immersive learning cases. We then discuss how the resulting description and interpretation can be leveraged to change immersion learning cases, by enriching them (considering low-effort changes or additions) or innovating (exploring more challenging avenues of transformation). The method holds significant promise to support better-grounded research in immersive learning.
Basics of crystallography, crystal systems, classes and different forms
High resolution alma_observations_of_sdp81_the_innermost_mass_profile_of_the_lensing_elliptical_galaxy_probed_by_30_milli_arcsecond_images
1. arXiv:1503.07605v2[astro-ph.GA]16Apr2015 Publ. Astron. Soc. Japan (2015) 00(0), 1–7
doi: 10.1093/pasj/xxx000
1
High-resolution ALMA observations of SDP.81.
I. The innermost mass profile of the lensing
elliptical galaxy probed by 30 milli-arcsecond
images
Yoichi TAMURA1
, Masamune OGURI,2,3,4
, Daisuke IONO5,6
,
Bunyo HATSUKADE5
, Yuichi MATSUDA5,6
and Masao HAYASHI5
1
Institute of Astronomy, University of Tokyo, Osawa, Mitaka, Tokyo 181-0015
2
Research Center for the Early Universe, University of Tokyo, Hongo, Bunkyo-ku, Tokyo
113-0033
3
Department of Physics, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033
4
Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), University
of Tokyo, Chiba 277-8583
5
National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo, 181-8588
6
SOKENDAI (The Graduate University for Advanced Studies), Osawa, Mitaka, Tokyo
181-8588
∗E-mail: ytamura@ioa.s.u-tokyo.ac.jp
Received 2015 March 25; Accepted 2015 April 16
Abstract
We report a detailed modeling of a mass profile of a z =0.2999 massive elliptical galaxy using 30
milli-arcsecond resolution 1-mm Atacama Large Millimeter/submillimeter Array (ALMA) images
of the galaxy–galaxy lensing system SDP.81. The detailed morphology of the lensed multiple
images of the z = 3.042 infrared-luminous galaxy, which is found to consist of tens of <
∼ 100-
pc-sized star-forming clumps embedded in a ∼ 2 kpc disk, are well reproduced by a lensing
galaxy modeled by an isothermal ellipsoid with a 400 pc core. The core radius is consistent
with that of the visible stellar light, and the mass-to-light ratio of ∼ 2M⊙ L−1
⊙ is comparable to
the locally measured value, suggesting that the inner 1 kpc region is dominated by luminous
matter. The position of the predicted mass centroid is consistent to within ≃ 30 mas with a
non-thermal source detected with ALMA, which likely traces an active galactic nucleus of the
foreground elliptical galaxy. While the black hole mass and the core radius of the elliptical
galaxy are degenerate, a point source mass of > 3 × 108
M⊙ mimicking a supermassive black
hole is required to explain the non-detection of a central image of the background galaxy. The
required mass is consistent with the prediction from the well-known correlation between black
hole mass and host velocity dispersion. Our analysis demonstrates the power of high resolution
imaging of strong gravitational lensing for studying the innermost mass profile and the central
supermassive black hole of distant elliptical galaxies.
Key words: black hole physics — gravitational lensing: strong — galaxies: individual (H-ATLAS
J090311.6+003906) — galaxies: structure — submillimeter: galaxies
c 2015. Astronomical Society of Japan.
2. 2 Publications of the Astronomical Society of Japan, (2015), Vol. 00, No. 0
1 Introduction
Galaxy–galaxy lensing occurs ubiquitously in the observable
universe. Magnified images from gravitational lensing al-
low us to understand the detailed mass structure of the in-
tervening galaxy as well as the background source structure
(e.g., Koopmans 2005; Inoue & Chiba 2005; Vegetti et al.
2012; Hezaveh 2013a; Hezaveh et al. 2013b; Hezaveh 2014).
Furthermore, a detection or absence of a central lensed image
offers a unique opportunity to map the innermost mass distribu-
tion of the lensing galaxy and to directly measure the mass of
the central supermassive black hole (SMBH, Mao et al. 2001;
Winn et al. 2004; Inada et al. 2008). Precise mass modeling re-
quires sensitive, extinction-free, and extremely high resolution
imaging toward the very center of a lensing galaxy (Hezaveh
et al. 2015). This is now possible with long baseline capa-
bilities offered by the Atacama Large Millimeter/submillimeter
Array (ALMA). Here we present a detailed modeling of a mass
profile of the z = 0.2999 elliptical galaxy, which is the fore-
ground galaxy in the galaxy–galaxy lensing system H-ATLAS
J090311.6+003906 (SDP.81), using 30 milli-arcsec (mas) reso-
lution 1-mm images obtained at ALMA.
SDP.81 is a gravitationally lensed z = 3.042 galaxy dis-
covered in the Herschel Astrophysical Terahertz Large Area
Survey (H-ATLAS, Eales et al. 2010). The characteris-
tic features (“Einstein ring”) are evident in the 2′′
resolu-
tion interferometric maps (Negrello et al. 2010; Omont et al.
2013; Bussmann et al. 2013) and the Hubble Space Telescope
(HST) image (Negrello et al. 2014; Dye et al. 2014), indi-
cating strong magnification. Carbon Monoxide (CO) and wa-
ter (H2O) emission were successfully detected from the back-
ground galaxy (Omont et al. 2013). The foreground elliptical
galaxy is identified in the Sloan Digital Sky Survey (SDSS)
as SDSS J090311.57+003906.5 (hereafter SDSS J0903) with
a spectroscopic redshift of z = 0.2999± 0.0002 (Negrello et al.
2014). We hereafter refer to the foreground and background
galaxies as SDSS J0903 and SDP.81, respectively. Detailed dis-
cussion on the spatial/kinematic structure and the star-formation
activity in SDP.81 will be presented in a subsequent paper
(Paper II; Hatsukade et al. 2015).
Throughout this paper, we assume a flat universe with Ωm =
0.26, ΩΛ = 0.74, and H0 = 72 km s−1
Mpc−1
. The angular
scale of 1′′
corresponds to 4.36 kpc at the lens redshift zl =
0.2999 and 7.78 kpc at source redshift zs = 3.042.
2 Data
2.1 ALMA observations and images
The ALMA data at wavelengths of 1.0, 1.3 and 2.0 mm
were obtained during the long baseline campaign of Science
Verification (ALMA Partnership 2015b). The resulting spatial
resolution achieved at 1.0, 1.3 and 2.0 mm are 23× 31 mas (PA
= 15◦
), 30 × 39 mas (PA = 20◦
) and 54 × 60 mas (PA = 18◦
),
with r.m.s. noise level of 10, 10, and 9 µJy beam−1
, respec-
tively. The CO (5–4), (8–7) and (10–9) images were also taken
simultaneously in the 2.0, 1.3 and 1.0 mm bands, respectively.
The CO images are uv-tapered to ≃170 mas in order to increase
the sensitivity to extended structure. Details of the observations
are given in ALMA Partnership (2015a) and ALMA Partnership
(2015b).
A three-color image composed from the 1.0 and 1.3 mm
data are shown in figure 1a. The quadruple images of SDP.81
are clearly resolved, three of which are bridged by a 3′′
-long
arc. The arcs consist of four bright knots connected by thin
smooth filaments. The grainy clumps seen around the arcs are
not coherent among the different frequency bands (figure 1a),
and thus they are likely to be artifacts due to phase calibra-
tion residuals. On the other hand, we find fainter, but sig-
nificant knots embedded in the arcs that are consistent in all
different waveband images. These are real features that are
likely tracing the internal substructures of SDP.81. A central
point source bracketed by the long and short arcs is not re-
solved with the Band 7 beam and has a 1.0–2.0 mm power-law
spectral index of α = −0.3 ± 0.7 (ALMA Partnership 2015a).
The extrapolated flux at 20 cm is consistent with that of the
cataloged radio source FIRST J090311.5+003906 (S20cm =
1.21 ± 0.16 mJy beam−1
, Becker et al. 1995). The power-law
spectral index from 1.0 mm to 20 cm is α = −0.64 ± 0.01 (see
inset of figure 1b), which is consistent with the spectral index
measured for 1.0–2.0 mm. If the non-thermal emission arises
from SDP.81, it should also dominate the emission from the
arcs. However, the observed spectral index of the arc is posi-
tive (typically α >
∼ 2), meaning that dust emission is the better
model to explain the emission characteristics of the arc ALMA
Partnership (2015a). Furthermore, no molecular lines of CO
and H2O at z = 3.042 are found at the position. It is there-
fore likely that the non-thermal emission arises from an Active
Galactic Nucleus (AGN) of SDSS J0903.
2.2 Hubble images
We retrieve the archival HST image (proposal ID: 12194,
Negrello et al. 2014) taken with the Wide Field Camera 3
(WFC3) at 1.6 µm (F160W, H band). The point spread func-
tion (PSF) is 151 mas in FWHM. We calibrate the coordinates
of the WFC3 image using the catalog data from the SDSS Data
Release 121
. We use 46 SDSS objects located in the WFC3 im-
age to derive the astrometric fit using IRAF. The r.m.s. errors of
the fit are 85 mas in right ascension and 100 mas in declination.
The nominal center of SDSS J0903 matches the position of the
central non-thermal source in the ALMA images within 15 mas.
We use the GALFIT software (Version 3.0.5, Peng et al.
1
http://skyserver.sdss.org/dr12
3. Publications of the Astronomical Society of Japan, (2015), Vol. 00, No. 0 3
Table 1. Lens model parameters.
xa ya σv
b ec θe
c rcore
d γ (×10−2)e θγ
e δ (×10−3)f θδ
f ǫ (×10−3)g θǫ
g
6+21
−32 5+13
−22 265+15
−4 0.14+0.11
−0.07 11 ± 13 48+169
−28 4.0+1.7
−3.2 3+35
−23 3.0+3.1
−2.3 41 ± 22 2.4+3.7
−1.7 35+23
−13
The errors represent 68% confidence intervals estimated from a Markov-chain Monte Carlo simulation. (a) The central position of an isothermal ellipsoid in units of mas,
relative to the position of the non-thermal source at 9h
3m
11.s
573, +0◦
39′
6.′′
54, respectively. (b) Velocity dispersion of the isothermal ellipsoid (km s−1
). (c) Ellipticity
and its position angle (deg). (d) core radius of the isothermal ellipsoid (mas). (e) external shear and its position angle (deg). (f) third-order external perturbation and its
position angle (deg). (g) multipole perturbation with (m, n) = (4, 2) and its position angle (deg). See Oguri (2010) for the definitions of the parameters.
Fig. 1. (a) ALMA 3-color image of SDP.81 (1.0, 1.15 and 1.3 mm for blue, green and red, respectively) overlaid with the Hubble WFC3/F160W (1.6 µm) image
where the stellar light of SDSS J0903 is subtracted (contours). Two sets of counter-images of stellar peaks are indicated by filled and open stars, respectively.
The synthesized beam size is indicated at the bottom-left corner. The origin of the image is taken at the position of a central compact non-thermal source. (b)
The ALMA 1.0 mm image. Upper inset shows CO (5–4) spectra at the positions of the source A (upper) and E (lower). Bottom inset shows the spectral energy
distribution of the central compact source, which is well fitted by a power-law function with a spectral index of −0.64 (solid line), suggesting the synchrotron
emission. (c) The modeled brightness distribution on the image plane. The image is smoothed by a Gaussian with FWHM = 23 mas. The inner and outer
ellipses represent radial and tangential critical curves, respectively. (d) The modeled brightness distribution on the source plane, which is 0.5′′
on a side. The
star represents the source position of the stellar peaks denoted as filled stars in (a). The position of this panel is indicated as a dotted square in (c). The solid
curves represent the caustics. The scale bar at the bottom-left corner shows a physical scale of 200 pc at z = 3.042.
4. 4 Publications of the Astronomical Society of Japan, (2015), Vol. 00, No. 0
Fig. 2. Correlation matrix of the lens parameters computed by a Marcov-chain Monte Carlo simulation. The probability distribution of two parameters are
indicated by a greyscale map with contours of 1σ, 2σ and 3σ. The diagonal panels show the probability distribution of each parameter in which the rest
parameters are marginalized over. The asterisk in the x–y correlation plot marks the position of the AGN at the center of SDSS J0903.
2010) to deblend the stellar light in SDP.81 from SDSS J0903.
Following the procedure adopted by Negrello et al. (2014), two
S´ersic profiles are simultaneously fitted to the HST image. As
a result, the radial profile of SDSS J0903 is decomposed into a
brighter (H-band absolute AB magnitude of MH = 17.56) ellip-
tical with a S´ersic index of ns =4.42 and a fainter (MH =18.69)
exponential disk with ns = 1.03. Although our total flux is 1.2×
higher, this is consistent with the model presented by Negrello
et al. (2014). The residual image shown in figure 1 clearly ex-
hibits the stellar arcs which are significantly (>
∼ 100 mas) offset
from the 1-mm ALMA arcs (see Paper II for the interpretation).
3 Gravitational lens model
3.1 Methods and results
We use the GLAFIC software (Oguri 2010)2
to reproduce the
lensed image using an isothermal ellipsoid with a flat core.
The choice of an isothermal ellipsoid is supported by the fact
that the radial density profile of SDSS J0903 is consistent with
ρ(r) ∝ r−2
(Dye et al. 2014; Rybak et al. 2015), which is the
profile expected for an isothermal ellipsoid. The structure of
SDP.81 is, however, too complex to be accounted for by a sin-
gle isothermal ellipsoid alone. We examine the SDSS clus-
ter catalog of Oguri (2014) and find a cluster of galaxies at
z = 0.306 with the richness of ∼ 21 and located ∼ 2′
away
2
http://www.slac.stanford.edu/%7Eoguri/glafic/
5. Publications of the Astronomical Society of Japan, (2015), Vol. 00, No. 0 5
Fig. 3. Surface mass density versus projected radius of the best-fit mass
model (blue shade), radial distribution of stellar light (dark yellow) and the
point spread function (PSF) of the 1.6 µm HST image (dotted curve, arbitrary
unit). The mass model smoothed by the HST PSF is shown in dashed curve.
The surface density is normalized by the cosmological critical density for a
source redshift zs = 3.042, Σcrit = 4.3 × 109
M⊙ kpc−2
.
from SDSS J0903. Therefore we include the third-order and
quadrupole perturbations of mass3
, in addition to the standard
external shear, to take into account the gravitational influence
of the cluster and large-scale structure.
We identify compact knots in the arcs that are common in
the 1.0, 1.3, and 2.0 mm images and then identify two sets of
counter-images of the knots in SDP.81. These are shown as
open squares in figure 1b (A and E). The counter-images of
each set are extracted by visually identifying continuum inten-
sity peaks which share the same/similar CO (5–4) and (8–7)
spectral profiles at each of the peaks. Figure 1b shows how the
counter-images are identified; all of the CO (5–4) spectra at the
positions of A have a peak at ∼ 100 km s−1
while the peaks
at E appear near −200 km s−1
and have broader line profiles
than A, which likely correspond to the red and blue compo-
nents reported by Omont et al. (2013) and ALMA Partnership
(2015a), respectively. This method allows us to predict that the
knots A are quadruple lensed images of a single source, whereas
the knots E are double images and thus the (tangential) caustics
should lie between A and E on the source plane. First, we ob-
tain an initial mass model only with the isothermal ellipsoid and
external shear using the positions of A and E. Then we use the
initial mass model to identify groups of counter-images of knots
found in the 1.0-mm continuum image. The knots within ≃ 50
mas from the predicted positions are identified as the counter-
images, resulting in identifications of 46 images. We then refine
3
We use GLAFIC mass models clus3 for the third-order external perturba-
tion and mpole with (m,n) = (4,2) for the quadrupole perturbation (equa-
tion 13 of Oguri 2010). The central positions of the perturbation compo-
nents are fixed to that of the isothermal ellipsoid.
the mass model by adding the higher-order perturbations (the
number of independent parameters is 12) and fitting all of the
identified multiple images. In the model calculation, we also
consider two sets of double images identified with the 1.6-µm
HST image, which is indicated by star symbols in figure 1a. The
number of degrees of freedom (DOF) is thus NDOF = 88. The
positional uncertainty of the knots used for optimization is set to
20 mas, while the uncertainties of the 10 knots which are close
to the critical curve and/or possibly suffering from blending are
set to 100–200 mas. The uncertainties of the four HST images
are set to 130–200 mas.
The best-fit parameters of the mass model4
are listed in
table 1, where the 1σ confidence intervals are computed by
Marcov-chain Monte Carlo simulations as shown in figure 2.
Note that the core radius (rcore) and velocity dispersion (σv)
of the isothermal ellipsoid are highly degenerate. The central
position of the isothermal ellipsoid is not only consistent with
the brightness peak of the stellar distribution within the 1σ as-
trometric uncertainty of HST (≃ 100 mas), but also with the
location of the candidate AGN, i.e., (x, y) = (0, 0), to within
≃ 30 mas (1σ). This suggests that the AGN is indeed located
at the bottom (innermost < 100-pc) of the potential well of
SDSS J0903. The best-fit parameters of the isothermal ellip-
soid and external shear are in good agreement with those inde-
pendently obtained using the same ALMA images (Rybak et al.
2015; Dye et al. 2015)5
and the HST images (Dye et al. 2014)
at 1σ level.
The crosses in figure 1b mark the positions of the counter-
images predicted by this model, and we find that the model is
qualitatively consistent with the peak positions of the 1.0-mm
brightness distribution (χ2
= 3.45). Figures 1c and 1d show
the predicted brightness distributions on the image and source
planes, respectively. The observed images are reproduced by 35
<
∼ 100-pc-sized knots embedded in an extended (≃ 2 kpc) disk.
While the uncertainty is relatively large, the total magnification
factor is expected to be µg ∼ 22. This is consistent with the
value obtained by Rybak et al. (2015) (µg = 17.6±0.4 for total,
µg = 25.2 ± 2.6 for a central star-forming disk), while it is ≃
2× higher than the value previously obtained with the SMA
(µg ≃ 11, Bussmann et al. 2013). This is likely because, as
suggested by Rybak et al. (2015), the ALMA image allows us to
identify more compact structures close to the caustics, resulting
in higher magnifications than those obtained previously.
3.2 Mass profile of SDSS J0903
In figure 3, we show the surface mass profile of the gravitational
lens model normalized by a cosmological critical density for a
source redshift zs = 3.042 (i.e., convergence κ(r)) and a radial
4
The GLAFIC model of SDP.81 is available at http://www.ioa.s.u-
tokyo.ac.jp/%7Eytamura/SDP81/.
5
Note that the ellipticity q used in Rybak et al. (2015) is related by e = 1−q.
6. 6 Publications of the Astronomical Society of Japan, (2015), Vol. 00, No. 0
Fig. 4. The flux density ratio of central counter-images relative to the all
counter-images, as a function of mass of a supermassive black hole of
SDSS J0903 (Solid line with circles). The source-plane components are
the same as shown in figure 1d. The horizontal dotted line shows the 3σ
upper limit of the ALMA 1.0-mm image on the flux ratio. The dashed line
with squares represents χ2
of model optimizations.
profile of the 1.6-µm stellar light obtained by the HST/WFC3
F160W imaging observations. The critical density is Σcrit =
4.3×109
M⊙ kpc−2
, and the stellar surface mass is scaled using
a fiducial mass-to-light ratio of 2 M⊙ L−1
⊙ at λrest ≃ 1 µm
(e.g., Bell et al. 2003), which is a typical value for local massive
ellipticals. Because the stellar profile is lowpass-filtered by the
PSF of HST (151 mas, see the dotted curve), the profile is only
reliable at r >
∼ 0.1′′
. It is evident that there is a knee in the stellar
profile at a characteristic radius of ≃ 0.15′′
.
In figure 3, we also show the lensing mass profile smoothed
by the HST PSF. The knee position and the amplitude of the
profile are in agreement with the lens model. Although the de-
rived core (rcore = 48+169
−28 mas, which corresponds to a core
diameter of ∼400 pc) is slightly smaller than the stellar core
(r ≃ 150 mas), the two core radii are consistent to within the 1σ
uncertainty. Furthermore, the position angle of the isothermal
ellipsoid (θe = 11 ± 13◦
) is consistent with that of the stellar
profile (10 ± 1◦
, Dye et al. 2014), suggesting that the bary-
onic matter, traced by the stellar light, dominates the mass in
the inner 1-kpc region of the galaxy. At larger radii (>
∼ 3 kpc),
however, the stellar light falls below the model surface density
(κ(r) ∝ r−1
), which can be interpreted as the presence of dark
matter in the outer parts of SDSS J0903.
4 Discussions and conclusions
The non-detection of the central ‘odd’ image of SDP.81 in the
deep ALMA images rules out a top-flat plateau in the gravita-
tional potential, but instead requires the presence of a steep (or
cuspy) radial profile in the innermost potential distribution. A
SMBH can make the central potential more cuspy even if the
stellar mass distribution is top-flat as suggested from the WFC3
radial profile. As a consequence, this can erase the central im-
age if the black hole is massive enough to fully perturb the core
potential. Since there is a clear sign of the presence of an AGN
at the center of SDSS J0903, we add a point source mimick-
ing the SMBH to the lens model in order to investigate how the
SMBH affects the flux of the central image. A point mass with
MBH = 107
to 109
M⊙ is placed at the position of the AGN and
rcore is fixed to the stellar core radius of 150 mas, while the rest
are treated as free parameters (NDOF = 89).
Figure 4 shows Scent/Stot (i.e. the ratio between the flux
from the central image to all of the counter-images) as a func-
tion of MBH. The fit to the model is generally good (χ2
≃ 3.7)
in the range of 107
< MBH/M⊙ < 109
. The ratio is insensi-
tive to the black hole mass if it is less than 1 × 108
M⊙, but
the central image rapidly dims as the black hole mass is higher
than 2 × 108
M⊙. The horizontal dotted line shows the 3σ up-
per limit of the 1.0-mm image (30 µJy) divided by the total flux
(37.7±1.5 mJy, ALMA Partnership 2015a), suggesting that the
ALMA non-detection places a constraint to the black hole mass
of MBH > 3 × 108
M⊙. Note that if we adopt rcore = 48 mas,
the limit is slightly relaxed to MBH > 1 × 108
M⊙.
A black hole mass can independently be estimated from
the well-known correlation between black hole mass and the
velocity dispersion of the bulge (e.g., Ferrarese & Merritt
2000; Gebhardt et al. 2000). The black hole estimated from the
velocity dispersion of the lens (σv = 265+15
−4 km s−1
, Table 1)
and using the local correlation (Kormendy & Ho 2013) is
MBH = (1±0.1)×109
M⊙, which is consistent with the lower
limit derived above. It will difficult to detect the central im-
age of SDP.81 even in future ALMA observations if MBH ∼
1×109
M⊙. We demonstrate in this work that the detailed grav-
itational lens modeling using sensitive, high-resolution imaging
with ALMA is capable of constraining the central <
∼ 1 kpc mass
profile and the black hole mass, which will help us understand
the co-evolution of the SMBHs and the host galaxies through,
for example, SMBH scouring (Hezaveh et al. 2015).
Finally, we note that a similar conclusion on the mass of the
SMBH (logMBH/M⊙ > 8.4) was made by a recent analysis by
Wong et al. (2015), where they used an independent code GLEE
(Suyu & Halkola 2010) and different sets of multiple images
from the ALMA images tapered to ∼170 mas to construct a lens
model. Nevertheless, we prefer to use the full resolution ALMA
images (up to 23 mas), which allows us to (1) accurately model
higher-order perturbations, and to (2) robustly identify multiple
features in the images and construct a reliable lens model.
Acknowledgments
We thank the anonymous referee for fruitful comments. This work is sup-
ported by KAKENHI (No. 25103503, 26800093 and 20647268). MO
is supported in part by World Premier International Research Center
Initiative (WPI Initiative), MEXT, Japan. DI is supported by the 2015
7. Publications of the Astronomical Society of Japan, (2015), Vol. 00, No. 0 7
Inamori Research Grants Program. This paper makes use of the follow-
ing ALMA data: ADS/JAO.ALMA #2011.0.00016.SV. ALMA is a part-
nership of ESO (representing its member states), NSF (USA) and NINS
(Japan), together with NRC (Canada), NSC, ASIAA (Taiwan) and KASI
(Republic of Korea), in cooperation with the Republic of Chile. The Joint
ALMA Observatory is operated by ESO, NAOJ and NRAO.
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