X-ray spectroscopy AGN - High-Excitation and Low-Excitation Radio Galaxies: a...Valentina Scipione
1) The study compares X-ray properties of 14 radio galaxies divided into high-excitation (HEG) and low-excitation (LEG) galaxies based on optical emission lines.
2) HEGs have higher average intrinsic neutral hydrogen column densities and X-ray luminosities than LEGs. They also have stronger optical [OIII] emission lines.
3) The distributions of column densities and X-ray luminosities between HEGs and LEGs are bimodal. HEGs also show evidence for accretion disks from detected iron K-alpha lines, which are absent in LEGs.
4) The results suggest LEGs have a less efficient accretion regime than HEGs, possibly only accre
Detectcion of noble_gas_molecular_ion_arh_in_the_crab_nebulaSérgio Sacani
Scientists detected emission lines from the ionized argon hydride (36ArH+) molecule in spectra of the Crab Nebula obtained with the Herschel Space Observatory. The detection of 36ArH+ confirms that argon originated from explosive nucleosynthesis during the core-collapse supernova that created the Crab Nebula. The likely excitation mechanism is electron collisions in partially ionized regions with electron densities of a few hundred per cubic centimeter. This is the first detection of a noble gas molecule in space.
Propagation of highly_efficient_star_formation_in_ngc7000Sérgio Sacani
This document summarizes a study of star formation in molecular clouds near the H II region NGC 7000. The authors surveyed NH3 and H2O maser emission toward the molecular cloud L935 located near NGC 7000. They identified five dense molecular clumps based on NH3 emission, which have similar gas temperatures but different levels of star formation activity. One clump located near the boundary of the H II region has a high star formation efficiency of 36-62%, suggesting triggered star formation due to its interaction with the expanding H II region.
This document summarizes the discovery of two planetary companions orbiting the metal-poor star HIP 11952 based on radial velocity measurements. The star HIP 11952 was observed over a period of 16 months using the FEROS spectrograph. Analysis of the spectra revealed periodic radial velocity variations of 6.95 days and 290 days, indicating the presence of two planets with minimum masses of 0.78 MJup and 2.93 MJup orbiting at 0.07 AU and 0.81 AU, respectively. HIP 11952 is a metal-poor star with [Fe/H] of -1.95, making it one of the few known systems with planets orbiting a star with such low metallicity
The document discusses the fireshell model for classifying gamma-ray bursts (GRBs). It presents an analysis of two short GRBs, 08024B and 140402A, within the fireshell model. The fireshell model proposes two families of short GRBs originating from neutron star mergers. It estimates redshifts and isotropic energies for the two GRBs. The analysis finds that not all short GRBs produce GeV emission, and that GeV emission may be associated with accretion onto a black hole. It also notes that the absence of X-ray detections after some short GRBs is not surprising given observational limitations.
The document discusses brown dwarfs and how their infrared spectroscopic properties and evolution can be studied using IR and sub-mm spectroscopy. It covers topics like effective temperature over time for objects of different masses, atmospheric composition changes from M dwarf to T dwarf, formation of dust in brown dwarf atmospheres, non-equilibrium chemistry, dynamical transport processes, and 3D radiation hydrodynamics simulations of brown dwarf atmospheres.
This document discusses the scientific opportunity of measuring prompt optical emission from gamma-ray bursts (GRBs) in order to better understand GRB emission mechanisms. It proposes a new instrument capable of simultaneous multi-color optical and infrared observations of GRBs with high time resolution. Such an instrument could measure prompt optical light curves and spectra, test models of GRB emission, and probe properties of dust around GRBs.
X-ray spectroscopy AGN - High-Excitation and Low-Excitation Radio Galaxies: a...Valentina Scipione
1) The study compares X-ray properties of 14 radio galaxies divided into high-excitation (HEG) and low-excitation (LEG) galaxies based on optical emission lines.
2) HEGs have higher average intrinsic neutral hydrogen column densities and X-ray luminosities than LEGs. They also have stronger optical [OIII] emission lines.
3) The distributions of column densities and X-ray luminosities between HEGs and LEGs are bimodal. HEGs also show evidence for accretion disks from detected iron K-alpha lines, which are absent in LEGs.
4) The results suggest LEGs have a less efficient accretion regime than HEGs, possibly only accre
Detectcion of noble_gas_molecular_ion_arh_in_the_crab_nebulaSérgio Sacani
Scientists detected emission lines from the ionized argon hydride (36ArH+) molecule in spectra of the Crab Nebula obtained with the Herschel Space Observatory. The detection of 36ArH+ confirms that argon originated from explosive nucleosynthesis during the core-collapse supernova that created the Crab Nebula. The likely excitation mechanism is electron collisions in partially ionized regions with electron densities of a few hundred per cubic centimeter. This is the first detection of a noble gas molecule in space.
Propagation of highly_efficient_star_formation_in_ngc7000Sérgio Sacani
This document summarizes a study of star formation in molecular clouds near the H II region NGC 7000. The authors surveyed NH3 and H2O maser emission toward the molecular cloud L935 located near NGC 7000. They identified five dense molecular clumps based on NH3 emission, which have similar gas temperatures but different levels of star formation activity. One clump located near the boundary of the H II region has a high star formation efficiency of 36-62%, suggesting triggered star formation due to its interaction with the expanding H II region.
This document summarizes the discovery of two planetary companions orbiting the metal-poor star HIP 11952 based on radial velocity measurements. The star HIP 11952 was observed over a period of 16 months using the FEROS spectrograph. Analysis of the spectra revealed periodic radial velocity variations of 6.95 days and 290 days, indicating the presence of two planets with minimum masses of 0.78 MJup and 2.93 MJup orbiting at 0.07 AU and 0.81 AU, respectively. HIP 11952 is a metal-poor star with [Fe/H] of -1.95, making it one of the few known systems with planets orbiting a star with such low metallicity
The document discusses the fireshell model for classifying gamma-ray bursts (GRBs). It presents an analysis of two short GRBs, 08024B and 140402A, within the fireshell model. The fireshell model proposes two families of short GRBs originating from neutron star mergers. It estimates redshifts and isotropic energies for the two GRBs. The analysis finds that not all short GRBs produce GeV emission, and that GeV emission may be associated with accretion onto a black hole. It also notes that the absence of X-ray detections after some short GRBs is not surprising given observational limitations.
The document discusses brown dwarfs and how their infrared spectroscopic properties and evolution can be studied using IR and sub-mm spectroscopy. It covers topics like effective temperature over time for objects of different masses, atmospheric composition changes from M dwarf to T dwarf, formation of dust in brown dwarf atmospheres, non-equilibrium chemistry, dynamical transport processes, and 3D radiation hydrodynamics simulations of brown dwarf atmospheres.
This document discusses the scientific opportunity of measuring prompt optical emission from gamma-ray bursts (GRBs) in order to better understand GRB emission mechanisms. It proposes a new instrument capable of simultaneous multi-color optical and infrared observations of GRBs with high time resolution. Such an instrument could measure prompt optical light curves and spectra, test models of GRB emission, and probe properties of dust around GRBs.
1) The document discusses the cosmic microwave background (CMB), which is remnant radiation from the Big Bang.
2) It describes the CMB temperature anisotropy and polarization patterns that have been observed, including the pursuit of detecting primordial gravitational waves through B-mode polarization patterns.
3) Kinetic inductance detectors (KIDs) are introduced as the detector technology to be used for the proposed ground-based telescope (GB) to map the CMB polarization at high angular resolution in search of primordial gravitational waves. Design details and simulations of KID arrays are presented.
This document summarizes a study that measured the lithium abundance in red giant branch stars in the globular cluster M54, which belongs to the Sagittarius dwarf galaxy. High-resolution spectra were obtained for 74 candidate member stars of M54 using the FLAMES instrument on the Very Large Telescope. Chemical abundances were derived for iron and sodium. Lithium abundances were measured from the Li resonance doublet at 6707 Angstroms by comparing observed spectra to synthetic spectra. The lithium abundance measured was A(Li)=0.93±0.11 dex, corresponding to an initial abundance of A(Li)0 between 2.35-2.29 dex depending on atomic diffusion models. This initial lithium abundance
Grb 130606a as_a_probe_of_the_intergalactic_medium_and_the_interstelar_medium...Sérgio Sacani
This document summarizes observations of the gamma-ray burst GRB 130606A at a redshift of z=5.913 using spectroscopy from the MMT and Gemini telescopes. The high quality spectra exhibit a smooth near-infrared continuum that is sharply cut off by Lyman-alpha absorption at z=5.91, with some flux transmitted through the Lyman-alpha forest at lower redshifts. Metal absorption lines in the host galaxy are used to constrain its metallicity between -1.7 and -0.5 solar. Transmission in the Lyman-alpha forest is found to evolve consistently with previous quasar observations. An extended region at z=5.77 shows no Lyman-alpha transmission,
This document discusses using future full-sky galaxy surveys from space telescopes to probe initial conditions and constrain primordial non-Gaussianity. It proposes launching a space telescope called SPHEREx to conduct a full-sky galaxy spectroscopy survey. This would allow probing the horizon-scale clustering needed to constrain the non-Gaussianity parameter fNL using both the galaxy power spectrum and bispectrum. Current forecasts suggest SPHEREx could achieve an uncertainty of σ(fNL) ~ 0.8 from the power spectrum alone and σ(fNL) ~ 0.2 when also including the bispectrum. However, challenges remain in applying photometric redshift indicators and understanding contributions to the squeezed bispectrum at higher orders.
Semi-Analytic Modeling: Creation of the Far-IR Populationsabenson
1. The document discusses semi-analytic modeling of galaxy formation using the GALFORM model.
2. It describes how the model tracks processes like gas cooling, star formation, feedback, black hole growth, and galaxy mergers.
3. The model is used to make predictions about far-IR galaxy populations, submillimeter galaxies, dust emission, and number counts that can be compared to observations.
Modeling extrasolar planetary atmospheres discusses techniques for modeling exoplanet atmospheres including:
1) 1D radiative models that reconstruct atmospheric temperature structures and simulate thermal emission and reflected light.
2) 2D and 3D global circulation models that simulate atmospheric winds and temperature distributions driven by stellar irradiation and planetary rotation.
3) Advanced 3D models that combine radiative transfer with hydrodynamics to model atmospheric chemistry, clouds, and winds. These simulations produce synthetic spectra and light curves for comparison to observations.
Detection of Radio Emission from FireballsCarlos Bella
This document summarizes the detection of radio emissions from fireballs (very bright meteors) using the Long Wavelength Array radio telescope. A search of over 11,000 hours of all-sky radio images found 49 long-duration radio transients. Ten of these transients correlated spatially and temporally with fireballs detected by an optical meteor monitoring network. This provides evidence that fireballs emit previously undiscovered low frequency radio pulses. Further analysis found characteristics inconsistent with expected radio reflections from meteor trails, suggesting a non-thermal radio emission mechanism from the fireballs. This identifies a new class of natural radio transients and provides a new probe to study meteor physics.
Plasma diagnostic in eruptive prominences from SDO/AIA observations at 304 ÅUniversity of Glasgow
The document discusses plasma diagnostic observations of eruptive solar prominences from SDO/AIA at 304 Angstroms. New non-LTE radiative transfer calculations allow plasma parameters like temperature, column mass, and radial velocity to vary, unlike previous models. The observations and new models show that the Helium II 304 Angstrom line intensity can either decrease or increase with increasing radial velocity, depending on changes in the plasma parameters. Allowing parameters to vary produces a range of intensities that matches the range seen in SDO/AIA observations qualitatively.
The document summarizes Spitzer observations of the supernova remnant IC 443. The MIPS images show the remnant's morphology in great detail, resembling a shell or loop. The dust temperature ranges from 18-30 K based on the 70/160um ratio. IRS spectroscopy confirms shock-excited atomic and molecular emission, with shock velocities of 60-90 km/s. H2 excitation diagrams show temperatures of 300-600 K and column densities varying across the remnant.
The BEER algorithm identified Kepler-76b, a hot Jupiter orbiting an F star, from its Kepler light curve. The light curve showed evidence of the beaming, ellipsoidal, and reflection effects consistent with a planetary companion. Follow-up spectroscopy confirmed Kepler-76b with a mass of 2.0 ± 0.26 MJup and orbital period of 1.5449 days. Analysis of the light curve effects provided evidence that Kepler-76b exhibits atmospheric superrotation, or an eastward jet stream that shifts the hottest atmospheric region.
The Palomar Transient Factory (PTF) uses the 48-inch Samuel Oschin Telescope at Palomar Observatory to discover transients and variables in the sky. It aims to study extragalactic and galactic phenomena such as supernovae, tidal disruption events, cataclysmic variables, and structures in the Milky Way. The PTF uses a wide-field imager to discover objects and then coordinates follow-up with spectrographs on the Palomar 200-inch and other telescopes. It has discovered over 2,000 supernovae and published numerous science papers. The Zwicky Transient Facility (ZTF) will improve on the PTF with a larger field of view
Uma equipe de astrofísicos usando o Observatório W. M. Keck no Havaí mediu com sucesso a galáxia mais distante já registrada e o mais interessante, capturou sua emissão de hidrogênio vista quando o universo tinha menos de 600 milhões de anos de vida. Adicionalmente, o método pelo qual a galáxia EGSY8p7 foi detectada dá uma ideia importante sobre como as primeiras estrelas no universo se acenderam depois do Big Bang.
Usando o poderoso espectrógrafo infravermelho do Observatório Keck, chamado MOSFIRE, a equipe datou a galáxia detectando sua linha de emissão Lyman-alpha – uma assinatura do gás hidrogênio quente, aquecido pela forte emissão ultravioleta de estrelas recém-nascidas. Embora, frequentemente seja possível detectar essa assinatura em galáxias próximas da Terra, a detecção da emissão Lyman-alpha nessas grandes distâncias é inesperada, já que ela é facilmente absorvida pelos numerosos átomos de hidrogênio que acredita-se existam no espaço entre as galáxias no nascer do universo. O resultado dá uma nova ideia sobre a reionização cósmica, o processo pelo qual nuvens escuras de hidrogênio foram partidas em seus prótons constituintes e elétrons pelas primeiras gerações de galáxias.
“Nós frequentemente observamos a linha de emissão Lyman-alpha do hidrogênio em objetos próximos já que eles são um dos traçadores mais confiáveis da formação de estrelas”, disse o astrônomo Adi Zitrin, do Instituto de Tecnologia da Califórnia, o Caltech, principal autor do estudo. “Contudo, à medida que penetramos mais fundo no universo, e então voltamos a tempos remotos, o espaço entre as galáxias continha um grande número de nuvens escuras de hidrogênio que absorviam esse sinal”.
1) The document analyzes satellite signal measurements taken at the University of Glamorgan to measure attenuation and scintillation.
2) Key factors analyzed include diurnal variation, clear air attenuation using ITU models, rain attenuation, total attenuation, and scintillation probability density.
3) The measurements were used to calculate various attenuation statistics which will help future satellite link design and understanding of attenuation in the region.
This document reports the first detection of hydrogen peroxide (HOOH) in interstellar space. Four HOOH transitions were detected toward the ρ Oph A molecular cloud core, including three transitions mapped over the densest part of the core. Analysis of the line intensities using a rotation diagram method derived a HOOH rotation temperature of 22 K and column density of 8×1012 cm-2, corresponding to an abundance relative to H2 of about 1×10-10. This detection provides evidence that HOOH plays a role in oxygen and water chemistry in molecular clouds.
The document summarizes a seismic experiment conducted in Krafla volcano called DRG. 20 additional seismic stations were deployed over 4 months to study seismic wave propagation and search for indications of magma. Data was recorded from distant earthquakes, explosions, and local seismic activity. P and S wave arrivals were identified. The data was loaded into analysis software and will be studied to characterize the deep roots of the Krafla geothermal system through techniques like tomography and looking for S wave shadows and seismic reflections. Unfortunately no PhD student was available to fully analyze the data, but Cornell University conducted some virtual refraction profiling of reflections.
Storm in teacup_a_radio_quiet_quasar_with_radio_emitting_bubblesSérgio Sacani
Artigo descreve descoberta feita com o VLA de uma tempestade nas ondas de rádio em uma galáxia até então calma, o que traz conclusões sobre a evolução das galáxias.
Energy level modeling of lanthanide defects in SrAl2O4:Eu2+Jonas Joos
Belgian Physical Society (BPS) meeting 2015, Liège.
Results published in Physical Review B:
http://journals.aps.org/prb/abstract/10.1103/PhysRevB.90.085147
The role of laboratory astrophysics in studies of Fe-group nucleosynthesis in...AstroAtom
1) The University of Wisconsin laboratory astrophysics group aims to study iron-group nucleosynthesis in the early universe through measurements of element abundances in ancient, metal-poor stars.
2) They use a laser fluorescence technique to measure radiative lifetimes and a Fourier transform spectrometer to measure branching fractions needed to determine accurate transition probabilities for iron-group elements.
3) Preliminary application of their manganese data shows interesting non-LTE trends in abundances that vary with excitation potential, highlighting the need for accurate transition probabilities.
4) They are upgrading their echelle spectrometer to better measure weak lines and branching fractions, which will provide more reliable abundance probes and help constrain models of iron-group nucle
Atomic data and spectral models for lowly ionized iron-peak speciesAstroAtom
This document discusses the need for reliable atomic data and spectral models for lowly ionized iron-peak species like Sc, Ti, V, Cr, Mn, Fe, Co, Ni, and Cu. Current models are inaccurate, with predicted line intensities disagreeing with observations by factors of several. The goals of the project are to compute new atomic data, construct improved spectral and opacity models, and implement the models in photoionization codes. The document outlines challenges in modeling these ions and describes ongoing work using relativistic R-matrix methods to calculate improved collision strengths and photoionization cross sections.
1) The document discusses the cosmic microwave background (CMB), which is remnant radiation from the Big Bang.
2) It describes the CMB temperature anisotropy and polarization patterns that have been observed, including the pursuit of detecting primordial gravitational waves through B-mode polarization patterns.
3) Kinetic inductance detectors (KIDs) are introduced as the detector technology to be used for the proposed ground-based telescope (GB) to map the CMB polarization at high angular resolution in search of primordial gravitational waves. Design details and simulations of KID arrays are presented.
This document summarizes a study that measured the lithium abundance in red giant branch stars in the globular cluster M54, which belongs to the Sagittarius dwarf galaxy. High-resolution spectra were obtained for 74 candidate member stars of M54 using the FLAMES instrument on the Very Large Telescope. Chemical abundances were derived for iron and sodium. Lithium abundances were measured from the Li resonance doublet at 6707 Angstroms by comparing observed spectra to synthetic spectra. The lithium abundance measured was A(Li)=0.93±0.11 dex, corresponding to an initial abundance of A(Li)0 between 2.35-2.29 dex depending on atomic diffusion models. This initial lithium abundance
Grb 130606a as_a_probe_of_the_intergalactic_medium_and_the_interstelar_medium...Sérgio Sacani
This document summarizes observations of the gamma-ray burst GRB 130606A at a redshift of z=5.913 using spectroscopy from the MMT and Gemini telescopes. The high quality spectra exhibit a smooth near-infrared continuum that is sharply cut off by Lyman-alpha absorption at z=5.91, with some flux transmitted through the Lyman-alpha forest at lower redshifts. Metal absorption lines in the host galaxy are used to constrain its metallicity between -1.7 and -0.5 solar. Transmission in the Lyman-alpha forest is found to evolve consistently with previous quasar observations. An extended region at z=5.77 shows no Lyman-alpha transmission,
This document discusses using future full-sky galaxy surveys from space telescopes to probe initial conditions and constrain primordial non-Gaussianity. It proposes launching a space telescope called SPHEREx to conduct a full-sky galaxy spectroscopy survey. This would allow probing the horizon-scale clustering needed to constrain the non-Gaussianity parameter fNL using both the galaxy power spectrum and bispectrum. Current forecasts suggest SPHEREx could achieve an uncertainty of σ(fNL) ~ 0.8 from the power spectrum alone and σ(fNL) ~ 0.2 when also including the bispectrum. However, challenges remain in applying photometric redshift indicators and understanding contributions to the squeezed bispectrum at higher orders.
Semi-Analytic Modeling: Creation of the Far-IR Populationsabenson
1. The document discusses semi-analytic modeling of galaxy formation using the GALFORM model.
2. It describes how the model tracks processes like gas cooling, star formation, feedback, black hole growth, and galaxy mergers.
3. The model is used to make predictions about far-IR galaxy populations, submillimeter galaxies, dust emission, and number counts that can be compared to observations.
Modeling extrasolar planetary atmospheres discusses techniques for modeling exoplanet atmospheres including:
1) 1D radiative models that reconstruct atmospheric temperature structures and simulate thermal emission and reflected light.
2) 2D and 3D global circulation models that simulate atmospheric winds and temperature distributions driven by stellar irradiation and planetary rotation.
3) Advanced 3D models that combine radiative transfer with hydrodynamics to model atmospheric chemistry, clouds, and winds. These simulations produce synthetic spectra and light curves for comparison to observations.
Detection of Radio Emission from FireballsCarlos Bella
This document summarizes the detection of radio emissions from fireballs (very bright meteors) using the Long Wavelength Array radio telescope. A search of over 11,000 hours of all-sky radio images found 49 long-duration radio transients. Ten of these transients correlated spatially and temporally with fireballs detected by an optical meteor monitoring network. This provides evidence that fireballs emit previously undiscovered low frequency radio pulses. Further analysis found characteristics inconsistent with expected radio reflections from meteor trails, suggesting a non-thermal radio emission mechanism from the fireballs. This identifies a new class of natural radio transients and provides a new probe to study meteor physics.
Plasma diagnostic in eruptive prominences from SDO/AIA observations at 304 ÅUniversity of Glasgow
The document discusses plasma diagnostic observations of eruptive solar prominences from SDO/AIA at 304 Angstroms. New non-LTE radiative transfer calculations allow plasma parameters like temperature, column mass, and radial velocity to vary, unlike previous models. The observations and new models show that the Helium II 304 Angstrom line intensity can either decrease or increase with increasing radial velocity, depending on changes in the plasma parameters. Allowing parameters to vary produces a range of intensities that matches the range seen in SDO/AIA observations qualitatively.
The document summarizes Spitzer observations of the supernova remnant IC 443. The MIPS images show the remnant's morphology in great detail, resembling a shell or loop. The dust temperature ranges from 18-30 K based on the 70/160um ratio. IRS spectroscopy confirms shock-excited atomic and molecular emission, with shock velocities of 60-90 km/s. H2 excitation diagrams show temperatures of 300-600 K and column densities varying across the remnant.
The BEER algorithm identified Kepler-76b, a hot Jupiter orbiting an F star, from its Kepler light curve. The light curve showed evidence of the beaming, ellipsoidal, and reflection effects consistent with a planetary companion. Follow-up spectroscopy confirmed Kepler-76b with a mass of 2.0 ± 0.26 MJup and orbital period of 1.5449 days. Analysis of the light curve effects provided evidence that Kepler-76b exhibits atmospheric superrotation, or an eastward jet stream that shifts the hottest atmospheric region.
The Palomar Transient Factory (PTF) uses the 48-inch Samuel Oschin Telescope at Palomar Observatory to discover transients and variables in the sky. It aims to study extragalactic and galactic phenomena such as supernovae, tidal disruption events, cataclysmic variables, and structures in the Milky Way. The PTF uses a wide-field imager to discover objects and then coordinates follow-up with spectrographs on the Palomar 200-inch and other telescopes. It has discovered over 2,000 supernovae and published numerous science papers. The Zwicky Transient Facility (ZTF) will improve on the PTF with a larger field of view
Uma equipe de astrofísicos usando o Observatório W. M. Keck no Havaí mediu com sucesso a galáxia mais distante já registrada e o mais interessante, capturou sua emissão de hidrogênio vista quando o universo tinha menos de 600 milhões de anos de vida. Adicionalmente, o método pelo qual a galáxia EGSY8p7 foi detectada dá uma ideia importante sobre como as primeiras estrelas no universo se acenderam depois do Big Bang.
Usando o poderoso espectrógrafo infravermelho do Observatório Keck, chamado MOSFIRE, a equipe datou a galáxia detectando sua linha de emissão Lyman-alpha – uma assinatura do gás hidrogênio quente, aquecido pela forte emissão ultravioleta de estrelas recém-nascidas. Embora, frequentemente seja possível detectar essa assinatura em galáxias próximas da Terra, a detecção da emissão Lyman-alpha nessas grandes distâncias é inesperada, já que ela é facilmente absorvida pelos numerosos átomos de hidrogênio que acredita-se existam no espaço entre as galáxias no nascer do universo. O resultado dá uma nova ideia sobre a reionização cósmica, o processo pelo qual nuvens escuras de hidrogênio foram partidas em seus prótons constituintes e elétrons pelas primeiras gerações de galáxias.
“Nós frequentemente observamos a linha de emissão Lyman-alpha do hidrogênio em objetos próximos já que eles são um dos traçadores mais confiáveis da formação de estrelas”, disse o astrônomo Adi Zitrin, do Instituto de Tecnologia da Califórnia, o Caltech, principal autor do estudo. “Contudo, à medida que penetramos mais fundo no universo, e então voltamos a tempos remotos, o espaço entre as galáxias continha um grande número de nuvens escuras de hidrogênio que absorviam esse sinal”.
1) The document analyzes satellite signal measurements taken at the University of Glamorgan to measure attenuation and scintillation.
2) Key factors analyzed include diurnal variation, clear air attenuation using ITU models, rain attenuation, total attenuation, and scintillation probability density.
3) The measurements were used to calculate various attenuation statistics which will help future satellite link design and understanding of attenuation in the region.
This document reports the first detection of hydrogen peroxide (HOOH) in interstellar space. Four HOOH transitions were detected toward the ρ Oph A molecular cloud core, including three transitions mapped over the densest part of the core. Analysis of the line intensities using a rotation diagram method derived a HOOH rotation temperature of 22 K and column density of 8×1012 cm-2, corresponding to an abundance relative to H2 of about 1×10-10. This detection provides evidence that HOOH plays a role in oxygen and water chemistry in molecular clouds.
The document summarizes a seismic experiment conducted in Krafla volcano called DRG. 20 additional seismic stations were deployed over 4 months to study seismic wave propagation and search for indications of magma. Data was recorded from distant earthquakes, explosions, and local seismic activity. P and S wave arrivals were identified. The data was loaded into analysis software and will be studied to characterize the deep roots of the Krafla geothermal system through techniques like tomography and looking for S wave shadows and seismic reflections. Unfortunately no PhD student was available to fully analyze the data, but Cornell University conducted some virtual refraction profiling of reflections.
Storm in teacup_a_radio_quiet_quasar_with_radio_emitting_bubblesSérgio Sacani
Artigo descreve descoberta feita com o VLA de uma tempestade nas ondas de rádio em uma galáxia até então calma, o que traz conclusões sobre a evolução das galáxias.
Energy level modeling of lanthanide defects in SrAl2O4:Eu2+Jonas Joos
Belgian Physical Society (BPS) meeting 2015, Liège.
Results published in Physical Review B:
http://journals.aps.org/prb/abstract/10.1103/PhysRevB.90.085147
The role of laboratory astrophysics in studies of Fe-group nucleosynthesis in...AstroAtom
1) The University of Wisconsin laboratory astrophysics group aims to study iron-group nucleosynthesis in the early universe through measurements of element abundances in ancient, metal-poor stars.
2) They use a laser fluorescence technique to measure radiative lifetimes and a Fourier transform spectrometer to measure branching fractions needed to determine accurate transition probabilities for iron-group elements.
3) Preliminary application of their manganese data shows interesting non-LTE trends in abundances that vary with excitation potential, highlighting the need for accurate transition probabilities.
4) They are upgrading their echelle spectrometer to better measure weak lines and branching fractions, which will provide more reliable abundance probes and help constrain models of iron-group nucle
Atomic data and spectral models for lowly ionized iron-peak speciesAstroAtom
This document discusses the need for reliable atomic data and spectral models for lowly ionized iron-peak species like Sc, Ti, V, Cr, Mn, Fe, Co, Ni, and Cu. Current models are inaccurate, with predicted line intensities disagreeing with observations by factors of several. The goals of the project are to compute new atomic data, construct improved spectral and opacity models, and implement the models in photoionization codes. The document outlines challenges in modeling these ions and describes ongoing work using relativistic R-matrix methods to calculate improved collision strengths and photoionization cross sections.
Globular clusters can be used to test theories of stellar evolution and nucleosynthesis by studying the variations in elements like carbon, nitrogen, sodium, and s-process and r-process elements within their stars. The author conducts high and medium resolution spectroscopic studies of stars in globular clusters like 47 Tucanae and Omega Centauri to infer elemental abundances and plans to extend this work to other clusters using instruments on telescopes like SALT.
This document discusses a study that used microwave spectroscopy to analyze the pure rotational spectra of the open-shell diatomic molecules lead monoiodide (PbI) and tin monoiodide (SnI) for the first time. Spectra were collected using a chirped pulsed Fourier transform microwave spectrometer over the 7-18.5 GHz region. Transitions from multiple isotopologues and vibrational states of PbI and SnI were assigned and fitted to determine rotational, centrifugal distortion, hyperfine, and quadrupole coupling constants. Analysis of the bond lengths and hyperfine interactions indicates that the bonding in both PbI and SnI is ionic in nature.
Solving Structural Topology of ROMK1 FINAL from 102313Kevin Ho
The document summarizes key findings from early research on the structural topology of the inward rectifier potassium channel ROMK1:
1) Initial analysis found ROMK1 had no sequence similarity to other known potassium channels but predicted two transmembrane segments flanked by hydrophilic regions.
2) Comparison to other potassium channel topologies revealed ROMK1 shared a common "signature" of a pore-forming region flanked by transmembrane segments.
3) This allowed researchers to develop the first topological model of ROMK1, defining it as the founding member of a new family of inward rectifier potassium channels.
This document discusses theoretical atomic and molecular physics research being conducted on recombination lines in nebulae spectra. The research group is investigating two recombination processes, radiative and dielectronic recombination, using atomic structure and R-matrix codes. They are studying carbon and magnesium ions to analyze planetary nebulae and draw conclusions about nebula conditions and compositions.
Herschel far infrared_spectroscopy_of_the_galactic_centerSérgio Sacani
The document summarizes observations from the Herschel Space Observatory of the Galactic Center region, focusing on a spectral scan toward Sagittarius A*. Key findings include:
1) Strong emission from atomic fine structure lines and rotationally excited lines of molecules like CO, H2O and HCO+ are detected.
2) The excitation of the CO ladder is consistent with either a hot isothermal gas component at 103.1 K and 104 cm-3, or a distribution of warmer gas at higher densities, with most CO at 300 K.
3) The detected molecular features suggest heating is from a combination of UV irradiation and shocks in the gas, rather than very enhanced X-ray or cosmic
Combinatorial Experimentation and Machine Learning for Materials Discoveryaimsnist
This document describes how machine learning and active learning can be used to enhance high-throughput combinatorial experimentation for materials discovery. Specifically, it discusses how active learning algorithms can direct experiments to optimally query samples and map out phase diagrams with fewer total measurements. An example is given of using these methods to autonomously map the composition-temperature phase diagram of tungsten-doped VO2 with only 10% of samples requiring direct measurement. The document concludes that machine learning has the potential to significantly reduce the number of experiments needed in combinatorial screening studies.
This document discusses accelerator plans at SLAC, including the status and improvements made to PEP-II. Some key points:
- PEP-II achieved a new peak luminosity record of 7.18x1033 in December 2003 through numerous upgrades like adding RF stations and improving feedback circuits.
- Future plans aim to further increase luminosity through higher beam currents, more bunches, and lowering the interaction point beta function. Goals are set to reach 20x1033 luminosity by 2006 and 30x1033 by 2008-2010.
- Long term, options are considered to upgrade PEP-II to achieve ultra-high luminosities around 1036 cm-2s-1 through techniques like very low beta functions
The document discusses modeling of helium line formation in solar prominences using radiative transfer modeling. It describes how the models account for the prominence-corona transition region and influence of radial plasma motions on line profiles and intensities. The modeling helps interpret observations from instruments like SOHO, Hinode, STEREO, and SDO to better understand the thermal structure and magnetic fields of prominences.
Energy level structure and transition probabilities in the spectra of the tri...Elias Serqueira
This document summarizes research on the energy level structure and transition probabilities in the spectra of trivalent lanthanides doped in LaF3 crystals. It presents experimental data on the absorption spectra of lanthanide-doped LaF3 from 4000-50000 cm-1. It also describes theoretical models used to interpret the spectra and calculate atomic and crystal field parameters. The models were optimized to fit the experimental data and identify trends in the parameters across the lanthanide series. Lifetimes of excited states were also calculated and compared to experimental measurements.
This document summarizes quantum oscillations in strongly correlated electron systems, with a focus on applications to cuprate superconductors. Key points include: (1) quantum oscillations can be used to measure the Fermi surface and quasiparticle properties; (2) in cuprates, oscillations provide evidence of long-lived quasiparticles and Fermi surface reconstruction near optimal doping; and (3) while oscillations support a small reconstructed Fermi surface in underdoped cuprates, details like the number of pockets are still controversial.
Assymetries in core_collapse_supernovae_from_maps_of_radioactive_ti_in_cassio...Sérgio Sacani
The document summarizes findings from observations of Cassiopeia A using the Nuclear Spectroscopic Telescope Array (NuSTAR).
1) NuSTAR detected two clear emission lines from the decay of radioactive titanium-44, confirming previous measurements of titanium-44 yield with high significance. The spatial distribution of titanium-44 emission shows it is clumpy and extended along the jet axis seen in X-ray images, with knots off the jet axis.
2) There is no correlation between the distribution of titanium-44 and iron detected by Chandra X-ray Observatory. This suggests much of the iron-rich ejecta has not been shock-heated and is "invisible", constraining models of the remnant.
Inverse Compton cooling limits the brightness temperature of the radiating plasma to a maximum of
1011.5 K. Relativistic boosting can increase its observed value, but apparent brightness temperatures
much in excess of 1013 K are inaccessible using ground-based very long baseline interferometry (VLBI)
at any wavelength. We present observations of the quasar 3C 273, made with the space VLBI mission
RadioAstron on baselines up to 171,000 km, which directly reveal the presence of angular structure as
small as 26 µas (2.7 light months) and brightness temperature in excess of 1013 K. These measurements
challenge our understanding of the non-thermal continuum emission in the vicinity of supermassive
black holes and require a much higher Doppler factor than what is determined from jet apparent
kinematics.
Keywords: galaxies: active — galaxies: jets — radio continuum: galaxies — techniques: interferometric
— quasars: individual (3C 273)
Growth, structural and optical studies of pure and kbr doped adp crystalseSAT Journals
Abstract Pure and KBr doped crystals of ADP were grown by slow evaporation technique from the supersaturated solution of ADP at room temperature. The tetragonal structure of the grown crystals was observed by powder X-ray diffraction analysis. FTIR spectra revealed the presence of functional groups present in the grown crystals. The UV-Vis spectral analysis shows high transparency in the entire visible region. The band gap value of the pure ADP crystal was found assuming indirect transition. Key Words: ADP, Powder XRD, FTIR, Band gap
1. The document analyzes seismic wave attenuation in the Koyna region of India by estimating quality factors (Q) for P, S, and coda waves using different methods.
2. Q values generally increase with frequency and show lateral variation likely due to heterogeneities. Q estimates indicate scattering is an important factor in body wave attenuation.
3. Comparison to other regions shows Koyna's coda wave attenuation is similar to active areas, while P wave attenuation is like more stable shields. Distance dependence of Q also suggests deeper scattering affects nearer recordings more.
This document summarizes research determining densities in diffuse molecular clouds using CO absorption spectroscopy. Spectroscopic observations along 17 sight lines detected CO absorption features, which were analyzed to determine relative populations between CO rotational energy levels. This provided excitation temperatures (Tex) that were used to estimate densities of hydrogen molecules (n(H2)) in each region, finding values from 102 to 104 cm-3. Higher Tex values and densities were found for sight lines with larger total CO column densities (N(CO)). Future work will use radiative transfer modeling to simultaneously infer kinetic temperatures and n(H2) without assumptions about temperature or Tex.
1) 1H NMR spectroscopy is a technique used to elucidate the structure of organic compounds by determining the number and environment of protons in a molecule.
2) The principle behind 1H NMR is that proton nuclei have a spin and when placed in a magnetic field will absorb radiofrequency energy, appearing as signals in the NMR spectrum.
3) The chemical shift of 1H NMR signals provides information about the electronic environment and bonding of protons. Signals are referenced to TMS and appear in different regions of the spectrum.
Effect of a_high_opacity_on_the_light_curves_of_radioactively_powered_transie...Sérgio Sacani
This document discusses how higher opacities from lanthanide elements in the ejecta of neutron star mergers could dramatically affect the predicted light curves of electromagnetic counterparts. The key points are:
1) Ab initio calculations show r-process element opacities are orders of magnitude higher than previously assumed iron opacities, particularly from lanthanide elements.
2) With these higher opacities, radiation transport models predict light curves that are longer (lasting about a week), dimmer, and redder, with emission peaked in the infrared rather than optical/ultraviolet.
3) A two-component light curve may result if there is both lanthanide-rich ejecta and a secondary
Similar to Comprehensive wavelengths and energy levels of Fe II, Cr II and other iron-group elements using Fourier transform and grating spectroscopy (20)
Exposición interactiva que se llevó a cabo en el Museo de Arte Contemporáneo de Caracas entre octubre 2015 y abril 2016 que involucró alumnos residentes en el barrio de San Agustín del Sur.
This document summarizes an interactive exhibition held in October and November 2015 at the Museo de Arte Contemporáneo in Caracas, Venezuela. The exhibition, called the "San Agustín del Sur Tourism Office", was designed to promote social and spatial integration in the city through art and community engagement. Over 300 children from three local schools participated in workshops and helped create maps of their vision for the city. Additional activities included discussions on local tourism, cooking workshops, and student-led tours of the neighborhood. The goal was to use art and culture to bring divided communities together and foster a more inclusive vision of the city.
La artista Natalya Critchley se sintió atraída desde temprana edad por los pintores fauvistas y reconoció que necesitaba más luz para su arte. Influenciada por su héroe Matisse, terminó mudándose a Venezuela y vivió en Ciudad Guayana durante casi dos décadas, donde encontró la luz que buscaba para su trabajo.
Benchmark Calculations of Atomic Data for Modelling ApplicationsAstroAtom
This document summarizes benchmark calculations of atomic data for modeling applications. It discusses numerical methods like close-coupling and distorted-wave approaches for calculating atomic collision data. It provides selected results on energy levels, oscillator strengths, and electron-impact excitation cross sections. It also discusses applications to modeling neon discharges and takes a closer look at ionization calculations and examples. The document concludes by discussing the production and assessment of atomic data and outlines challenges in obtaining reliable data from both experiments and calculations.
Charge exchange and spectroscopy with isolated highly-charged ionsAstroAtom
This document discusses using Penning traps to capture and store highly charged ions extracted from an electron beam ion trap (EBIT) for charge exchange and optical spectroscopy studies. Specific ion species captured include Ne and Ar ions. The Penning traps use permanent magnets and allow storage of ions for up to 1 second. Future work aims to study hydrogen-like ions using a new apparatus combining a Penning trap with a miniature EBIT ion source.
Fluorescence and resonant ionization in astrophysical plasmas, with emphasis ...AstroAtom
The document discusses fluorescence and resonant ionization processes in Eta Carinae, an astrophysical laboratory. It describes how fluorescence produces emission lines in spectra of the Weigelt blobs near Eta Carinae. Resonance enhanced two-photon ionization (RETPI) can explain the formation of strongly varying emission lines through a process involving hydrogen Lyman lines. RETPI can control the ionization equilibrium of ions during periods of high radiation from the central star. These fluorescence and RETPI processes must be considered when using emission line ratios to determine physical conditions in astrophysical plasmas.
The document discusses the Virtual Atomic and Molecular Data Center (VAMDC) project, which aims to build an interoperable infrastructure for exchanging atomic and molecular data. VAMDC involves partners from multiple European countries and integrates several existing research databases. It intends to allow users to seamlessly search and retrieve data from over 20 atomic and molecular databases. VAMDC is developing standards like XSAMS, an XML schema, and technologies like the TAP protocol to enable interoperable data exchange between the distributed databases. The goal is to provide a virtual data warehouse to serve the needs of the atomic and molecular research community.
Electron impact excitation of H-like, He-like and Li-like ions with Z ≤ 30AstroAtom
The document describes energy levels, radiative rates, and collision strengths for electron impact excitation of hydrogen-like, helium-like, and lithium-like ions with atomic numbers Z ≤ 30. It provides tables of calculated energy levels from various structure codes and compares them to experimental values from NIST. It also lists applications of these data to astrophysical, solar, lasing, and fusion plasmas and describes common structure and scattering codes used to perform the calculations.
Application of X-ray plasma diagnostics to nova windsAstroAtom
Talk presented by Jan-Uwe Ness (XMM-Newton Science Operations Centre) at the symposium "From atoms to stars: the impact of spectroscopy on astrophysics", Oxford, UK, 28-28 July 2011.
Plasma diagnostics for planetary nebulae and H II regions using N II and O IIAstroAtom
This document analyzes plasma diagnostics for planetary nebulae and H II regions using optical recombination lines of N II and O II. It calculates effective recombination coefficients over ranges of electron temperature and density. It fits observed line intensities of several nebulae against theoretical predictions to determine optimal temperature and density. Comparisons with other diagnostics confirm a two-abundance model with a cold, metal-rich component.
New light element opacities from the Los Alamos atomic codeAstroAtom
This document summarizes new light element opacity calculations from the Los Alamos ATOMIC code. It compares the code's opacity results for carbon, oxygen, hydrogen, helium, and carbon/hydrogen mixtures to previous Los Alamos calculations and other databases. The comparisons show generally good agreement. The ATOMIC code features improved atomic structure calculations and equation of state models over previous efforts. Future plans include providing more detailed opacity tables for astrophysically important elements like iron.
Neon and oxygen in stellar coronae - a unification with the SunAstroAtom
This document discusses measurements of the ratio of neon to oxygen (Ne/O) in stellar coronae and how it relates to resolving discrepancies in solar modeling. It finds that the Ne/O ratio increases with stellar activity level in weakly active stars, from around 0.2 for the least active up to 0.4 for more moderate activity levels. These ratios are typical of the quiet Sun. Understanding how elemental abundances like Ne/O vary with activity provides insights into chemical fractionation processes on the Sun and other stars.
Dielectronic recombination and stability of warm gas in AGNAstroAtom
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An R-matrix approach for plasma modelling and the interpretation of astrophys...AstroAtom
This document provides a 3-sentence summary of an expert presentation on plasma modeling and interpretation using an R-matrix approach:
The presentation discussed comprehensive plasma modeling capabilities using R-matrix calculations of electron-impact ionization, excitation, and photoionization of mid-Z elements, which have been parallelized to efficiently utilize modern high performance computing architectures. Scripted R-matrix calculations along iso-nuclear sequences automate the calculation of effective collision strengths. Examples were given of parallel calculations of electron-impact excitation of Fe III and photoionization of Kr II and Xe II using the Dirac Atomic R-matrix Codes that agree well with experimental results.
Helium line emission - Its relation to atmospheric structureAstroAtom
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Threats to mobile devices are more prevalent and increasing in scope and complexity. Users of mobile devices desire to take full advantage of the features
available on those devices, but many of the features provide convenience and capability but sacrifice security. This best practices guide outlines steps the users can take to better protect personal devices and information.
TrustArc Webinar - 2024 Global Privacy SurveyTrustArc
How does your privacy program stack up against your peers? What challenges are privacy teams tackling and prioritizing in 2024?
In the fifth annual Global Privacy Benchmarks Survey, we asked over 1,800 global privacy professionals and business executives to share their perspectives on the current state of privacy inside and outside of their organizations. This year’s report focused on emerging areas of importance for privacy and compliance professionals, including considerations and implications of Artificial Intelligence (AI) technologies, building brand trust, and different approaches for achieving higher privacy competence scores.
See how organizational priorities and strategic approaches to data security and privacy are evolving around the globe.
This webinar will review:
- The top 10 privacy insights from the fifth annual Global Privacy Benchmarks Survey
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Monitoring and Managing Anomaly Detection on OpenShift.pdfTosin Akinosho
Monitoring and Managing Anomaly Detection on OpenShift
Overview
Dive into the world of anomaly detection on edge devices with our comprehensive hands-on tutorial. This SlideShare presentation will guide you through the entire process, from data collection and model training to edge deployment and real-time monitoring. Perfect for those looking to implement robust anomaly detection systems on resource-constrained IoT/edge devices.
Key Topics Covered
1. Introduction to Anomaly Detection
- Understand the fundamentals of anomaly detection and its importance in identifying unusual behavior or failures in systems.
2. Understanding Edge (IoT)
- Learn about edge computing and IoT, and how they enable real-time data processing and decision-making at the source.
3. What is ArgoCD?
- Discover ArgoCD, a declarative, GitOps continuous delivery tool for Kubernetes, and its role in deploying applications on edge devices.
4. Deployment Using ArgoCD for Edge Devices
- Step-by-step guide on deploying anomaly detection models on edge devices using ArgoCD.
5. Introduction to Apache Kafka and S3
- Explore Apache Kafka for real-time data streaming and Amazon S3 for scalable storage solutions.
6. Viewing Kafka Messages in the Data Lake
- Learn how to view and analyze Kafka messages stored in a data lake for better insights.
7. What is Prometheus?
- Get to know Prometheus, an open-source monitoring and alerting toolkit, and its application in monitoring edge devices.
8. Monitoring Application Metrics with Prometheus
- Detailed instructions on setting up Prometheus to monitor the performance and health of your anomaly detection system.
9. What is Camel K?
- Introduction to Camel K, a lightweight integration framework built on Apache Camel, designed for Kubernetes.
10. Configuring Camel K Integrations for Data Pipelines
- Learn how to configure Camel K for seamless data pipeline integrations in your anomaly detection workflow.
11. What is a Jupyter Notebook?
- Overview of Jupyter Notebooks, an open-source web application for creating and sharing documents with live code, equations, visualizations, and narrative text.
12. Jupyter Notebooks with Code Examples
- Hands-on examples and code snippets in Jupyter Notebooks to help you implement and test anomaly detection models.
OpenID AuthZEN Interop Read Out - AuthorizationDavid Brossard
During Identiverse 2024 and EIC 2024, members of the OpenID AuthZEN WG got together and demoed their authorization endpoints conforming to the AuthZEN API
Digital Marketing Trends in 2024 | Guide for Staying AheadWask
https://www.wask.co/ebooks/digital-marketing-trends-in-2024
Feeling lost in the digital marketing whirlwind of 2024? Technology is changing, consumer habits are evolving, and staying ahead of the curve feels like a never-ending pursuit. This e-book is your compass. Dive into actionable insights to handle the complexities of modern marketing. From hyper-personalization to the power of user-generated content, learn how to build long-term relationships with your audience and unlock the secrets to success in the ever-shifting digital landscape.
Ivanti’s Patch Tuesday breakdown goes beyond patching your applications and brings you the intelligence and guidance needed to prioritize where to focus your attention first. Catch early analysis on our Ivanti blog, then join industry expert Chris Goettl for the Patch Tuesday Webinar Event. There we’ll do a deep dive into each of the bulletins and give guidance on the risks associated with the newly-identified vulnerabilities.
Main news related to the CCS TSI 2023 (2023/1695)Jakub Marek
An English 🇬🇧 translation of a presentation to the speech I gave about the main changes brought by CCS TSI 2023 at the biggest Czech conference on Communications and signalling systems on Railways, which was held in Clarion Hotel Olomouc from 7th to 9th November 2023 (konferenceszt.cz). Attended by around 500 participants and 200 on-line followers.
The original Czech 🇨🇿 version of the presentation can be found here: https://www.slideshare.net/slideshow/hlavni-novinky-souvisejici-s-ccs-tsi-2023-2023-1695/269688092 .
The videorecording (in Czech) from the presentation is available here: https://youtu.be/WzjJWm4IyPk?si=SImb06tuXGb30BEH .
In the rapidly evolving landscape of technologies, XML continues to play a vital role in structuring, storing, and transporting data across diverse systems. The recent advancements in artificial intelligence (AI) present new methodologies for enhancing XML development workflows, introducing efficiency, automation, and intelligent capabilities. This presentation will outline the scope and perspective of utilizing AI in XML development. The potential benefits and the possible pitfalls will be highlighted, providing a balanced view of the subject.
We will explore the capabilities of AI in understanding XML markup languages and autonomously creating structured XML content. Additionally, we will examine the capacity of AI to enrich plain text with appropriate XML markup. Practical examples and methodological guidelines will be provided to elucidate how AI can be effectively prompted to interpret and generate accurate XML markup.
Further emphasis will be placed on the role of AI in developing XSLT, or schemas such as XSD and Schematron. We will address the techniques and strategies adopted to create prompts for generating code, explaining code, or refactoring the code, and the results achieved.
The discussion will extend to how AI can be used to transform XML content. In particular, the focus will be on the use of AI XPath extension functions in XSLT, Schematron, Schematron Quick Fixes, or for XML content refactoring.
The presentation aims to deliver a comprehensive overview of AI usage in XML development, providing attendees with the necessary knowledge to make informed decisions. Whether you’re at the early stages of adopting AI or considering integrating it in advanced XML development, this presentation will cover all levels of expertise.
By highlighting the potential advantages and challenges of integrating AI with XML development tools and languages, the presentation seeks to inspire thoughtful conversation around the future of XML development. We’ll not only delve into the technical aspects of AI-powered XML development but also discuss practical implications and possible future directions.
Introduction of Cybersecurity with OSS at Code Europe 2024Hiroshi SHIBATA
I develop the Ruby programming language, RubyGems, and Bundler, which are package managers for Ruby. Today, I will introduce how to enhance the security of your application using open-source software (OSS) examples from Ruby and RubyGems.
The first topic is CVE (Common Vulnerabilities and Exposures). I have published CVEs many times. But what exactly is a CVE? I'll provide a basic understanding of CVEs and explain how to detect and handle vulnerabilities in OSS.
Next, let's discuss package managers. Package managers play a critical role in the OSS ecosystem. I'll explain how to manage library dependencies in your application.
I'll share insights into how the Ruby and RubyGems core team works to keep our ecosystem safe. By the end of this talk, you'll have a better understanding of how to safeguard your code.
5th LF Energy Power Grid Model Meet-up SlidesDanBrown980551
5th Power Grid Model Meet-up
It is with great pleasure that we extend to you an invitation to the 5th Power Grid Model Meet-up, scheduled for 6th June 2024. This event will adopt a hybrid format, allowing participants to join us either through an online Mircosoft Teams session or in person at TU/e located at Den Dolech 2, Eindhoven, Netherlands. The meet-up will be hosted by Eindhoven University of Technology (TU/e), a research university specializing in engineering science & technology.
Power Grid Model
The global energy transition is placing new and unprecedented demands on Distribution System Operators (DSOs). Alongside upgrades to grid capacity, processes such as digitization, capacity optimization, and congestion management are becoming vital for delivering reliable services.
Power Grid Model is an open source project from Linux Foundation Energy and provides a calculation engine that is increasingly essential for DSOs. It offers a standards-based foundation enabling real-time power systems analysis, simulations of electrical power grids, and sophisticated what-if analysis. In addition, it enables in-depth studies and analysis of the electrical power grid’s behavior and performance. This comprehensive model incorporates essential factors such as power generation capacity, electrical losses, voltage levels, power flows, and system stability.
Power Grid Model is currently being applied in a wide variety of use cases, including grid planning, expansion, reliability, and congestion studies. It can also help in analyzing the impact of renewable energy integration, assessing the effects of disturbances or faults, and developing strategies for grid control and optimization.
What to expect
For the upcoming meetup we are organizing, we have an exciting lineup of activities planned:
-Insightful presentations covering two practical applications of the Power Grid Model.
-An update on the latest advancements in Power Grid -Model technology during the first and second quarters of 2024.
-An interactive brainstorming session to discuss and propose new feature requests.
-An opportunity to connect with fellow Power Grid Model enthusiasts and users.
Salesforce Integration for Bonterra Impact Management (fka Social Solutions A...Jeffrey Haguewood
Sidekick Solutions uses Bonterra Impact Management (fka Social Solutions Apricot) and automation solutions to integrate data for business workflows.
We believe integration and automation are essential to user experience and the promise of efficient work through technology. Automation is the critical ingredient to realizing that full vision. We develop integration products and services for Bonterra Case Management software to support the deployment of automations for a variety of use cases.
This video focuses on integration of Salesforce with Bonterra Impact Management.
Interested in deploying an integration with Salesforce for Bonterra Impact Management? Contact us at sales@sidekicksolutionsllc.com to discuss next steps.
HCL Notes and Domino License Cost Reduction in the World of DLAUpanagenda
Webinar Recording: https://www.panagenda.com/webinars/hcl-notes-and-domino-license-cost-reduction-in-the-world-of-dlau/
The introduction of DLAU and the CCB & CCX licensing model caused quite a stir in the HCL community. As a Notes and Domino customer, you may have faced challenges with unexpected user counts and license costs. You probably have questions on how this new licensing approach works and how to benefit from it. Most importantly, you likely have budget constraints and want to save money where possible. Don’t worry, we can help with all of this!
We’ll show you how to fix common misconfigurations that cause higher-than-expected user counts, and how to identify accounts which you can deactivate to save money. There are also frequent patterns that can cause unnecessary cost, like using a person document instead of a mail-in for shared mailboxes. We’ll provide examples and solutions for those as well. And naturally we’ll explain the new licensing model.
Join HCL Ambassador Marc Thomas in this webinar with a special guest appearance from Franz Walder. It will give you the tools and know-how to stay on top of what is going on with Domino licensing. You will be able lower your cost through an optimized configuration and keep it low going forward.
These topics will be covered
- Reducing license cost by finding and fixing misconfigurations and superfluous accounts
- How do CCB and CCX licenses really work?
- Understanding the DLAU tool and how to best utilize it
- Tips for common problem areas, like team mailboxes, functional/test users, etc
- Practical examples and best practices to implement right away
Deep Dive: AI-Powered Marketing to Get More Leads and Customers with HyperGro...
Comprehensive wavelengths and energy levels of Fe II, Cr II and other iron-group elements using Fourier transform and grating spectroscopy
1. Comprehensive wavelengths and energy levels of Fe II, Cr
II and other iron-group elements using Fourier transform
and grating spectroscopy
PI: Gillian Nave
Co I: Craig J. Sansonet
National Institute of Standards and Technology,
Gaithersburg, MD
NASA inter-agency agreement NNH10AN38I.
Start Date: January 2010.
End Date: December 2012.
2. Objectives
1)Prepare a comprehensive linelist of about 15 000 lines in Fe II. Wavelengths from 90
nm to 5.5 µm. Wavelength uncertainty around 1:107
. Identify lines using about 1000
energy levels with uncertainties of around 0.002 cm-1
.
2)Prepare similar linelist for Cr II, containing over 4000 lines from 700 levels.
3)Record and analyze spectra of additional iron-group element, selected by
consultation with astronomical community.
Research this year has focused on finishing Fe II and the UV/visible spectrum of Cr II.
3. High-resolution UV spectra from the
Hubble Space Telescope
J. C. Brandt et al., AsJ 117, 1505 (1999)
Data for synthetic spectra require
accurate wavelengths and oscillator
strengths with comprehensive coverage
for all elements and ionization stages
present in the stellar spectrum.
4. Background to objectives: Fe II
●
Last major analysis of Fe II in 1978. Contained 3272 lines from 576 levels:
S. Johansson, “The spectrum and term system of Fe II,” Phys. Scr. 18, 217 (1978).
●
FT spectra of Fe-Ne and Fe-Ar hollow cathode lamps analyzed by G. Nave: Precise
wavelengths in Fe I published: 1991 and 1992.
●
Collaboration with S. Johansson (Lund Univ., Sweden) begun in 1992 – combined FTS
& grating spectra contain 34000 lines from 83 nm to 5.5 µm.
●
9500 of these lines are Fe I:
G. Nave, S. Johansson, R. C. M. Learner, A. P. Thorne, J. W. Brault, “A new multplet
table for Fe I,” ApJS, 94, 221 (1994).
●
About 15000 are Fe II. Analysis begun by S. Johansson, but remained uncompleted
when Johansson died in 2008.
8. High-excitation levels from HR6000
•
109 new levels from 3d6
(3
L)4f (L=P, H, F, G) found using UVSE
spectra of HR600 & 46 Aql Castelli & Kurucz (A&A 520, A57
(2010))
•
Majority of lines too high excitation to give lines in laboratory
spectra, but some lines from these levels in lab
•
Currently verifying which of the lines from these levels in lab
spectra are correct.
•
Calculations of Kurucz helpful, but not predictive.
•
Are all levels correct?
10. Current status of Fe II
•
Identifications for 13500 spectral lines in Fe II confirmed.
About 500 have more than one identification.
•
Verifying levels of Kurucz & Castelli – roughly 100 more lines.
•
Need to add (5
D)5g-6h lines (about 60 lines).
•
Revise intensity scale?
•
Aim to finish by end of 2011.
12. Background to research: Cr II
●
Last major analysis of Cr II in 1951. Contained 1843 lines from 99 levels:
●
C. C. Kiess, “Descripton and analysis of the second spectrum of chromium, Cr II,” J. Res.
NBS 47, 385.
●
ASD contains 743 levels, most of variable quality, unpublished with no published lines.
●
Spectra of low-current Pt-Cr-Ne lamps taken at NIST for calibration of STIS using FTS and
grating:
C. J. Sansonet, F. Kerber, J. Reader, M R. Rosa, “Characterizaton of the far-ultraviolet
spectrum of Pt/Cr-Ne hollow cathode lamps as used on the space telescope imaging
spectrograph on board the Hubble space telescope,” ApJ 153, 555 (2004).
These are the spectra being used in the current analysis. Will be combined with IR spectra
of high-current hollow cathode lamp recorded using NIST 2-m FTS.
13. 2-m FTS
High Current HCL
2.0 A
2.0 Torr Ne
Si photodiode
FT700 VUV FTS
Low Current HCL
20 mA
≈ 5.0 Torr Ne
R106UH PMT
UG11 Filter
FT700 VUV FTS
Low Current HCL
20 mA
≈ 5.0 Torr Ne
R1220 PMT
14. Current Status of Cr II Project
●
Grating spectra recorded in region 1131 – 1844 Å
928 Cr II lines
●
FTS spectra and measured in region 1568 – 4000 Å
2750 Cr II lines
●
FTS spectra recorded from 3000 – 11000 Å.
●
Energy levels optimization
3457 total classified lines
3361 used in level optimization
284 of 334 even levels optimized
347 of 369 odd levels optimized
15. Many level values change far
outside the estimated 0.05 cm-1
uncertainty of the levels from
Sugar & Corliss
61% of optimized levels
have uncertainties
<0.005 cm-1
. 91% have
uncertainties <0.02 cm-1
16. •
Chromium is more abundant in chemically peculiar stars than the sun.
•
Ritz wavelength of the Cr II line 4848 Å agrees poorly with astronomical
spectra. There is no precise laboratory wavelength for this line.
•
From our optimized levels the Cr II 4848 Å line wavelength is
4848.2506(5) Å, an increase of 0.0156 Å from the original Ritz value.
Ryabchikova, unpublished
17. Future directions.
● Fe II to be finished by end of 2011.
● Cr II vis/UV finished soon, IR region to be measured and
analyzed.
● Plan to start another singly-ionized element next year: Mn II?
18. 1994 2010
Lab (full time) 3 1
Lab (part time) 0 1/4
Data compilations (full time) 2 3
Data compilations
(part time)
3 4
NIST atomic spectroscopy group
Then and now
19. Other astronomy projects in NIST Atomic Spectroscopy
Group
● Calibration of Pt/Ne hollow cathode lamps for GHRS (NASA-
funded).
● Calibration of Pt/Cr/Ne hcls for STIS (NASA funded).
● Aging tests of Pt lamps for COS (NASA funded).
● Calibration of Th/Ar lamps in infrared (ESO/NASA funded) for
CRIRES.
● Calibration of U/Ne lamps in IR (NRC postdoctoral project).
NASA funding essential to continuation of laboratory
program in NIST Atomic Spectroscopy Group.