The XMM-Newton Bright Serendipitous Survey
... optical counterpart using the existing optical surveys (i.e. the DSS I/II1 and the SDSS2 ). In particular, we have found the optical counterpart of about 88% of the XBS sources on the DSS with a red magnitude (the APM3 red magnitude) brighter than ∼20.5. All but 6 of the remaining sources have been ...
... optical counterpart using the existing optical surveys (i.e. the DSS I/II1 and the SDSS2 ). In particular, we have found the optical counterpart of about 88% of the XBS sources on the DSS with a red magnitude (the APM3 red magnitude) brighter than ∼20.5. All but 6 of the remaining sources have been ...
Particle Physics from Stars
... hypothetical elementary particles and their interactions. The “heavenly laboratories” are complementary to accelerator and non-accelerator experiments, notably at the “low-energy frontier” of particle physics, which includes the physics of neutrinos and other weakly interacting low-mass particles su ...
... hypothetical elementary particles and their interactions. The “heavenly laboratories” are complementary to accelerator and non-accelerator experiments, notably at the “low-energy frontier” of particle physics, which includes the physics of neutrinos and other weakly interacting low-mass particles su ...
Development of a Software Package for the Reduction and Analysis
... position of a meteor was computed to be 0.2−3.0 pixels, with a median value of 0.3 pixels. Sub-pixel accuracy (0.2−0.5 pixels) was also reached for the uncertainties in the astrometric transformation. Different modules of SPARVM were compared with 3 other software packages indicating that SPARVM is ...
... position of a meteor was computed to be 0.2−3.0 pixels, with a median value of 0.3 pixels. Sub-pixel accuracy (0.2−0.5 pixels) was also reached for the uncertainties in the astrometric transformation. Different modules of SPARVM were compared with 3 other software packages indicating that SPARVM is ...
SOFA Astrometry Tools
... The “current” coordinates are the intermediary stage between a star’s catalog entry and the direction seen by the observer. The SOFA astrometry routines use the Celestial Intermediate Reference System (CIRS) for this purpose. The pole is the celestial intermediate pole (CIP), and the α zero-point th ...
... The “current” coordinates are the intermediary stage between a star’s catalog entry and the direction seen by the observer. The SOFA astrometry routines use the Celestial Intermediate Reference System (CIRS) for this purpose. The pole is the celestial intermediate pole (CIP), and the α zero-point th ...
2010/2011 Venus Observation
... • In 1996, two GO Venus proposals (6607 and 6771) were approved by the TAC; and there was one GTO/WF2 program (6851) to observe Venus. All of these were cancelled by the STScI Director shortly after phase 2 submission. • In 1997, there was a GTO/STIS program (7581) to observe Venus. Much implementat ...
... • In 1996, two GO Venus proposals (6607 and 6771) were approved by the TAC; and there was one GTO/WF2 program (6851) to observe Venus. All of these were cancelled by the STScI Director shortly after phase 2 submission. • In 1997, there was a GTO/STIS program (7581) to observe Venus. Much implementat ...
Unfolding the Milky Way bulge - International Max Planck Research
... bulge population formed on a short timescale and the drop produced by the contribution of SN Ia during a more extended process. The absolute values of these trends depend on the IMF and the SFR of the population. . . . . . . . . . . . . . 14 ...
... bulge population formed on a short timescale and the drop produced by the contribution of SN Ia during a more extended process. The absolute values of these trends depend on the IMF and the SFR of the population. . . . . . . . . . . . . . 14 ...
2010/2011 Venus Observation
... • In 1995, the Venus observation was originally lost due to an unrelated safing; but it was quickly replanned and executed successfully. • The 2003 Venus observations were delayed from 2001 due to the failure of the STIS side 1 electronics. ...
... • In 1995, the Venus observation was originally lost due to an unrelated safing; but it was quickly replanned and executed successfully. • The 2003 Venus observations were delayed from 2001 due to the failure of the STIS side 1 electronics. ...
The Lupus clouds - European Southern Observatory
... still uncomfortably large, as it implies an uncertainty by a factor near 3 in important quantities that depend on the square of the distance, such as the mass of clouds and cores or the luminosity of its member stars. Some of the most highly discrepant values refer to specific clouds, suggesting tha ...
... still uncomfortably large, as it implies an uncertainty by a factor near 3 in important quantities that depend on the square of the distance, such as the mass of clouds and cores or the luminosity of its member stars. Some of the most highly discrepant values refer to specific clouds, suggesting tha ...
An Atlas of Stellar Spectra
... the common kinds of stellar spectra observed in stars brighter than the eighth magnitude. The dispersion selected is intermediate between that used for very faint stars, where only a few spectral features are visible, and the larger-scale slit spectra which show a multitude of details. A sufficient ...
... the common kinds of stellar spectra observed in stars brighter than the eighth magnitude. The dispersion selected is intermediate between that used for very faint stars, where only a few spectral features are visible, and the larger-scale slit spectra which show a multitude of details. A sufficient ...
The VIMOS Ultra-Deep Survey (VUDS): Fast Increase in the Fraction
... have found that Lyα photons escape more easily from galaxies with low dust content. At high redshift, although on samples that are much smaller than the one we use in this paper, a similar trend has been found by Kornei et al. (2010) and Mallery et al. (2012), respectively at z ∼ 3 and at 4 < z < 6. ...
... have found that Lyα photons escape more easily from galaxies with low dust content. At high redshift, although on samples that are much smaller than the one we use in this paper, a similar trend has been found by Kornei et al. (2010) and Mallery et al. (2012), respectively at z ∼ 3 and at 4 < z < 6. ...
Galaxy Assembly through Mergers
... another challenge, even though, given their massive nature, they may be responsible for the high mass end of the mass function. Understanding the latter in the local universe, dubbed dry mergers, constitutes the basis of this work. With the availability of large dedicated surveys such as the Sloan D ...
... another challenge, even though, given their massive nature, they may be responsible for the high mass end of the mass function. Understanding the latter in the local universe, dubbed dry mergers, constitutes the basis of this work. With the availability of large dedicated surveys such as the Sloan D ...
The evolution of close binaries with white dwarf components
... When one of the stars overflows its Roche lobe, it tends to lose most of its envelope. The evolution of the star is significantly shortened or even stopped prematurely. In the latter case, nuclear burning ceases after the mass transfer phase. Consequently, the inert core contracts and cools down to fo ...
... When one of the stars overflows its Roche lobe, it tends to lose most of its envelope. The evolution of the star is significantly shortened or even stopped prematurely. In the latter case, nuclear burning ceases after the mass transfer phase. Consequently, the inert core contracts and cools down to fo ...
Zweijahresbericht 2000-2001
... by Günther’s moving spirit – and impressive work load (7 days a week at all geographic longitudes!) – now came to an end. We all would like to use this public place to express our sincerest thanks for his outstanding and hearty engagement for the institute and astronomy in general. A year earlier, ...
... by Günther’s moving spirit – and impressive work load (7 days a week at all geographic longitudes!) – now came to an end. We all would like to use this public place to express our sincerest thanks for his outstanding and hearty engagement for the institute and astronomy in general. A year earlier, ...
Astronomy Astrophysics
... the differences in the final color–magnitude diagram from field to field were marginal. The decontamination algorithm divides the full range of magnitude and colors of a CMD into a 3D grid of cells with axes along KS , (H−KS ), and (J−KS ). Initially, cell dimensions were ΔKS = 1.0 and Δ(H−KS ) = Δ(J ...
... the differences in the final color–magnitude diagram from field to field were marginal. The decontamination algorithm divides the full range of magnitude and colors of a CMD into a 3D grid of cells with axes along KS , (H−KS ), and (J−KS ). Initially, cell dimensions were ΔKS = 1.0 and Δ(H−KS ) = Δ(J ...
Europium, Samarium, and Neodymium Isotopic Fractions in Metal
... are very insensitive to the model atmosphere parameters. The wavelength of a spectral line is split by two effects, hyperfine structure (HFS) and isotope shifts, and the isotopic fractions can be measured by detailed comparisons of an observed absorption line profile to synthetic spectra of these li ...
... are very insensitive to the model atmosphere parameters. The wavelength of a spectral line is split by two effects, hyperfine structure (HFS) and isotope shifts, and the isotopic fractions can be measured by detailed comparisons of an observed absorption line profile to synthetic spectra of these li ...
1 Globular Cluster Systems - McMaster Physics and Astronomy
... and thus to elongate their whole distribution along the line of sight (roughly, the X axis). (3) The fundamental distance scale used by Shapley { essentially, the luminosity of the RR Lyraes or the tip of the red-giant branch { was about one magnitude brighter than the value adopted today; again, th ...
... and thus to elongate their whole distribution along the line of sight (roughly, the X axis). (3) The fundamental distance scale used by Shapley { essentially, the luminosity of the RR Lyraes or the tip of the red-giant branch { was about one magnitude brighter than the value adopted today; again, th ...
kdtalk_jun2005 - The HST Treasury Program on Eta Carinae
... · WFPC2 1994-2000: Proper motion studies of the Homunculus. Dominant ejection date was 1843, during the Great Eruption. · STIS 2000: Spectra seen from various latitudes via reflection by dust. Result: The stellar wind is essentially polar -- a fairly revolutionary result for wind theory in general. ...
... · WFPC2 1994-2000: Proper motion studies of the Homunculus. Dominant ejection date was 1843, during the Great Eruption. · STIS 2000: Spectra seen from various latitudes via reflection by dust. Result: The stellar wind is essentially polar -- a fairly revolutionary result for wind theory in general. ...
A Universal Stellar Initial Mass Function? A Critical Look Further
... disconcerting that the break from the Salpeter law identified in many IMF studies needs to be invoked near the place where the correction becomes important (around 1 M% ). Knowledge of the SFH of the Galaxy is also required to understand the opposite end of the mass spectrum. Substellar objects neve ...
... disconcerting that the break from the Salpeter law identified in many IMF studies needs to be invoked near the place where the correction becomes important (around 1 M% ). Knowledge of the SFH of the Galaxy is also required to understand the opposite end of the mass spectrum. Substellar objects neve ...
High-mass star-forming cloud G0.38+0.04 in the Galactic center dust
... detected – W51 North, Sgr B2 (M), and Orion KL – they closely trace the location of the high-mass YSO, likely pinpointing the base of a high-velocity outflow (Goddi et al. 2015). Cloud C, G0.38+0.04, is one of the high-column-density clouds along the central molecular zone (CMZ) dust ridge (Lis et a ...
... detected – W51 North, Sgr B2 (M), and Orion KL – they closely trace the location of the high-mass YSO, likely pinpointing the base of a high-velocity outflow (Goddi et al. 2015). Cloud C, G0.38+0.04, is one of the high-column-density clouds along the central molecular zone (CMZ) dust ridge (Lis et a ...
Stellar Oscillations Lecture Notes on Jørgen Christensen-Dalsgaard
... very many, stars pulsate in more complicated manners than the Cepheids. In many instances more than one mode of oscillation is excited simultaneously in a star; these modes may include both radial overtones, in addition to the fundamental, and nonradial modes, where the motion does not preserve sphe ...
... very many, stars pulsate in more complicated manners than the Cepheids. In many instances more than one mode of oscillation is excited simultaneously in a star; these modes may include both radial overtones, in addition to the fundamental, and nonradial modes, where the motion does not preserve sphe ...
The physics of line-driven winds of hot massive stars
... Galaxies are comprised of stars and clouds of gas. Stars that appear equally bright to the naked eye may either be nearby objects that are relatively dim or distant objects that are very luminous. The intrinsically brightest stars are the topic of this thesis. Their luminosities can be more than a m ...
... Galaxies are comprised of stars and clouds of gas. Stars that appear equally bright to the naked eye may either be nearby objects that are relatively dim or distant objects that are very luminous. The intrinsically brightest stars are the topic of this thesis. Their luminosities can be more than a m ...
X-ray astronomy of stellar coronae (Review)
... to interpreting stellar coronae without requiring the imaging capabilities that have been so central to solar studies. The field of stellar coronal X-ray astronomy was in fact opened around the same time, in 1975 when Catura et al. (1975) reported the detection of Capella as the first stellar corona ...
... to interpreting stellar coronae without requiring the imaging capabilities that have been so central to solar studies. The field of stellar coronal X-ray astronomy was in fact opened around the same time, in 1975 when Catura et al. (1975) reported the detection of Capella as the first stellar corona ...