astro-ph/9808039 PDF
... FUV calibration error was nearly canceled in this ratio by a similar error in the Hα. The plausibility of the combined results hindered the discovery of both problems. In fact, all of the optical fluxes reported in Paper I were a factor of 1.7 too high, because an incorrect aperture diameter was app ...
... FUV calibration error was nearly canceled in this ratio by a similar error in the Hα. The plausibility of the combined results hindered the discovery of both problems. In fact, all of the optical fluxes reported in Paper I were a factor of 1.7 too high, because an incorrect aperture diameter was app ...
BD−21 3873: another yellow-symbiotic barium star
... to the binary barium and CH stars which are also s-process enriched. These binary systems, which exhibit overabundances of the heavy elements, owe their abundance peculiarities to mass transfer from thermally-pulsing asymptotic giant branch stars, which have since evolved to become white-dwarf compa ...
... to the binary barium and CH stars which are also s-process enriched. These binary systems, which exhibit overabundances of the heavy elements, owe their abundance peculiarities to mass transfer from thermally-pulsing asymptotic giant branch stars, which have since evolved to become white-dwarf compa ...
the density profiles of massive, relaxed galaxy clusters. i. the total
... dispersion profiles of the BCGs. Lensing-derived mass profiles typically agree with independent X-ray estimates within 15%, suggesting that departures from hydrostatic equilibrium are small and that the clusters in our sample (except A383) are not strongly elongated or compressed along the line of ...
... dispersion profiles of the BCGs. Lensing-derived mass profiles typically agree with independent X-ray estimates within 15%, suggesting that departures from hydrostatic equilibrium are small and that the clusters in our sample (except A383) are not strongly elongated or compressed along the line of ...
THE UV-OPTICAL GALAXY COLOR-MAGNITUDE DIAGRAM. III
... an extinction-corrected Hess function in order to determine the number density of transition galaxies. We do not use the method of Johnson et al. (2007a, 2007b) because we use the combination of Dn (4000) and NUV r later as a transition rate metric. Kauffmann et al. (2003) measured dust extinction ...
... an extinction-corrected Hess function in order to determine the number density of transition galaxies. We do not use the method of Johnson et al. (2007a, 2007b) because we use the combination of Dn (4000) and NUV r later as a transition rate metric. Kauffmann et al. (2003) measured dust extinction ...
Booklet - Centrum Astronomiczne im. M.Kopernika PAN
... 1992. Currently, the OGLE project monitors brightness of about 109 stars, which is a unique tool for detecting and studying variable stars of all kinds. The catalogs prepared on the basis of the OGLE photometric databases contain over 105 stars in the late stages of evolution - long-period variables ...
... 1992. Currently, the OGLE project monitors brightness of about 109 stars, which is a unique tool for detecting and studying variable stars of all kinds. The catalogs prepared on the basis of the OGLE photometric databases contain over 105 stars in the late stages of evolution - long-period variables ...
Munshi_washington_0250E_12611
... mass ratio as a function of halo mass for a new sample of simulated field galaxies using fully cosmological, LCDM, high resolution SPH + N-Body simulations carried to the present time. I find there is extremely good agreement between the simulations and predictions from the statistical Halo Occupati ...
... mass ratio as a function of halo mass for a new sample of simulated field galaxies using fully cosmological, LCDM, high resolution SPH + N-Body simulations carried to the present time. I find there is extremely good agreement between the simulations and predictions from the statistical Halo Occupati ...
PPT (Download!) - SDSS SkyServer
... Give results table a name (for your MyDB) Give your query a name Wait until it says “started” ...
... Give results table a name (for your MyDB) Give your query a name Wait until it says “started” ...
evolución química de la nube grande de magallanes.
... In addition, an age of 1.45 Gyr (σ = 0.2Gyr) was estimated for SL869 using isochrone fitting. One of the most important results in this study is that from the mean [α/Fe] vs [Fe/H] plot (Fig. 3.7). We find that H11 lies in the range of the dSph trend and below the Galactic one. This result confirms ...
... In addition, an age of 1.45 Gyr (σ = 0.2Gyr) was estimated for SL869 using isochrone fitting. One of the most important results in this study is that from the mean [α/Fe] vs [Fe/H] plot (Fig. 3.7). We find that H11 lies in the range of the dSph trend and below the Galactic one. This result confirms ...
The Density Profiles of Massive, Relaxed Galaxy Clusters - HAL-Insu
... Ostriker 2010). The observation from that massive ellipticals have nearly isothermal total mass profiles within their effective radii – with very little scatter – is a strong constraint on their formation and evolution (Koopmans et al. 2009). On the other hand, the structure of halos may constrain D ...
... Ostriker 2010). The observation from that massive ellipticals have nearly isothermal total mass profiles within their effective radii – with very little scatter – is a strong constraint on their formation and evolution (Koopmans et al. 2009). On the other hand, the structure of halos may constrain D ...
A Variability Study of the Typical Red Supergiant Antares A
... many of the features of this variability have been associated with large convective cells. Unfortunately, due to the long timescales of these variations they are not well studied, with the exception of the bright M-class supergiant Betelgeuse (α Orionis, M2 Iab). Betelgeuse has been well studied bot ...
... many of the features of this variability have been associated with large convective cells. Unfortunately, due to the long timescales of these variations they are not well studied, with the exception of the bright M-class supergiant Betelgeuse (α Orionis, M2 Iab). Betelgeuse has been well studied bot ...
Preliminary Talk Abstract Book - MoCA
... Galactic winds are necessary to reduce the star formation rate in simulated galaxies to match observations. However, these outflows can be so violent that they completely destroy the gas disc. Maintaining a gas disc for a sufficiently long time in order to form a stellar disc thus becomes difficult. ...
... Galactic winds are necessary to reduce the star formation rate in simulated galaxies to match observations. However, these outflows can be so violent that they completely destroy the gas disc. Maintaining a gas disc for a sufficiently long time in order to form a stellar disc thus becomes difficult. ...
constraints on grain formation around carbon stars
... without previously formed internal crystals of titanium carbide ( TiC ). A lower mass limit of 1.1 M for stars capable of contributing grains to the solar nebula is derived. This mass limit, in conjunction with a mass-luminosity relation for carbon stars, identifies the region of the H-R diagram re ...
... without previously formed internal crystals of titanium carbide ( TiC ). A lower mass limit of 1.1 M for stars capable of contributing grains to the solar nebula is derived. This mass limit, in conjunction with a mass-luminosity relation for carbon stars, identifies the region of the H-R diagram re ...
Annual Report 2011 - Max Planck Institute for Astrophysics
... computer system is organized by the Computer Executive Committee. This group of scientists and system managers also evaluates user requests concerning resources or system structure, with scientific necessity being the main criterion for decisions. RZG and MPA coordinate activities and development pl ...
... computer system is organized by the Computer Executive Committee. This group of scientists and system managers also evaluates user requests concerning resources or system structure, with scientific necessity being the main criterion for decisions. RZG and MPA coordinate activities and development pl ...
Low radioderived star formation rates in z < 0.5 gammaray burst host
... 4.2 Radio properties of GRB host galaxies Berger et al. (2003) studied 20 GRB host galaxies at 0.7 < z < 4.5, 12 of them at 8.46 GHz with the VLA and four at 1.39 GHz at the ATCA, with the remainder observed only in the submillimetre. Although the majority of his sample yielded non-detections, he es ...
... 4.2 Radio properties of GRB host galaxies Berger et al. (2003) studied 20 GRB host galaxies at 0.7 < z < 4.5, 12 of them at 8.46 GHz with the VLA and four at 1.39 GHz at the ATCA, with the remainder observed only in the submillimetre. Although the majority of his sample yielded non-detections, he es ...
THE EVOLUTION OF GALAXY NUMBER DENSITY AT Z < 8 AND
... There are a few reasons for why deep imaging programs are not easily able to convert observations to total numbers of galaxies. One of these issues is that all deep observations are incomplete. This is due to limitations in exposure times and depth such that certain galaxies will be detected more re ...
... There are a few reasons for why deep imaging programs are not easily able to convert observations to total numbers of galaxies. One of these issues is that all deep observations are incomplete. This is due to limitations in exposure times and depth such that certain galaxies will be detected more re ...
matter and dark energy Gravitational lensing: a unique probe of dark
... temporary brightening of a star due to the magnification induced by a foreground object that crosses the line of sight to the observer. In this rare post-1919 article about lensing by its discoverer, he states ‘of course there is no hope of observing this phenomenon’. The Caltech astronomer Fritz Zw ...
... temporary brightening of a star due to the magnification induced by a foreground object that crosses the line of sight to the observer. In this rare post-1919 article about lensing by its discoverer, he states ‘of course there is no hope of observing this phenomenon’. The Caltech astronomer Fritz Zw ...
Hubble 2006: Science Year in Review
... data-recording system to replace the aging magnetic tape drives, and the gyroscopes needed for pointing control. A month prior to launch, a gyroscope failure had forced Hubble into “safe mode,” with no ability to observe astronomical targets. When a premature loss of solid-nitrogen coolant cut short ...
... data-recording system to replace the aging magnetic tape drives, and the gyroscopes needed for pointing control. A month prior to launch, a gyroscope failure had forced Hubble into “safe mode,” with no ability to observe astronomical targets. When a premature loss of solid-nitrogen coolant cut short ...
Catalogs of Hot White Dwarfs in the Milky Way from GALEX`s
... colors are insensitive (see e.g. Bianchi (2007), Bianchi et al. (2007a), Bianchi et al. (2007b)) as well as to their very short lifetimes on the constant-luminosity post-AGB phase. To make matters more difficult, the post-AGB luminosity at a given stellar temperature varies significantly according t ...
... colors are insensitive (see e.g. Bianchi (2007), Bianchi et al. (2007a), Bianchi et al. (2007b)) as well as to their very short lifetimes on the constant-luminosity post-AGB phase. To make matters more difficult, the post-AGB luminosity at a given stellar temperature varies significantly according t ...
Astronomy Astrophysics - Max Planck Institut für Radioastronomie
... can mainly be traced by the spectral lines, which for pre-mainsequence stars are often found in emission. While some information about the kinematics of the gas can already be extracted from the line profile, the spatial origin of the gas emission and the physical processes they trace are still stro ...
... can mainly be traced by the spectral lines, which for pre-mainsequence stars are often found in emission. While some information about the kinematics of the gas can already be extracted from the line profile, the spatial origin of the gas emission and the physical processes they trace are still stro ...
The Collision Between The Milky Way And Andromeda
... 16% (Spergel et al. 2003). Since the Milky Way and Andromeda galaxy models only include baryons in the galactic disk and bulge components, they are far short of this value. We therefore set the Local Group medium to be 20% primordial gas, by mass, so that the entire region approaches the cosmic mean ...
... 16% (Spergel et al. 2003). Since the Milky Way and Andromeda galaxy models only include baryons in the galactic disk and bulge components, they are far short of this value. We therefore set the Local Group medium to be 20% primordial gas, by mass, so that the entire region approaches the cosmic mean ...
The impact of protocluster environments at z = 1.6
... of the protocluster, which are labelled. Groups 5 and 6 have stellar masses <1011 M and we do not classify them as massive groups. The size of the circles are proportional to the stellar mass of the galaxy with larger symbols indicating more massive galaxies. ...
... of the protocluster, which are labelled. Groups 5 and 6 have stellar masses <1011 M and we do not classify them as massive groups. The size of the circles are proportional to the stellar mass of the galaxy with larger symbols indicating more massive galaxies. ...
The dark matter crisis: falsification of the current standard model of
... (e.g. Freire & Wex 2010). Albert Einstein had developed his field equation such that the Newtonian equations of motion be derivable from it, and thus that it be consistent with the then available celestial phenomena1 . The currently popular understanding of cosmology is based on the null hypothesis ( ...
... (e.g. Freire & Wex 2010). Albert Einstein had developed his field equation such that the Newtonian equations of motion be derivable from it, and thus that it be consistent with the then available celestial phenomena1 . The currently popular understanding of cosmology is based on the null hypothesis ( ...
Cold dark matter heats up
... explain without significant galactic winds. Mounting evidence also suggests that much of the in-flowing material into galaxies may also be metal-enriched37, consistent with a picture in which much of the wind does not attain the escape velocity but instead re-accretes38. A separate argument also poi ...
... explain without significant galactic winds. Mounting evidence also suggests that much of the in-flowing material into galaxies may also be metal-enriched37, consistent with a picture in which much of the wind does not attain the escape velocity but instead re-accretes38. A separate argument also poi ...
Le PHARE
... % prog-name -c configuration-file [-Parameter value] ... where prog-name is the name of the program, followed by a configuration file called with -c configurationfile and a list of parameters. Any -Parameter value statement in the command-line overrides the values written in the configuration file. ...
... % prog-name -c configuration-file [-Parameter value] ... where prog-name is the name of the program, followed by a configuration file called with -c configurationfile and a list of parameters. Any -Parameter value statement in the command-line overrides the values written in the configuration file. ...
Population effects on the red giant clump absolute magnitude, and
... Key words: Hertzsprung±Russell (HR) diagram ± stars: horizontal branch ± stars: luminosity function, mass function ± solar neighbourhood ± Magellanic Clouds ± galaxies: stellar content. ...
... Key words: Hertzsprung±Russell (HR) diagram ± stars: horizontal branch ± stars: luminosity function, mass function ± solar neighbourhood ± Magellanic Clouds ± galaxies: stellar content. ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.