DISCOVERY OF THREE z > 6.5 QUASARS IN THE VISTA KILO
... Galaxy (VIKING) survey, thus extending the number from 1 to 4. The newly discovered quasars have redshifts of z = 6.60, 6.75, and 6.89. The absolute magnitudes are between −26.0 and −25.5, 0.6–1.1 mag fainter than ULAS J1120+0641. Near-infrared spectroscopy revealed the Mg ii emission line in all th ...
... Galaxy (VIKING) survey, thus extending the number from 1 to 4. The newly discovered quasars have redshifts of z = 6.60, 6.75, and 6.89. The absolute magnitudes are between −26.0 and −25.5, 0.6–1.1 mag fainter than ULAS J1120+0641. Near-infrared spectroscopy revealed the Mg ii emission line in all th ...
Observational Studies of Interacting Galaxies and the Development
... understanding of galaxy merger evolution through both observational studies and instrument developments. Observationally, I approach the goal photometrically and spectroscopically. The photometric studies better constrain the number density evolution of wet and dry mergers through five CFHTLS broad ...
... understanding of galaxy merger evolution through both observational studies and instrument developments. Observationally, I approach the goal photometrically and spectroscopically. The photometric studies better constrain the number density evolution of wet and dry mergers through five CFHTLS broad ...
Abstract Title of Dissertation: BLACK HOLE DYNAMICS AND GRAVITATIONAL RADIATION IN GALACTIC NUCLEI
... small galaxies, and mergers and tidal separations of black hole binaries in galaxies that host supermassive black holes. Mergers between stellar-mass black holes will be key sources of gravitational radiation for ground-based detectors. However, the rates of these events are highly uncertain, becaus ...
... small galaxies, and mergers and tidal separations of black hole binaries in galaxies that host supermassive black holes. Mergers between stellar-mass black holes will be key sources of gravitational radiation for ground-based detectors. However, the rates of these events are highly uncertain, becaus ...
X-ray binaries in the Milky Way and other galaxies
... 6.3. Total X-ray luminosity as SFR indicator . . . . . . . . . . . . . . . . . . . 6.4. Theoretical LX –SFR relation . . . . . . . . . . . . . . . . . . . . . . . . . 6.5. LX –SFR relation: comparison with the data . . . . . . . . . . . . . . . . . 6.6. Hubble Deep Field North . . . . . . . . . . . ...
... 6.3. Total X-ray luminosity as SFR indicator . . . . . . . . . . . . . . . . . . . 6.4. Theoretical LX –SFR relation . . . . . . . . . . . . . . . . . . . . . . . . . 6.5. LX –SFR relation: comparison with the data . . . . . . . . . . . . . . . . . 6.6. Hubble Deep Field North . . . . . . . . . . . ...
Presolar History Recorded in Extraterrestrial Materials
... solar value (indicated in Figure 4) and small to modest depletions in 18O (18O/16O between 0.001 and solar). The range of 17O/16O ratios agrees quite well with astrophysical models of low-mass stars and with the observed O isotope ratios of red giant and AGB stars. ...
... solar value (indicated in Figure 4) and small to modest depletions in 18O (18O/16O between 0.001 and solar). The range of 17O/16O ratios agrees quite well with astrophysical models of low-mass stars and with the observed O isotope ratios of red giant and AGB stars. ...
Cross-Path LIDAR for Turbulence Profile Determination Mikhail S
... Knowledge of the turbulence profile is important for various applications including directed energy systems such as Airborne Laser and Tactical Airborne Laser, ground-based adaptive optics telescopes, and laser communication systems. The known methods for turbulence profile determination have variou ...
... Knowledge of the turbulence profile is important for various applications including directed energy systems such as Airborne Laser and Tactical Airborne Laser, ground-based adaptive optics telescopes, and laser communication systems. The known methods for turbulence profile determination have variou ...
EL CVn-type binaries - Discovery of 17 helium white dwarf
... (WASP 0247−25 B). The remnant is in a rarely-observed state evolving to higher effective temperatures at nearly constant luminosity prior to becoming a very low-mass white dwarf composed almost entirely of helium, i.e., it is a pre-He-WD. We have used the WASP photometric database to find 17 eclipsi ...
... (WASP 0247−25 B). The remnant is in a rarely-observed state evolving to higher effective temperatures at nearly constant luminosity prior to becoming a very low-mass white dwarf composed almost entirely of helium, i.e., it is a pre-He-WD. We have used the WASP photometric database to find 17 eclipsi ...
diplomov a prace - Univerzita Karlova
... studies about nova cycles, novae’s recurrence and the dependence of maximum light on the rate of decline. The known relation between maximum magnitude versus rate of decline makes novae good distance indicators. The spatial distribution of novae in galaxies is another often discussed question. The p ...
... studies about nova cycles, novae’s recurrence and the dependence of maximum light on the rate of decline. The known relation between maximum magnitude versus rate of decline makes novae good distance indicators. The spatial distribution of novae in galaxies is another often discussed question. The p ...
An Optical Study of Young Stellar Clusters
... are stars with a range of masses. The distribution of the stellar masses in a given volume of space in a stellar system at the time of their formation is known as the Initial Mass Function (IMF) of the system (Salpeter, 1955; Scalo, 1986; Kroupa, 2002; Chabrier, 2003). Together with the time modulat ...
... are stars with a range of masses. The distribution of the stellar masses in a given volume of space in a stellar system at the time of their formation is known as the Initial Mass Function (IMF) of the system (Salpeter, 1955; Scalo, 1986; Kroupa, 2002; Chabrier, 2003). Together with the time modulat ...
Evolution of Stars and Stellar Populations
... d beyond the edge of the visible matter distribution (as expected from Keplerian orbits after the limit of the mass distribution is reached) show a flat profile over large distances well beyond this limit. This can be explained only by a steady increase with distance of the galaxy mass, beyond the e ...
... d beyond the edge of the visible matter distribution (as expected from Keplerian orbits after the limit of the mass distribution is reached) show a flat profile over large distances well beyond this limit. This can be explained only by a steady increase with distance of the galaxy mass, beyond the e ...
A Universal Stellar Initial Mass Function? A Critical Look Further
... that the IMF is constant over some spatial or temporal scale. Measuring the IMF of a complex, multicomponent stellar population like the Milky Way disk provides a useful case study. The first step appears straightforward: Count stars within a limited volume as a function of mass. Low-mass stars are ...
... that the IMF is constant over some spatial or temporal scale. Measuring the IMF of a complex, multicomponent stellar population like the Milky Way disk provides a useful case study. The first step appears straightforward: Count stars within a limited volume as a function of mass. Low-mass stars are ...
THE COBE DIRBE POINT SOURCE CATALOG
... were selected in order to avoid missing variable stars that may have been faint during the 2MASS, IRAS, or MSX mission and to improve the completeness at 3.5 and 4.9 m (see x 6). Since the filtering process improves the average per measurement uncertainty (see x 5), a sensitive selection criterion ...
... were selected in order to avoid missing variable stars that may have been faint during the 2MASS, IRAS, or MSX mission and to improve the completeness at 3.5 and 4.9 m (see x 6). Since the filtering process improves the average per measurement uncertainty (see x 5), a sensitive selection criterion ...
TMT Science Overview - GSMT Program Office
... Bullock & Johnstone 2005). TMT.PSC.PRE.06.032.REL01 ...
... Bullock & Johnstone 2005). TMT.PSC.PRE.06.032.REL01 ...
The Day We Found the Universe
... spiraling nebulae were nothing less than separate galaxies. At the same time, a few hundred miles south at Mount Wilson, near Los Angeles, Harlow Shapley resized the Milky Way, measuring it as far larger than previously thought and shoving our Sun o to the side, away from the galaxy's hub. As Shaple ...
... spiraling nebulae were nothing less than separate galaxies. At the same time, a few hundred miles south at Mount Wilson, near Los Angeles, Harlow Shapley resized the Milky Way, measuring it as far larger than previously thought and shoving our Sun o to the side, away from the galaxy's hub. As Shaple ...
γ Doradus pulsation in two pre-main sequence stars discovered by
... which corresponds to a distance modulus of 9.40 ± 0.25 mag. The age of NGC 2264 can only be determined with a relatively large error because its main sequence consists only of massive O and B stars and stars of later spectral types are still in their PMS phase. Additionally, not all cluster members ...
... which corresponds to a distance modulus of 9.40 ± 0.25 mag. The age of NGC 2264 can only be determined with a relatively large error because its main sequence consists only of massive O and B stars and stars of later spectral types are still in their PMS phase. Additionally, not all cluster members ...
Modelling the observed properties of carbon-enhanced metal
... system. In this work we generate synthetic populations of binary stars at metallicity Z = 0.0001 ([Fe/H] ≈ −2.3), with the aim of reproducing the observed fraction of CEMP stars in the halo. In addition, we aim to constrain our model of the wind masstransfer process, in particular the wind-accretion ...
... system. In this work we generate synthetic populations of binary stars at metallicity Z = 0.0001 ([Fe/H] ≈ −2.3), with the aim of reproducing the observed fraction of CEMP stars in the halo. In addition, we aim to constrain our model of the wind masstransfer process, in particular the wind-accretion ...
An artificial neural network approach to the classification of galaxy
... 'NormaI26' spectra have been selected as being representative spectra for galaxies of normal morphological type, i.e., galaxies which conform simply to the Hubble classification scheme (Hubble 1936). the 'Unusual29' spectra comprise the remainder of the galaxies observed by Kennicutt. These spectra ...
... 'NormaI26' spectra have been selected as being representative spectra for galaxies of normal morphological type, i.e., galaxies which conform simply to the Hubble classification scheme (Hubble 1936). the 'Unusual29' spectra comprise the remainder of the galaxies observed by Kennicutt. These spectra ...
University of Groningen Late-type spiral galaxies Ganda, Katia
... for a representative census of ellipticals, lenticulars and early-type spiral galaxies, to which in the rest of this chapter we will refer as ‘the SAURON survey’. Our project can be regarded as an extension of the SAURON survey towards later-type objects. First results based on our data are presente ...
... for a representative census of ellipticals, lenticulars and early-type spiral galaxies, to which in the rest of this chapter we will refer as ‘the SAURON survey’. Our project can be regarded as an extension of the SAURON survey towards later-type objects. First results based on our data are presente ...
The X-shooter Spectral Library (XSL): I. DR1. Near
... When the sky lines are very weak in stare mode, which is often the case in short-exposure frames, such as in the UVB arm, the background model constructed by the pipeline can fail catastrophically, particularly if weak pattern noise is not properly subtracted by the master bias. This arises from ele ...
... When the sky lines are very weak in stare mode, which is often the case in short-exposure frames, such as in the UVB arm, the background model constructed by the pipeline can fail catastrophically, particularly if weak pattern noise is not properly subtracted by the master bias. This arises from ele ...
my dissertation (PhD. Thesis) - Argelander
... of all sizes and distances ranging from our “backyard”, namely the Milky Way itself and the Local Group to galaxies at a redshift of z ' 11 and higher. Each approach can deliver different information and has its advantages and disadvantages. In the following, I briefly describe what can be learned b ...
... of all sizes and distances ranging from our “backyard”, namely the Milky Way itself and the Local Group to galaxies at a redshift of z ' 11 and higher. Each approach can deliver different information and has its advantages and disadvantages. In the following, I briefly describe what can be learned b ...
... The relative importance of the different physical processes of galaxy evolution (Figure 1) changes as the Universe expands. Rapid processes that happen in discrete events are giving way to slow, ongoing processes. At early times, galactic evolution was dominated by a combination of dissipative colla ...
Modeling Spatially and Spectrally Resolved Observations to
... This thesis owes much to the support of my officemate, Zach Berta, for five years of advice on life, computers, and astronomy. I thank Diego Muñoz, Robert Harris, Ragnhild Lunnan, and Sarah Rugheimer for countless snack and coffee breaks; Wen-fai Fong and Nick Stone for leading camping trips and t ...
... This thesis owes much to the support of my officemate, Zach Berta, for five years of advice on life, computers, and astronomy. I thank Diego Muñoz, Robert Harris, Ragnhild Lunnan, and Sarah Rugheimer for countless snack and coffee breaks; Wen-fai Fong and Nick Stone for leading camping trips and t ...
The correlation between galaxy morphology and star
... statistical fashion the correlations between galaxy structures and star-formation activity at z ∼ 2, i.e. the epoch when the cosmic star–formation activity reached its peak, to their counterparts in the local universe. The structure of this paper is as follows. The optical and infrared data and sele ...
... statistical fashion the correlations between galaxy structures and star-formation activity at z ∼ 2, i.e. the epoch when the cosmic star–formation activity reached its peak, to their counterparts in the local universe. The structure of this paper is as follows. The optical and infrared data and sele ...
Full Text - Digital Access to Scholarship at Harvard
... burn. These heavy elements are expelled into the interstellar medium in stellar winds and in more violent eruptions and explosions. The heavy elements are reprocessed in the interstellar medium forming dust grains (Draine, 2003; Li & Greenberg, 2003). That said, dust is in some sense more an empiric ...
... burn. These heavy elements are expelled into the interstellar medium in stellar winds and in more violent eruptions and explosions. The heavy elements are reprocessed in the interstellar medium forming dust grains (Draine, 2003; Li & Greenberg, 2003). That said, dust is in some sense more an empiric ...
Stellar activity in exoplanet hosts Enrique Herrero Casas
... Most of the efforts on the search and characterization of Earth-like exoplanets are currently focused on low mass stars. These represent the vast majority of the population in our galaxy (about 75% of the stars have a lower mass than the Sun) and their interest lies in the fact that the photometric a ...
... Most of the efforts on the search and characterization of Earth-like exoplanets are currently focused on low mass stars. These represent the vast majority of the population in our galaxy (about 75% of the stars have a lower mass than the Sun) and their interest lies in the fact that the photometric a ...
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.