Abstract book
... Abstract. Oscillations in cluster stars are important for gaining a deeper understanding about stellar structure and evolution. We present the results from a detailed ensemble study of solar-like oscillations in 115 red giants in the three open clusters, NGC 6791, NGC 6811, and NGC 6819, based on ph ...
... Abstract. Oscillations in cluster stars are important for gaining a deeper understanding about stellar structure and evolution. We present the results from a detailed ensemble study of solar-like oscillations in 115 red giants in the three open clusters, NGC 6791, NGC 6811, and NGC 6819, based on ph ...
Chapter 10 Formation and evolution of the Local Group
... diameter of ∼3 Mpc having a total mass of 2-5 × 1012 M⊙ . A strong morphologydensity relation exists in which gas-poor dwarf spheroidals (dSphs) are preferentially found closer to the Galaxy/M 31 than gas-rich dwarf irregulars (dIrrs). This is often promoted as evidence of environmental processes du ...
... diameter of ∼3 Mpc having a total mass of 2-5 × 1012 M⊙ . A strong morphologydensity relation exists in which gas-poor dwarf spheroidals (dSphs) are preferentially found closer to the Galaxy/M 31 than gas-rich dwarf irregulars (dIrrs). This is often promoted as evidence of environmental processes du ...
Cosmological dynamics with non-minimally coupled scalar field and
... components in order to distinguish spectroscopic pairs from false pairs created by projection along the line of sight. Of six pair candidates observed, companions (estimated mass ratios 5:1 and 7:1) are detected for two galaxies down to a 3σ limiting emission-line flux of ∼ 10−17 erg s−1 cm−2 . This ...
... components in order to distinguish spectroscopic pairs from false pairs created by projection along the line of sight. Of six pair candidates observed, companions (estimated mass ratios 5:1 and 7:1) are detected for two galaxies down to a 3σ limiting emission-line flux of ∼ 10−17 erg s−1 cm−2 . This ...
Episode 705: Cosmology - Teaching Advanced Physics
... A graph of measured values of Hubble’s constant The following graph, taken from Physics World, July 1999, shows how measured values of the Hubble constant have changed since the 1920s, when Hubble made his original measurement. ...
... A graph of measured values of Hubble’s constant The following graph, taken from Physics World, July 1999, shows how measured values of the Hubble constant have changed since the 1920s, when Hubble made his original measurement. ...
Word version of Episode 705
... A graph of measured values of Hubble’s constant The following graph, taken from Physics World, July 1999, shows how measured values of the Hubble constant have changed since the 1920s, when Hubble made his original measurement. ...
... A graph of measured values of Hubble’s constant The following graph, taken from Physics World, July 1999, shows how measured values of the Hubble constant have changed since the 1920s, when Hubble made his original measurement. ...
lecture course
... somewhat less secure than for stars. This is in part due to the extreme conditions near these very massive black holes of 106 to 109 solar masses, which is quite unlike anything we can test in laboratories on Earth (we are in the strong field limit of general relativity). On the other hand, atomic s ...
... somewhat less secure than for stars. This is in part due to the extreme conditions near these very massive black holes of 106 to 109 solar masses, which is quite unlike anything we can test in laboratories on Earth (we are in the strong field limit of general relativity). On the other hand, atomic s ...
PS1-12SK IS A PECULIAR SUPERNOVA FROM A HE
... We report on our discovery and observations of the Pan-STARRS1 supernova (SN) PS1-12sk, a transient with properties that indicate atypical star formation in its host galaxy cluster or pose a challenge to popular progenitor system models for this class of explosion. The optical spectra of PS112sk cla ...
... We report on our discovery and observations of the Pan-STARRS1 supernova (SN) PS1-12sk, a transient with properties that indicate atypical star formation in its host galaxy cluster or pose a challenge to popular progenitor system models for this class of explosion. The optical spectra of PS112sk cla ...
No Slide Title
... • Within the visible spiral, radial velocities (and masses) can be measured directly. • Outside the visible spiral, observe multiple galaxy systems. • Only radial velocity determined with Doppler shift. • Reliable statistical information from lots of observation. ...
... • Within the visible spiral, radial velocities (and masses) can be measured directly. • Outside the visible spiral, observe multiple galaxy systems. • Only radial velocity determined with Doppler shift. • Reliable statistical information from lots of observation. ...
Sample pages 1 PDF
... shown in Figs. 1.1 and 1.2, one of which we are viewing from above (face-on), the other from the side (edge-on). These are all stellar systems in which the majority of stars are confined to a relatively thin disk. In our own Galaxy, this disk can be seen as the band of stars stretched across the nig ...
... shown in Figs. 1.1 and 1.2, one of which we are viewing from above (face-on), the other from the side (edge-on). These are all stellar systems in which the majority of stars are confined to a relatively thin disk. In our own Galaxy, this disk can be seen as the band of stars stretched across the nig ...
P1 The Earth in the Universe
... Because of this, when we see stars in the night sky we are actually seeing them as they were in the past. ...
... Because of this, when we see stars in the night sky we are actually seeing them as they were in the past. ...
Document
... Because of this, when we see stars in the night sky we are actually seeing them as they were in the past. ...
... Because of this, when we see stars in the night sky we are actually seeing them as they were in the past. ...
looking for progenitors of cool Ap stars
... the main-sequence phase, or are intrinsically slow rotators from their formation on. He also found no hint of magnetic braking on the MS from a study of the distribution of the rotation periods as a function of the gravity (North 1985), and this has been confirmed recently on the basis of new surfac ...
... the main-sequence phase, or are intrinsically slow rotators from their formation on. He also found no hint of magnetic braking on the MS from a study of the distribution of the rotation periods as a function of the gravity (North 1985), and this has been confirmed recently on the basis of new surfac ...
Influence of the Gould Belt on Interstellar Extinction
... higher than that of the model by Arenou et al. (1992) is unlikely to be possible. To achieve a high accuracy of the extinction correction, it is more preferable to reveal specific absorbing clouds or to determine the individual extinction for each star from its highly accurate multiband photometry. ...
... higher than that of the model by Arenou et al. (1992) is unlikely to be possible. To achieve a high accuracy of the extinction correction, it is more preferable to reveal specific absorbing clouds or to determine the individual extinction for each star from its highly accurate multiband photometry. ...
Radial distribution of gas and dust in spiral galaxies - ORCA
... a derived dust mass is that they are independent of the specific, not yet well studied, model assumptions in this new wavelength range. They both decrease with radius, which suggests that the dust in the outermost regions is colder than in the centre of the galaxies. This is naturally explained by a ...
... a derived dust mass is that they are independent of the specific, not yet well studied, model assumptions in this new wavelength range. They both decrease with radius, which suggests that the dust in the outermost regions is colder than in the centre of the galaxies. This is naturally explained by a ...
FREE Sample Here
... km or 8 light minutes) away. How far away, to scale, would the nearest stars to the Sun be? Pick the closest answer. a. About the distance between New York and Boston. (330 km) b. 100 meters away c. About the distance across the United States from New York to Los Angeles (4300 km). d. About the dist ...
... km or 8 light minutes) away. How far away, to scale, would the nearest stars to the Sun be? Pick the closest answer. a. About the distance between New York and Boston. (330 km) b. 100 meters away c. About the distance across the United States from New York to Los Angeles (4300 km). d. About the dist ...
Statistical analysis of stellar evolution
... of the Sun, M , its core will ignite in a thermonuclear reaction that is powered by the fusion of hydrogen into helium. This reaction at the star’s core can continue for millions or billions of years depending on the original mass and composition of the star. More massive stars are denser, and thus ...
... of the Sun, M , its core will ignite in a thermonuclear reaction that is powered by the fusion of hydrogen into helium. This reaction at the star’s core can continue for millions or billions of years depending on the original mass and composition of the star. More massive stars are denser, and thus ...
How special are brightest group and cluster galaxies?
... • ~30% of the BCG were missed by fiber collision and this is corrected by photometric objects(but low-reliability). ...
... • ~30% of the BCG were missed by fiber collision and this is corrected by photometric objects(but low-reliability). ...
Extragalactic Background Light Encyclopedia of Astronomy & Astrophysics eaa.iop.org Rebecca A Bernstein
... Extragalactic Background Light Extragalactic background light (EBL) is the integrated flux from all extragalactic sources, including those which are not individually detected. In keeping with the COSMOLOGICAL PRINCIPLE—that the universe should appear homogeneous and isotropic to a typical observer—t ...
... Extragalactic Background Light Extragalactic background light (EBL) is the integrated flux from all extragalactic sources, including those which are not individually detected. In keeping with the COSMOLOGICAL PRINCIPLE—that the universe should appear homogeneous and isotropic to a typical observer—t ...
Galaxies
... 1) Is there a connection between the types of galaxies? 2) Does one type of galaxy evolve from the other? All galaxies are of about the same age Spiral galaxies have stars just as old as the stars in elliptical galaxies Hubble tried to devise an evolutionary scheme for galaxies There is no evolution ...
... 1) Is there a connection between the types of galaxies? 2) Does one type of galaxy evolve from the other? All galaxies are of about the same age Spiral galaxies have stars just as old as the stars in elliptical galaxies Hubble tried to devise an evolutionary scheme for galaxies There is no evolution ...
MAPPING THE GALAXY DISTRIBUTION AT LARGE DISTANCES1
... However, the redshift extent of these structures is nearly an order of magnitude larger than the typical velocity dispersion for clusters of galaxies (Zabludoff, Huchra, & Geller 1990), and their projections on the sky have no clear density enhancement. These elongated structures are, therefore, eit ...
... However, the redshift extent of these structures is nearly an order of magnitude larger than the typical velocity dispersion for clusters of galaxies (Zabludoff, Huchra, & Geller 1990), and their projections on the sky have no clear density enhancement. These elongated structures are, therefore, eit ...
Dark Stars: Dark Matter Annihilation in the First Stars.
... • Helps explain observed black holes: • (I) in centers of galaxies • (ii) billion solar mass BH at z=6 • (iii) excess extragalactic radio signal in ARCADE reported at AAS meeting by Kogut (1K at 1GHz), power law spectrum could come from synchrotron radiation from accretion onto early black holes ...
... • Helps explain observed black holes: • (I) in centers of galaxies • (ii) billion solar mass BH at z=6 • (iii) excess extragalactic radio signal in ARCADE reported at AAS meeting by Kogut (1K at 1GHz), power law spectrum could come from synchrotron radiation from accretion onto early black holes ...
11.1 Introduction
... Galaxy’s largest star-forming regions. It is rich is clusters of newly formed O and B stars, harbouring a significant fraction of the most massive stars known in the Milky Way, including several O3 V stars and the LBV η Carinae. The picture on the left highlights the interstellar matter in the nebul ...
... Galaxy’s largest star-forming regions. It is rich is clusters of newly formed O and B stars, harbouring a significant fraction of the most massive stars known in the Milky Way, including several O3 V stars and the LBV η Carinae. The picture on the left highlights the interstellar matter in the nebul ...
swire
... • Evolutionary relationship between galaxies and AGN, and the contribution of AGN accretion energy to the cosmic backgrounds ...
... • Evolutionary relationship between galaxies and AGN, and the contribution of AGN accretion energy to the cosmic backgrounds ...
The colour–magnitude relation of early
... redshift estimate. We used the 15 galaxies with spectroscopic redshifts in order to assess the uncertainty of the technique. The agreement between our estimates and the spectroscopic ones is generally good, with redshift errors of jDzj , 0:08. This uncertainty is propagated through to the rest-frame ...
... redshift estimate. We used the 15 galaxies with spectroscopic redshifts in order to assess the uncertainty of the technique. The agreement between our estimates and the spectroscopic ones is generally good, with redshift errors of jDzj , 0:08. This uncertainty is propagated through to the rest-frame ...
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.