Where is the angular momentum in elliptical galaxies?
... Ages of the Formation Epoch(s) How to get ages of GC populations? Optical colors good for finding metallicity peaks, but bad for ages because of age-metallicity degeneracy – older age and higher metal content have same effect on optical colors (colors can be red because of old age or high metal con ...
... Ages of the Formation Epoch(s) How to get ages of GC populations? Optical colors good for finding metallicity peaks, but bad for ages because of age-metallicity degeneracy – older age and higher metal content have same effect on optical colors (colors can be red because of old age or high metal con ...
The 2008 RBSE Journal - National Optical Astronomy Observatory
... A Double Radio Source Associated with a Galactic Nucleus (DRAGN) is a radio source that is produced by jets produced by active galactic nucleus that is not in the Milky Way. This happens when an accretion disk forms around a black hole and spins, converts gravitational and rotational energy into exc ...
... A Double Radio Source Associated with a Galactic Nucleus (DRAGN) is a radio source that is produced by jets produced by active galactic nucleus that is not in the Milky Way. This happens when an accretion disk forms around a black hole and spins, converts gravitational and rotational energy into exc ...
Galactic Winds Sylvain Veilleux
... theoretical predictions to discuss critically the properties of GWs in the local and distant universe, and to evaluate the importance of these winds for the formation and evolution of galaxies and the IGM. We focus on material published within the past 15 years. Our discussion centers on three funda ...
... theoretical predictions to discuss critically the properties of GWs in the local and distant universe, and to evaluate the importance of these winds for the formation and evolution of galaxies and the IGM. We focus on material published within the past 15 years. Our discussion centers on three funda ...
structure and evolution of white dwarfs and their
... Theoretical and observational study of stellar evolution has placed white dwarfs as one possible end point of the process. In general terms, all stars with masses below about eight times that of the Sun will pass through one or more red giant phases before losing most of their original mass to form ...
... Theoretical and observational study of stellar evolution has placed white dwarfs as one possible end point of the process. In general terms, all stars with masses below about eight times that of the Sun will pass through one or more red giant phases before losing most of their original mass to form ...
PS1-10jh: The Disruption of a Main-Sequence Star of Near
... fan intercepts a significant fraction of the light is incorrect. As noted by Kochanek (1994), the width of the stream of unbound material is still controlled by the stream’s self-gravity in the transverse direction, restricting its width to only be a fraction of the star’s original pericenter distan ...
... fan intercepts a significant fraction of the light is incorrect. As noted by Kochanek (1994), the width of the stream of unbound material is still controlled by the stream’s self-gravity in the transverse direction, restricting its width to only be a fraction of the star’s original pericenter distan ...
Carbon-enhanced metal-poor stars in dwarf galaxies
... in the Galactic halo. Moreover, we can see that the frequency of CEMP-no stars among these “hyper-iron-poor stars” is extremely high: 8 out of 9 stars at [Fe/H]≤ −4.5 are CEMP-no stars. These objects have peculiar chemical abundance patterns consistent with the yields predicted for primordial faint ...
... in the Galactic halo. Moreover, we can see that the frequency of CEMP-no stars among these “hyper-iron-poor stars” is extremely high: 8 out of 9 stars at [Fe/H]≤ −4.5 are CEMP-no stars. These objects have peculiar chemical abundance patterns consistent with the yields predicted for primordial faint ...
8-4.9 - S2TEM Centers SC
... light year is equal to the distance light travel in one year. NOTE TO TEACHER: Students may come with a misconception that the Milky Way galaxy is in the solar system because they may have seen the band of stars in the night sky. The relationship between objects within the solar system and those out ...
... light year is equal to the distance light travel in one year. NOTE TO TEACHER: Students may come with a misconception that the Milky Way galaxy is in the solar system because they may have seen the band of stars in the night sky. The relationship between objects within the solar system and those out ...
Distance
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
Слайд 1 - Tuorla Observatory
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
... parameters are more accurate than for single star • (b) All stars are of the same age. Star clusters are the only objects that enable direct age estimate, study of the galactic evolution and the star-formation history • (c) All stars have nearly the same chemical composition, and the differences in ...
Spiral arm structures revealed in the M31 galaxy
... Striking regularities are found in the northwestern arm of the M31 galaxy. Star complexes located in this arm are spaced 1.2 kpc apart and have similar sizes of about 0.6 kpc. This pattern is observed within the arm region where Beck et al. (1989) detected a strong regular magnetic field with the wa ...
... Striking regularities are found in the northwestern arm of the M31 galaxy. Star complexes located in this arm are spaced 1.2 kpc apart and have similar sizes of about 0.6 kpc. This pattern is observed within the arm region where Beck et al. (1989) detected a strong regular magnetic field with the wa ...
The Spectra ot Novae
... of absorption systems in the early post-maximum stages. A secondary minimum in the very early decline may be accompanied by strong emergence of the diffuse enhanced spectrum which will weaken again as the star recovers. Farther down the decline, a fading of the star may be correlated with weakening ...
... of absorption systems in the early post-maximum stages. A secondary minimum in the very early decline may be accompanied by strong emergence of the diffuse enhanced spectrum which will weaken again as the star recovers. Farther down the decline, a fading of the star may be correlated with weakening ...
ppt - NRAO
... E.g.: Taurus (of course), Orion is much larger than the Orion Nebula, It is not clear if all of Perseus is at the same distance (NGC1333 vs. IC 348), Ophiuchus streamers, etc.. (Note that these regions tend to be heavily obscured, so optical experiments are unlikely to improve significantly the situ ...
... E.g.: Taurus (of course), Orion is much larger than the Orion Nebula, It is not clear if all of Perseus is at the same distance (NGC1333 vs. IC 348), Ophiuchus streamers, etc.. (Note that these regions tend to be heavily obscured, so optical experiments are unlikely to improve significantly the situ ...
Chapter 1-3
... binaries). In particular for so called double-lined eclipsing binaries, in which the spectral lines of both stars vary, it is possible to accurately measure both the masses and radii (with 1–2 % accuracy in some cases) by fitting the radial-velocity curves and the eclipse lightcurve. Together with ...
... binaries). In particular for so called double-lined eclipsing binaries, in which the spectral lines of both stars vary, it is possible to accurately measure both the masses and radii (with 1–2 % accuracy in some cases) by fitting the radial-velocity curves and the eclipse lightcurve. Together with ...
Stages of star formation (the classical view)
... For a low-mass star tKH>> tff (for a 1 Msol star, tKH = 3x107 yr) The protostar becomes a pre-main sequence star (T Tauri star). However, for a high-mass star tKH<< tff (for a 50 Msol star, tKH= 3x104 yr) The star has not enough time to accrete more than ~10 Msol before starting to burn hydrogen, io ...
... For a low-mass star tKH>> tff (for a 1 Msol star, tKH = 3x107 yr) The protostar becomes a pre-main sequence star (T Tauri star). However, for a high-mass star tKH<< tff (for a 50 Msol star, tKH= 3x104 yr) The star has not enough time to accrete more than ~10 Msol before starting to burn hydrogen, io ...
WORD - Astrophysics
... for the exploration of our own Solar System, where planets and their moons will be studied with resolution comparable only to those of space missions. An E-ELT will be capable of detecting giant planets (Jupiter to Neptune-like) orbiting at separations smaller than 1 AU around thousands of stars up ...
... for the exploration of our own Solar System, where planets and their moons will be studied with resolution comparable only to those of space missions. An E-ELT will be capable of detecting giant planets (Jupiter to Neptune-like) orbiting at separations smaller than 1 AU around thousands of stars up ...
ASTRONOMY AND ASTROPHYSICS Elemental abundances of
... damped Lyα systems and the Lyα-forest. We selected quasars with no strong contamination since we are predominantly interested in the emission line flux and profiles. The quasars had to be brighter than 20 mag to achieve a sufficient S/N ratio of at least 20 for the continuum for reasonable integrati ...
... damped Lyα systems and the Lyα-forest. We selected quasars with no strong contamination since we are predominantly interested in the emission line flux and profiles. The quasars had to be brighter than 20 mag to achieve a sufficient S/N ratio of at least 20 for the continuum for reasonable integrati ...
Modelling the sulphur chemistry evolution in Orion KL
... Aims. Our aim is to investigate the processes that dominate the sulphur chemistry in Orion KL and to determine how physical and chemical parameters, such as the final mass of the star and the initial elemental abundances, influence the evolution of the hot core and of the surrounding outflows and sh ...
... Aims. Our aim is to investigate the processes that dominate the sulphur chemistry in Orion KL and to determine how physical and chemical parameters, such as the final mass of the star and the initial elemental abundances, influence the evolution of the hot core and of the surrounding outflows and sh ...
The PAH emission spectra of Large Magellanic Cloud H II regions
... spectra, the spline points for this continuum were located at ∼5.8 µm, in the 9–10 µm region, and at the blue base of the [S iv] 10.5 µm line. The wavelength coverage of ISOPHOT (ending at 11.6 µm) hampers the determination of the continuum redwards of the [S iv] 10.5 µm line. Without continuum poin ...
... spectra, the spline points for this continuum were located at ∼5.8 µm, in the 9–10 µm region, and at the blue base of the [S iv] 10.5 µm line. The wavelength coverage of ISOPHOT (ending at 11.6 µm) hampers the determination of the continuum redwards of the [S iv] 10.5 µm line. Without continuum poin ...
A subaru/suprime-cam wide
... centre) of GCs around M87 with Subaru/Suprime-Cam Secure selection of GC candidates with an extended source cut and a colour selection on the B-V vs. V-I diagram. Analyzed the Suprime-Cam data on the control fields through the BVI bands, which enable to select contaminating objects with the identica ...
... centre) of GCs around M87 with Subaru/Suprime-Cam Secure selection of GC candidates with an extended source cut and a colour selection on the B-V vs. V-I diagram. Analyzed the Suprime-Cam data on the control fields through the BVI bands, which enable to select contaminating objects with the identica ...
CONNECTING ANGULAR MOMENTUM AND GALACTIC DYNAMICS
... the galaxy spins with their surrounding filaments, using the Horizon-AGN simulation (Dubois et al. 2014). They find that halos experiencing major mergers often lower the spin, while in general minor mergers can increase the amount of angular momentum. If a halo does not undergo any mergers but only ...
... the galaxy spins with their surrounding filaments, using the Horizon-AGN simulation (Dubois et al. 2014). They find that halos experiencing major mergers often lower the spin, while in general minor mergers can increase the amount of angular momentum. If a halo does not undergo any mergers but only ...
Stellar populations in the nuclear regions of nearby radio galaxies
... We obtained flux standards (HZ 44 and G1912 B2B) for the four nights and gratings, except in 1998 February 20, when we were unable to acquire the red spectrum of the corresponding standard because of a technical failure. One calibration lamp CuAr+CuNe exposure per spectral region and telescope posit ...
... We obtained flux standards (HZ 44 and G1912 B2B) for the four nights and gratings, except in 1998 February 20, when we were unable to acquire the red spectrum of the corresponding standard because of a technical failure. One calibration lamp CuAr+CuNe exposure per spectral region and telescope posit ...
Document
... their host galaxies in less than 1Gyr?? – The universe was ~20 tedd old – Initial assembly from seed BH at z>>10 – Little or no feedback to stop BH/galaxy growth ...
... their host galaxies in less than 1Gyr?? – The universe was ~20 tedd old – Initial assembly from seed BH at z>>10 – Little or no feedback to stop BH/galaxy growth ...
Objective Classification of Galaxy Spectra using the Information Bottleneck Method
... results of any objective classi cation algorithm, we must relate the derived classes to the physical and observable galaxy ...
... results of any objective classi cation algorithm, we must relate the derived classes to the physical and observable galaxy ...
UvA-DARE (Digital Academic Repository)
... The intermediate regime: Growth of dust grains is most difficult to understand in the regime where grains are too large to grow by coagulation (Blum & Wurm 2008), but too small to grow by gravitational interaction. In addition, should particles reach one meter in size, they would feel a strong headw ...
... The intermediate regime: Growth of dust grains is most difficult to understand in the regime where grains are too large to grow by coagulation (Blum & Wurm 2008), but too small to grow by gravitational interaction. In addition, should particles reach one meter in size, they would feel a strong headw ...
The drop in the cosmic star formation rate below redshift 2 is caused
... that our results are insensitive to the choice for β as long as it is chosen to be large (see Booth & Schaye 2009). A fraction of 1.5 per cent of the rest-mass energy of the accreted gas is injected into the surrounding medium in the form of heat, by increasing the temperature of at least one neighb ...
... that our results are insensitive to the choice for β as long as it is chosen to be large (see Booth & Schaye 2009). A fraction of 1.5 per cent of the rest-mass energy of the accreted gas is injected into the surrounding medium in the form of heat, by increasing the temperature of at least one neighb ...