AGN surveys to study galaxy evolution along cosmic times
... measuring the AGN and starburst contributions to their bolometric luminosities over a wide range of cosmological epochs, through their spectroscopic signatures. SPICA (Nakagawa et al. 2011) will be the next-generation, space infrared observatory, which, for the first time, will contain a large (3.2-m ...
... measuring the AGN and starburst contributions to their bolometric luminosities over a wide range of cosmological epochs, through their spectroscopic signatures. SPICA (Nakagawa et al. 2011) will be the next-generation, space infrared observatory, which, for the first time, will contain a large (3.2-m ...
Black Hole`` Systems.`
... accretion disk. The magnetic propeller also creates radial outflows of atomic nuclei (shown in indigo blue) and relativistic jets of electrons (shown in red) along the rotation axis. A bright blue-white ring forms where the MECO's rotating magnetic field sweeps the inner edge of the accretion disk, ...
... accretion disk. The magnetic propeller also creates radial outflows of atomic nuclei (shown in indigo blue) and relativistic jets of electrons (shown in red) along the rotation axis. A bright blue-white ring forms where the MECO's rotating magnetic field sweeps the inner edge of the accretion disk, ...
Rich Clusters of Galaxies
... Module 8: Clusters of Galaxies. • General properties, masses and mass-to-light ratios, galaxy interactions, dynamic stability, the inter-galactic medium, magnetic fields, x-ray emission, • Virial temperature, gravitational lensing, dark matter content, mass derived from x-ray observations. • Rich Cl ...
... Module 8: Clusters of Galaxies. • General properties, masses and mass-to-light ratios, galaxy interactions, dynamic stability, the inter-galactic medium, magnetic fields, x-ray emission, • Virial temperature, gravitational lensing, dark matter content, mass derived from x-ray observations. • Rich Cl ...
History of Star Formation in Local Galaxies
... What can we do to further constrain the rate of inflow of pristine gas and outflow of metal-enriched winds? Measure chemical abundances for individual red giant stars in the dSphs. Also, determine abundances for numerous elements that are created on different ...
... What can we do to further constrain the rate of inflow of pristine gas and outflow of metal-enriched winds? Measure chemical abundances for individual red giant stars in the dSphs. Also, determine abundances for numerous elements that are created on different ...
HEIC0007 Photo release: Stephan`s Quintet
... foreground galaxy, 35 million light years away, projected onto the more distant (270 million light years) compact group by chance. The other galaxies in the region appear to be intimately connected in space. A few hundred million years ago the galaxy NGC 7320C (just outside the left-hand edge of th ...
... foreground galaxy, 35 million light years away, projected onto the more distant (270 million light years) compact group by chance. The other galaxies in the region appear to be intimately connected in space. A few hundred million years ago the galaxy NGC 7320C (just outside the left-hand edge of th ...
G. Kacprzak "Galaxy-halo and gas connection 0.5 email
... Study Mg II quasar absorption line systems in order to understand the kinematics of halos probing distances out to 70 kpcs from the galaxies. Therefore the galaxies in our sample are selected by the known presence of Mg II absorption ...
... Study Mg II quasar absorption line systems in order to understand the kinematics of halos probing distances out to 70 kpcs from the galaxies. Therefore the galaxies in our sample are selected by the known presence of Mg II absorption ...
Polarimetric evidence of a white dwarf pulsar in
... tating neutron stars (1). The star AR Scorpii was recently discovered to be a 3.56 h close binary, containing a fast rotating (117 s) white dwarf, showing strong brightness variations across most of the electromagnetic spectrum (ultraviolet to radio), most strongly modulated on the 118.2 s beat (sy ...
... tating neutron stars (1). The star AR Scorpii was recently discovered to be a 3.56 h close binary, containing a fast rotating (117 s) white dwarf, showing strong brightness variations across most of the electromagnetic spectrum (ultraviolet to radio), most strongly modulated on the 118.2 s beat (sy ...
Carbon monoxide in clouds at low metallicity in the dwarf irregular
... Carbon monoxide (CO) is the primary tracer for interstellar clouds where stars form, but it has never been detected in galaxies in which the oxygen abundance relative to hydrogen is less than 20 per cent of that of the Sun, even though such ‘low-metallicity’ galaxies often form stars. This raises th ...
... Carbon monoxide (CO) is the primary tracer for interstellar clouds where stars form, but it has never been detected in galaxies in which the oxygen abundance relative to hydrogen is less than 20 per cent of that of the Sun, even though such ‘low-metallicity’ galaxies often form stars. This raises th ...
Stellar Population Modeling of Galaxies in Nearby Groups
... dwarf galaxies are the best places to study the processes of star formation. SFHs of the Local Group dwarf galaxies were studied in details from deep images, which were obtained with large ground-based telescopes and the Hubble Space Telescope (see, for example, Holtzman et al. (2000), Han et al. (1 ...
... dwarf galaxies are the best places to study the processes of star formation. SFHs of the Local Group dwarf galaxies were studied in details from deep images, which were obtained with large ground-based telescopes and the Hubble Space Telescope (see, for example, Holtzman et al. (2000), Han et al. (1 ...
Astronomy 401 Lecture 18 Galaxy Interactions Here we briefly
... Consider a small galaxy or cluster of mass M moving through an infinite collection of stars, gas clouds and dark matter, with constant mass density ρ. There are no collisions, and the masses of the individual objects are too small to deflect M , so it continues forward. However, the gravitational fo ...
... Consider a small galaxy or cluster of mass M moving through an infinite collection of stars, gas clouds and dark matter, with constant mass density ρ. There are no collisions, and the masses of the individual objects are too small to deflect M , so it continues forward. However, the gravitational fo ...
No Slide Title
... White Dwarfs Mass: similar to the Sun’s Diameter: about that of the Earth Hot (at least initially): 25,000 K; Dim (very small) Light they emit comes from heat (blackbody) Carbon and Oxygen; thin H/He surface layer White dwarf will cool over time (many billion of years) until it becomes a ...
... White Dwarfs Mass: similar to the Sun’s Diameter: about that of the Earth Hot (at least initially): 25,000 K; Dim (very small) Light they emit comes from heat (blackbody) Carbon and Oxygen; thin H/He surface layer White dwarf will cool over time (many billion of years) until it becomes a ...
Astrophysical explosions: from solar flares to cosmic gamma
... the system. These explosions include solar and stellar flares, eruptive phenomena in accretion discs, thermonuclear combustion on the surfaces of white dwarfs and neutron stars, violent magnetic reconnection in neutron stars, thermonuclear and gravitational collapse supernovae and cosmic gamma-ray bu ...
... the system. These explosions include solar and stellar flares, eruptive phenomena in accretion discs, thermonuclear combustion on the surfaces of white dwarfs and neutron stars, violent magnetic reconnection in neutron stars, thermonuclear and gravitational collapse supernovae and cosmic gamma-ray bu ...
Chandra News The Secret X-ray Lives of Planetary Nebulae
... far too energetic to originate from a blackbody-like white dwarf photosphere (see image and spectrum on back cover). For old white dwarfs in the field, such hard X-ray emission is typically attributed to coronal emission from a late-type, main-sequence companion (O’Dwyer et al. 2003) — and, in at le ...
... far too energetic to originate from a blackbody-like white dwarf photosphere (see image and spectrum on back cover). For old white dwarfs in the field, such hard X-ray emission is typically attributed to coronal emission from a late-type, main-sequence companion (O’Dwyer et al. 2003) — and, in at le ...
Gas and dust evolution in distant AGN
... Chemical version of the cosmic downsizing (anti-hierarchical growth) Evolution of the Mass-Metallicity relation: massive galaxies chemically evolve rapidly at high-z QSOs ...
... Chemical version of the cosmic downsizing (anti-hierarchical growth) Evolution of the Mass-Metallicity relation: massive galaxies chemically evolve rapidly at high-z QSOs ...
AAS Plenary Talk, May 2011 - National Radio Astronomy Observatory
... Microwave observations of edge-on protoplanetary disks (Melis) First results from a 1.3cm EVLA survey of massive protostellar objects (Brogan) Unveiling the sources of heating in the vicinity of the Orion-KL hot core as traced by High-J rotational transitions of NH3 (Goddi) EVLA continuum ob ...
... Microwave observations of edge-on protoplanetary disks (Melis) First results from a 1.3cm EVLA survey of massive protostellar objects (Brogan) Unveiling the sources of heating in the vicinity of the Orion-KL hot core as traced by High-J rotational transitions of NH3 (Goddi) EVLA continuum ob ...
–1– 28. HIGH-MASS STAR FORMATION: THEORY 28.1. The Effects
... s−1 considered by Keto, this restricts the accretion rate to ṁ∗ . 3 × 10−5 M¯ yr−1 , smaller than the values he considers. (One can show that when one generalizes the Bondi accretion model to approximately include the self gravity of the gas, the accretion rate is indeed about c 3 /G.) Bonnell and ...
... s−1 considered by Keto, this restricts the accretion rate to ṁ∗ . 3 × 10−5 M¯ yr−1 , smaller than the values he considers. (One can show that when one generalizes the Bondi accretion model to approximately include the self gravity of the gas, the accretion rate is indeed about c 3 /G.) Bonnell and ...
Media Alert A new spin on star-forming galaxies
... A new spin on star-forming galaxies Australian researchers have discovered why some galaxies are “clumpy” rather than spiral in shape—and it appears low spin is to blame. The finding challenges an earlier theory that high levels of gas cause clumpy galaxies and sheds light on the conditions that bro ...
... A new spin on star-forming galaxies Australian researchers have discovered why some galaxies are “clumpy” rather than spiral in shape—and it appears low spin is to blame. The finding challenges an earlier theory that high levels of gas cause clumpy galaxies and sheds light on the conditions that bro ...
Starburst Galaxies Under the Microscope: High
... which a large area becomes globally unstable, after which individual star-forming complexes form stochastically. There is thus no evidence for propagating star formation in this region. However, a global trigger is still needed. Presumably this may be found in the accumulation of gas in the barred p ...
... which a large area becomes globally unstable, after which individual star-forming complexes form stochastically. There is thus no evidence for propagating star formation in this region. However, a global trigger is still needed. Presumably this may be found in the accumulation of gas in the barred p ...
An absence of ex-companion stars in the type Ia supernova remnant
... nearest galaxy to our own, the Large Magellanic Cloud (LMC). We consider the case of SNR 0509267.5, which was an type Ia supernova (of the SN 1991T class) 400 6 50 years ago19,20,25,26. SNR 0509267.5 has excellent images in the public domain that were taken by the Hubble Space Telescope (HST). All o ...
... nearest galaxy to our own, the Large Magellanic Cloud (LMC). We consider the case of SNR 0509267.5, which was an type Ia supernova (of the SN 1991T class) 400 6 50 years ago19,20,25,26. SNR 0509267.5 has excellent images in the public domain that were taken by the Hubble Space Telescope (HST). All o ...
The role of black holes in galaxy formation and evolution
... The energy that jets pump into cavities in a sound crossing time matches the heat needed to keep the gas in thermal equilibrium if this energy equals to pgasVcav with a scatter of a factor of four39 (Fig. 5a). This proportionality, which extends over four orders of magnitude, suggests a self-regulat ...
... The energy that jets pump into cavities in a sound crossing time matches the heat needed to keep the gas in thermal equilibrium if this energy equals to pgasVcav with a scatter of a factor of four39 (Fig. 5a). This proportionality, which extends over four orders of magnitude, suggests a self-regulat ...
v1 - ESO
... the faint limit, at least down to the Horizontal Branch (V,I,K ∼ 32, in Virgo) in regions with a range of stellar density and stellar luminosity. These CMDs can then be used to determine accurate star formation histories and also to give targets for follow up spectroscopy to directly measure metalli ...
... the faint limit, at least down to the Horizontal Branch (V,I,K ∼ 32, in Virgo) in regions with a range of stellar density and stellar luminosity. These CMDs can then be used to determine accurate star formation histories and also to give targets for follow up spectroscopy to directly measure metalli ...
Additional Cosmology Images
... A cauldron of stars at the Galaxy's center. This dazzling infrared image from NASA's Spitzer Space Telescope shows hundreds of thousands of stars crowded into the swirling core of our spiral Milky Way. In visible-light pictures, this region cannot be seen at all because dust lying between Earth and ...
... A cauldron of stars at the Galaxy's center. This dazzling infrared image from NASA's Spitzer Space Telescope shows hundreds of thousands of stars crowded into the swirling core of our spiral Milky Way. In visible-light pictures, this region cannot be seen at all because dust lying between Earth and ...
FRA2015_mmMM_Junzhi_Wang
... • Masers in galaxies had been found since 1970s • Some of them are similar to that in the Milky Way sources, and are just the collection of such maser emissions • Another type, the so-called mega-masers, with the isotropic luminosity greater than 1 million times than typical Galactic masers, and are ...
... • Masers in galaxies had been found since 1970s • Some of them are similar to that in the Milky Way sources, and are just the collection of such maser emissions • Another type, the so-called mega-masers, with the isotropic luminosity greater than 1 million times than typical Galactic masers, and are ...
The role of black holes in galaxy formation and evolution
... accretion rates to provide the energy that is needed to maintain it at constant temperature46–48, either through a continuous series of minor events44,45,49, or through episodic quasar activity50,51. The strongest evidence for this loop cycle is in galaxy clusters. Its action reduces considerably th ...
... accretion rates to provide the energy that is needed to maintain it at constant temperature46–48, either through a continuous series of minor events44,45,49, or through episodic quasar activity50,51. The strongest evidence for this loop cycle is in galaxy clusters. Its action reduces considerably th ...
Astrophysical X-ray source
Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.