Abstract Book - Documentation Index
... From Santiago (1978), to Mérida (Venezuela, 1981), Buenos Aires (1983), Rio de Janeiro (1984), Mérida (México, 1986), Gramado (1989), Viña del Mar (1992), Montevideo (1995), Tonantzintla (1998), Córdoba (2001), Pucón (2005), Isla Margarita (2007), and Morélia (2010), Latin American Regional I ...
... From Santiago (1978), to Mérida (Venezuela, 1981), Buenos Aires (1983), Rio de Janeiro (1984), Mérida (México, 1986), Gramado (1989), Viña del Mar (1992), Montevideo (1995), Tonantzintla (1998), Córdoba (2001), Pucón (2005), Isla Margarita (2007), and Morélia (2010), Latin American Regional I ...
The rate of supernovae at redshift 0.1-1.0
... Magnelli et al. (2009, 2011) find that the star formation from these infrared bright galaxies dominate the global star formation at redshift 0.7 and higher. In these galaxies the SN explosions can be completely obscured by the large amounts of dust within the nuclear regions. For low to moderate amo ...
... Magnelli et al. (2009, 2011) find that the star formation from these infrared bright galaxies dominate the global star formation at redshift 0.7 and higher. In these galaxies the SN explosions can be completely obscured by the large amounts of dust within the nuclear regions. For low to moderate amo ...
GAS ACCRETION AND COUNTER-ROTATION IN DISK GALAXIES
... wavelengths at SW, i.e. they are redshifted (blueshifted). The opposite happens at NE. This redshift (blueshift) of lines is due to the Doppler eect, for which receding (approaching) sources emit/absorb lines at redder (bluer) wavelengths with respect to the rest wavelength values of the lines. The ...
... wavelengths at SW, i.e. they are redshifted (blueshifted). The opposite happens at NE. This redshift (blueshift) of lines is due to the Doppler eect, for which receding (approaching) sources emit/absorb lines at redder (bluer) wavelengths with respect to the rest wavelength values of the lines. The ...
Probing Galaxy Evolution with Environment: Ram Pressure Stripping and Major Mergers in Group Environments
... rather than ≈ 2, as would be expected if interactions between subhalos had no effect on the merger rate. The right panel examines how the increased merger rate in hosts with multiple subhalos, due to interactions between subhalos, affects the frequency of merger remnants among halos with grouplike V ...
... rather than ≈ 2, as would be expected if interactions between subhalos had no effect on the merger rate. The right panel examines how the increased merger rate in hosts with multiple subhalos, due to interactions between subhalos, affects the frequency of merger remnants among halos with grouplike V ...
Co-Evolution of Galactic Nuclei and Globular Cluster Systems
... to the Galaxy, where the most detailed observations are available, in §3. We extend the model to the M87 system in §4 and find that, in order to reproduce the observed distribution of globular clusters, we must account for the evolution of the galaxy structure over cosmic time, in a fashion that mat ...
... to the Galaxy, where the most detailed observations are available, in §3. We extend the model to the M87 system in §4 and find that, in order to reproduce the observed distribution of globular clusters, we must account for the evolution of the galaxy structure over cosmic time, in a fashion that mat ...
Smooth (er) Stellar Mass Maps in CANDELS: Constraints on the
... at the observed epoch to double their mass. Figure 1 illustrates that this selection effectively removes systems that already formed the bulk of their stars and lie below the MS, although we note that our results do not sensitively depend on the precise value of the SF R/M limit. We excluded 17 obje ...
... at the observed epoch to double their mass. Figure 1 illustrates that this selection effectively removes systems that already formed the bulk of their stars and lie below the MS, although we note that our results do not sensitively depend on the precise value of the SF R/M limit. We excluded 17 obje ...
Simulations of Dwarf Galaxy Formation
... The final objects have halo masses between 2.3 × 108 and 1.1 × 109 M⊙ , mean velocity dispersions between 6.5 and 9.7 kms−1 , stellar masses ranging from 5 × 105 to 1.2 × 107 M⊙ , median metallicities between [Fe/H] = −1.8 and −1.1, and halflight radii of the order of 200 to 300 pc, all comparable w ...
... The final objects have halo masses between 2.3 × 108 and 1.1 × 109 M⊙ , mean velocity dispersions between 6.5 and 9.7 kms−1 , stellar masses ranging from 5 × 105 to 1.2 × 107 M⊙ , median metallicities between [Fe/H] = −1.8 and −1.1, and halflight radii of the order of 200 to 300 pc, all comparable w ...
Study of the Far Infrared Emission of Nearby Spiral Galaxies
... At present, it is common knowledge that the farthest celestial phenomenon whose light can be detected is the Cosmic Microwave Background (CMB). This is the testimony to ages approximately 13.79 billion years ago (as found by Planck Collaboration, 2013b) roughly 378,000 years after the Big Bang (at r ...
... At present, it is common knowledge that the farthest celestial phenomenon whose light can be detected is the Cosmic Microwave Background (CMB). This is the testimony to ages approximately 13.79 billion years ago (as found by Planck Collaboration, 2013b) roughly 378,000 years after the Big Bang (at r ...
Probing Dark Energy with Lensing Magnification in Photometric
... shears (cosmic shear) is well established as an important cosmological probe [e.g. 13]. Current and next generation surveys targeted at measuring dark energy properties via cosmic shear will rely on ‘photometric redshifts’ (photoz’s) that measure a galaxy spectrum in a few broadband optical filters. ...
... shears (cosmic shear) is well established as an important cosmological probe [e.g. 13]. Current and next generation surveys targeted at measuring dark energy properties via cosmic shear will rely on ‘photometric redshifts’ (photoz’s) that measure a galaxy spectrum in a few broadband optical filters. ...
Early star formation and the evolution of the stellar initial mass
... (6) Standard hot-big-bang cosmology suggests that most of the baryonic matter in the Universe is in a dark form, and one possibility could be the dark remnants of early generations of massive stars. The claimed detection via microlensing of stellar-mass ‘machos’ in the halo of our Galaxy has led to ...
... (6) Standard hot-big-bang cosmology suggests that most of the baryonic matter in the Universe is in a dark form, and one possibility could be the dark remnants of early generations of massive stars. The claimed detection via microlensing of stellar-mass ‘machos’ in the halo of our Galaxy has led to ...
The origin of dust in galaxies revisited: the mechanism
... and may change from the gas phase to the solid phase. Note that, unlike the sticking growth of grains well studied in protoplanetary disks, this accretion growth causes an increase in dust mass. This type of growth is favored to explain the observed depletions of some elements in the gas phase of th ...
... and may change from the gas phase to the solid phase. Note that, unlike the sticking growth of grains well studied in protoplanetary disks, this accretion growth causes an increase in dust mass. This type of growth is favored to explain the observed depletions of some elements in the gas phase of th ...
Infall times for Milky Way satellites from their present
... Way satellite galaxies. Assuming that the Milky Way’s assembly can be modelled by VL2, we show that the infall times of some satellites are well constrained given only their Galactocentric positions and line-of-sight velocities. The constraints sharpen for satellites with proper motion measurements. ...
... Way satellite galaxies. Assuming that the Milky Way’s assembly can be modelled by VL2, we show that the infall times of some satellites are well constrained given only their Galactocentric positions and line-of-sight velocities. The constraints sharpen for satellites with proper motion measurements. ...
Evolutionary Population Synthesis models
... 5. Intermediate (0.5-2 Gyr) : Balmer and CaII H and K line ratios 6. Old population (>2 Gyr): 4000 Ang break and other Lick indices ...
... 5. Intermediate (0.5-2 Gyr) : Balmer and CaII H and K line ratios 6. Old population (>2 Gyr): 4000 Ang break and other Lick indices ...
Models of galaxy collisions in Stephan`s Quintet and other
... with an initial disk surrounded by a few hundred massless test particles. The models were very simplified by modern standards (considering only the inverse-square force of gravity and ignoring anything else, for example self-gravity), however, they convincingly illustrated the formation of narrow el ...
... with an initial disk surrounded by a few hundred massless test particles. The models were very simplified by modern standards (considering only the inverse-square force of gravity and ignoring anything else, for example self-gravity), however, they convincingly illustrated the formation of narrow el ...
Morphological evolution of galaxies over the last 8 billion years
... galaxies form by merging of smaller ones, but also bulge dominated galaxies form from disks, either through mergers or by dynamical instabilities. Therefore, at the same time, both the number density of the most massive objects and the fraction of bulge-dominated galaxies are expected to decrease at ...
... galaxies form by merging of smaller ones, but also bulge dominated galaxies form from disks, either through mergers or by dynamical instabilities. Therefore, at the same time, both the number density of the most massive objects and the fraction of bulge-dominated galaxies are expected to decrease at ...
Globular Clusters as Fossils of Galaxy Formation
... of these clusters might provide some information about the chronology of the galaxy building process. However, the cluster ages themselves do not necessarily directly record the merger history of the halo, since the halo clusters could have been formed in satellite systems long before these satellit ...
... of these clusters might provide some information about the chronology of the galaxy building process. However, the cluster ages themselves do not necessarily directly record the merger history of the halo, since the halo clusters could have been formed in satellite systems long before these satellit ...
Super Star Clusters in Blue Compact Galaxies
... Paper I. In this paper, a comprehensive multiwavelength study of the luminous infrared galaxy (LIRG) IRAS 19115-2124, dubbed the Bird, is presented. The system is a rare example of a triple galaxy merger. It is a quite obscured system at optical wavebands, but reveals numerous star cluster knots in ...
... Paper I. In this paper, a comprehensive multiwavelength study of the luminous infrared galaxy (LIRG) IRAS 19115-2124, dubbed the Bird, is presented. The system is a rare example of a triple galaxy merger. It is a quite obscured system at optical wavebands, but reveals numerous star cluster knots in ...
CH15.Ast1001.F13.EDS
... The highly redshifted spectra of quasars indicate large distances. From brightness and distance, we find that luminosities of some quasars are >1012LSun! Variability shows that all this energy comes from a region smaller than the solar system. Copyright © 2012 Pearson Education, Inc. ...
... The highly redshifted spectra of quasars indicate large distances. From brightness and distance, we find that luminosities of some quasars are >1012LSun! Variability shows that all this energy comes from a region smaller than the solar system. Copyright © 2012 Pearson Education, Inc. ...
Galaxy And Mass Assembly (GAMA): Gas Fueling of Spiral Galaxies
... et al. 2011). For cosmological DMH detailed thermodynamic considerations of this process find a transition mass between these two modes, i.e., where the free-fall timescale equals the cooling timescale at the virial radius of ∼1011–1012 Me (Kereš et al. 2005; Dekel & Birnboim 2006).20 As such, the ac ...
... et al. 2011). For cosmological DMH detailed thermodynamic considerations of this process find a transition mass between these two modes, i.e., where the free-fall timescale equals the cooling timescale at the virial radius of ∼1011–1012 Me (Kereš et al. 2005; Dekel & Birnboim 2006).20 As such, the ac ...
Cold galaxies at low and high z
... the IRAS all-sky survey of infrared point-sources: white: star-forming regions, blue: red giant stars, green: galaxies Nov 27th 2008 ...
... the IRAS all-sky survey of infrared point-sources: white: star-forming regions, blue: red giant stars, green: galaxies Nov 27th 2008 ...
Galaxies through Cosmic Time: The Role of Molecular and Atomic Gas
... has significantly advanced our understanding of the history of gas consumption by star formation in galaxies, revealing the high redshift universe to be similar in many ways to what we know locally. Specifically, molecular gas studies suggest that at both high and low redshift, the molecular gas reser ...
... has significantly advanced our understanding of the history of gas consumption by star formation in galaxies, revealing the high redshift universe to be similar in many ways to what we know locally. Specifically, molecular gas studies suggest that at both high and low redshift, the molecular gas reser ...
スライド 1 - Subaru Telescope
... of Supernova Type Ia. • We found new spectral luminosity indicators for independent checks of the decline rate. The equivalent width of “CaII3945” line at the “max” epoch is found to be positively correlated with ⊿m15. The equivalent widths of “SiII4000” lines at the “post-max” epoch also show posit ...
... of Supernova Type Ia. • We found new spectral luminosity indicators for independent checks of the decline rate. The equivalent width of “CaII3945” line at the “max” epoch is found to be positively correlated with ⊿m15. The equivalent widths of “SiII4000” lines at the “post-max” epoch also show posit ...
The Colors of the Universe - Naples Free-Net
... diameter of 11 light years and is expanding at a rate of about 3.4 million miles per hour. At the center of the nebula lies the Crab Pulsar, a neutron star (or spinning ball of neutrons) which is only 28–30 km across, and has a spin rate of 30.2 times per second. The nebula was the first astronomica ...
... diameter of 11 light years and is expanding at a rate of about 3.4 million miles per hour. At the center of the nebula lies the Crab Pulsar, a neutron star (or spinning ball of neutrons) which is only 28–30 km across, and has a spin rate of 30.2 times per second. The nebula was the first astronomica ...
Seyfert galaxy
Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei (very luminous, distant and bright sources of electromagnetic radiation) with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.Seyfert galaxies account for about 10% of all galaxies and are some of the most intensely studied objects in astronomy, as they are thought to be powered by the same phenomena that occur in quasars, although they are closer and less luminous than quasars. These galaxies have supermassive black holes at their centers which are surrounded by accretion discs of in-falling material. The accretion discs are believed to be the source of the observed ultraviolet radiation. Ultraviolet emission and absorption lines provide the best diagnostics for the composition of the surrounding material.Seen in visible light, most Seyfert galaxies look like normal spiral galaxies, but when studied under other wavelengths, it becomes clear that the luminosity of their cores is of comparable intensity to the luminosity of whole galaxies the size of the Milky Way.Seyfert galaxies are named after Carl Seyfert, who first described this class in 1943.