ULTRA-COMPACT HII REGIONS AND MASSIVE STAR FORMATION
... (1999), Gregersen et al. (2000), and Gregersen & Evans (2000) have identified over a dozen PSC candidates with infall signatures. Claims for other PSCs have been based on indirect arguments such as high densities, Lbol too low to be consistent with an accreting protostar, low temperatures (indicatin ...
... (1999), Gregersen et al. (2000), and Gregersen & Evans (2000) have identified over a dozen PSC candidates with infall signatures. Claims for other PSCs have been based on indirect arguments such as high densities, Lbol too low to be consistent with an accreting protostar, low temperatures (indicatin ...
A catalogue of the Chandra Deep Field South with multi
... Fig. 1. COMBO-17 filter set: Total system efficiencies in the COMBO-17 bands. They include two telescope mirrors, the WFI instrument, CCD detector and an average La Silla atmosphere. Photometric calibrations of such datasets are best achieved with spectrophotometric standards inside the target field ...
... Fig. 1. COMBO-17 filter set: Total system efficiencies in the COMBO-17 bands. They include two telescope mirrors, the WFI instrument, CCD detector and an average La Silla atmosphere. Photometric calibrations of such datasets are best achieved with spectrophotometric standards inside the target field ...
Distance to VY Canis Majoris with VERA
... (Kovalev et al. 2007). Because these offsets are constant at all epochs, it dose not affect the parallax measurements. Also, when the reference source is not a point source, the positional errors of the target source could occur due to the structure and its variation of the reference source. However ...
... (Kovalev et al. 2007). Because these offsets are constant at all epochs, it dose not affect the parallax measurements. Also, when the reference source is not a point source, the positional errors of the target source could occur due to the structure and its variation of the reference source. However ...
Th`ese d`astrophysique Chemodynamical Simulations of Evolution
... Giant molecular cloud Initial mass function Interstellar medium Large Magellanic Cloud Molecular cloud Polycyclic aromatic hydrocarbon Spectral emission distribution Star formation Star formation history Star formation rate Small Magellanic Cloud Smooth particle hydrodynamic The HI nearby galaxy sur ...
... Giant molecular cloud Initial mass function Interstellar medium Large Magellanic Cloud Molecular cloud Polycyclic aromatic hydrocarbon Spectral emission distribution Star formation Star formation history Star formation rate Small Magellanic Cloud Smooth particle hydrodynamic The HI nearby galaxy sur ...
Constraints on the physical properties and chemical evolution of star
... constrain the physical properties and chemical enrichment of the gas in galaxies at all cosmic epochs. This is important, because galaxies are being detected at always higher redshift and upcoming observations with large telescopes, such as the James Webb Space Telescope, will gather high-quality sp ...
... constrain the physical properties and chemical enrichment of the gas in galaxies at all cosmic epochs. This is important, because galaxies are being detected at always higher redshift and upcoming observations with large telescopes, such as the James Webb Space Telescope, will gather high-quality sp ...
Observations, Modeling and Theory of Debris Disks
... concentrated on disks previously identified at other wavelengths, a few statistical surveys have been carried out, e.g., the JCMT survey by Najita and Williams (2005) and the CSO/IRAM survey of Roccatagliata et al. (2009). Najita and Williams (2005) detected 3 sources out of 13 nearby solar-mass sta ...
... concentrated on disks previously identified at other wavelengths, a few statistical surveys have been carried out, e.g., the JCMT survey by Najita and Williams (2005) and the CSO/IRAM survey of Roccatagliata et al. (2009). Najita and Williams (2005) detected 3 sources out of 13 nearby solar-mass sta ...
Dawes Review. The tidal downsizing hypothesis of planet formation
... not accrete more gas in this picture. They may actually loose most of their primordial gas if tidal forces from the host stars are stronger than self-gravity of the clumps. However, before the clumps are destroyed, solid planetary cores are formed inside them when grains grow and sediment to the cen ...
... not accrete more gas in this picture. They may actually loose most of their primordial gas if tidal forces from the host stars are stronger than self-gravity of the clumps. However, before the clumps are destroyed, solid planetary cores are formed inside them when grains grow and sediment to the cen ...
Observations, Modeling and Theory of Debris Disks
... concentrated on disks previously identified at other wavelengths, a few statistical surveys have been carried out, e.g., the JCMT survey by Najita and Williams (2005) and the CSO/IRAM survey of Roccatagliata et al. (2009). Najita and Williams (2005) detected 3 sources out of 13 nearby solar-mass sta ...
... concentrated on disks previously identified at other wavelengths, a few statistical surveys have been carried out, e.g., the JCMT survey by Najita and Williams (2005) and the CSO/IRAM survey of Roccatagliata et al. (2009). Najita and Williams (2005) detected 3 sources out of 13 nearby solar-mass sta ...
Astrophysics for Physicists.
... Sciences as well as our Joint Astronomy and Astrophysics Programme. I must have taught this course to more than half a dozen batches. Over the years, several excellent textbooks suitable for use in one-semester courses on particle physics and solid state physics have been written. The situation with ...
... Sciences as well as our Joint Astronomy and Astrophysics Programme. I must have taught this course to more than half a dozen batches. Over the years, several excellent textbooks suitable for use in one-semester courses on particle physics and solid state physics have been written. The situation with ...
H i AND CO IN BLUE COMPACT DWARF GALAXIES: HARO 2 AND
... Blue compact dwarf (BCD) galaxies are dwarf irregular systems that are currently experiencing a burst of star formation. Their appearance is dominated by the starburst, which appears compact and blue, hence their name. Their spectra show all the characteristics of H ii regions, which has led many BC ...
... Blue compact dwarf (BCD) galaxies are dwarf irregular systems that are currently experiencing a burst of star formation. Their appearance is dominated by the starburst, which appears compact and blue, hence their name. Their spectra show all the characteristics of H ii regions, which has led many BC ...
Annual Report 2012
... 2.5.10 Surveys for High-z Galaxies . . . . . . . . . . . . . . . . . . 2.5.11 The star formation rate functions of the Universe in the first 1–2 billion years . . . . . . . . . . . . . . . . . . . . . . 2.5.12 Gravitational weak lensing . . . . . . . . . . . . . . . . . . Theoretical studies of gala ...
... 2.5.10 Surveys for High-z Galaxies . . . . . . . . . . . . . . . . . . 2.5.11 The star formation rate functions of the Universe in the first 1–2 billion years . . . . . . . . . . . . . . . . . . . . . . 2.5.12 Gravitational weak lensing . . . . . . . . . . . . . . . . . . Theoretical studies of gala ...
Markov Chain Monte Carlo Modeling of High-Redshift Quasar
... processes in the Universe. As matter falls into the central black hole, it is accelerated and collisionally heated, and the radiation emitted can outshine the combined light of all the stars in the host galaxy. Studies of quasar host galaxies at ultraviolet to near-infrared wavelengths are fundament ...
... processes in the Universe. As matter falls into the central black hole, it is accelerated and collisionally heated, and the radiation emitted can outshine the combined light of all the stars in the host galaxy. Studies of quasar host galaxies at ultraviolet to near-infrared wavelengths are fundament ...
The Physics and Chemistry of Nebular Evolution
... time, and ready access of all chemical species to one another. These studies have been applied to infer the conditions present at the location in the solar nebula where and when a given meteorite, or its components, formed. While condensation calculations act as a guide for the chemical evolution of ...
... time, and ready access of all chemical species to one another. These studies have been applied to infer the conditions present at the location in the solar nebula where and when a given meteorite, or its components, formed. While condensation calculations act as a guide for the chemical evolution of ...
Modeling Spatially and Spectrally Resolved Observations to
... a model for the rate of merger-induced post-starburst galaxies selected from optical spectra, resolving tension between their observed rarity and merger rates from other iii ...
... a model for the rate of merger-induced post-starburst galaxies selected from optical spectra, resolving tension between their observed rarity and merger rates from other iii ...
The Oort Cloud
... approach the sun at the very edge of their orbits, and then take off again to distances as much as a hundred thousand times greater than the distance of the Earth from the Sun. As a result these comets spend most of their time far beyond the orbit of the outermost planets, and, if they preserve thei ...
... approach the sun at the very edge of their orbits, and then take off again to distances as much as a hundred thousand times greater than the distance of the Earth from the Sun. As a result these comets spend most of their time far beyond the orbit of the outermost planets, and, if they preserve thei ...
Far-ultraviolet and far-infrared bivariate luminosity function of galaxies:
... dominance of the hidden SF continues even toward higher redshifts (z ∼ 3) (e.g., Murphy et al., 2011; Cucciati et al., ...
... dominance of the hidden SF continues even toward higher redshifts (z ∼ 3) (e.g., Murphy et al., 2011; Cucciati et al., ...
Tracing the Evolution and Impact of the Stellar Winds
... boundary where the winds of the Sun are expected to meet the material of the ISM, and is shown as the boundary between Regions 2 and 3 in Figure 1.2. The heliosphere has been adopted as a marker for determining Voyager 1 ’s transition from the inside to the outside of the solar system. The difficult ...
... boundary where the winds of the Sun are expected to meet the material of the ISM, and is shown as the boundary between Regions 2 and 3 in Figure 1.2. The heliosphere has been adopted as a marker for determining Voyager 1 ’s transition from the inside to the outside of the solar system. The difficult ...
Galaxies in the Universe: An Introduction, Second Edition
... This text is aimed primarily at third- and fourth-year undergraduate students of astronomy or physics, who have undertaken the first year or two of university-level studies in physics. We hope that graduate students and research workers in related areas will also find it useful as an introduction to t ...
... This text is aimed primarily at third- and fourth-year undergraduate students of astronomy or physics, who have undertaken the first year or two of university-level studies in physics. We hope that graduate students and research workers in related areas will also find it useful as an introduction to t ...
Volatiles in protoplanetary disks
... The solar system was formed from a protoplanetary disk during a time frame of 2-3 million years, spanning ages of at least 4567-4564 Myr – a number known to a high degree of precision, thanks to accurate radiometric dating of primitive meteoritic material formed by gas-condensation processes (Scott ...
... The solar system was formed from a protoplanetary disk during a time frame of 2-3 million years, spanning ages of at least 4567-4564 Myr – a number known to a high degree of precision, thanks to accurate radiometric dating of primitive meteoritic material formed by gas-condensation processes (Scott ...
Volatiles in protoplanetary disks
... The solar system was formed from a protoplanetary disk during a time frame of 2-3 million years, spanning ages of at least 4567-4564 Myr – a number known to a high degree of precision, thanks to accurate radiometric dating of primitive meteoritic material formed by gas-condensation processes (Scott ...
... The solar system was formed from a protoplanetary disk during a time frame of 2-3 million years, spanning ages of at least 4567-4564 Myr – a number known to a high degree of precision, thanks to accurate radiometric dating of primitive meteoritic material formed by gas-condensation processes (Scott ...
The Celestial Sphere CHAPTER 1
... motion was a good approximation. Furthermore, since a geocentric model maintains circular motion, it was very difficult to make any observational distinction between geocentric and heliocentric universes. (Parallax effects are far too small to be noticeable with the naked eye.) ...
... motion was a good approximation. Furthermore, since a geocentric model maintains circular motion, it was very difficult to make any observational distinction between geocentric and heliocentric universes. (Parallax effects are far too small to be noticeable with the naked eye.) ...
Galaxies Astronomy 1 — Elementary Astronomy LA Mission College Spring F2015
... Astronomy 1 — Elementary Astronomy LA Mission College Spring F2015 ...
... Astronomy 1 — Elementary Astronomy LA Mission College Spring F2015 ...
The low-mass dispersed population around the Lupus clouds
... appearance dominated at wavelengths shorter than 9000 Å by the strong telluric O2 features near 6870 Å and 7600 Å, with weak or no indications of the TiO bands that dominate M-type spectra, thus making the determination of the spectral subtype and the estimate of the temperature more uncertain. Spec ...
... appearance dominated at wavelengths shorter than 9000 Å by the strong telluric O2 features near 6870 Å and 7600 Å, with weak or no indications of the TiO bands that dominate M-type spectra, thus making the determination of the spectral subtype and the estimate of the temperature more uncertain. Spec ...
Galaxy And Mass Assembly (GAMA): Gas Fuelling of Spiral Galaxies
... luminous galaxies form and initially evolve as disk galaxies at the center of isolated dark matter halos (DMH). Under this paradigm, as dark matter over-densities decouple from the large scale flow and collapse, the baryons of the ambient intergalactic medium bound to the potential well of the nasce ...
... luminous galaxies form and initially evolve as disk galaxies at the center of isolated dark matter halos (DMH). Under this paradigm, as dark matter over-densities decouple from the large scale flow and collapse, the baryons of the ambient intergalactic medium bound to the potential well of the nasce ...
THE KINEMATICS OF ARP 295 IN Hα EMISSION
... rates (SFRs) of 2.1 and 17.2 M yr−1 . They find that the more active Arp295b is also more gas-rich than the larger galaxy, with MHI ' 1.69 × 1010 M compared to 4.9 × 109 M . Dopita et al. (2002) measure a Hα flux of 3.13 × 10−13 ergs cm−2 s−1 for Arp 295b, which corresponds to LHα = 3.85×1041 erg ...
... rates (SFRs) of 2.1 and 17.2 M yr−1 . They find that the more active Arp295b is also more gas-rich than the larger galaxy, with MHI ' 1.69 × 1010 M compared to 4.9 × 109 M . Dopita et al. (2002) measure a Hα flux of 3.13 × 10−13 ergs cm−2 s−1 for Arp 295b, which corresponds to LHα = 3.85×1041 erg ...