Evolution of the Highest Redshift Quasars
... • Probing dust and star formation in the most massive high-z systems ...
... • Probing dust and star formation in the most massive high-z systems ...
UNIVERSITY OF PADUA Master degree in
... The interstellar medium (ISM) is the medium that exists between stars and star systems within a galaxy and is the intermediate region between stellar and galactic scales. The ISM spans a wide range of densities and temperatures; it ranges from cold dense gas (HI or diffuse clouds) with typical densi ...
... The interstellar medium (ISM) is the medium that exists between stars and star systems within a galaxy and is the intermediate region between stellar and galactic scales. The ISM spans a wide range of densities and temperatures; it ranges from cold dense gas (HI or diffuse clouds) with typical densi ...
Girardi
... NO. 6 Gyr old RC stars are ∼ 1.4 times more frequent than the 10-Gyr old, mainly because they leave the MS at a faster rate, and despite the IMF favouring old stars. Similar conclusions will apply to RGB stars. ...
... NO. 6 Gyr old RC stars are ∼ 1.4 times more frequent than the 10-Gyr old, mainly because they leave the MS at a faster rate, and despite the IMF favouring old stars. Similar conclusions will apply to RGB stars. ...
Chandra Observation of Pulsar Wind Nebula
... with a bright radiant light.” He goes on to describe how it rivaled Venus (magnitude -4.6 at the time) and how sharp-eyed “country folk” could spot ...
... with a bright radiant light.” He goes on to describe how it rivaled Venus (magnitude -4.6 at the time) and how sharp-eyed “country folk” could spot ...
A re-examination of galactic conformity and a comparison with semi
... 4–5 Mpc. The analysis of Kauffmann et al. (2010) showed that correlations between satellite and central properties were still clearly present at projected separations of ∼1 Mpc. The analysis of Wang & White (2012) was restricted to satellites within a projected distance of 300 kpc from the primary g ...
... 4–5 Mpc. The analysis of Kauffmann et al. (2010) showed that correlations between satellite and central properties were still clearly present at projected separations of ∼1 Mpc. The analysis of Wang & White (2012) was restricted to satellites within a projected distance of 300 kpc from the primary g ...
Starburst Galaxies - Beck-Shop
... In those regions the massive hot young stars are extremely bright and outshine the far more numerous less massive stars. Few starforming regions are to be found in the remainder of the disk and so, despite there still being many stars in those regions, they appear dark in comparison with the arms. M ...
... In those regions the massive hot young stars are extremely bright and outshine the far more numerous less massive stars. Few starforming regions are to be found in the remainder of the disk and so, despite there still being many stars in those regions, they appear dark in comparison with the arms. M ...
radioactive 26a1 in the galaxy: observations versus theory
... target for the HEAO-3 detectors. Moreover it was pointed out that, because of its long mean life, 26A1 would have enough time to be thermalised in the interstellar medium; therefore, it would de-excite essentially at rest and emit a narrow line, making easier its detection and identification with su ...
... target for the HEAO-3 detectors. Moreover it was pointed out that, because of its long mean life, 26A1 would have enough time to be thermalised in the interstellar medium; therefore, it would de-excite essentially at rest and emit a narrow line, making easier its detection and identification with su ...
Radiatively driven Rayleigh-Taylor instability candidates around a
... the dissipation of intense radiation pressure in the early stages of massive protostellar collapse, which is thought to be capable of reversing accretion flows (see Zinnecker & Yorke 2007). The work-around solution to this problem suggested by theory argues that stars as massive as 140 M can form t ...
... the dissipation of intense radiation pressure in the early stages of massive protostellar collapse, which is thought to be capable of reversing accretion flows (see Zinnecker & Yorke 2007). The work-around solution to this problem suggested by theory argues that stars as massive as 140 M can form t ...
Sunyaev±Zel'dovich distortion from early galactic winds Subhabrata Majumdar, Biman B. Nath
... first objects form at redshifts z , 40 with masses of order 105 M(, UV radiation from stars formed in these objects obliterate the molecular hydrogen in other objects in the vicinity, thereby suppressing further formation of objects with masses M # 108 M( (Haiman, Rees & Loeb 1997; Ciardi et al. 200 ...
... first objects form at redshifts z , 40 with masses of order 105 M(, UV radiation from stars formed in these objects obliterate the molecular hydrogen in other objects in the vicinity, thereby suppressing further formation of objects with masses M # 108 M( (Haiman, Rees & Loeb 1997; Ciardi et al. 200 ...
Hypervelocity Stars and the Galactic Center
... s−1 from a three-body interaction with a MBH. HVSs are a general consequence of MBHs in any galaxy (e.g. Sherwin et al. 2008), but the HVSs we can observe are the stars ejected from our own Galaxy. Yu & Tremaine (2003) predict that Sgr A∗ ejects one HVS every ∼105 yrs. Thus HVSs are rare: of the Gal ...
... s−1 from a three-body interaction with a MBH. HVSs are a general consequence of MBHs in any galaxy (e.g. Sherwin et al. 2008), but the HVSs we can observe are the stars ejected from our own Galaxy. Yu & Tremaine (2003) predict that Sgr A∗ ejects one HVS every ∼105 yrs. Thus HVSs are rare: of the Gal ...
formation of z 6 quasars from hierarchical
... 6 Nagoya University, Dept. of Physics, Nagoya, Aichi 464-8602, Japan and 7 Spitzer Fellow Accepted to ApJ ...
... 6 Nagoya University, Dept. of Physics, Nagoya, Aichi 464-8602, Japan and 7 Spitzer Fellow Accepted to ApJ ...
Dust and molecular gas in the most distant quasars
... emission region is estimated to be a few kpc => Consistent with the size of the CO and C+ emission region. – CO detections – Luminosity correlations • FIR-to-radio emission consistent with typical star forming galaxies. • LFIR – Lbol correlation: follow the trends defined by local IR quasars – likel ...
... emission region is estimated to be a few kpc => Consistent with the size of the CO and C+ emission region. – CO detections – Luminosity correlations • FIR-to-radio emission consistent with typical star forming galaxies. • LFIR – Lbol correlation: follow the trends defined by local IR quasars – likel ...
Curriculum Vitae - Centre for Astrophysics and Supercomputing
... Research Interests • Modelling spectral energy distributions of galaxies • Stellar population synthesis models • Statistical interpretation of spectroscopic and photometric galaxy surveys • The formation and evolution of galaxies, comparison between theory/models and observations • The connections b ...
... Research Interests • Modelling spectral energy distributions of galaxies • Stellar population synthesis models • Statistical interpretation of spectroscopic and photometric galaxy surveys • The formation and evolution of galaxies, comparison between theory/models and observations • The connections b ...
Extragalactic Astronomical Masers I
... artificial light and it is very different from other lights in that a laser light is highly collimated and coherently emits in space. Similarly, maser emits very narrow and intense emission at microwave or radio wavelengths over long distances. Thus, sources of maser emit collimated emission. Astron ...
... artificial light and it is very different from other lights in that a laser light is highly collimated and coherently emits in space. Similarly, maser emits very narrow and intense emission at microwave or radio wavelengths over long distances. Thus, sources of maser emit collimated emission. Astron ...
Nebula
... materials 'clump' together to form larger masses, which attract further matter, and eventually will become big enough to form stars. The remaining materials are then believed to form planets, and other planetary system objects. ...
... materials 'clump' together to form larger masses, which attract further matter, and eventually will become big enough to form stars. The remaining materials are then believed to form planets, and other planetary system objects. ...
RADIO OBSERVATIONS RELATED TO STAR FORMATION P. G.
... central part of the nuclear disk, < 200 pc from the nucleus of our Galaxy. A large number of small HII regions are located between the main spiral arms, and are often associated with dense clouds (CO-clouds). These small HII regions represent Ο star formation in the interarm region. By counting Lyma ...
... central part of the nuclear disk, < 200 pc from the nucleus of our Galaxy. A large number of small HII regions are located between the main spiral arms, and are often associated with dense clouds (CO-clouds). These small HII regions represent Ο star formation in the interarm region. By counting Lyma ...
S282_2 Introduction to active galaxies
... Active galaxies seem to be quite rare in the nearby Universe. Whether every galaxy goes through an active phase in its lifetime, or whether active galaxies are a separate class of object is not clear. We have been aware of these objects only since the 1940s, and the galaxies have been around for at ...
... Active galaxies seem to be quite rare in the nearby Universe. Whether every galaxy goes through an active phase in its lifetime, or whether active galaxies are a separate class of object is not clear. We have been aware of these objects only since the 1940s, and the galaxies have been around for at ...
Massive Star Formation in the Galactic Center
... are extraordinarily dense (n > 104 cm−3 ) and warm (T ∼ 70 K) with respect to those found in the disk of the Galaxy. Stark et al. (1989) argue that the density and internal velocities of clouds in the GC are a direct result of the strong tidal fields in the region, i.e. only the dense survive. Seraby ...
... are extraordinarily dense (n > 104 cm−3 ) and warm (T ∼ 70 K) with respect to those found in the disk of the Galaxy. Stark et al. (1989) argue that the density and internal velocities of clouds in the GC are a direct result of the strong tidal fields in the region, i.e. only the dense survive. Seraby ...
rcw 49 at mid-infrared wavelengths: a glimpse from the
... bands, the diffuse emission is produced primarily by polycyclic aromatic hydrocarbon (PAH) features and Br line emission, which we discuss below. In Figure 2 (Plate 2) we show two sets of three-color images centered on RCW 49 composed of subsets of the OSV data (360 frames per band). The top panel ...
... bands, the diffuse emission is produced primarily by polycyclic aromatic hydrocarbon (PAH) features and Br line emission, which we discuss below. In Figure 2 (Plate 2) we show two sets of three-color images centered on RCW 49 composed of subsets of the OSV data (360 frames per band). The top panel ...
11 The Interstellar Medium
... forming many stars at one time. b) One star forms; other matter goes into planets, moons, asteroids, & comets. c) Clouds rotate & throw off mass until only enough is left to form one star. ...
... forming many stars at one time. b) One star forms; other matter goes into planets, moons, asteroids, & comets. c) Clouds rotate & throw off mass until only enough is left to form one star. ...
Investigating Black Hole Kicks
... X-ray binaries are divided into two main class, as according to the mass of the noncompact star: low-mass X-ray binaries (LMXBs) and high mass X-ray binaries (HMXBs) ([29]). In both cases, the accreting star can be either a neutron star or a black hole. F HMXB: the donor is a young and massive O/B s ...
... X-ray binaries are divided into two main class, as according to the mass of the noncompact star: low-mass X-ray binaries (LMXBs) and high mass X-ray binaries (HMXBs) ([29]). In both cases, the accreting star can be either a neutron star or a black hole. F HMXB: the donor is a young and massive O/B s ...
Cloud angular momentum and effective viscosity in
... the formation and evolution of molecular clouds. Feedback contributes to turbulence and the destruction of clouds, leading to a population of clouds that is younger, less massive, and with more retrograde rotation. We investigate the evolution of clouds as they interact with each other and the diffu ...
... the formation and evolution of molecular clouds. Feedback contributes to turbulence and the destruction of clouds, leading to a population of clouds that is younger, less massive, and with more retrograde rotation. We investigate the evolution of clouds as they interact with each other and the diffu ...
SUPERNOVA REMNANT SHOCKS IN AN INHOMOGENEOUS
... (McKee and Ostriker 1977). Although fh is high in the local ISM, its value at a typical point in the galactic disk remains controversial (Cox 1987). It is quite likely that fh depends on both the nature of the galaxy and the location within it. In principle, observations of SNRs could provide the me ...
... (McKee and Ostriker 1977). Although fh is high in the local ISM, its value at a typical point in the galactic disk remains controversial (Cox 1987). It is quite likely that fh depends on both the nature of the galaxy and the location within it. In principle, observations of SNRs could provide the me ...
The Jansky Very Large Array – New Capabilities, New Science
... • Three of the four prior examples employed mm (PdBI) interferometer observations as well as VLA. • The rise of ALMA will strengthen this complementarity, with stellar scientific results. • New example – Wagg and Carilli combine VLA and ALMA for early forming galaxies: – Massive galaxies at z~2 must ...
... • Three of the four prior examples employed mm (PdBI) interferometer observations as well as VLA. • The rise of ALMA will strengthen this complementarity, with stellar scientific results. • New example – Wagg and Carilli combine VLA and ALMA for early forming galaxies: – Massive galaxies at z~2 must ...
Mass-to-light ratio gradients in early-type galaxy haloes
... kinematics in early-type galaxies – representing the first unbiased study of halo masses in a wide range of early-type galaxy luminosities – and find a correlation between luminosity and ∇ ϒ, such that the brightest galaxies appear the most dark-matter dominated. We find that the gradients in most ...
... kinematics in early-type galaxies – representing the first unbiased study of halo masses in a wide range of early-type galaxy luminosities – and find a correlation between luminosity and ∇ ϒ, such that the brightest galaxies appear the most dark-matter dominated. We find that the gradients in most ...