1 Pau Amaro Seoane - modest 15-s
... radii between 10 to 100 pc they are more than a factor 1000 denser than dwarf galaxies of the same mass. They also show evidence for elevated mass-to-light ratios, which could be due to the presence of massive black holes or unusual stellar IMFs as a result of their extreme densities. While the firs ...
... radii between 10 to 100 pc they are more than a factor 1000 denser than dwarf galaxies of the same mass. They also show evidence for elevated mass-to-light ratios, which could be due to the presence of massive black holes or unusual stellar IMFs as a result of their extreme densities. While the firs ...
The Magellan 20 Telescope Science Goals
... diameter field would be well suited to this experiment and could exhaust all the background galaxies in a one square degree field in 5 nights. If we take 100 physical Mpc at z=3 representative of the largest scales to be investigated the field must be as large as 3.8 x 3.8 or 14.4 square degrees. To ...
... diameter field would be well suited to this experiment and could exhaust all the background galaxies in a one square degree field in 5 nights. If we take 100 physical Mpc at z=3 representative of the largest scales to be investigated the field must be as large as 3.8 x 3.8 or 14.4 square degrees. To ...
A SIGNIFICANTLY LOW CO ABUNDANCE TOWARD THE TW Hya
... In this Letter we report the CO abundance relative to H2 derived toward the circumstellar disk of the T-Tauri star TW Hya from the HD (1 − 0) and C18 O (2 − 1) emission lines. The HD (1 − 0) line was observed by the Herschel Space Observatory Photodetector Array Camera and Spectrometer whereas C18 O ...
... In this Letter we report the CO abundance relative to H2 derived toward the circumstellar disk of the T-Tauri star TW Hya from the HD (1 − 0) and C18 O (2 − 1) emission lines. The HD (1 − 0) line was observed by the Herschel Space Observatory Photodetector Array Camera and Spectrometer whereas C18 O ...
Aryabhatta Research Institute of Observational Sciences
... Project for spectral extinction measurements of directly transmitted solar radiation that reaches the ground. It has successfully been used for day-time aerosol optical depths (AODs) measurements since January 2002. Results based on analysis of these extensive (from January 2002 to December 2004) me ...
... Project for spectral extinction measurements of directly transmitted solar radiation that reaches the ground. It has successfully been used for day-time aerosol optical depths (AODs) measurements since January 2002. Results based on analysis of these extensive (from January 2002 to December 2004) me ...
The absence of CO from the dust peak around ϵ Eri
... Assuming that the gas and dust are thermalized with an equilibrium temperature of 35 K (Dent et al. 2000), the formalism of Knapp et al. (1980) allows the conversion of the observed 3σ upper limit of 0.0156 K km s−1 (in units of T mb now) into a column density of CO molecules of 8.7 × 1011 cm−2 , im ...
... Assuming that the gas and dust are thermalized with an equilibrium temperature of 35 K (Dent et al. 2000), the formalism of Knapp et al. (1980) allows the conversion of the observed 3σ upper limit of 0.0156 K km s−1 (in units of T mb now) into a column density of CO molecules of 8.7 × 1011 cm−2 , im ...
Discovery of an Unusual Optical Transient with the Hubble Space
... months. Three additional photometry points were obtained with the Faint Object Camera and Spectrograph (FOCAS; Kashikawa et al. 2002) on the Subaru telescope on 2006 June 28, 2006 August 23, and the next year on 2007 May 18. The June observations suffered from poor weather conditions (seeing ≥ 2′′ ) ...
... months. Three additional photometry points were obtained with the Faint Object Camera and Spectrograph (FOCAS; Kashikawa et al. 2002) on the Subaru telescope on 2006 June 28, 2006 August 23, and the next year on 2007 May 18. The June observations suffered from poor weather conditions (seeing ≥ 2′′ ) ...
Lives of the Stars Lecture 5: Star birth
... forming both low- and high-mass stars. The conditions for a young star forming in Orion must be very different for a star forming in the relative quiet of Taurus-Auriga. As soon as massive stars form, you get intense radiation, powerful winds, and supernova explosions. The hot stars reshape their ow ...
... forming both low- and high-mass stars. The conditions for a young star forming in Orion must be very different for a star forming in the relative quiet of Taurus-Auriga. As soon as massive stars form, you get intense radiation, powerful winds, and supernova explosions. The hot stars reshape their ow ...
The fate of black hole singularities and the parameters of the
... puzzle becomes a crisis, as first realized by Hawking in 1974, because of the problem of the loss of information constituting the quantum state of the star whose collapse formed the black hole[3]. Another basic problem of physics is to understand why the masses and coupling constants of the elementa ...
... puzzle becomes a crisis, as first realized by Hawking in 1974, because of the problem of the loss of information constituting the quantum state of the star whose collapse formed the black hole[3]. Another basic problem of physics is to understand why the masses and coupling constants of the elementa ...
Astronomy 112: The Physics of Stars Class 19 Notes: The Stellar
... of a more general idea called stellar population synthesis. For star clusters, we assumed all the stars formed in a single burst with a given IMF, and then we computed how the stellar population would look at later times. Obviously we could easily generalize this to the case of a cluster that, for s ...
... of a more general idea called stellar population synthesis. For star clusters, we assumed all the stars formed in a single burst with a given IMF, and then we computed how the stellar population would look at later times. Obviously we could easily generalize this to the case of a cluster that, for s ...
Formation and evolution of giant molecular clouds in a barred spiral
... Understanding where and how gas is converted into stars in a galaxy is important for understanding a galaxy’s formation and evolution through each epoch of the universe. Which physical processes control the star formation in a galaxy is heavily debated. We are now at a stage where it is possible to ...
... Understanding where and how gas is converted into stars in a galaxy is important for understanding a galaxy’s formation and evolution through each epoch of the universe. Which physical processes control the star formation in a galaxy is heavily debated. We are now at a stage where it is possible to ...
Chapter 4 The Formation of Population III stars in a ΛCDM universe
... evolution and optically thin radiative cooling of the primordial gas is modeled as described in Section 2.2.5, following 9 separate species including molecular hydrogen (but excluding deuterium). Adaptive mesh refinement is turned on such that cells are refined by factors of two along each axis, wit ...
... evolution and optically thin radiative cooling of the primordial gas is modeled as described in Section 2.2.5, following 9 separate species including molecular hydrogen (but excluding deuterium). Adaptive mesh refinement is turned on such that cells are refined by factors of two along each axis, wit ...
The surface composition of Beta Pictoris
... stars with equatorial velocities of 125 km s−1 or less, and accreting at a rate of 10−13 M yr−1 , rotationally induced meridional circulation has no significant influence on the evolution of surface abundances, during the accretion episode itself.’ The true equatorial velocity of β Pic is probably ...
... stars with equatorial velocities of 125 km s−1 or less, and accreting at a rate of 10−13 M yr−1 , rotationally induced meridional circulation has no significant influence on the evolution of surface abundances, during the accretion episode itself.’ The true equatorial velocity of β Pic is probably ...
Draft paper (submitted to MNRAS)
... MB ∼ −16, or, equivalently, with stellar masses below 109 M⊙ ) located within ∼ 4.5 Mpc from the Local Group barycenter, but excluding the satellites of the Milky Way and Andromeda, as well as those of M81 and M82. Satellite galaxies (defined here as those within 300 kpc from any of those giant gala ...
... MB ∼ −16, or, equivalently, with stellar masses below 109 M⊙ ) located within ∼ 4.5 Mpc from the Local Group barycenter, but excluding the satellites of the Milky Way and Andromeda, as well as those of M81 and M82. Satellite galaxies (defined here as those within 300 kpc from any of those giant gala ...
Galaxy Evolution
... the cosmic evolution that followed the BIG BANG when there were no galaxies, and the universe was filled with matter and radiation uniformly distributed throughout the space. Only very tenuous perturbations of the density of matter and radiation altered this otherwise almost perfect homogeneity. The ...
... the cosmic evolution that followed the BIG BANG when there were no galaxies, and the universe was filled with matter and radiation uniformly distributed throughout the space. Only very tenuous perturbations of the density of matter and radiation altered this otherwise almost perfect homogeneity. The ...
Annual Report 2012 - Max Planck Institute for Astrophysics
... the MPE and therefore has to serve the needs of two institutes with differing research emphases – predominantly theoretical astrophysics at MPA and predominantly observational/instrumental astrophysics at the MPE. At present the library holds a unique collection of about 45000 books and journals and ...
... the MPE and therefore has to serve the needs of two institutes with differing research emphases – predominantly theoretical astrophysics at MPA and predominantly observational/instrumental astrophysics at the MPE. At present the library holds a unique collection of about 45000 books and journals and ...
Gamma-Ray Line Emission from Radioactive Isotopes in Stars and
... Al abundance present in the hydrogen shell is ejected unmodified in the supernova explosion or, in more massive stars during their Wolf-Rayet phase, by a stellar wind. The 26Al synthesized in the oxygen-neon shell may be significantly enhanced because of operation of the neutrino process (Woosley et ...
... Al abundance present in the hydrogen shell is ejected unmodified in the supernova explosion or, in more massive stars during their Wolf-Rayet phase, by a stellar wind. The 26Al synthesized in the oxygen-neon shell may be significantly enhanced because of operation of the neutrino process (Woosley et ...
Debris disks and the search for life in the universe Gianni Cataldi
... try to map the universe and gather information about it, the big difference being of course that astronomy is dependent on remote observations in most of the cases—only the solar system can be explored by means of space travel at the moment. However, astronomers not only try to find out what our uni ...
... try to map the universe and gather information about it, the big difference being of course that astronomy is dependent on remote observations in most of the cases—only the solar system can be explored by means of space travel at the moment. However, astronomers not only try to find out what our uni ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... the cosmic evolution that followed the BIG BANG when there were no galaxies, and the universe was filled with matter and radiation uniformly distributed throughout the space. Only very tenuous perturbations of the density of matter and radiation altered this otherwise almost perfect homogeneity. The ...
... the cosmic evolution that followed the BIG BANG when there were no galaxies, and the universe was filled with matter and radiation uniformly distributed throughout the space. Only very tenuous perturbations of the density of matter and radiation altered this otherwise almost perfect homogeneity. The ...
![Detection of [Ne ii] Emission from Young Circumstellar Disks](http://s1.studyres.com/store/data/014394769_1-fdf9c6283148d488005c87b005dab353-300x300.png)
Detection of [Ne ii] Emission from Young Circumstellar Disks
... due to stellar activity is larger than the quoted uncertainty and amounts to at least a few tenths of a dex (e.g. Marino et al. 2003). Our X–ray luminosities agree with values from the literature (Alcalá et al. 1997 for source 1; Mamajek et al. 2002 for source 2; Sciortino et al. 1998 for source 3; ...
... due to stellar activity is larger than the quoted uncertainty and amounts to at least a few tenths of a dex (e.g. Marino et al. 2003). Our X–ray luminosities agree with values from the literature (Alcalá et al. 1997 for source 1; Mamajek et al. 2002 for source 2; Sciortino et al. 1998 for source 3; ...
13.1 Galaxy Evolution: Introduction
... interstellar medium. It also turns out that this is the estimated timescale of active galactic nucleus episodes, and it's not obvious whether this is coincidence or not. The internal timescales within galaxies are commensurate with their free-fall timescales, which would be ...
... interstellar medium. It also turns out that this is the estimated timescale of active galactic nucleus episodes, and it's not obvious whether this is coincidence or not. The internal timescales within galaxies are commensurate with their free-fall timescales, which would be ...
The ionized gas in the central region of NGC 5253
... emission. Additionally, the information associated to auxiliary properties such as stellar extinction in the V band, the stellar velocity and velocity dispersion, the reduced χ2 and the absolute deviation of the fit (in %) were reformatted and saved as a file suitable for manipulation with standard ...
... emission. Additionally, the information associated to auxiliary properties such as stellar extinction in the V band, the stellar velocity and velocity dispersion, the reduced χ2 and the absolute deviation of the fit (in %) were reformatted and saved as a file suitable for manipulation with standard ...
Galaxy formation in the Planck cosmology - II. Star
... We adapt the L-GALAXIES semi-analytic model to follow the star formation histories (SFHs) of galaxies – by which we mean a record of the formation time and metallicities of the stars that are present in each galaxy at a given time. We use these to construct stellar spectra in postprocessing, which o ...
... We adapt the L-GALAXIES semi-analytic model to follow the star formation histories (SFHs) of galaxies – by which we mean a record of the formation time and metallicities of the stars that are present in each galaxy at a given time. We use these to construct stellar spectra in postprocessing, which o ...
AN ULTRA-DEEP NEAR-INFRARED SPECTRUM OF
... Several recent studies have shown that about half of the massive galaxies at z ∼ 2 are in a quiescent phase. Moreover, these galaxies are commonly found to be ultra-compact with half-light radii of ∼ 1 kpc. We have obtained a ∼ 29 hr spectrum of a typical quiescent, ultra-dense galaxy at z = 2.1865 ...
... Several recent studies have shown that about half of the massive galaxies at z ∼ 2 are in a quiescent phase. Moreover, these galaxies are commonly found to be ultra-compact with half-light radii of ∼ 1 kpc. We have obtained a ∼ 29 hr spectrum of a typical quiescent, ultra-dense galaxy at z = 2.1865 ...
The early stages of planet formation Ormel, Christiaan Wessel
... How do planets form? It is a simple question but the answer involves an array of diverse physical processes — complex as well as fascinating. It requires, first of all, to realize what planets really are. For centuries, humans were mystified by the ‘wandering stars,’ moving relative to a sky compose ...
... How do planets form? It is a simple question but the answer involves an array of diverse physical processes — complex as well as fascinating. It requires, first of all, to realize what planets really are. For centuries, humans were mystified by the ‘wandering stars,’ moving relative to a sky compose ...
Building galaxies Hunt, Leslie Kipp
... that atomic gas mass fraction also varies along the Hubble sequence. On the other hand, the massto-light ratio measured in the B band remains relatively constant with morphology, even toward the very late spiral types (although see Burstein 1982). With data from Roberts & Haynes (1994), Figure 3 sho ...
... that atomic gas mass fraction also varies along the Hubble sequence. On the other hand, the massto-light ratio measured in the B band remains relatively constant with morphology, even toward the very late spiral types (although see Burstein 1982). With data from Roberts & Haynes (1994), Figure 3 sho ...