– 1 – 1. Galaxy Observations 1.1.
... wide luminosity (i.e. mass) range with moderate resolution but high accuracy spectra. A fixed aperture size is used for each galaxy, corresponding to a fixed physical size for each of the two galaxy clusters. The Coma cluster of galaxies is the nearest virialized large cluster of galaxies with a wel ...
... wide luminosity (i.e. mass) range with moderate resolution but high accuracy spectra. A fixed aperture size is used for each galaxy, corresponding to a fixed physical size for each of the two galaxy clusters. The Coma cluster of galaxies is the nearest virialized large cluster of galaxies with a wel ...
the origin of binary stars - Institut d`Astronomie et d`Astrophysique
... In this way, observationally identifiable “molecular cloud cores” are formed. Stage II: The star formation process begins in earnest when a condensing cloud core “passes the brink of instability” (Shu et al. 1987) and collapses dynamically toward stellar densities. This leads to the formation of a c ...
... In this way, observationally identifiable “molecular cloud cores” are formed. Stage II: The star formation process begins in earnest when a condensing cloud core “passes the brink of instability” (Shu et al. 1987) and collapses dynamically toward stellar densities. This leads to the formation of a c ...
X-ray emission from supernova shock waves Tanja Kramer Nymark Department of Astronomy
... The field of supernova research is a quite new one, compared with astronomy in general – it is only about eighty years since astronomers first became aware that some of the “new stars” which occasionally appeared were far too energetic to be understood in the context of what was at the time known ab ...
... The field of supernova research is a quite new one, compared with astronomy in general – it is only about eighty years since astronomers first became aware that some of the “new stars” which occasionally appeared were far too energetic to be understood in the context of what was at the time known ab ...
distance
... luminosity goes up the density goes down, and the absorption lines are no longer as good at trapping ...
... luminosity goes up the density goes down, and the absorption lines are no longer as good at trapping ...
A large-scale CO survey of the Rosette Molecular Cloud: assessing
... lines. The image also shows that many of the clumps and clouds are limb brightening on their edge facing the O stars. By consideration of the full data cube, we identify three distinct spatiovelocity structures: (1) relatively compact regions with broad line wings, identified as compact or well-coll ...
... lines. The image also shows that many of the clumps and clouds are limb brightening on their edge facing the O stars. By consideration of the full data cube, we identify three distinct spatiovelocity structures: (1) relatively compact regions with broad line wings, identified as compact or well-coll ...
Astronomy Astrophysics - Georg-August
... in AGN have been published by different authors. They investigated radiatively-driven wind models (e.g. Murray & Chiang 1997; Proga et al. 2000) and/or magnetically-driven disk outflow models (Blandford & Payne 1982; Bottorff et al. 1997; Emmering et al. 1992; Königl & Kartje 1994). There are other ...
... in AGN have been published by different authors. They investigated radiatively-driven wind models (e.g. Murray & Chiang 1997; Proga et al. 2000) and/or magnetically-driven disk outflow models (Blandford & Payne 1982; Bottorff et al. 1997; Emmering et al. 1992; Königl & Kartje 1994). There are other ...
New INTEGRAL High Mass X
... The thin equatorial disk of the B-supergiant is inclined with respect to the orbital plane The star has also a polar wind with higher velocity and lower mass loss rate (~0.01 * Mass loss rate in the disk) thus, in order to explain the low X-ray emission level out of the outburst, we need anyway a no ...
... The thin equatorial disk of the B-supergiant is inclined with respect to the orbital plane The star has also a polar wind with higher velocity and lower mass loss rate (~0.01 * Mass loss rate in the disk) thus, in order to explain the low X-ray emission level out of the outburst, we need anyway a no ...
FIELD GALAXIES AND THEIR AGNs: NATURE VERSUS
... The critical mass ∼ 2 × 1010 M¯ in simulations (the cold mode dominates below this mass and the hot mode dominates above it) is close to the observed characteristic mass for a shift in galaxy properties, Mgal ∼ 3 × 1010 M¯ (Kauffmann et al. 2004, Kannappan 2004). Galaxies below the critical mass of ...
... The critical mass ∼ 2 × 1010 M¯ in simulations (the cold mode dominates below this mass and the hot mode dominates above it) is close to the observed characteristic mass for a shift in galaxy properties, Mgal ∼ 3 × 1010 M¯ (Kauffmann et al. 2004, Kannappan 2004). Galaxies below the critical mass of ...
THE MORPHOLOGICAL DEMOGRAPHICS OF GALAXIES IN THE
... were f (R) = 2π 0R I(r)dr is the integrated flux within the radius R. The determination of the radius R up to where to integrate the light is of importance particularly for the asymmetry values. As we sample galaxies over ever larger cosmic ages, the surface brightness of galaxies at higher redshift ...
... were f (R) = 2π 0R I(r)dr is the integrated flux within the radius R. The determination of the radius R up to where to integrate the light is of importance particularly for the asymmetry values. As we sample galaxies over ever larger cosmic ages, the surface brightness of galaxies at higher redshift ...
black holes can play a constructive role as well
... 2001; Morganti et al. 1999). A pair of inner lobes at 5 kpc from the nucleus co-exist with a single Northern Middle Lobe at 25-30 kpc (Fig. 1). On the largest scales, a pair of outer lobes is seen at around 100 kpc from the nucleus (Feain et al. 2009). The bent nature and re-orientation of the jets ...
... 2001; Morganti et al. 1999). A pair of inner lobes at 5 kpc from the nucleus co-exist with a single Northern Middle Lobe at 25-30 kpc (Fig. 1). On the largest scales, a pair of outer lobes is seen at around 100 kpc from the nucleus (Feain et al. 2009). The bent nature and re-orientation of the jets ...
Properties of Galactic B supergiants
... (e.g. Mokiem et al. 2006ab). Unfortunately, O dwarfs are visually faint in external galaxies due to their large bolometric corrections and small radii, with typically MV = -5.0 mag. O star abundances of CNO elements are difficult to derive (Crowther et al. 2002), yet these are sensitive to early rot ...
... (e.g. Mokiem et al. 2006ab). Unfortunately, O dwarfs are visually faint in external galaxies due to their large bolometric corrections and small radii, with typically MV = -5.0 mag. O star abundances of CNO elements are difficult to derive (Crowther et al. 2002), yet these are sensitive to early rot ...
THE VELOCITY DISTRIBUTION OF THE NEAREST
... to probe the history of a diffuse cloud and the relevance of small-scale structure to ISM physics and to gauge the past and future Galactic environment of the Sun (Frisch 19971). Nearby ISM provides a unique set of constraints for determining diffuse cloud physics. Observations of both pickup ions ins ...
... to probe the history of a diffuse cloud and the relevance of small-scale structure to ISM physics and to gauge the past and future Galactic environment of the Sun (Frisch 19971). Nearby ISM provides a unique set of constraints for determining diffuse cloud physics. Observations of both pickup ions ins ...
Large scale kinematics and dynamical modelling of the Milky Way
... the Galactic centre, but only 15 of their targets are within 8 pc from the Galactic centre, and therefore likely cluster members. McGinn et al. (1989) obtained integrated light spectra of selected fields with a 2000 (0.78 pc) aperture at 2.3 µm out to ∼4 pc (1.70 ) distance along the Galactic plane ...
... the Galactic centre, but only 15 of their targets are within 8 pc from the Galactic centre, and therefore likely cluster members. McGinn et al. (1989) obtained integrated light spectra of selected fields with a 2000 (0.78 pc) aperture at 2.3 µm out to ∼4 pc (1.70 ) distance along the Galactic plane ...
Wandering in the Redshift Desert
... relief may be offered by Ly-α, if the specSQNFQ@OG HR DEjBHDMS DMNTFG HM SGD 45 Indeed, even if not in emission, Ly-α is such a strong feature that it helps a lot in getting redshifts. However, in a spectrograph such as e.g., VIMOS, Ly-α does not enter before z ~ 1.8, hence the range 1.4 < z < 1.8 i ...
... relief may be offered by Ly-α, if the specSQNFQ@OG HR DEjBHDMS DMNTFG HM SGD 45 Indeed, even if not in emission, Ly-α is such a strong feature that it helps a lot in getting redshifts. However, in a spectrograph such as e.g., VIMOS, Ly-α does not enter before z ~ 1.8, hence the range 1.4 < z < 1.8 i ...
Anisotropy of the Hectometer Cosmic Radio Background
... ANISOTROPY OF THE HECTOMETER COSMIC RADIO BACKGROUND ...
... ANISOTROPY OF THE HECTOMETER COSMIC RADIO BACKGROUND ...
FOE 2017 Poster Contributions - College of Science | Oregon State
... Epeak, Tγ,Ta, etc. So far with this method we obtained a promising correlation coefficient, about 0.70, between the observed redshift and the predicted one after N-1 cross validation method is applied (Dainotti, Bogdan & Hastie in preparation) while the correlation is only 58% for random forest. Thi ...
... Epeak, Tγ,Ta, etc. So far with this method we obtained a promising correlation coefficient, about 0.70, between the observed redshift and the predicted one after N-1 cross validation method is applied (Dainotti, Bogdan & Hastie in preparation) while the correlation is only 58% for random forest. Thi ...
Measuring distances to the edge of the local group
... estimating the size of a galaxy based on its rotational velocity, but changed at certain mass limits. Was this caused by an underlying physical phenomenon that we did not understand the mechanics of? Or was it potentially a problem with our measuring techniques? Noordermeer & Verheijen (2007) took a ...
... estimating the size of a galaxy based on its rotational velocity, but changed at certain mass limits. Was this caused by an underlying physical phenomenon that we did not understand the mechanics of? Or was it potentially a problem with our measuring techniques? Noordermeer & Verheijen (2007) took a ...
Molecular Cloud Turbulence and Star Formation. Ballesteros
... three dimensions suggest that the standard deviation of the logarithm of the density fluctuations σlog ρ scales with the logarithm of the Mach number (Padoan et al., 1997a; Mac Low et al., 2005). Similar features appear to persist in the isothermal, ideal MHD case (Ostriker et al., 1999; 2001; Falle ...
... three dimensions suggest that the standard deviation of the logarithm of the density fluctuations σlog ρ scales with the logarithm of the Mach number (Padoan et al., 1997a; Mac Low et al., 2005). Similar features appear to persist in the isothermal, ideal MHD case (Ostriker et al., 1999; 2001; Falle ...
Astrophysics Lab “A”
... Ultraviolet Explorer) satellite, one of the most important (earlier) instruments for the wind diagnostics of hot stars, and displays Galactic objects. A second series displays UV-spectra from typical stars in the Small and Large Magellanic Cloud (SMC and LMC), collected by the more recent and well-k ...
... Ultraviolet Explorer) satellite, one of the most important (earlier) instruments for the wind diagnostics of hot stars, and displays Galactic objects. A second series displays UV-spectra from typical stars in the Small and Large Magellanic Cloud (SMC and LMC), collected by the more recent and well-k ...
The Young Stars
... displayed erratic optical variability, strong chromospheric lines and could be identified through their strong Hα emission lines. They were found to congregate at the periphery of dark clouds. The nearest were located in the Taurus molecular cloud and the ρ Ophiuchus cloud. Given our present knowled ...
... displayed erratic optical variability, strong chromospheric lines and could be identified through their strong Hα emission lines. They were found to congregate at the periphery of dark clouds. The nearest were located in the Taurus molecular cloud and the ρ Ophiuchus cloud. Given our present knowled ...
The rebirth of Supernova 1987A a study of the ejecta-ring collision
... they have throughout history fascinated people as they appeared as new stars in the sky. Supernova (SN) 1987A exploded in the nearby satellite galaxy, the Large Magellanic Cloud (LMC), at a distance of only 168 000 light years. The proximity of SN 1987A offers a unique opportunity to study the mediu ...
... they have throughout history fascinated people as they appeared as new stars in the sky. Supernova (SN) 1987A exploded in the nearby satellite galaxy, the Large Magellanic Cloud (LMC), at a distance of only 168 000 light years. The proximity of SN 1987A offers a unique opportunity to study the mediu ...
HI in Early-type Galaxies
... event. A good example of this is NGC 5266 (Figure 4; see Morganti et al. 1997a). This is a minor-axis dust-lane elliptical with a large amount of HI (∼1010 M¯ , MHI /LB ∼ 0 · 2). Almost all the HI is in an elongated structure parallel to the optical major axis. Most of this gas is rotating in a reas ...
... event. A good example of this is NGC 5266 (Figure 4; see Morganti et al. 1997a). This is a minor-axis dust-lane elliptical with a large amount of HI (∼1010 M¯ , MHI /LB ∼ 0 · 2). Almost all the HI is in an elongated structure parallel to the optical major axis. Most of this gas is rotating in a reas ...
Chapter 6 in the LSST Science Book
... are distributed in a halo that extends beyond 25 kpc. Their spatial distribution, chemical composition and kinematics provide clues about the Milky Way’s early history, as well as its continued interaction with neighboring galaxies. If the Clouds also have similar halos, the history of their formati ...
... are distributed in a halo that extends beyond 25 kpc. Their spatial distribution, chemical composition and kinematics provide clues about the Milky Way’s early history, as well as its continued interaction with neighboring galaxies. If the Clouds also have similar halos, the history of their formati ...
The stellar populations in the low-luminosity, early
... Low-luminosity galaxies may be the building blocks of more luminous systems. Southern African Large Telescope observations of the low-luminosity, early-type galaxy NGC 59 are obtained and analysed. These data are used to measure the stellar population parameters in the centre and off-centre regions ...
... Low-luminosity galaxies may be the building blocks of more luminous systems. Southern African Large Telescope observations of the low-luminosity, early-type galaxy NGC 59 are obtained and analysed. These data are used to measure the stellar population parameters in the centre and off-centre regions ...