AN INTENSIVE HUBBLE SPACE TELESCOPE
... Additional observations indicate that SNe Ia properties are correlated with host-galaxy properties. The average SN Ia hosted by a passive galaxy has a faster rise and fall than the average SN Ia hosted by a star-forming galaxy (Sullivan et al. 2006). The rate of SN Ia production per unit mass increa ...
... Additional observations indicate that SNe Ia properties are correlated with host-galaxy properties. The average SN Ia hosted by a passive galaxy has a faster rise and fall than the average SN Ia hosted by a star-forming galaxy (Sullivan et al. 2006). The rate of SN Ia production per unit mass increa ...
Full text - UvA/FNWI - University of Amsterdam
... sources in our sample in lighter colors as a reference. All components exceed a 3σ confidence level except for the 2.0σ detection in a selection of observations (from region Ei in the color-color diagram) of a Lorentzian with ν = 65 Hz that follows the same relation with νu as Lh . The simultaneousl ...
... sources in our sample in lighter colors as a reference. All components exceed a 3σ confidence level except for the 2.0σ detection in a selection of observations (from region Ei in the color-color diagram) of a Lorentzian with ν = 65 Hz that follows the same relation with νu as Lh . The simultaneousl ...
Hypervelocity Stars and the Galactic Center
... HVS with g ′ < 21.5 per 50 deg2 of sky (Kollmeier & Gould 2007). In the Galactic Center, there is some indication that the stellar mass function is top heavy (Maness et al. 2007). A Salpeter mass function predicts an order-of-magnitude lower density of F-type HVSs, 1 per ∼500 deg2 (Brown et al. 2007 ...
... HVS with g ′ < 21.5 per 50 deg2 of sky (Kollmeier & Gould 2007). In the Galactic Center, there is some indication that the stellar mass function is top heavy (Maness et al. 2007). A Salpeter mass function predicts an order-of-magnitude lower density of F-type HVSs, 1 per ∼500 deg2 (Brown et al. 2007 ...
Galactic Winds Sylvain Veilleux
... theoretical predictions to discuss critically the properties of GWs in the local and distant universe, and to evaluate the importance of these winds for the formation and evolution of galaxies and the IGM. We focus on material published within the past 15 years. Our discussion centers on three funda ...
... theoretical predictions to discuss critically the properties of GWs in the local and distant universe, and to evaluate the importance of these winds for the formation and evolution of galaxies and the IGM. We focus on material published within the past 15 years. Our discussion centers on three funda ...
Head–tail Galaxies: beacons of high
... believed to be formed via ram pressure in the cases where the host galaxy has a peculiar velocity of the order of 600 km s−1 and is embedded in a hot, dense plasma (Venkatesan et al. 1994), and wide-angle tailed galaxies (WATs) believed to be the result of ‘cluster weather’ (Klamer et al. 2004). NAT ...
... believed to be formed via ram pressure in the cases where the host galaxy has a peculiar velocity of the order of 600 km s−1 and is embedded in a hot, dense plasma (Venkatesan et al. 1994), and wide-angle tailed galaxies (WATs) believed to be the result of ‘cluster weather’ (Klamer et al. 2004). NAT ...
Andrea Santangelo
... A. Santangelo, D. Klochkov, V. Doroshenko, D. Müller, R. Doroshenko, R. Staubert, M. Sasaki (IAAT), J. Wilms, L. ...
... A. Santangelo, D. Klochkov, V. Doroshenko, D. Müller, R. Doroshenko, R. Staubert, M. Sasaki (IAAT), J. Wilms, L. ...
PPT
... deep interior of these stars. At lower temperatures, white dwarfs are expected to crystallize and phase separation of the main constituents of the core of a typical white dwarf, 12C and 16O, is expected to occur. This sequence of events is expected to introduce significant delays in the cooling ...
... deep interior of these stars. At lower temperatures, white dwarfs are expected to crystallize and phase separation of the main constituents of the core of a typical white dwarf, 12C and 16O, is expected to occur. This sequence of events is expected to introduce significant delays in the cooling ...
the origin of binary stars - Institut d`Astronomie et d`Astrophysique
... poles, creating an observable bipolar flow. Stage IV: The amount of material added to the protostar via direct infall continues to decrease, and the opening angle of the wind steadily widens until the young central star (along with its surrounding nebular disk) is revealed as a bonafide PMS star—for ...
... poles, creating an observable bipolar flow. Stage IV: The amount of material added to the protostar via direct infall continues to decrease, and the opening angle of the wind steadily widens until the young central star (along with its surrounding nebular disk) is revealed as a bonafide PMS star—for ...
The Distribution, Classification, and Color Evolution of Galaxies
... largest spectroscopic survey of the SDSS, used around 1800 plates, while SEGUE-1 has 407 plates and SEGUE-2 204. Each has holes drilled on it, into which 640 optical fibers are plugged. During each spectroscopic exposure, typically 900s, two spectrographs (one covering wavelengths from 3800Å to 6100 ...
... largest spectroscopic survey of the SDSS, used around 1800 plates, while SEGUE-1 has 407 plates and SEGUE-2 204. Each has holes drilled on it, into which 640 optical fibers are plugged. During each spectroscopic exposure, typically 900s, two spectrographs (one covering wavelengths from 3800Å to 6100 ...
Multiwavelength optical observations of chromospherically active
... profile of the very active star HU Vir. These profiles are well matched using a two-component Gaussian fit (narrow and broad) and the broad component can be interpreted as arising from microflaring. Red-shifted absorption features in the Hα line have been detected in several systems and excess emiss ...
... profile of the very active star HU Vir. These profiles are well matched using a two-component Gaussian fit (narrow and broad) and the broad component can be interpreted as arising from microflaring. Red-shifted absorption features in the Hα line have been detected in several systems and excess emiss ...
Thesis
... to their relatively easy detection at every redshift. Since stars form out of cold and dense gas, a comprehensive model for galaxy evolution should explain any observed connection between SFR and the amount and properties of the molecular gas of the interstellar medium (ISM). In proposed models of t ...
... to their relatively easy detection at every redshift. Since stars form out of cold and dense gas, a comprehensive model for galaxy evolution should explain any observed connection between SFR and the amount and properties of the molecular gas of the interstellar medium (ISM). In proposed models of t ...
paper - Harvard-Smithsonian Center for Astrophysics
... 236.34 GHz in the lower sideband and 244.36 to 246.34 GHz in the upper sideband. The phase center was at α(2000) = 07h 22m 58.s 27, δ(2000) = −25◦ 46 03. 4. The quasars 0730-116 and 0538-440 were observed every 20 minutes for gain calibration, and the spectral bandpass was calibrated using quasar ...
... 236.34 GHz in the lower sideband and 244.36 to 246.34 GHz in the upper sideband. The phase center was at α(2000) = 07h 22m 58.s 27, δ(2000) = −25◦ 46 03. 4. The quasars 0730-116 and 0538-440 were observed every 20 minutes for gain calibration, and the spectral bandpass was calibrated using quasar ...
Galaxy Pairs in the Sloan Digital Sky Survey
... 2006; Cox et al. 2008). Simulations also predict that the orientation and relative rotation directions can dramatically affect the efficiency of a starburst, much more so than simply the presence of an adequate gas supply (Di Matteo et al. 2007; Cox et al. 2008). The efficiency may also increase at ...
... 2006; Cox et al. 2008). Simulations also predict that the orientation and relative rotation directions can dramatically affect the efficiency of a starburst, much more so than simply the presence of an adequate gas supply (Di Matteo et al. 2007; Cox et al. 2008). The efficiency may also increase at ...
SPT 0538−50: PHYSICAL CONDITIONS IN THE ISM OF A STRONGLY... GALAXY AT Z=2.8
... on board the Spitzer Space Telescope (Werner et al. 2004) on 2009 August 2, as part of a large program to obtain follow-up imaging of the SPT sources (PID 60194; PI Vieira). The basic calibrated data, pre-processed by the Spitzer Science Center (SSC)’s standard pipeline, were combined into a re-samp ...
... on board the Spitzer Space Telescope (Werner et al. 2004) on 2009 August 2, as part of a large program to obtain follow-up imaging of the SPT sources (PID 60194; PI Vieira). The basic calibrated data, pre-processed by the Spitzer Science Center (SSC)’s standard pipeline, were combined into a re-samp ...
as a PDF
... lines in classical T-Tauri stars (Appenzeller et al. 1984; Edwards et al. 1987) has long be taken as evidence of opaque circumstellar disks: disks which occlude the receding component of the stellar wind or outflow, allowing only the blueshifted emission to be observed. There has been some controver ...
... lines in classical T-Tauri stars (Appenzeller et al. 1984; Edwards et al. 1987) has long be taken as evidence of opaque circumstellar disks: disks which occlude the receding component of the stellar wind or outflow, allowing only the blueshifted emission to be observed. There has been some controver ...
FIELD GALAXIES AND THEIR AGNs: NATURE VERSUS
... Most likely scenario today is the formation of SMBH seeds from the accretion of low angular momentum gas in a dark matter halo (Koushiappas et al. 2004, Bromm and Loeb 2003, 2004). These seeds would form as supermassive stellar remnants, with the initial masses of 104 –106 M¯ from the direct collaps ...
... Most likely scenario today is the formation of SMBH seeds from the accretion of low angular momentum gas in a dark matter halo (Koushiappas et al. 2004, Bromm and Loeb 2003, 2004). These seeds would form as supermassive stellar remnants, with the initial masses of 104 –106 M¯ from the direct collaps ...
astro-ph/9808039 PDF
... to make the FUV fluxes too high by a factor of ∼ 2. The corrected rocket calibration is consistent with that for an earlier flight using the same detector (Smith et al. 1992). Many of the arguments of Paper I relied on the Hα/FUV flux ratio. Coincidentally, the FUV calibration error was nearly cance ...
... to make the FUV fluxes too high by a factor of ∼ 2. The corrected rocket calibration is consistent with that for an earlier flight using the same detector (Smith et al. 1992). Many of the arguments of Paper I relied on the Hα/FUV flux ratio. Coincidentally, the FUV calibration error was nearly cance ...
Intraday Variability in Quasars and BL LAC Objects
... scattering of the relativistic electrons with the low-energyphotons emitted by them wouldquickly lead to catastrophic cooling and unobserved high X-ray fluxes (Hoyle et al 1966) unless the objects were close by. This led to the suggestion of bulk relativistic motion(Rees 1966, Woltjer 1966). VLBIobs ...
... scattering of the relativistic electrons with the low-energyphotons emitted by them wouldquickly lead to catastrophic cooling and unobserved high X-ray fluxes (Hoyle et al 1966) unless the objects were close by. This led to the suggestion of bulk relativistic motion(Rees 1966, Woltjer 1966). VLBIobs ...
First Results from the WISE Enhanced Resolution Galaxy Atlas
... Following closely in succession to the AKARI all-sky survey (Murakami et al. 2006), the Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010) is the latest generation infrared space telescope. As with AKARI but unlike Spitzer, it was designed and implemented to map the entire sky. It was th ...
... Following closely in succession to the AKARI all-sky survey (Murakami et al. 2006), the Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010) is the latest generation infrared space telescope. As with AKARI but unlike Spitzer, it was designed and implemented to map the entire sky. It was th ...
Massive Star Formation - Max-Planck
... that the initial conditions for intermediate and massive star formation are gravitationally bound cores, scaled up in mass from the low-mass examples known to form low-mass stars. Different versions of these models invoke varying properties of the cores, including their expected densities, density p ...
... that the initial conditions for intermediate and massive star formation are gravitationally bound cores, scaled up in mass from the low-mass examples known to form low-mass stars. Different versions of these models invoke varying properties of the cores, including their expected densities, density p ...
Munshi_washington_0250E_12611
... mass ratio as a function of halo mass for a new sample of simulated field galaxies using fully cosmological, LCDM, high resolution SPH + N-Body simulations carried to the present time. I find there is extremely good agreement between the simulations and predictions from the statistical Halo Occupati ...
... mass ratio as a function of halo mass for a new sample of simulated field galaxies using fully cosmological, LCDM, high resolution SPH + N-Body simulations carried to the present time. I find there is extremely good agreement between the simulations and predictions from the statistical Halo Occupati ...
pptx
... TMT Era –Origin of GRB– ・GRB production requires low-metallicity environment suggested by theoretical simulations (MacFadyen& Woosley 1999; Woosley & Heger 2006; Yoon et al. 2006; Niino et al. 2009) ・Many GRB hosts are less massive and low metallicity, But… ・High metallicity environment of dark GRB ...
... TMT Era –Origin of GRB– ・GRB production requires low-metallicity environment suggested by theoretical simulations (MacFadyen& Woosley 1999; Woosley & Heger 2006; Yoon et al. 2006; Niino et al. 2009) ・Many GRB hosts are less massive and low metallicity, But… ・High metallicity environment of dark GRB ...
Mapping the Pathways of Galaxy Transformation Across Time and
... outcomes from the IMACS Cluster-Building Survey: our finding that most z∼0.5 poststarbursts are rejuvenated passive galaxies, and a simple model positing that every galaxy has a lognormal SFH whose parameters are set at birth. Both studies reinterpreted key metrics of galaxy evolution typically seen ...
... outcomes from the IMACS Cluster-Building Survey: our finding that most z∼0.5 poststarbursts are rejuvenated passive galaxies, and a simple model positing that every galaxy has a lognormal SFH whose parameters are set at birth. Both studies reinterpreted key metrics of galaxy evolution typically seen ...
The redMaPPer Galaxy Cluster Catalog From DES Science
... cosmological constraints (The Dark Energy Survey Collaboration et al. 2015). Therefore, the runs were performed on regions with very tight tolerance for image quality, and were restricted to the largest contiguous region (SPT-E) as well as supplementary runs on the SN fields. These regions comprise ...
... cosmological constraints (The Dark Energy Survey Collaboration et al. 2015). Therefore, the runs were performed on regions with very tight tolerance for image quality, and were restricted to the largest contiguous region (SPT-E) as well as supplementary runs on the SN fields. These regions comprise ...
Lecture 3
... Other Galaxies at z=3 • Lyman Break Galaxies are selected to be UVbright Strongly star forming Not too much dust extinction • They can’t account for all the material at z=3, so other techniques must fill in the gaps: – DLAs – Narrow Band Surveys – Sub-millimeter or Infrared selection ...
... Other Galaxies at z=3 • Lyman Break Galaxies are selected to be UVbright Strongly star forming Not too much dust extinction • They can’t account for all the material at z=3, so other techniques must fill in the gaps: – DLAs – Narrow Band Surveys – Sub-millimeter or Infrared selection ...
Astrophysical X-ray source
Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.