Radial distribution of gas and dust in spiral galaxies - ORCA
... for references) and it will be another pice of the puzzle to be explained by the various proposed models. The rising profile in the inner part of M 100 is related to the more prominent bulge, bar, or inner-disk component, which is discussed in more detail in Sauvage et al. (2010). To investigate the ...
... for references) and it will be another pice of the puzzle to be explained by the various proposed models. The rising profile in the inner part of M 100 is related to the more prominent bulge, bar, or inner-disk component, which is discussed in more detail in Sauvage et al. (2010). To investigate the ...
AMUSE-Virgo AGN Multi-wavelength Survey
... - separate hot gas from low mass X-ray binaries (LMXBs) - search for point like nuclear X-ray source ...
... - separate hot gas from low mass X-ray binaries (LMXBs) - search for point like nuclear X-ray source ...
Astro 3303 - Cornell Astronomy
... • The sky is dark at night. • Hubble’s Law & the expansion of the Universe (Edwin Hubble: 1927) • If the universe is finite in space and time and is expanding, it must have been smaller in the past. • The Cosmic Microwave Background (CMB) Radiation (Arno Penzias and Robert Wilson: 1965) • Thermal sp ...
... • The sky is dark at night. • Hubble’s Law & the expansion of the Universe (Edwin Hubble: 1927) • If the universe is finite in space and time and is expanding, it must have been smaller in the past. • The Cosmic Microwave Background (CMB) Radiation (Arno Penzias and Robert Wilson: 1965) • Thermal sp ...
Revisiting the Hubble sequence in the SDSS DR7
... For morphological classification, the training sample is typically built using a visually classified subsample. We therefore used [2] classification as the training sample. In their paper, they provide a visual classification of 2253 SDSS galaxies brighter than mr = 16 (compared to the full DR7 samp ...
... For morphological classification, the training sample is typically built using a visually classified subsample. We therefore used [2] classification as the training sample. In their paper, they provide a visual classification of 2253 SDSS galaxies brighter than mr = 16 (compared to the full DR7 samp ...
swire
... SIRTF is ideally designed for detailed study of the history of star formation MIPS is optimized for star-forming galaxies and AGN IRAC is optimized for old and/or reddened stellar populations ...
... SIRTF is ideally designed for detailed study of the history of star formation MIPS is optimized for star-forming galaxies and AGN IRAC is optimized for old and/or reddened stellar populations ...
The density of very massive evolved galaxies to z≃ 1.7
... of the seven galaxies are shown. The spectra drops very rapidly at ∼0.9–1 µm concurrent with the 4000 Å break placing the galaxies at z > 1.3 and suggesting an early-type spectral nature. We searched for the best-fitting template by comparing the observed spectral energy distribution (SED) of each g ...
... of the seven galaxies are shown. The spectra drops very rapidly at ∼0.9–1 µm concurrent with the 4000 Å break placing the galaxies at z > 1.3 and suggesting an early-type spectral nature. We searched for the best-fitting template by comparing the observed spectral energy distribution (SED) of each g ...
Linking Gas Fractions to Bimodalities in Galaxy Properties
... calibration given here could significantly underestimate actual gas-to-stellar mass ratios if stellar M/L ratios are much lower than assumed and/or molecular gas corrections are large (a controversial topic; see Casoli et al. 1998; Boselli et al. 2002). The M/L ratios used here are roughly consisten ...
... calibration given here could significantly underestimate actual gas-to-stellar mass ratios if stellar M/L ratios are much lower than assumed and/or molecular gas corrections are large (a controversial topic; see Casoli et al. 1998; Boselli et al. 2002). The M/L ratios used here are roughly consisten ...
Chapter 17
... the gravity due to a massive body between a distant object and the viewer bends light from the distant object and causes it to be seen as two or more objects. 3. Since 1979 many examples of gravitational lensing have been found. 4. When the alignment between the viewer, distant object and massive bo ...
... the gravity due to a massive body between a distant object and the viewer bends light from the distant object and causes it to be seen as two or more objects. 3. Since 1979 many examples of gravitational lensing have been found. 4. When the alignment between the viewer, distant object and massive bo ...
Cosmic Hide and Seek: the Search for the Missing Mass
... matter gravitationally--they pass right through ordinary matter. Since each WIMP has only a small amount of mass, there needs to be a large number of them to make up the bulk of the missing matter. That means that millions of WIMPs are passing through ordinary matter--the Earth and you and me-every ...
... matter gravitationally--they pass right through ordinary matter. Since each WIMP has only a small amount of mass, there needs to be a large number of them to make up the bulk of the missing matter. That means that millions of WIMPs are passing through ordinary matter--the Earth and you and me-every ...
Weak gravitational lensing
While the presence of any mass bends the path of light passing near it, this effect rarely produces the giant arcs and multiple images associated with strong gravitational lensing. Most lines of sight in the universe are thoroughly in the weak lensing regime, in which the deflection is impossible to detect in a single background source. However, even in these cases, the presence of the foreground mass can be detected, by way of a systematic alignment of background sources around the lensing mass. Weak gravitational lensing is thus an intrinsically statistical measurement, but it provides a way to measure the masses of astronomical objects without requiring assumptions about their composition or dynamical state.