Hypothesis of dark matter and dark energy with negative
... From the observance of the HSS team and SCP team in 1998, they gained the mass density of the negative(HSS: ΩM = −0.38(±0.22), SCP: ΩM = −0.4(±0.1) ), using field equations which do not have the cosmological constant. In they thought, the quantity of the mass couldn’t be a negative value, so the val ...
... From the observance of the HSS team and SCP team in 1998, they gained the mass density of the negative(HSS: ΩM = −0.38(±0.22), SCP: ΩM = −0.4(±0.1) ), using field equations which do not have the cosmological constant. In they thought, the quantity of the mass couldn’t be a negative value, so the val ...
Annual Report 2012
... a revolutionary new sub-millimetre spectrograph. The heart of the instrument is based on developments in nanotechnology that allow ultra-sensitive detectors to be created. In addition, the ‘technologiestichting’ STW approved funding for the transfer of astronomical technology to other sciences. Base ...
... a revolutionary new sub-millimetre spectrograph. The heart of the instrument is based on developments in nanotechnology that allow ultra-sensitive detectors to be created. In addition, the ‘technologiestichting’ STW approved funding for the transfer of astronomical technology to other sciences. Base ...
Classification of extremely red objects in the Hubble Ultra Deep Field
... law introduced by Calzetti et al. 2000) in turn. Figure 3 in Kong et al. (2008a) shows a comparison of the photometric redshifts from our SED fitting method with their spectroscopic redshifts for 33 galaxies in the UDF. From that figure, we found that our photometric redshifts fit the spectroscopic ...
... law introduced by Calzetti et al. 2000) in turn. Figure 3 in Kong et al. (2008a) shows a comparison of the photometric redshifts from our SED fitting method with their spectroscopic redshifts for 33 galaxies in the UDF. From that figure, we found that our photometric redshifts fit the spectroscopic ...
Effective Operators for Dark Matter Detection
... behind Dark Matter (DM) modeling in relation with detection experiments. In fact, while model independent analyses should in principle allow to investigate the DM problem in its full generality, strong assumptions are usually made in order to reduce it to a form that can be tackled with our limited ...
... behind Dark Matter (DM) modeling in relation with detection experiments. In fact, while model independent analyses should in principle allow to investigate the DM problem in its full generality, strong assumptions are usually made in order to reduce it to a form that can be tackled with our limited ...
The Westerbork Hydrogen Accretion in LOcal GAlaxieS \(HALOGAS
... Hubble types between Sa and Sd; (ii) because the WSRT is an east-west interferometer, we require that the source declination δ > +25◦ to ensure that the synthesized beamsize is 30 ; (iii) we only select nearby galaxies with distance D < 11 Mpc, in order to observe at adequate physical resolution ...
... Hubble types between Sa and Sd; (ii) because the WSRT is an east-west interferometer, we require that the source declination δ > +25◦ to ensure that the synthesized beamsize is 30 ; (iii) we only select nearby galaxies with distance D < 11 Mpc, in order to observe at adequate physical resolution ...
Giant Molecular Clouds in Local Group Galaxies
... Wilson, 1994) using the OVRO and BIMA interferometers. Her efforts were hampered by small survey areas in a few galaxies, so general conclusions could only be made by extrapolation. Numerous other authors subsequently studied one or a few extragalactic GMCs, both in the Local Group and beyond. An ex ...
... Wilson, 1994) using the OVRO and BIMA interferometers. Her efforts were hampered by small survey areas in a few galaxies, so general conclusions could only be made by extrapolation. Numerous other authors subsequently studied one or a few extragalactic GMCs, both in the Local Group and beyond. An ex ...
THE LUMINOSITY FUNCTION OF X
... matured SMBH population with sub-Eddington accretion rates. The former scenario has been substantiated by Barger et al. (2005) based on the optical luminosities of the galaxies hosting X-rayY selected AGNs and by Heckman et al. (2004) using type 2 AGNs from the SDSS with the [O iii] emission line lu ...
... matured SMBH population with sub-Eddington accretion rates. The former scenario has been substantiated by Barger et al. (2005) based on the optical luminosities of the galaxies hosting X-rayY selected AGNs and by Heckman et al. (2004) using type 2 AGNs from the SDSS with the [O iii] emission line lu ...
Grand Design and Flocculent Spirals in the Spitzer Survey of Stellar
... that later Hubble types have larger relative bar torques because the bulges are weaker. Combes & Elmegreen (1993) and Athanassoula & Misiriotis (2002) simulated flat and exponential bars by varying the inner rotation curve or halo concentration. Flat bars tend to occur in galaxies with sharply risin ...
... that later Hubble types have larger relative bar torques because the bulges are weaker. Combes & Elmegreen (1993) and Athanassoula & Misiriotis (2002) simulated flat and exponential bars by varying the inner rotation curve or halo concentration. Flat bars tend to occur in galaxies with sharply risin ...
Galaxy Evolution Over the Past Eleven Billion Years: Mergers and
... only visible at near-infrared wavelengths, was discovered. They were previously overlooked, since they are invisible even in the deepest Hubble Space Telescope (HST) optical surveys. Their stellar populations, characterized using deep near-infrared photometric and spectroscopic observations, reveal ...
... only visible at near-infrared wavelengths, was discovered. They were previously overlooked, since they are invisible even in the deepest Hubble Space Telescope (HST) optical surveys. Their stellar populations, characterized using deep near-infrared photometric and spectroscopic observations, reveal ...
Galaxy And Mass Assembly (GAMA): Gas Fuelling of Spiral Galaxies
... Thus, regardless of the exact underlying cause, 1012 M represents a critical mass in understanding environment dependent galaxy evolution and gas-fuelling in particular. In addition to centrals, the hierarchical formation of large-scale structure expected for a ΛCDM universe gives rise to a populat ...
... Thus, regardless of the exact underlying cause, 1012 M represents a critical mass in understanding environment dependent galaxy evolution and gas-fuelling in particular. In addition to centrals, the hierarchical formation of large-scale structure expected for a ΛCDM universe gives rise to a populat ...
Modeling Spatially and Spectrally Resolved Observations to
... was a joy to write this thesis with the assistance of Jean Collins, Donna Adams, Peg Herlihy, Robb Schofield, Peg Hedstrom, Nina Zonnevylle, and Uma Mirani, who run the Department of Astronomy and the ITC so smoothly. While writing this thesis, I was thrilled to participate in a number of activities ...
... was a joy to write this thesis with the assistance of Jean Collins, Donna Adams, Peg Herlihy, Robb Schofield, Peg Hedstrom, Nina Zonnevylle, and Uma Mirani, who run the Department of Astronomy and the ITC so smoothly. While writing this thesis, I was thrilled to participate in a number of activities ...
the Ëg infrared search for extraterrestrial civilizations with large
... 24.75′′ in W1-W3 and 11′′ to 49.5’′′ in W48 . They provide these in the form of parameters named W#MAG 1 for the first aperture of 5.5′′ in W1 through W3 and 11′′ in W4, W#MAG 2 for the 2nd aperture, W#MAG 3 for the 3rd aperture and so on. The elliptical aperture measurements, referred to as W#GMAG ...
... 24.75′′ in W1-W3 and 11′′ to 49.5’′′ in W48 . They provide these in the form of parameters named W#MAG 1 for the first aperture of 5.5′′ in W1 through W3 and 11′′ in W4, W#MAG 2 for the 2nd aperture, W#MAG 3 for the 3rd aperture and so on. The elliptical aperture measurements, referred to as W#GMAG ...
Three Binary Millisecond Pulsars in NGC 6266
... pulsar, whereas no new cluster joined the list in the following 6 years. More recently, pulsars have been detected in a further three GCs (Ransom et al. 2003; Ransom 2003;8 Jacoby 20039), bringing the current total to 73 pulsars in 22 clusters.10 ...
... pulsar, whereas no new cluster joined the list in the following 6 years. More recently, pulsars have been detected in a further three GCs (Ransom et al. 2003; Ransom 2003;8 Jacoby 20039), bringing the current total to 73 pulsars in 22 clusters.10 ...
A numerical study of recent tidal interactions between dwarf galaxies
... - Dwarf ellipticals (dE): These dwarf galaxies don’t have a lot of gas left and barely form any stars at the moment. They are mostly found in clusters of galaxies. Their magnitudes in the blue band are in the interval: -18 < MB < -14. As can be seen, this is not completely in agreement with the defi ...
... - Dwarf ellipticals (dE): These dwarf galaxies don’t have a lot of gas left and barely form any stars at the moment. They are mostly found in clusters of galaxies. Their magnitudes in the blue band are in the interval: -18 < MB < -14. As can be seen, this is not completely in agreement with the defi ...
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.