The Physical Origins of The Morphology
... structure and gas content of a galaxy. Tidal interactions with other galaxies or the potential of a large halo can strip an in-falling galaxy from gas, and reduce the stellar disk as well (Moore et al. 1996). There are two reasons why it is surprisingly difficult to interpret the MDR, constrain its ...
... structure and gas content of a galaxy. Tidal interactions with other galaxies or the potential of a large halo can strip an in-falling galaxy from gas, and reduce the stellar disk as well (Moore et al. 1996). There are two reasons why it is surprisingly difficult to interpret the MDR, constrain its ...
Infrared identification of high-mass X
... Methods. After previous photometric and spectroscopic observing campaigns in the optical and near-infrared, new photometry and spectroscopy was performed in the near-infrared with the SofI instrument on the ESO/NTT telescope in 2008 and 2010 on a sample of INTEGRAL sources. These observations, and s ...
... Methods. After previous photometric and spectroscopic observing campaigns in the optical and near-infrared, new photometry and spectroscopy was performed in the near-infrared with the SofI instrument on the ESO/NTT telescope in 2008 and 2010 on a sample of INTEGRAL sources. These observations, and s ...
THE COBE DIRBE POINT SOURCE CATALOG
... AFGL survey. Thus, DIRBE covers the 85% of the sky not surveyed by MSX to a sensitivity per scan at 4 m similar to that of MSX. Another DIRBE advantage is its excellent temporal coverage, which permits a careful investigation of possible infrared variability of stars. A typical location on the sky ...
... AFGL survey. Thus, DIRBE covers the 85% of the sky not surveyed by MSX to a sensitivity per scan at 4 m similar to that of MSX. Another DIRBE advantage is its excellent temporal coverage, which permits a careful investigation of possible infrared variability of stars. A typical location on the sky ...
Chapter 6 in the LSST Science Book
... are the only sufficiently complex systems (for the purpose of understanding galaxy assembly) where the spatial perspective allows us to know where in the galaxy the stars we are examining lie, while at the same time being close enough for us to examine and parse its component stellar populations in ...
... are the only sufficiently complex systems (for the purpose of understanding galaxy assembly) where the spatial perspective allows us to know where in the galaxy the stars we are examining lie, while at the same time being close enough for us to examine and parse its component stellar populations in ...
MOLECULAR OUTFLOWS AND A MID
... Figure 4 illustrating the velocity structure in the dense gas show that blueshifted emission extends from the UC H ii region to the west. A possible redshifted outflow lobe east of the UC H ii may be visible in 13CO emission in the top right panel in Figure 4 although the identification is not defin ...
... Figure 4 illustrating the velocity structure in the dense gas show that blueshifted emission extends from the UC H ii region to the west. A possible redshifted outflow lobe east of the UC H ii may be visible in 13CO emission in the top right panel in Figure 4 although the identification is not defin ...
the Ëg infrared search for extraterrestrial civilizations with large
... photometry. They used eight apertures from 5.5′′ to 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 elli ...
... photometry. They used eight apertures from 5.5′′ to 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 elli ...
Annual Report 2014 - Max Planck Institute for Astrophysics
... tific necessity being the main criterion for decisions. RZG and MPA coordinate their activities and development plans through regular meetings to ensure continuity in the working environment experienced by the users. The most important resources provided by the RZG are parallel supercomputers, PByte ...
... tific necessity being the main criterion for decisions. RZG and MPA coordinate their activities and development plans through regular meetings to ensure continuity in the working environment experienced by the users. The most important resources provided by the RZG are parallel supercomputers, PByte ...
paper - Harvard-Smithsonian Center for Astrophysics
... perform this analysis using the RADEX package (van der Tak et al. 2007), which calculates expected line intensities for a given column density of SO2 , kinetic temperature (Tkin ), and volume density of H2 . For each source, we assume spatially homogeneous kinetic temperature and volume density. The ...
... perform this analysis using the RADEX package (van der Tak et al. 2007), which calculates expected line intensities for a given column density of SO2 , kinetic temperature (Tkin ), and volume density of H2 . For each source, we assume spatially homogeneous kinetic temperature and volume density. The ...
radioactive 26a1 in the galaxy: observations versus theory
... target for the HEAO-3 detectors. Moreover it was pointed out that, because of its long mean life, 26A1 would have enough time to be thermalised in the interstellar medium; therefore, it would de-excite essentially at rest and emit a narrow line, making easier its detection and identification with su ...
... target for the HEAO-3 detectors. Moreover it was pointed out that, because of its long mean life, 26A1 would have enough time to be thermalised in the interstellar medium; therefore, it would de-excite essentially at rest and emit a narrow line, making easier its detection and identification with su ...
Ch 26
... observer sees only one color, because only one color travels at the proper angle to reach the observer. The observer sees the full spectrum in the rainbow because each color originates from water droplets that lie at different elevation angles. As shown in Figure 26.21, the sun must be located behin ...
... observer sees only one color, because only one color travels at the proper angle to reach the observer. The observer sees the full spectrum in the rainbow because each color originates from water droplets that lie at different elevation angles. As shown in Figure 26.21, the sun must be located behin ...
SPT 0538−50: PHYSICAL CONDITIONS IN THE ISM OF A STRONGLY... GALAXY AT Z=2.8
... The advent of millimeter/submillimeter (submm) instruments capable of surveying large areas of sky, including Herschel -SPIRE (Pilbratt et al. 2010; Griffin et al. 2010) and the South Pole Telescope (SPT; Carlstrom et al. 2011), has opened new vistas for the study of these submm bright systems (Viei ...
... The advent of millimeter/submillimeter (submm) instruments capable of surveying large areas of sky, including Herschel -SPIRE (Pilbratt et al. 2010; Griffin et al. 2010) and the South Pole Telescope (SPT; Carlstrom et al. 2011), has opened new vistas for the study of these submm bright systems (Viei ...
Oscillatory Motion
... a. The total energy is proportional to the square of the amplitude of the motion. b. The acceleration is maximum at the equilibrium position c. The kinetic energy is minimum at the equilibrium position d. The speed decreases as the particle moves toward the equilibrium position 3. The period of SHM ...
... a. The total energy is proportional to the square of the amplitude of the motion. b. The acceleration is maximum at the equilibrium position c. The kinetic energy is minimum at the equilibrium position d. The speed decreases as the particle moves toward the equilibrium position 3. The period of SHM ...
An overview of the photometric events, trends and
... JHK peak amplitudes are smaller. We suspect that this has a consequence for the height of the egress-maximum, which tends to be smaller as well. The behaviour in L during the 1997.9 and 1992.4 peaks and at other wavelengths is even more peculiar than in 2003.5 and 1981.3. Apparently, the maximum is ...
... JHK peak amplitudes are smaller. We suspect that this has a consequence for the height of the egress-maximum, which tends to be smaller as well. The behaviour in L during the 1997.9 and 1992.4 peaks and at other wavelengths is even more peculiar than in 2003.5 and 1981.3. Apparently, the maximum is ...
Physics Class X for SA-II 2015-16
... 1. Find the focal length of a convex mirror of radius of curvature 1m. 2. Focal length of a convex mirror is 50 cm. What is its radius of curvature? 3. Radius of curvature of a concave mirror is 25 cm. What is its focal length? 4. A concave mirror produces 10 cm long image of an object of height of ...
... 1. Find the focal length of a convex mirror of radius of curvature 1m. 2. Focal length of a convex mirror is 50 cm. What is its radius of curvature? 3. Radius of curvature of a concave mirror is 25 cm. What is its focal length? 4. A concave mirror produces 10 cm long image of an object of height of ...
physics - My Study materials – Kumar
... 1. Find the focal length of a convex mirror of radius of curvature 1m. 2. Focal length of a convex mirror is 50 cm. What is its radius of curvature? 3. Radius of curvature of a concave mirror is 25 cm. What is its focal length? 4. A concave mirror produces 10 cm long image of an object of height of ...
... 1. Find the focal length of a convex mirror of radius of curvature 1m. 2. Focal length of a convex mirror is 50 cm. What is its radius of curvature? 3. Radius of curvature of a concave mirror is 25 cm. What is its focal length? 4. A concave mirror produces 10 cm long image of an object of height of ...
of refraction - Mrs. Brenner`s Biology
... Explain why, if you are standing by the side of a pool, you cannot see a swimmer who is underwater near the surface, and on the opposite side of the pool. A. This is because the light from the swimmer’s body refracts along the boundary of air and water. B. This is because the light from the swimmer’ ...
... Explain why, if you are standing by the side of a pool, you cannot see a swimmer who is underwater near the surface, and on the opposite side of the pool. A. This is because the light from the swimmer’s body refracts along the boundary of air and water. B. This is because the light from the swimmer’ ...
distribution and properties of a sample of massive young stars
... of our campaign as without these we cannot accurately calculate source luminosities, and thus, distinguish between nearby low and intermediate-mass YSOs from the more generally more distance MYSOs. As mentioned in the introduction, kinematic distance ambiguities affect a large proportion of our samp ...
... of our campaign as without these we cannot accurately calculate source luminosities, and thus, distinguish between nearby low and intermediate-mass YSOs from the more generally more distance MYSOs. As mentioned in the introduction, kinematic distance ambiguities affect a large proportion of our samp ...
Galaxies
... •Gravitational Lensing: a massive galaxy deflects light rays like a lens so that an observer sees multiple distorted images of a more distant galaxy •Gravitational lensing is predicted by Einstein’s general theory of relativity: space is curved due to gravity ...
... •Gravitational Lensing: a massive galaxy deflects light rays like a lens so that an observer sees multiple distorted images of a more distant galaxy •Gravitational lensing is predicted by Einstein’s general theory of relativity: space is curved due to gravity ...
ongoing massive star formation in the bulge of m511 hjglm lamers,2
... best model is found for a relative orbit that is almost in the plane of M51, for a mass ratio of NGC 5194/5195 ^ 2, a pericenter distance of 17È20 kpc, and a time since pericenter of 2.5 ] 108 yr \ t \ 4 ] 108 yr (Barnes 1998). The NGC 5194/5195 system is ideally suited for the study of triggered st ...
... best model is found for a relative orbit that is almost in the plane of M51, for a mass ratio of NGC 5194/5195 ^ 2, a pericenter distance of 17È20 kpc, and a time since pericenter of 2.5 ] 108 yr \ t \ 4 ] 108 yr (Barnes 1998). The NGC 5194/5195 system is ideally suited for the study of triggered st ...
Example
... Example: What is the vergence of a light source located infinitely far away? Wave fronts become progressively flatter as the distance from their center of curvature increases. Therefore, as the radius of the wave front becomes infinitely long, the vergence approaches zero. Think of it this way: sinc ...
... Example: What is the vergence of a light source located infinitely far away? Wave fronts become progressively flatter as the distance from their center of curvature increases. Therefore, as the radius of the wave front becomes infinitely long, the vergence approaches zero. Think of it this way: sinc ...
Light and Image Formation
... How can the law of reflection help us to explain how an image is formed in a plane mirror? What happens to the light rays that are scattered from your nose? Tracing these rays from their origin at the nose and following them through reflection from the mirror using the law of reflection shows what h ...
... How can the law of reflection help us to explain how an image is formed in a plane mirror? What happens to the light rays that are scattered from your nose? Tracing these rays from their origin at the nose and following them through reflection from the mirror using the law of reflection shows what h ...
25 geometric optics - Wright State University
... We already know that visible light is the type of electromagnetic waves to which our eyes respond. That knowledge still leaves many questions regarding the nature of light and vision. What is color, and how do our eyes detect it? Why do diamonds sparkle? How does light travel? How do lenses and mirr ...
... We already know that visible light is the type of electromagnetic waves to which our eyes respond. That knowledge still leaves many questions regarding the nature of light and vision. What is color, and how do our eyes detect it? Why do diamonds sparkle? How does light travel? How do lenses and mirr ...
Statistical survey of widely spread out solar electron events
... By the end of the 1990s, events with wider spreads were clas- spacecraft. EUV observations by SDO/AIA (Lemen et al. 2012) sified as gradual, not flare-associated events. These proton-rich and the coronograph LASCO (Brueckner et al. 1995) on board events were associated with CME-driven shocks that bu ...
... By the end of the 1990s, events with wider spreads were clas- spacecraft. EUV observations by SDO/AIA (Lemen et al. 2012) sified as gradual, not flare-associated events. These proton-rich and the coronograph LASCO (Brueckner et al. 1995) on board events were associated with CME-driven shocks that bu ...
Research paper
... determined from a trace-back of the H2 proper motions (Bally et al. 2011). Most streamers are barely resolved with widths ranging from 100 to 200 . They exhibit low-amplitude intensity variations indicating clumpy structure and arcsecond-scale wiggles. The line-widths of the streamers range from sli ...
... determined from a trace-back of the H2 proper motions (Bally et al. 2011). Most streamers are barely resolved with widths ranging from 100 to 200 . They exhibit low-amplitude intensity variations indicating clumpy structure and arcsecond-scale wiggles. The line-widths of the streamers range from sli ...
Gravitational microlensing
Gravitational microlensing is an astronomical phenomenon due to the gravitational lens effect. It can be used to detect objects that range from the mass of a planet to the mass of a star, regardless of the light they emit. Typically, astronomers can only detect bright objects that emit much light (stars) or large objects that block background light (clouds of gas and dust). These objects make up only a tiny portion of the mass of a galaxy. Microlensing allows the study of objects that emit little or no light.When a distant star or quasar gets sufficiently aligned with a massive compact foreground object, the bending of light due to its gravitational field, as discussed by Einstein in 1915, leads to two distorted unresolved images resulting in an observable magnification. The time-scale of the transient brightening depends on the mass of the foreground object as well as on the relative proper motion between the background 'source' and the foreground 'lens' object.Since microlensing observations do not rely on radiation received from the lens object, this effect therefore allows astronomers to study massive objects no matter how faint. It is thus an ideal technique to study the galactic population of such faint or dark objects as brown dwarfs, red dwarfs, planets, white dwarfs, neutron stars, black holes, andMassive Compact Halo Objects. Moreover, the microlensing effect is wavelength-independent, allowing study of source objects that emit any kind of electromagnetic radiation.Microlensing by an isolated object was first detected in 1989. Since then, microlensing has been used to constrain the nature of the dark matter, detect extrasolar planets, study limb darkening in distant stars, constrain the binary star population, and constrain the structure of the Milky Way's disk. Microlensing has also been proposed as a means to find dark objects like brown dwarfs and black holes, study starspots, measure stellar rotation, and probe quasars including their accretion disks.