from z=0 to z=1
... < 10^10.2 L_sun, the IR/UV ratio does not show any evolution from z=0 to z=0.6. • for brighter galaxies of L_FUV > 10^10.2 L_sun, there seems to be a negative evolution in the sense that z=0.6 galaxies have lower ratios. ...
... < 10^10.2 L_sun, the IR/UV ratio does not show any evolution from z=0 to z=0.6. • for brighter galaxies of L_FUV > 10^10.2 L_sun, there seems to be a negative evolution in the sense that z=0.6 galaxies have lower ratios. ...
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 ...
mg_colloq - University of Massachusetts Amherst
... – Dynamical properties being explored; certainly consistent with being massive, compact spheroids (Onodera et al. 2012; van Dokkum et al. 2011) – Some suggest that they include a significant (25-50%) fraction of compact disks (Bruce et al. 2012) or even that they are mostly compact disks (van der We ...
... – Dynamical properties being explored; certainly consistent with being massive, compact spheroids (Onodera et al. 2012; van Dokkum et al. 2011) – Some suggest that they include a significant (25-50%) fraction of compact disks (Bruce et al. 2012) or even that they are mostly compact disks (van der We ...
ROTATION CURVES OF HIGH-LUMINOSITY SPIRAL GALAXIES
... values as discrepant as A = +26, B = -37 (Asteriadis, 1977). At the la level, A = -B is not excluded, i.e., the rotation curve could be flat in the solar vicinity. More likely, there is a negative velocity gra dient at the position of the sun. Because spiral arms show positive velocity gradients, t ...
... values as discrepant as A = +26, B = -37 (Asteriadis, 1977). At the la level, A = -B is not excluded, i.e., the rotation curve could be flat in the solar vicinity. More likely, there is a negative velocity gra dient at the position of the sun. Because spiral arms show positive velocity gradients, t ...
From Cosmic Birth to Living Earth - Association of Universities for
... towards constructing a general purpose, long-life, space-based observatory that is capable of finding planets showing signs of life. Such an observatory would be able to survey hundreds of planetary systems and detect dozens of Earth-like planets in the habitable zones around their stars. It would a ...
... towards constructing a general purpose, long-life, space-based observatory that is capable of finding planets showing signs of life. Such an observatory would be able to survey hundreds of planetary systems and detect dozens of Earth-like planets in the habitable zones around their stars. It would a ...
X-ray observations of the hot CGM of nearby disk galaxies
... Q2: Does the X-ray emission trace the accretion or feedback of the galaxies? • The observed X-ray emission is too concentrated toward the disks, while the predicted scale of the X-ray emitting CGM is substantially greater. • The emission is observed from low-mass galaxies for which little hot CGM ...
... Q2: Does the X-ray emission trace the accretion or feedback of the galaxies? • The observed X-ray emission is too concentrated toward the disks, while the predicted scale of the X-ray emitting CGM is substantially greater. • The emission is observed from low-mass galaxies for which little hot CGM ...
Power Point
... Radio Continuum vs. [OII] Star Formation Rate Average 87 red [OII] emission galaxies 81 blue [OII] emission galaxies line from Bell 2003 ...
... Radio Continuum vs. [OII] Star Formation Rate Average 87 red [OII] emission galaxies 81 blue [OII] emission galaxies line from Bell 2003 ...
Lecture 15
... We see the disk of our galaxy (i.e. the Milky Way) We know that the universe doesn’t look exactly the same from every galaxy: For example, the the universe may look very different to an alien race in the middle of a galaxy cluster. How do we think about this? ...
... We see the disk of our galaxy (i.e. the Milky Way) We know that the universe doesn’t look exactly the same from every galaxy: For example, the the universe may look very different to an alien race in the middle of a galaxy cluster. How do we think about this? ...
AST 346, Galaxies, Part 6
... older than the disk. Alternatively, they could have formed later as gas spirals to center. Some z > 3 galaxies are apparently building bulges, but a rare case, NGC 7331, has some bulge stars orbiting opposite to the bulge itself, J.M. Lattimer ...
... older than the disk. Alternatively, they could have formed later as gas spirals to center. Some z > 3 galaxies are apparently building bulges, but a rare case, NGC 7331, has some bulge stars orbiting opposite to the bulge itself, J.M. Lattimer ...
Galaxy Sorting
... galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Interstellar ...
... galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Interstellar ...
Embryology of Elliptical Galaxies
... are modelled with 10243 fixed Cartesian grids for a proto-galaxy with the total mass of 1011 M. The total mass of gaseous matter is assumed to be 1.3×1010 M initially. Following a standard scenario of the ΛCDM universe (ΩM = 0.3, ΩΛ = 0.7, Ωb = 0.04, and a Hubble constant of H0 = 70 km s-1 Mpc-1), ...
... are modelled with 10243 fixed Cartesian grids for a proto-galaxy with the total mass of 1011 M. The total mass of gaseous matter is assumed to be 1.3×1010 M initially. Following a standard scenario of the ΛCDM universe (ΩM = 0.3, ΩΛ = 0.7, Ωb = 0.04, and a Hubble constant of H0 = 70 km s-1 Mpc-1), ...
galaxies2_3_complete
... Galaxies are not slowed down enough to become a bound pair. Galaxies separate, but their disks are ‘dishevelled’: stars acquire random motions, causing disks to ‘puff up’. ...
... Galaxies are not slowed down enough to become a bound pair. Galaxies separate, but their disks are ‘dishevelled’: stars acquire random motions, causing disks to ‘puff up’. ...
3D Tour of the Universe Template
... o) Zoom out, go around past Virgo for Antennae (grid is about 1/5th of the screen size), explain galaxy mergers. You may need to scale down Tully labels and increase luminosity (A/N: description may change based on the images uploaded into the software). Here's a more violent example of galaxy inter ...
... o) Zoom out, go around past Virgo for Antennae (grid is about 1/5th of the screen size), explain galaxy mergers. You may need to scale down Tully labels and increase luminosity (A/N: description may change based on the images uploaded into the software). Here's a more violent example of galaxy inter ...
Extraplanar
... AGN triggered by mergers? HI tracer of the origin and evolution of the galaxy allows to put the AGN activity in the evolutionary sequence ...
... AGN triggered by mergers? HI tracer of the origin and evolution of the galaxy allows to put the AGN activity in the evolutionary sequence ...
Quasars and AGN
... – Bridging the gap between QSOs and galaxies. • QSOs are 1000x brighter than normal galaxies why are there not intermediate luminosity galaxies? • There are. A class of galaxies called Seyferts (I and II). • These galaxies have bright compact nuclei (Active Galactic Nuclei - AGN) and have luminositi ...
... – Bridging the gap between QSOs and galaxies. • QSOs are 1000x brighter than normal galaxies why are there not intermediate luminosity galaxies? • There are. A class of galaxies called Seyferts (I and II). • These galaxies have bright compact nuclei (Active Galactic Nuclei - AGN) and have luminositi ...
Cosmology Physics 466E Olbers Paradox Cosmological principle
... *Universe is 13.7 billion years old with a margin of error of close to 1%. *First stars ignited 200 million years after the Big Bang. *Light in WMAP picture from 379,000 years after the Big Bang. *Content of the Universe: 4% Atoms, 23% Cold Dark Matter, 73% Dark energy. *The data places new constrai ...
... *Universe is 13.7 billion years old with a margin of error of close to 1%. *First stars ignited 200 million years after the Big Bang. *Light in WMAP picture from 379,000 years after the Big Bang. *Content of the Universe: 4% Atoms, 23% Cold Dark Matter, 73% Dark energy. *The data places new constrai ...
Big Bang, worksheet - Starkville Science Club
... Meanwhile, in the outer parts of the disk, gas and dust formed small asteroid-like bodies called planetesimals. These formed the building blocks of the planets. Planetesimals collided and grew larger by sticking together and eventually combining to form the planets. New observations have led many as ...
... Meanwhile, in the outer parts of the disk, gas and dust formed small asteroid-like bodies called planetesimals. These formed the building blocks of the planets. Planetesimals collided and grew larger by sticking together and eventually combining to form the planets. New observations have led many as ...
Sloshing, Stripping, Bubbles, & Shocks In the NGC 5846 Group
... The NGC5846 galaxy group shares many properties with highly evolved fossil groups, yet its intra-cluster medium is far from relaxed. We use a combined 120 ks Chandra exposure to study the `sloshing’ gas motions, established by galaxy interactions in the group, and AGN activity, driven by AGN activit ...
... The NGC5846 galaxy group shares many properties with highly evolved fossil groups, yet its intra-cluster medium is far from relaxed. We use a combined 120 ks Chandra exposure to study the `sloshing’ gas motions, established by galaxy interactions in the group, and AGN activity, driven by AGN activit ...
Astronomy Ch 20 The Universe
... The telescope allowed astronomers to study stars in more detail for the first time. ...
... The telescope allowed astronomers to study stars in more detail for the first time. ...
An Analysis of Collisional Ring Galaxies
... It also appears that a set of “spokes” extends from the center of the galaxy to its ring. Although very uncommon, there are three theories of their origin: 1) the spokes were caused by internal gravitational instabilities following the impact of the smaller galaxy, 2) they are similar to spirals and ...
... It also appears that a set of “spokes” extends from the center of the galaxy to its ring. Although very uncommon, there are three theories of their origin: 1) the spokes were caused by internal gravitational instabilities following the impact of the smaller galaxy, 2) they are similar to spirals and ...
File 11 - School of Astronomy, IPM
... • Elliptical galaxies are denoted En where: b/a = 1-n/10 i.e. an E4 galaxy has an axis ratio of b/a = 0.6 and E0 have circular isophotes • Massive (~1013 M⦿) • About 20% of field galaxies are Ellipticals, but most E’s are in clusters • There are a number of different subtypes: E’s (normal elliptical ...
... • Elliptical galaxies are denoted En where: b/a = 1-n/10 i.e. an E4 galaxy has an axis ratio of b/a = 0.6 and E0 have circular isophotes • Massive (~1013 M⦿) • About 20% of field galaxies are Ellipticals, but most E’s are in clusters • There are a number of different subtypes: E’s (normal elliptical ...
The Red-Sequence Cluster Survey
... Discretionary Time, soon after the cluster was discovered. This initial spectroscopy demonstrated that the cluster was at z = 0.773, and showed that one of the arcs (the arc labelled ’C’, visible in Figure 5) was extremely distant, at a redshift of 4.8786 (Gladders et al. 2002). The FORS spectrum of ...
... Discretionary Time, soon after the cluster was discovered. This initial spectroscopy demonstrated that the cluster was at z = 0.773, and showed that one of the arcs (the arc labelled ’C’, visible in Figure 5) was extremely distant, at a redshift of 4.8786 (Gladders et al. 2002). The FORS spectrum of ...
D109: A Spectactularly Forgotten Galaxy Aggregate
... power for the mean stellar age, extends the requested time to 2 orbits. In sum, this unique collection of extremely blue and bright individual knots which are dynamically bound to one another and appear to have very young stellar populations may well be the best nearby example of a galaxy assembly p ...
... power for the mean stellar age, extends the requested time to 2 orbits. In sum, this unique collection of extremely blue and bright individual knots which are dynamically bound to one another and appear to have very young stellar populations may well be the best nearby example of a galaxy assembly p ...
PH607lec08
... • Few E galaxies actually have flat luminosity profiles at small radii; instead, the profiles rise inward to the last measured point . • Cores may exhibit unusual kinematics; for example, about a quarter of all elliptical galaxies have cores which appear to counter-rotate with respect to the rest of ...
... • Few E galaxies actually have flat luminosity profiles at small radii; instead, the profiles rise inward to the last measured point . • Cores may exhibit unusual kinematics; for example, about a quarter of all elliptical galaxies have cores which appear to counter-rotate with respect to the rest of ...
Atlas of Peculiar Galaxies
The Atlas of Peculiar Galaxies is a catalog of peculiar galaxies produced by Halton Arp. A total of 338 galaxies are presented in the atlas, which was originally published in 1966 by the California Institute of Technology.The primary goal of the catalog was to present photographs of examples of the different kinds of peculiar structures found among nearby galaxies. Arp realized that the reason why galaxies formed into spiral or elliptical shapes was not well understood. He perceived peculiar galaxies as small ""experiments"" that astronomers could use to understand the physical processes that distort spiral or elliptical galaxies. With this atlas, astronomers had a sample of peculiar galaxies that they could study in more detail. The atlas does not present a complete overview of every peculiar galaxy in the sky but instead provides examples of the different phenomena as observed in nearby galaxies.Because little was known at the time of publication about the physical processes that caused the different shapes, the galaxies in the atlas are sorted based on their appearance. Objects 1–101 are individual peculiar spiral galaxies or spiral galaxies that apparently have small companions. Objects 102–145 are elliptical and elliptical-like galaxies. Individual or groups of galaxies with neither elliptical nor spiral shapes are listed as objects 146–268. Objects 269–327 are double galaxies. Finally, objects that simply do not fit into any of the above categories are listed as objects 332–338. Most objects are best known by their other designations, but a few galaxies are best known by their Arp numbers (such as Arp 220).Today, the physical processes that lead to the peculiarities seen in the Arp atlas are now well understood. A large number of the objects are interacting galaxies, including M51 (Arp 85), Arp 220, and the Antennae Galaxies (NGC 4038/NGC 4039, or Arp 244). A few of the galaxies are simply dwarf galaxies that do not have enough mass to produce enough gravity to allow the galaxies to form any cohesive structure. NGC 1569 (Arp 210) is an example of one of the dwarf galaxies in the atlas. A few other galaxies are radio galaxies. These objects contain active galactic nuclei that produce powerful jets of gas called radio jets. The atlas includes the nearby radio galaxies M87 (Arp 152) and Centaurus A (Arp 153).