The Norma cluster (ACO3627) – II. The near-infrared Ks
... Not all clusters can be modelled by a Schechter function, however. The Virgo cluster, for example, has a LF with a ‘double-wave’ structure (Binggeli et al. 1988). Clusters containing cD galaxies seem to have a steeper bright end than those without cD galaxies. Often the brightest galaxy is excluded ...
... Not all clusters can be modelled by a Schechter function, however. The Virgo cluster, for example, has a LF with a ‘double-wave’ structure (Binggeli et al. 1988). Clusters containing cD galaxies seem to have a steeper bright end than those without cD galaxies. Often the brightest galaxy is excluded ...
Girardi
... The RGB tip Sharp limit to bolometric luminosity of RGB stars. appears flattest in the I -band of metal-poor populations (that’s why it’s a distance indicator) but more generally it will appear as a broad fan, fainter for red optical colours in the near-infrared, it appears narrow in colour (but bri ...
... The RGB tip Sharp limit to bolometric luminosity of RGB stars. appears flattest in the I -band of metal-poor populations (that’s why it’s a distance indicator) but more generally it will appear as a broad fan, fainter for red optical colours in the near-infrared, it appears narrow in colour (but bri ...
Gas Mass Fractions and the Evolution of Spiral Galaxies
... Flux limited surveys are most efficient at identifying the brightest (L∗ ) and highest contrast (µ0 ∗ ) galaxies that exist in the intrinsic distributions in a given passband. As a direct consequence, galaxy catalogs are numerically dominated by such objects far out of proportion to their actual num ...
... Flux limited surveys are most efficient at identifying the brightest (L∗ ) and highest contrast (µ0 ∗ ) galaxies that exist in the intrinsic distributions in a given passband. As a direct consequence, galaxy catalogs are numerically dominated by such objects far out of proportion to their actual num ...
Jul y 9- 11,
... central supermassive black holes (SMBHs) will be more often present even in smaller galaxies when seeds are generated from the remnants of the first massive stars rather than via direct gas collapse. Consequently, measurement of the local occupation fraction provides an observational discriminator b ...
... central supermassive black holes (SMBHs) will be more often present even in smaller galaxies when seeds are generated from the remnants of the first massive stars rather than via direct gas collapse. Consequently, measurement of the local occupation fraction provides an observational discriminator b ...
bars and secular evolution
... Unambiguous evidence for r1/4 law - would this kind of analysis have found it ? M31 surface brightness distribution Pritchet & van den Bergh 1994 ...
... Unambiguous evidence for r1/4 law - would this kind of analysis have found it ? M31 surface brightness distribution Pritchet & van den Bergh 1994 ...
Sample pages 1 PDF
... elements) was considered a wide-field instrument. In 2003 a camera called Megacam began operating; it has .18 000/2 pixels and images a square degree of the sky at a sampling rate of 0:00 2 in a single exposure. Such a camera produces roughly 100 GB of data every night, the reduction of which requir ...
... elements) was considered a wide-field instrument. In 2003 a camera called Megacam began operating; it has .18 000/2 pixels and images a square degree of the sky at a sampling rate of 0:00 2 in a single exposure. Such a camera produces roughly 100 GB of data every night, the reduction of which requir ...
Ellipticity, Its Origin and Progression in Comoving Galaxies
... That which cannot be predicted cannot be understood, and therefore, cannot be explained. –apodictic assertion Without any doubt, there can be no plausible explanation for elliptical galaxies —no explanation for their characteristic features, no explanation for their evolution— within an expanding-ty ...
... That which cannot be predicted cannot be understood, and therefore, cannot be explained. –apodictic assertion Without any doubt, there can be no plausible explanation for elliptical galaxies —no explanation for their characteristic features, no explanation for their evolution— within an expanding-ty ...
Essential physics of early galaxy formation
... medium (IGM) or to be brought in by mergers to re-ignite further star formation. As halos build-up mass with time, their DM potential well can sustain much larger star formation rates (SFR) without losing gas. This naturally implies that, at any given time, there is a limiting star formation efficie ...
... medium (IGM) or to be brought in by mergers to re-ignite further star formation. As halos build-up mass with time, their DM potential well can sustain much larger star formation rates (SFR) without losing gas. This naturally implies that, at any given time, there is a limiting star formation efficie ...
The role of black holes in galaxy formation and evolution
... Galaxies come in two basic types: ‗football-shaped‘ ellipticals and ‗disk-shaped‘ spirals (Fig. 1). Spirals contain plenty of cold gas, which forms stars, whereas the gas in ellipticals is too hot to form stars. Thus, ellipticals lack the young blue stars that are usually seen in spirals, and are g ...
... Galaxies come in two basic types: ‗football-shaped‘ ellipticals and ‗disk-shaped‘ spirals (Fig. 1). Spirals contain plenty of cold gas, which forms stars, whereas the gas in ellipticals is too hot to form stars. Thus, ellipticals lack the young blue stars that are usually seen in spirals, and are g ...
Abstract - UChicago High Energy Physics
... and self interaction potentials of the same sign. For example, for the case of core collapse supernovae neutrinos, it has been pointed out that several types of transformations can occur in such systems which have a slight electron neutrino excess, start at high neutrino density and end at low neutr ...
... and self interaction potentials of the same sign. For example, for the case of core collapse supernovae neutrinos, it has been pointed out that several types of transformations can occur in such systems which have a slight electron neutrino excess, start at high neutrino density and end at low neutr ...
Joint formation of QSOs and spheroids: QSOs as clocks of star
... bulges of spiral galaxies exhibit a tight correlation between the Mg2 index and the intrinsic luminosity similar to that of the ellipticals (Jablonka, Martin & Arimoto 1996). These facts support the conclusion that spheroids formed stars very rapidly at early epochs (see, e.g., Renzini 1999). The ra ...
... bulges of spiral galaxies exhibit a tight correlation between the Mg2 index and the intrinsic luminosity similar to that of the ellipticals (Jablonka, Martin & Arimoto 1996). These facts support the conclusion that spheroids formed stars very rapidly at early epochs (see, e.g., Renzini 1999). The ra ...
Introduction to Observational Cosmology
... Structure (Size, bulge-to-disc ratio, etc..) Dynamical mass Star formation rate Color (or spectral energy distribution) of the stellar population ...
... Structure (Size, bulge-to-disc ratio, etc..) Dynamical mass Star formation rate Color (or spectral energy distribution) of the stellar population ...
M81/M82/NGC3077
... The two galaxies have indeed passed each other not long ago. The line-of-sight separation is 0.27 Mpc. Calculated using the velocity difference gives a time scale of approximately 1x109 years, consistent with the enhanced star ...
... The two galaxies have indeed passed each other not long ago. The line-of-sight separation is 0.27 Mpc. Calculated using the velocity difference gives a time scale of approximately 1x109 years, consistent with the enhanced star ...
Can we account for the dust
... Origin and evolution of dust in galaxies Can we account for the dust in galaxies by stellar sources? Mikako Matsuura Origin’s fellow, Institute of Origins, University College London M.J. Barlow, G.C. Sloan, A.A. Zijlstra, D. Stock, P.A. Whitelock, P. R. Wood, ...
... Origin and evolution of dust in galaxies Can we account for the dust in galaxies by stellar sources? Mikako Matsuura Origin’s fellow, Institute of Origins, University College London M.J. Barlow, G.C. Sloan, A.A. Zijlstra, D. Stock, P.A. Whitelock, P. R. Wood, ...
Quasars
... like fuzzy, blue stars, but had strange spectra with a lot of ultraviolet excess. • One of them, 3C273 had its position very accurately measured by C. Hazard and co-workers, using lunar occultations. • In 1962, M. Schmidt obtained a spectrum of this “object", which showed a large redshift of 0.158, ...
... like fuzzy, blue stars, but had strange spectra with a lot of ultraviolet excess. • One of them, 3C273 had its position very accurately measured by C. Hazard and co-workers, using lunar occultations. • In 1962, M. Schmidt obtained a spectrum of this “object", which showed a large redshift of 0.158, ...
lecture course
... common weaker AGNs like Seyfert galaxies, etc. are also found. Many of the most luminous AGNs are dust-enshrouded, particularly when they are very young and have just formed. AGNs have non-thermal spectra and so emit quite a lot of energy outside visible wavebands. They are much brighter than stars ...
... common weaker AGNs like Seyfert galaxies, etc. are also found. Many of the most luminous AGNs are dust-enshrouded, particularly when they are very young and have just formed. AGNs have non-thermal spectra and so emit quite a lot of energy outside visible wavebands. They are much brighter than stars ...
Module 11.1.1: Galaxies: Morphology and the Hubble Sequence
... are found in clusters or maybe dense groups, a relatively modest number in the general field. Hubble classified them according to the apparent ellipticity projected on sky, having no other phys ...
... are found in clusters or maybe dense groups, a relatively modest number in the general field. Hubble classified them according to the apparent ellipticity projected on sky, having no other phys ...
Lab 14 Galaxy Morphology
... Figure 14.11: An irregular galaxy that is the result of the collision between two galaxies. The larger galaxy appears to have once been a normal spiral galaxy. But another galaxy (visible in the bottom right corner) ran into the bigger galaxy, and destroyed the symmetry typically found in a spiral ...
... Figure 14.11: An irregular galaxy that is the result of the collision between two galaxies. The larger galaxy appears to have once been a normal spiral galaxy. But another galaxy (visible in the bottom right corner) ran into the bigger galaxy, and destroyed the symmetry typically found in a spiral ...
script
... Why is this? As it turns out, the light from these distant galaxies takes a much longer time to reach us than the light from objects nearby. When the light left distant galaxies many billions of years ago, it “recorded” information about what those galaxies looked like many billions of years ago. Ma ...
... Why is this? As it turns out, the light from these distant galaxies takes a much longer time to reach us than the light from objects nearby. When the light left distant galaxies many billions of years ago, it “recorded” information about what those galaxies looked like many billions of years ago. Ma ...
The Evolution of Galaxy - Tufts Institute of Cosmology
... emission, these bright spots are coming from some of the Messier galaxies rather than from clumps of gas [see right illustration on page 56]. Only the core region in the northern part of Virgo has a nearly symmetrical structure. Such x-ray images have led astronomers to conclude that clusters form f ...
... emission, these bright spots are coming from some of the Messier galaxies rather than from clumps of gas [see right illustration on page 56]. Only the core region in the northern part of Virgo has a nearly symmetrical structure. Such x-ray images have led astronomers to conclude that clusters form f ...
8-4.9 - S2TEM Centers SC
... ecliptic, they are not normally in alignment with each other because their orbital velocities and orbital periods vary.) Planets cannot be seen with the naked eye. The earth is the center of the solar system. (The planets, sun and moon revolve around the earth.) The solar system contains only ...
... ecliptic, they are not normally in alignment with each other because their orbital velocities and orbital periods vary.) Planets cannot be seen with the naked eye. The earth is the center of the solar system. (The planets, sun and moon revolve around the earth.) The solar system contains only ...
Measuring distances to the edge of the local group
... No. Nights Moon Optimal Months Accept. Months KP-2.1m Spectrograph 4 New Nov-Dec October-Jan KP-2.1m Spectrograph 2 New May-June April-July ...
... No. Nights Moon Optimal Months Accept. Months KP-2.1m Spectrograph 4 New Nov-Dec October-Jan KP-2.1m Spectrograph 2 New May-June April-July ...
A Zoo of Galaxies - Cambridge University Press
... To say our understanding of the “zoo” of galaxies that are found in our Universe has changed a lot over the last century or two is a bit of an understatement. In 1845 the state of the art picture of an external galaxy, was an image of M51, or the Whirlpool galaxy drawn by William Parsons, Third Earl ...
... To say our understanding of the “zoo” of galaxies that are found in our Universe has changed a lot over the last century or two is a bit of an understatement. In 1845 the state of the art picture of an external galaxy, was an image of M51, or the Whirlpool galaxy drawn by William Parsons, Third Earl ...
3.1 Radio Astronomy Research Results For much of PY 2010, radio
... which was originally developed to process LIGO data for coherent gravitational wave signals. E@H now devotes 1/3 of its processing resources to PALFA data to search for very compact binary pulsars in circular orbits. A total of ~200k clients around the world have signed on to E@H, of which some frac ...
... which was originally developed to process LIGO data for coherent gravitational wave signals. E@H now devotes 1/3 of its processing resources to PALFA data to search for very compact binary pulsars in circular orbits. A total of ~200k clients around the world have signed on to E@H, of which some frac ...
Clusters as laboratories for the study of galaxy evolution
... No dependence on zero-point or slope of CMR with regard to richness and x-ray luminosity “The Environmental Dependence of Galaxy Colors in Intermediate-Redshift X-Ray-selected Clusters” – Wake et al., 2005 ApJ 627, 186 “We find that the “red” galaxies form a tight color-magnitude relation (CMR) and ...
... No dependence on zero-point or slope of CMR with regard to richness and x-ray luminosity “The Environmental Dependence of Galaxy Colors in Intermediate-Redshift X-Ray-selected Clusters” – Wake et al., 2005 ApJ 627, 186 “We find that the “red” galaxies form a tight color-magnitude relation (CMR) and ...
Pea galaxy
A Pea galaxy, also referred to as a Pea or Green Pea, might be a type of Luminous Blue Compact Galaxy which is undergoing very high rates of star formation. Pea galaxies are so-named because of their small size and greenish appearance in the images taken by the Sloan Digital Sky Survey (SDSS).Pea Galaxies were first discovered in 2007 by the volunteer users within the forum section of the online astronomy project Galaxy Zoo (GZ).