A new view of galaxy evolution
... was obvious that fainter, and presumably more distant galaxies, look and are quite different from the galaxies we see in today’s universe. Understanding what this means, and how we can understand the physics of galaxy formation from these objects, have been major goals in astronomy for the past 15 y ...
... was obvious that fainter, and presumably more distant galaxies, look and are quite different from the galaxies we see in today’s universe. Understanding what this means, and how we can understand the physics of galaxy formation from these objects, have been major goals in astronomy for the past 15 y ...
Brown et al. 2008 Studying Resolved Stellar
... JWST will observe the birth of galaxies at high redshift, but it will complement that research by reconstructing the star formation histories of nearby galaxies, using multiband photometry of their resolved stellar populations. In a complex population hosting a mix of chemical abundances and ages, a ...
... JWST will observe the birth of galaxies at high redshift, but it will complement that research by reconstructing the star formation histories of nearby galaxies, using multiband photometry of their resolved stellar populations. In a complex population hosting a mix of chemical abundances and ages, a ...
The Magellan 20 Telescope Science Goals
... kinematics of the IGM becomes possible, mapping tenuous structures with densities down to the mean density of the universe. A combination with a traditional galaxy redshift survey of the same volume sampled by the lines of sight to the background galaxies would allow us to correlate the properties o ...
... kinematics of the IGM becomes possible, mapping tenuous structures with densities down to the mean density of the universe. A combination with a traditional galaxy redshift survey of the same volume sampled by the lines of sight to the background galaxies would allow us to correlate the properties o ...
Results from the search for tidal disruption flares in the GALEX Deep
... Constraints on MBH: MBH(t0-tD) > 1 x 108 Msun MBH() ~ 1+1-.5 x 109 Msun Critical upper limit on MBH for RT > Rs: Mcrit = 1 x 108 Msun (no spin) Mcrit = 8 x 108 Msun (O5 star) Mcrit = 8 x 108 Msun (with spin) Upper limit on MBH for RBB > Rms: RBB < 4 x 1013 cm ...
... Constraints on MBH: MBH(t0-tD) > 1 x 108 Msun MBH() ~ 1+1-.5 x 109 Msun Critical upper limit on MBH for RT > Rs: Mcrit = 1 x 108 Msun (no spin) Mcrit = 8 x 108 Msun (O5 star) Mcrit = 8 x 108 Msun (with spin) Upper limit on MBH for RBB > Rms: RBB < 4 x 1013 cm ...
ROTATION CURVES OF HIGH-LUMINOSITY SPIRAL GALAXIES
... pered by very incomplete observations of rotation curves of external galaxies. Optical observations generally determined velocities only across the nucleus and inner regions; velocities at large nuclear dis tances were rarely obtained. Radio 21-cm line observations generally integrated all the neut ...
... pered by very incomplete observations of rotation curves of external galaxies. Optical observations generally determined velocities only across the nucleus and inner regions; velocities at large nuclear dis tances were rarely obtained. Radio 21-cm line observations generally integrated all the neut ...
Quasars- The Brightest Black Holes
... all quasars are variable in their brightness. Today we know that only about 10% of quasars have the strong radio emission – most have none. Surveys (using observations taken in a range of wavebands) are continually identifying and collecting more and more quasars to the present day – hundreds of tho ...
... all quasars are variable in their brightness. Today we know that only about 10% of quasars have the strong radio emission – most have none. Surveys (using observations taken in a range of wavebands) are continually identifying and collecting more and more quasars to the present day – hundreds of tho ...
Local group
... which live 'forever', • massive stars inject into ISM a mass pDMtotal of heavy elements (p depends on the IMF and the yield of SN- normalized to total mass of stars). • Assumptions: galaxies gas is well mixed, no infall or outflow, high mass stars return metals to ISM faster than time to form new st ...
... which live 'forever', • massive stars inject into ISM a mass pDMtotal of heavy elements (p depends on the IMF and the yield of SN- normalized to total mass of stars). • Assumptions: galaxies gas is well mixed, no infall or outflow, high mass stars return metals to ISM faster than time to form new st ...
PDF format
... e) False, you would have an equal chance of finding an elliptical galaxy in any environment in the universe. © 2014 Pearson Education, Inc. ...
... e) False, you would have an equal chance of finding an elliptical galaxy in any environment in the universe. © 2014 Pearson Education, Inc. ...
PH607lec08
... A large fraction of disk galaxies have bars: narrow linear structures crossing the face of the galaxy. In barred S0 galaxies the bar is often the only structure visible in the disk. In types SBa and later the bar often connects to a spiral pattern extending to larger radii (e.g. NGC 1300). Viewed fa ...
... A large fraction of disk galaxies have bars: narrow linear structures crossing the face of the galaxy. In barred S0 galaxies the bar is often the only structure visible in the disk. In types SBa and later the bar often connects to a spiral pattern extending to larger radii (e.g. NGC 1300). Viewed fa ...
Galaxy / Cluster Ecosystem Ming Sun (University of Alabama in Huntsville)
... Coronae survived for many cluster galaxies, esp. massive ones (e.g., > 60 % for L > 2 L* galaxies); they are metal rich ( ~ solar) and hotter than stars (spec = 0.3 – 1.1). Origin: a) galactic cool cores (stellar mass loss); b) remnants of large cool cores after stripping or AGN heating? Embedded c ...
... Coronae survived for many cluster galaxies, esp. massive ones (e.g., > 60 % for L > 2 L* galaxies); they are metal rich ( ~ solar) and hotter than stars (spec = 0.3 – 1.1). Origin: a) galactic cool cores (stellar mass loss); b) remnants of large cool cores after stripping or AGN heating? Embedded c ...
Document
... Time and space did not exist until the Big-Bang event (estimated to have occurred about 15 billion years ago). The contents of the entire Universe was once compressed into a point the ‘size’ of a single electron. The Universe must have initially “inflated” in size, expanding many times faster than t ...
... Time and space did not exist until the Big-Bang event (estimated to have occurred about 15 billion years ago). The contents of the entire Universe was once compressed into a point the ‘size’ of a single electron. The Universe must have initially “inflated” in size, expanding many times faster than t ...
Characteristics of Our Galaxy
... variables (useful for judging distances), pre-main sequence stars, T-Tauri stars, Herbigharo objects, and even some A stars can be found in the arms. These stars are very metal rich and have highly circular orbits, although they comprise likely less than one percent of Milky Way stars. Young thin d ...
... variables (useful for judging distances), pre-main sequence stars, T-Tauri stars, Herbigharo objects, and even some A stars can be found in the arms. These stars are very metal rich and have highly circular orbits, although they comprise likely less than one percent of Milky Way stars. Young thin d ...
Building` a Galaxy SED
... Fundamental problem: We live in one, and want to understand our origin. Fun problem: galaxy astrophysics spans a wide range of scales: deeply rooted in cosmology, large variation in physics (fluid dynamics, quantum physics) Practical problem: galaxies are biased tracers of underlying mass distributi ...
... Fundamental problem: We live in one, and want to understand our origin. Fun problem: galaxy astrophysics spans a wide range of scales: deeply rooted in cosmology, large variation in physics (fluid dynamics, quantum physics) Practical problem: galaxies are biased tracers of underlying mass distributi ...
The National Centre for Radio Astrophysics
... The absorption of radio waves from background quasars by gas in intervening galaxies helps us to trace the neutral hydrogen distribution of the distant Universe, as well as physical conditions in the absorbing galaxies. Understanding conditions in such absorption-selected high-redshift galaxies is a ...
... The absorption of radio waves from background quasars by gas in intervening galaxies helps us to trace the neutral hydrogen distribution of the distant Universe, as well as physical conditions in the absorbing galaxies. Understanding conditions in such absorption-selected high-redshift galaxies is a ...
sections 23-25 powerpoint
... The luminosity differences between elliptical galaxies is tied to overall dimensions: cD galaxies. Huge elliptical galaxies dominating some clusters of galaxies. “cD” stands for “cluster dominating” galaxy. Some are incredibly large, massive, and luminous. Normal ellipticals. Standard E galaxies com ...
... The luminosity differences between elliptical galaxies is tied to overall dimensions: cD galaxies. Huge elliptical galaxies dominating some clusters of galaxies. “cD” stands for “cluster dominating” galaxy. Some are incredibly large, massive, and luminous. Normal ellipticals. Standard E galaxies com ...
instructor notes: weeks 9/10
... Lenticular galaxies get their name because they are “lenslike,” but are more like spiral and barred spiral galaxies in possessing a flattened disk, rather than like elliptical galaxies which mostly possess an ellipsoidal symmetry. The distinguishing feature of lenticulars relative to spiral galaxie ...
... Lenticular galaxies get their name because they are “lenslike,” but are more like spiral and barred spiral galaxies in possessing a flattened disk, rather than like elliptical galaxies which mostly possess an ellipsoidal symmetry. The distinguishing feature of lenticulars relative to spiral galaxie ...
81 KB - CSIRO Publishing
... Gilmore et al. have argued that the few objects within this zone of avoidance are special cases which are probably not in equilibrium but are in the throes of disruption. However the zone of avoidance is rapidly being filled, with several UCD-like objects having measured half-light sizes as large as ...
... Gilmore et al. have argued that the few objects within this zone of avoidance are special cases which are probably not in equilibrium but are in the throes of disruption. However the zone of avoidance is rapidly being filled, with several UCD-like objects having measured half-light sizes as large as ...
Robert_Minchin_Galaxies_2011_REU
... • The HI mass to luminosity ratio (MHI/L) tells us how gas-rich a galaxy is. – Gas-rich galaxies are often blue, late-type galaxies with active star formation. – Some are more intriguing objects with low SF rates. A number of these have been turned up by HI surveys. ...
... • The HI mass to luminosity ratio (MHI/L) tells us how gas-rich a galaxy is. – Gas-rich galaxies are often blue, late-type galaxies with active star formation. – Some are more intriguing objects with low SF rates. A number of these have been turned up by HI surveys. ...
Supermassive Black Holes in Inactive Galaxies Encyclopedia of Astronomy & Astrophysics eaa.iop.org
... galaxy outside our own. It can therefore be studied in unusual detail. M31 contains the nearest example of a nuclear star cluster embedded in a normal bulge. When examined with HST, the nucleus appears double (figure 3). This is very surprising. At a separation of 2r = 0".49 = 1.7 pc, a relative vel ...
... galaxy outside our own. It can therefore be studied in unusual detail. M31 contains the nearest example of a nuclear star cluster embedded in a normal bulge. When examined with HST, the nucleus appears double (figure 3). This is very surprising. At a separation of 2r = 0".49 = 1.7 pc, a relative vel ...
Disk Galaxies and problem 3
... disk galaxies as a population. Disk galaxies have many components, including • a disk which contains metal rich stars, gas (HI, molecular hydrogen, dust and hot gas), with strong ordered rotations. • a bulge which contains metal-poor to metal-rich stars that show diverse properties. They show weaker ...
... disk galaxies as a population. Disk galaxies have many components, including • a disk which contains metal rich stars, gas (HI, molecular hydrogen, dust and hot gas), with strong ordered rotations. • a bulge which contains metal-poor to metal-rich stars that show diverse properties. They show weaker ...
3. Cosmology and the Origin and Evolution of Galaxies
... of the gas and infer a dynamical gas-mass. ...
... of the gas and infer a dynamical gas-mass. ...
3D Tour of the Universe Template
... M104 was named the Sombrero Galaxy because of its appearance as viewed from just 6 degrees south of its equatorial plane and outlined by a thick dark rim of obscuring dust. This galaxy shows both a big bright core, and as one can see in shorter exposures, also well-defined spiral arms. It also has a ...
... M104 was named the Sombrero Galaxy because of its appearance as viewed from just 6 degrees south of its equatorial plane and outlined by a thick dark rim of obscuring dust. This galaxy shows both a big bright core, and as one can see in shorter exposures, also well-defined spiral arms. It also has a ...
Estimating the mass and star formation rate in galaxies
... though space, dust absorbs a fraction of this. The exact amount depends primarily on the total quantity of dust between the observed and the emitting source. Since dust is formed during the late stages of stellar evolution regions such as nuclei of galaxies, where many generations of stars are ...
... though space, dust absorbs a fraction of this. The exact amount depends primarily on the total quantity of dust between the observed and the emitting source. Since dust is formed during the late stages of stellar evolution regions such as nuclei of galaxies, where many generations of stars are ...
Galaxy Formation and Evolution
... In massive halos, where the virial temperature T >107 K, gas is fully collisionally ionized: cools mainly through Bremsstrahlung emission from free electrons. In the temperature range 104 K < T < 106 K, a number of excitation and de-excitation mechanisms can play a role: Electrons can recombine with ...
... In massive halos, where the virial temperature T >107 K, gas is fully collisionally ionized: cools mainly through Bremsstrahlung emission from free electrons. In the temperature range 104 K < T < 106 K, a number of excitation and de-excitation mechanisms can play a role: Electrons can recombine with ...
1Cmoles.pdf
... spectroscopic surveys cannot go as deep as the photometric surveys, reaching only I ≈ 24 with the use of large telescopes. The covered fields are necessarily small and cannot cope with the complex variety of objects in the Universe. To get the optimum compromise between large area and depth, good sp ...
... spectroscopic surveys cannot go as deep as the photometric surveys, reaching only I ≈ 24 with the use of large telescopes. The covered fields are necessarily small and cannot cope with the complex variety of objects in the Universe. To get the optimum compromise between large area and depth, good sp ...
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).