ASPEN WORKSHOP 2003
... ellipticals, larger in bluer galaxies, up to few tenths. AI(Red), or AI(Blue) >0.3 suggests interaction, as in half of ULIRGS [as long as they are identified as “single galaxy”!] Simulations show that AI stays above 0.35 for about 700 Myears, but NOT for face-on HDF application: rest frame B morphol ...
... ellipticals, larger in bluer galaxies, up to few tenths. AI(Red), or AI(Blue) >0.3 suggests interaction, as in half of ULIRGS [as long as they are identified as “single galaxy”!] Simulations show that AI stays above 0.35 for about 700 Myears, but NOT for face-on HDF application: rest frame B morphol ...
Starburst Galaxies - Beck-Shop
... Stars of spectral classes O and B (Box 2.3) have very high surface temperatures and emit a great deal of ultraviolet radiation. The lives of such stars are short (Box 2.1) and so they are usually still to be seen in the groups where they were produced by the star-forming region, along with many cool ...
... Stars of spectral classes O and B (Box 2.3) have very high surface temperatures and emit a great deal of ultraviolet radiation. The lives of such stars are short (Box 2.1) and so they are usually still to be seen in the groups where they were produced by the star-forming region, along with many cool ...
PDF
... magnitudes merely as a result of this effect. Likewise, lower surface brightness features such as spiral disks will rapidly be dimmed beyond detection at great distances and so certain classes of galaxies may appear more concentrated and dominated by their nuclear regions than would otherwise be the ...
... magnitudes merely as a result of this effect. Likewise, lower surface brightness features such as spiral disks will rapidly be dimmed beyond detection at great distances and so certain classes of galaxies may appear more concentrated and dominated by their nuclear regions than would otherwise be the ...
SUB-KILOPARSEC IMAGING OF COOL MOLECULAR GAS IN
... of three CO lines in two high-redshift gravitationally lensed dusty star-forming galaxies, discovered by the South Pole Telescope. Strong lensing allows us to probe the structure and dynamics of the molecular gas in these two objects, at z = 2.78 and z = 5.66, with effective source-plane resolution ...
... of three CO lines in two high-redshift gravitationally lensed dusty star-forming galaxies, discovered by the South Pole Telescope. Strong lensing allows us to probe the structure and dynamics of the molecular gas in these two objects, at z = 2.78 and z = 5.66, with effective source-plane resolution ...
Practical cosmology with the Local Volume galaxies
... 4. The local Hubble flow While having accurate velocities and distances for ~250 LV galaxies, one can study distribution of peculiar velocities within the Volume. A peculiar velocity map for the LV galaxies in the LG reference frame shows the local Hubble flow to be generally calm with peculiar vel ...
... 4. The local Hubble flow While having accurate velocities and distances for ~250 LV galaxies, one can study distribution of peculiar velocities within the Volume. A peculiar velocity map for the LV galaxies in the LG reference frame shows the local Hubble flow to be generally calm with peculiar vel ...
Lecture 3 - University of Washington
... for grand design spirals. • The spiral arms are overdense regions which move around at a different speed than star: stars thus move in and out of the spiral arm • How these density waves are set up is unclear, but it may have to do with interactions. Once they are set up, they must last for a long e ...
... for grand design spirals. • The spiral arms are overdense regions which move around at a different speed than star: stars thus move in and out of the spiral arm • How these density waves are set up is unclear, but it may have to do with interactions. Once they are set up, they must last for a long e ...
SXDS Highlights : Subaru / FOCAS Spectroscopy
... Natural guide star AO system on Subaru telescope with IRCS. 154 hours of observation in total. 13 FoVs with 36 LBGs , 1 RadioG., and 7 DRGs are observed. Typical on-source effective integration is 5 hours. Typical PSF size at the target position is FWHM=0.2” (~1.5kpc@z=3) ...
... Natural guide star AO system on Subaru telescope with IRCS. 154 hours of observation in total. 13 FoVs with 36 LBGs , 1 RadioG., and 7 DRGs are observed. Typical on-source effective integration is 5 hours. Typical PSF size at the target position is FWHM=0.2” (~1.5kpc@z=3) ...
Starburst Galaxies Encyclopedia of Astronomy & Astrophysics eaa.iop.org T Heckman
... (suggesting a similar amount of reddening due to dust absorption), and their ultraviolet and visible spectra show that they have similar stellar populations and gas dynamics. One important difference is that the regions of star formation in the high-redshift galaxies are typically larger and more lu ...
... (suggesting a similar amount of reddening due to dust absorption), and their ultraviolet and visible spectra show that they have similar stellar populations and gas dynamics. One important difference is that the regions of star formation in the high-redshift galaxies are typically larger and more lu ...
Galaxies - University of Iowa Astrophysics
... 1. Measure the distance to star A to be 200 pc. 2. Measure the flux of star A. 3. Measure the flux of star B, which is known to have the same luminosity as star A, to be lower by a factor of 1600 (or the flux of A is 1600 times the flux of B). 4. Find the distance to star B. ...
... 1. Measure the distance to star A to be 200 pc. 2. Measure the flux of star A. 3. Measure the flux of star B, which is known to have the same luminosity as star A, to be lower by a factor of 1600 (or the flux of A is 1600 times the flux of B). 4. Find the distance to star B. ...
21. Galaxy Evolution Agenda The Monty Hall Problem/Paradox 21.1
... these objects, sometimes forming huge lobes (revealed by radio observations) at great distances from the center of the galaxy. ...
... these objects, sometimes forming huge lobes (revealed by radio observations) at great distances from the center of the galaxy. ...
Introduction to Galaxies - West Jefferson Local Schools
... Recall, luminosity of stars scales with mass of stars… therefore, luminosity of galaxy scales with number of stars (and thus, mass of stars). Thus, luminosity of galaxy gives mass of galaxy. Going backwards… measure the velocity to “weigh” the galaxy to obtain luminosity. ...
... Recall, luminosity of stars scales with mass of stars… therefore, luminosity of galaxy scales with number of stars (and thus, mass of stars). Thus, luminosity of galaxy gives mass of galaxy. Going backwards… measure the velocity to “weigh” the galaxy to obtain luminosity. ...
IR Universe
... formed. Some of them are large enough to have been given the name “dwarf planets”. In fact, Pluto, was recently relegated to the status of a dwarf planet. The pictures below show the location of the trans-Neptunian belt and the sizes of some known dwarf planets in ...
... formed. Some of them are large enough to have been given the name “dwarf planets”. In fact, Pluto, was recently relegated to the status of a dwarf planet. The pictures below show the location of the trans-Neptunian belt and the sizes of some known dwarf planets in ...
Molecular Gas in Galactic Environments Abstracts (Poster)
... have questioned this ingrained classification. Most notably, the ATLAS3D survey of 260 ETGs within ∼40 Mpc found that 22% contain CO, a common tracer for molecular gas. The presence of cold molecular gas also implies the possibility for current star formation within these galaxies. Simulations do no ...
... have questioned this ingrained classification. Most notably, the ATLAS3D survey of 260 ETGs within ∼40 Mpc found that 22% contain CO, a common tracer for molecular gas. The presence of cold molecular gas also implies the possibility for current star formation within these galaxies. Simulations do no ...
M81/M82/NGC3077
... M81 — -35 km/sec (3.63 ± 0.34 Mpc) (CBR value: 48 km/sec) M82 — 202 km/sec (3.9 ± 0.3 Mpc) (CBR value: 296 km/sec) M81 is closer and approaching, while M82 is farther away and receding; ...
... M81 — -35 km/sec (3.63 ± 0.34 Mpc) (CBR value: 48 km/sec) M82 — 202 km/sec (3.9 ± 0.3 Mpc) (CBR value: 296 km/sec) M81 is closer and approaching, while M82 is farther away and receding; ...
The Milky Way - The Independent School
... Our Milky Way Galaxy is only one of the many billions of galaxies visible in the sky. This chapter will expand your horizon to discuss the different kinds of galaxies and their complex histories. Here you can expect ...
... Our Milky Way Galaxy is only one of the many billions of galaxies visible in the sky. This chapter will expand your horizon to discuss the different kinds of galaxies and their complex histories. Here you can expect ...
Emission from dust in galaxies: Metallicity dependence
... τLyα means that the resonant scattering is assumed to be a random-walk process of photons. Next, we define an optical depth of dust grains for Lyα photons over the length of lpath as τdust . It is estimated as τdust ∼ πa2 lpath ndust , where a is the size of grains and ndust is their number density. ...
... τLyα means that the resonant scattering is assumed to be a random-walk process of photons. Next, we define an optical depth of dust grains for Lyα photons over the length of lpath as τdust . It is estimated as τdust ∼ πa2 lpath ndust , where a is the size of grains and ndust is their number density. ...
Populations of Galaxies and their Formation at z < 7
... Using GOODS images, there are luminous diffuse objects (LDOs) at z > 1, with large outer HII regions that create un-concentrated galaxies These systems have sizes suggesting they are disks There are very few at z < 1, but many at 1 < z < 2 ...
... Using GOODS images, there are luminous diffuse objects (LDOs) at z > 1, with large outer HII regions that create un-concentrated galaxies These systems have sizes suggesting they are disks There are very few at z < 1, but many at 1 < z < 2 ...
Ch17_Galaxies
... fuzzy-looking objects that appear to be ordinary galaxies • Based on output fluctuations, quasars resemble the AGNs of radio galaxies and Seyfert galaxies in that they are small (fractions of a light-year in some cases) ...
... fuzzy-looking objects that appear to be ordinary galaxies • Based on output fluctuations, quasars resemble the AGNs of radio galaxies and Seyfert galaxies in that they are small (fractions of a light-year in some cases) ...
Lecture 16
... First identified as bright radio sources - without visible counterparts In 1962 Maarten Schmidt identified a “star” coincident with the radio source and obtained a spectrum. He discovered it was not a star, and named it a QUASAR. ...
... First identified as bright radio sources - without visible counterparts In 1962 Maarten Schmidt identified a “star” coincident with the radio source and obtained a spectrum. He discovered it was not a star, and named it a QUASAR. ...
Elliptical galaxies
... •The central surface brightness is tightly correlated with total luminosity. •The plot shows the central brightness IV(0), the core radius rc (the radius at which the surface brightness has dropped to half its central value) as functions of the total luminosity or absolute magnitude ...
... •The central surface brightness is tightly correlated with total luminosity. •The plot shows the central brightness IV(0), the core radius rc (the radius at which the surface brightness has dropped to half its central value) as functions of the total luminosity or absolute magnitude ...
3.1 Radio Astronomy Research Results For much of PY 2010, radio
... An AGES objective is to investigate the number of low mass gas rich dwarf galaxies that reside around isolated galaxies and within galaxy groups, as hierarchical models of galaxy formation predict hundreds of dwarf companions for each giant galaxy. AGES typically finds only one or two new dwarf gala ...
... An AGES objective is to investigate the number of low mass gas rich dwarf galaxies that reside around isolated galaxies and within galaxy groups, as hierarchical models of galaxy formation predict hundreds of dwarf companions for each giant galaxy. AGES typically finds only one or two new dwarf gala ...
Lecture notes 18: Galaxies and galaxy clusters
... where the Sun was but one of many. Kant went on to propose that if the Milky Way were limited then perhaps the diffuse “elliptical nebulae” seen in the night sky may also be distant disklike systems similar to our own but seperate. Kant called these objects island universes. Charles Messier (1730–181 ...
... where the Sun was but one of many. Kant went on to propose that if the Milky Way were limited then perhaps the diffuse “elliptical nebulae” seen in the night sky may also be distant disklike systems similar to our own but seperate. Kant called these objects island universes. Charles Messier (1730–181 ...
Megamaser
A megamaser is a type of astrophysical maser, which is a naturally occurring source of stimulated spectral line emission. Megamasers are distinguished from astrophysical masers by their large isotropic luminosity. Megamasers have typical luminosities of 103 solar luminosities (L☉), which is 100 million times brighter than masers in the Milky Way, hence the prefix mega. Likewise, the term kilomaser is used to describe masers outside the Milky Way that have luminosities of order L☉, or thousands of times stronger than the average maser in the Milky Way, gigamaser is used to describe masers billions of times stronger than the average maser in the Milky Way, and extragalactic maser encompasses all masers found outside the Milky Way. Most known extragalactic masers are megamasers, and the majority of megamasers are hydroxyl (OH) megamasers, meaning the spectral line being amplified is one due to a transition in the hydroxyl molecule. There are known megamasers for three other molecules: water (H2O), formaldehyde (H2CO), and methine (CH).Water megamasers were the first type of megamaser discovered. The first water megamaser was found in 1979 in NGC 4945, a galaxy in the nearby Centaurus A/M83 Group. The first hydroxyl megamaser was found in 1982 in Arp 220, which is the nearest ultraluminous infrared galaxy to the Milky Way. All subsequent OH megamasers that have been discovered are also in luminous infrared galaxies, and there are a small number of OH kilomasers hosted in galaxies with lower infrared luminosities. Most luminous infrared galaxies have recently merged or interacted with another galaxy, and are undergoing a burst of star formation. Many of the characteristics of the emission in hydroxyl megamasers are distinct from that of hydroxyl masers within the Milky Way, including the amplification of background radiation and the ratio of hydroxyl lines at different frequencies. The population inversion in hydroxyl molecules is produced by far infrared radiation that results from absorption and re-emission of light from forming stars by surrounding interstellar dust. Zeeman splitting of hydroxyl megamaser lines may be used to measure magnetic fields in the masing regions, and this application represents the first detection of Zeeman splitting in a galaxy other than the Milky Way.Water megamasers and kilomasers are found primarily associated with active galactic nuclei, while galactic and weaker extragalactic water masers are found in star forming regions. Despite different environments, the circumstances that produce extragalactic water masers do not seem to be very different from those that produce galactic water masers. Observations of water megamasers have been used to make accurate measurements of distances to galaxies in order to provide constraints on the Hubble constant.