redshift
... Light from a distant galaxy is found to contain the spectral lines of hydrogen. The light causing one of these lines has (an observed) measured wavelength of 466 nm. When the same line is observed (at rest) from a hydrogen source on Earth it has a wavelength of 434 nm. (a) Calculate the Doppler shif ...
... Light from a distant galaxy is found to contain the spectral lines of hydrogen. The light causing one of these lines has (an observed) measured wavelength of 466 nm. When the same line is observed (at rest) from a hydrogen source on Earth it has a wavelength of 434 nm. (a) Calculate the Doppler shif ...
Galaxy Morphology Classification - CS229
... kernel, decision tree, AdaBoost classifier, K-nearestneighbors and random forest. The classification accuracies for these algorithms as determined using 10-fold cross validation (CV) are shown in table I. The best performing algorithm was the random forest with 67% accuracy. The random forest confus ...
... kernel, decision tree, AdaBoost classifier, K-nearestneighbors and random forest. The classification accuracies for these algorithms as determined using 10-fold cross validation (CV) are shown in table I. The best performing algorithm was the random forest with 67% accuracy. The random forest confus ...
AKARI Infrared Camera (IRC) Spectroscopy Observations: Highlights
... independent arrays; NIR, MIRS, and MIRL, which cover the 1.8–5.5um, 4.6–13.4um, and 12.6–26.5 um wavelength range, respectively. Each of the three arrays has three imaging filters, which can be switched during the observation. Each of the arrays has a wide field of view of about 10’x10’, suitable fo ...
... independent arrays; NIR, MIRS, and MIRL, which cover the 1.8–5.5um, 4.6–13.4um, and 12.6–26.5 um wavelength range, respectively. Each of the three arrays has three imaging filters, which can be switched during the observation. Each of the arrays has a wide field of view of about 10’x10’, suitable fo ...
The Milky Way is on a collision course with its neighbor, the
... our galaxy experiences its gravitational dance with Andromeda. Because only a small fraction of a galaxy’s mass ends up in tidal tails, it is more likely the Sun will go for a much less dramatic ride. Most of the stars in merging galaxies remain relatively close to their host galaxies. The chance of ...
... our galaxy experiences its gravitational dance with Andromeda. Because only a small fraction of a galaxy’s mass ends up in tidal tails, it is more likely the Sun will go for a much less dramatic ride. Most of the stars in merging galaxies remain relatively close to their host galaxies. The chance of ...
Astronomy Ch 20 The Universe
... deeper scientists look into space, the more galaxies they find. There may be more than 100 billion galaxies. If you counted 1,000 galaxies per night, it would take 275,000 years to count all of them. ...
... deeper scientists look into space, the more galaxies they find. There may be more than 100 billion galaxies. If you counted 1,000 galaxies per night, it would take 275,000 years to count all of them. ...
Big Bang, worksheet - Starkville Science Club
... larger than the period at the end of this sentence. This tiny universe was incredibly hot and dense. The universe then exploded in what astronomers call the big bang. According to the big bang theory, the universe formed in an instant, billions of years ago, in an enormous explosion. Edwin Hubble di ...
... larger than the period at the end of this sentence. This tiny universe was incredibly hot and dense. The universe then exploded in what astronomers call the big bang. According to the big bang theory, the universe formed in an instant, billions of years ago, in an enormous explosion. Edwin Hubble di ...
Peculiar (Interacting) Galaxies
... formation, due to collisions between gas clouds. In addition • Gas which loses enough angular momentum during the encounter will fall into the center. (This is especially true if a bar is formed.) This can lead to strong nuclear starbursts. § M82 is currently forming a few M¤/year of stars (simila ...
... formation, due to collisions between gas clouds. In addition • Gas which loses enough angular momentum during the encounter will fall into the center. (This is especially true if a bar is formed.) This can lead to strong nuclear starbursts. § M82 is currently forming a few M¤/year of stars (simila ...
Student Reading
... Classification of Galaxies Galaxies can be classified according to their shapes: elliptical, spiral, or irregular. Edwin Hubble, for whom the Hubble Space Telescope is named, devised another famous classification scheme for galaxies. Hubble’s system included elliptical and spiral galaxies but exclud ...
... Classification of Galaxies Galaxies can be classified according to their shapes: elliptical, spiral, or irregular. Edwin Hubble, for whom the Hubble Space Telescope is named, devised another famous classification scheme for galaxies. Hubble’s system included elliptical and spiral galaxies but exclud ...
The Co-evolution of Galaxies and their Supermassive Black Holes
... The Co-evolution of Galaxies and their Supermassive Black Holes What have we learned from the SDSS? ...
... The Co-evolution of Galaxies and their Supermassive Black Holes What have we learned from the SDSS? ...
PH607lec09-3gal1
... galaxy, are seen. • The fraction of field E galaxies with shell-like features is at least 17% and possibly more than 44%. • The colours of shells indicate that they are composed of stars. In many cases the shells are somewhat more blue than the galaxies they occupy. • Shell systems have a variety of ...
... galaxy, are seen. • The fraction of field E galaxies with shell-like features is at least 17% and possibly more than 44%. • The colours of shells indicate that they are composed of stars. In many cases the shells are somewhat more blue than the galaxies they occupy. • Shell systems have a variety of ...
PH607lec10-3gal1
... galaxy, are seen. • The fraction of field E galaxies with shell-like features is at least 17% and possibly more than 44%. • The colours of shells indicate that they are composed of stars. In many cases the shells are somewhat more blue than the galaxies they occupy. • Shell systems have a variety of ...
... galaxy, are seen. • The fraction of field E galaxies with shell-like features is at least 17% and possibly more than 44%. • The colours of shells indicate that they are composed of stars. In many cases the shells are somewhat more blue than the galaxies they occupy. • Shell systems have a variety of ...
Stellar Populations in the Interacting System Arp94 with SITELLE
... SITELLE is the new Imaging Fourier Transform Spectrograph of the Canada-France-Hawaii Telescope. It produces an impressive number of 4 million spectra in a single datacube in selected bandpasses of the visible from 350 to 900 nm. Its large FoV (11'x11') and its high spatial sampling (0.32’’/pixel, s ...
... SITELLE is the new Imaging Fourier Transform Spectrograph of the Canada-France-Hawaii Telescope. It produces an impressive number of 4 million spectra in a single datacube in selected bandpasses of the visible from 350 to 900 nm. Its large FoV (11'x11') and its high spatial sampling (0.32’’/pixel, s ...
14 full-time tuners in Chicago - Pomona College Astronomy Program
... This part will include some interesting information on early radar studies; some calculations for distances to different planets. Try to find some good footage of lunar ranging (email our friend teaching with us - ask for talk slides or movie) Include information on spacecraft and alternate theories ...
... This part will include some interesting information on early radar studies; some calculations for distances to different planets. Try to find some good footage of lunar ranging (email our friend teaching with us - ask for talk slides or movie) Include information on spacecraft and alternate theories ...
SWIRE
... number of distant and high-z galaxies • This is one of the main targets of our Legacy Program, SWIRE • SWIRE will devote 500 hours to survey with IRAC a very large area (70 sq.deg.) to moderate depths (+ 400 hours with MIPS at longer-λ) ...
... number of distant and high-z galaxies • This is one of the main targets of our Legacy Program, SWIRE • SWIRE will devote 500 hours to survey with IRAC a very large area (70 sq.deg.) to moderate depths (+ 400 hours with MIPS at longer-λ) ...
Homework #1 Questions
... Question for Review #3: What is the evidence for a black hole at the center of the Milky Way? Problem #1: Given that the Sun moves in a circular orbit of radius 8 kiloparsecs around the center of the Milky Way, and its orbital speed is 220 km/sec, work out how long it takes the Sun to complete one o ...
... Question for Review #3: What is the evidence for a black hole at the center of the Milky Way? Problem #1: Given that the Sun moves in a circular orbit of radius 8 kiloparsecs around the center of the Milky Way, and its orbital speed is 220 km/sec, work out how long it takes the Sun to complete one o ...
What Globular Clusters Teach Us About Oleg Gnedin
... • In the first two days of this meeting, we talked about matching galaxies to halos, in the full range from faint galaxies to massive galaxy clusters • While the distribution of dark matter is approximately self-similar on different mass scales, the baryon physics is not: Inside galaxies, the gas ha ...
... • In the first two days of this meeting, we talked about matching galaxies to halos, in the full range from faint galaxies to massive galaxy clusters • While the distribution of dark matter is approximately self-similar on different mass scales, the baryon physics is not: Inside galaxies, the gas ha ...
2007_spitzer_lecture_series_kennicutt_talk3
... H2 surface density, and not with HI density • A kinematic star formation law does not seem to extend as well to local scales • The disk-averaged SF law is confirmed with more/better observations. Some metal-poor galaxies lie systematically above the mean relation. ...
... H2 surface density, and not with HI density • A kinematic star formation law does not seem to extend as well to local scales • The disk-averaged SF law is confirmed with more/better observations. Some metal-poor galaxies lie systematically above the mean relation. ...
Chapter 15
... • What is the power source for quasars and other active galactic nuclei? — The only model that adequately explains our observations holds that supermassive black holes are the power source. ...
... • What is the power source for quasars and other active galactic nuclei? — The only model that adequately explains our observations holds that supermassive black holes are the power source. ...
Stars, Galaxies and Black Holes
... • There are a few types of stars, one type is a Red Dwarf. • Red Dwarf’s are not as hot as the others. The colour depends on the heat of the actual star. Red Dwarfs are the most common stars. • The brightest star is called a cappella. A group of stars is called a constellation. ...
... • There are a few types of stars, one type is a Red Dwarf. • Red Dwarf’s are not as hot as the others. The colour depends on the heat of the actual star. Red Dwarfs are the most common stars. • The brightest star is called a cappella. A group of stars is called a constellation. ...
How to kill a galaxy - University of Waterloo
... • GALFORM is Durham model of galaxy formation (Cole et al. 2000) – parameters fixed to reproduce global properties of galaxies at z=0 (e.g. luminosity function) and abundance of SCUBA galaxies at high redshift ...
... • GALFORM is Durham model of galaxy formation (Cole et al. 2000) – parameters fixed to reproduce global properties of galaxies at z=0 (e.g. luminosity function) and abundance of SCUBA galaxies at high redshift ...
Epoch of Reionization
... • Chemical abundances of the most metal poor stars in the MW and stars in LG dwarfs look normal, unlike those of Pop III ejecta. ...
... • Chemical abundances of the most metal poor stars in the MW and stars in LG dwarfs look normal, unlike those of Pop III ejecta. ...
Seyfert galaxy
Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei (very luminous, distant and bright sources of electromagnetic radiation) with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.Seyfert galaxies account for about 10% of all galaxies and are some of the most intensely studied objects in astronomy, as they are thought to be powered by the same phenomena that occur in quasars, although they are closer and less luminous than quasars. These galaxies have supermassive black holes at their centers which are surrounded by accretion discs of in-falling material. The accretion discs are believed to be the source of the observed ultraviolet radiation. Ultraviolet emission and absorption lines provide the best diagnostics for the composition of the surrounding material.Seen in visible light, most Seyfert galaxies look like normal spiral galaxies, but when studied under other wavelengths, it becomes clear that the luminosity of their cores is of comparable intensity to the luminosity of whole galaxies the size of the Milky Way.Seyfert galaxies are named after Carl Seyfert, who first described this class in 1943.