Part2
... We’ve focused on lines, what about the continuum at 1-3mm? (though many 30m observing modes deliberately filter out continuum via references). o 3mm is a low point in the SED of a (non-”monster”) galaxy. Emission from longer than ~ 1mm makes up < 10-4 of the bolometric luminosity. o Dust emission do ...
... We’ve focused on lines, what about the continuum at 1-3mm? (though many 30m observing modes deliberately filter out continuum via references). o 3mm is a low point in the SED of a (non-”monster”) galaxy. Emission from longer than ~ 1mm makes up < 10-4 of the bolometric luminosity. o Dust emission do ...
ASTRONOMY 0089: EXAM 3 Class Meets M,W,F, 1:00 PM April 19
... 17. Two quasars are observed to lie near each other (within a few arcseconds) on the sky. The objects have identical spectra (and hence redshifts) and colors. Photometric monitoring of the quasars reveals that both quasars uctuate in brightness in the same way. Which of the following statements is ...
... 17. Two quasars are observed to lie near each other (within a few arcseconds) on the sky. The objects have identical spectra (and hence redshifts) and colors. Photometric monitoring of the quasars reveals that both quasars uctuate in brightness in the same way. Which of the following statements is ...
Chapter 15
... What have we learned? • What are the three major types of galaxies? — Spiral galaxies, elliptical galaxies, and irregular galaxies — Spirals have both disk and spheroidal components; ellipticals have no disk. • How are galaxies grouped together? — Spiral galaxies tend to collect into groups of up t ...
... What have we learned? • What are the three major types of galaxies? — Spiral galaxies, elliptical galaxies, and irregular galaxies — Spirals have both disk and spheroidal components; ellipticals have no disk. • How are galaxies grouped together? — Spiral galaxies tend to collect into groups of up t ...
SWIRE
... The case for SWIRE • SIRTF will offer a unique chance to sample a largely unexplored waveband at 3 <λ<10 μm • This will allow photometric measurements of the baryonic mass in stars for an enormous number of distant and high-z galaxies • This is one of the main targets of our Legacy Program, SWIRE • ...
... The case for SWIRE • SIRTF will offer a unique chance to sample a largely unexplored waveband at 3 <λ<10 μm • This will allow photometric measurements of the baryonic mass in stars for an enormous number of distant and high-z galaxies • This is one of the main targets of our Legacy Program, SWIRE • ...
Small galaxies are growing smaller
... his contemporaries believed that the luminosity function (LF) of galaxies, that is the number of galaxies per unit volume of different luminosities, was a peaked, roughly Gaussian shaped curve. Known local galaxies spanned the range from the giant spiral M31 in Andromeda and our own galaxy, with lum ...
... his contemporaries believed that the luminosity function (LF) of galaxies, that is the number of galaxies per unit volume of different luminosities, was a peaked, roughly Gaussian shaped curve. Known local galaxies spanned the range from the giant spiral M31 in Andromeda and our own galaxy, with lum ...
Document
... Digital Sky Survey. This feature spans about 250 Mpc. On larger scales than this the Universe begins to look uniform (at least once we account for undersampling of dimmer galaxies very far away). ...
... Digital Sky Survey. This feature spans about 250 Mpc. On larger scales than this the Universe begins to look uniform (at least once we account for undersampling of dimmer galaxies very far away). ...
SUMSS - 京都大学
... • Techniques: Selection of candidates by colour or other criteria, spectroscopy with large optical/IR telescopes. • Elliptical galaxies: Ellipticals at z~1 (lookback time 8-9 Gyr) still look ‘old’, main epoch of formation probably earlier than z=3. • Cosmic evolution: Powerful radio galaxies much mo ...
... • Techniques: Selection of candidates by colour or other criteria, spectroscopy with large optical/IR telescopes. • Elliptical galaxies: Ellipticals at z~1 (lookback time 8-9 Gyr) still look ‘old’, main epoch of formation probably earlier than z=3. • Cosmic evolution: Powerful radio galaxies much mo ...
The evolution of spiral galaxies in clusters Kutdemir, Elif
... and 340 Gyr respectively. A merger between spirals of unequal mass can form an S0 galaxy (Bekki 1998), while major mergers likely result in a giant elliptical galaxy (Naab & Burkert 2003). Fig. 1.3 from Moran (2008) shows the regions where these mechanisms are expected to be effective for two interm ...
... and 340 Gyr respectively. A merger between spirals of unequal mass can form an S0 galaxy (Bekki 1998), while major mergers likely result in a giant elliptical galaxy (Naab & Burkert 2003). Fig. 1.3 from Moran (2008) shows the regions where these mechanisms are expected to be effective for two interm ...
Module 5: To the Galaxies and Beyond!
... flattened they look. For example, an elliptical galaxy that was perfectly round like a basketball would be called E0, while the one that looked like a football that had been badly squished would be called E7. Elliptical galaxies tend to made up of only very old stars and have far less dust and gas t ...
... flattened they look. For example, an elliptical galaxy that was perfectly round like a basketball would be called E0, while the one that looked like a football that had been badly squished would be called E7. Elliptical galaxies tend to made up of only very old stars and have far less dust and gas t ...
15-1/15-2 Reading Questions
... 12. Detail the five steps in the formation of the milky way galaxy from the images on 319. ...
... 12. Detail the five steps in the formation of the milky way galaxy from the images on 319. ...
Wandering in the Redshift Desert
... ploration of the redshift desert, an enterprise which is at the core of the zCOSMOS-Deep project (Lilly et al., 2007), the largest ongoing spectroscopic survey of the desert. This survey is targeting star-forming galaxies whose spectrum is pretty much like that shown in Figure 2, and does so with VI ...
... ploration of the redshift desert, an enterprise which is at the core of the zCOSMOS-Deep project (Lilly et al., 2007), the largest ongoing spectroscopic survey of the desert. This survey is targeting star-forming galaxies whose spectrum is pretty much like that shown in Figure 2, and does so with VI ...
Globular Cluster Formation in CDM Cosmologies
... • Hubble Diagram (1929): all galaxies receed from us. Speed of separation (v) is measured from the red shift of some typical well-observed line. - Hubble founds that v is proportional to the distance to the galaxy – HUBBLE’S LAW: v H d o ...
... • Hubble Diagram (1929): all galaxies receed from us. Speed of separation (v) is measured from the red shift of some typical well-observed line. - Hubble founds that v is proportional to the distance to the galaxy – HUBBLE’S LAW: v H d o ...
Lecture 18, Structure of spiral galaxies
... • plenty of high and lowmass stars, blue and red • Stars in the halo are old. • fraction of heavy elements much less than the Sun • mostly lowmass, red stars • Stars in the halo must have formed early in the Milky Way Galaxy’s history. • they formed at a time when few heavy elements existed • th ...
... • plenty of high and lowmass stars, blue and red • Stars in the halo are old. • fraction of heavy elements much less than the Sun • mostly lowmass, red stars • Stars in the halo must have formed early in the Milky Way Galaxy’s history. • they formed at a time when few heavy elements existed • th ...
Homework #8 - Leslie Looney
... Which of the following statements correctly describes the rotation of our Galaxy? 1. The disk rotates like a solid object (objects at all distances take the same time to complete an orbit), and the halo objects have random orbits with no net rotation of the halo about the center of the Galaxy. j 2. ...
... Which of the following statements correctly describes the rotation of our Galaxy? 1. The disk rotates like a solid object (objects at all distances take the same time to complete an orbit), and the halo objects have random orbits with no net rotation of the halo about the center of the Galaxy. j 2. ...
Time From the Perspective of a Particle Physicist
... each other missing mass first observed by Fritz Zwicky in the 1930s (Caltech; he also introduced name “supernova”) • look at gravitation lensing by a nearby galaxy of a more distant galaxy (many including NIU students Donna Kubik and Matt Weisner. see their theses at www.physics.niu.edu/physics/ac ...
... each other missing mass first observed by Fritz Zwicky in the 1930s (Caltech; he also introduced name “supernova”) • look at gravitation lensing by a nearby galaxy of a more distant galaxy (many including NIU students Donna Kubik and Matt Weisner. see their theses at www.physics.niu.edu/physics/ac ...
2007_spitzer_lecture_series_kennicutt_talk3
... • spectra best fitted with IMF ~ Salpeter for M* > 1 Mo • SF is ubiquitous when cold gas is present - <4% S-Irr non-detects in Ha, nearly all show trace SF in UV ...
... • spectra best fitted with IMF ~ Salpeter for M* > 1 Mo • SF is ubiquitous when cold gas is present - <4% S-Irr non-detects in Ha, nearly all show trace SF in UV ...
File - Mr. Catt`s Class
... gas/dust clouds. Rapid star formation then used up the gas/dust before a disk had a chance to form. 2. Clouds with lower density would have formed stars less frequently, and the dust and gas would have collapsed into a disk before star formation used it all up. ...
... gas/dust clouds. Rapid star formation then used up the gas/dust before a disk had a chance to form. 2. Clouds with lower density would have formed stars less frequently, and the dust and gas would have collapsed into a disk before star formation used it all up. ...
The first billion years of galaxy formation and evolution
... Molecular hydrogen (H2) is by far the main component of the ISM – but its lack of a permanent dipole moment makes it virtually impossible to observe directly Instead the rotational lines of CO are mainly used to study the ISM ...
... Molecular hydrogen (H2) is by far the main component of the ISM – but its lack of a permanent dipole moment makes it virtually impossible to observe directly Instead the rotational lines of CO are mainly used to study the ISM ...
1 Introduction - Wiley-VCH
... work in any kind of extragalactic source, and are thus widely used as constraints in models of galaxy formation and evolution. Because of their tightness, they are also powerful distance tracers generally used to study the large scale galaxy distribution within the universe. Clearly, a coherent and ...
... work in any kind of extragalactic source, and are thus widely used as constraints in models of galaxy formation and evolution. Because of their tightness, they are also powerful distance tracers generally used to study the large scale galaxy distribution within the universe. Clearly, a coherent and ...
1.5 The Big Bang - Animated Science
... For all we know the Sun stopped shining just over 8 minutes ago. ...
... For all we know the Sun stopped shining just over 8 minutes ago. ...
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).