Ch24
... The luminosity is a measure of absolute brightness. The fact that the apparent brightness is less than the absolute brightness is a consequence of distance. Hence the distance, D. ...
... The luminosity is a measure of absolute brightness. The fact that the apparent brightness is less than the absolute brightness is a consequence of distance. Hence the distance, D. ...
Galaxies
... Figure 9.7 shows the magnitude–radius relation for dwarf galaxies at a variety of distances. Nearby dwarf galaxies within a few Mpc and distant faint galaxies are well-separated in this space; their low photometric redshifts will further help to distinguish them. An important question will be the ex ...
... Figure 9.7 shows the magnitude–radius relation for dwarf galaxies at a variety of distances. Nearby dwarf galaxies within a few Mpc and distant faint galaxies are well-separated in this space; their low photometric redshifts will further help to distinguish them. An important question will be the ex ...
Here - Cornell Astronomy
... taught during the fall semester of 2008 by Professors Don Campbell and Martha Haynes with the always willing and able assistance of Astronomy graduate student Kassie Wells. In addition to providing an overview of the diverse science that is based on observations made with the Arecibo telescope, Astr ...
... taught during the fall semester of 2008 by Professors Don Campbell and Martha Haynes with the always willing and able assistance of Astronomy graduate student Kassie Wells. In addition to providing an overview of the diverse science that is based on observations made with the Arecibo telescope, Astr ...
The SAMI Galaxy Survey: extraplanar gas, galactic winds, and their
... et al. 2005 for a review). The optical line-emitting gas usually presents well-defined conical structures, which are the limb-brightened parts of the expanding X-ray bubbles that also entrain the ambient cold gas. As the bubbles expand supersonically, shock waves excite optical emission lines and pr ...
... et al. 2005 for a review). The optical line-emitting gas usually presents well-defined conical structures, which are the limb-brightened parts of the expanding X-ray bubbles that also entrain the ambient cold gas. As the bubbles expand supersonically, shock waves excite optical emission lines and pr ...
Far-ultraviolet and far-infrared bivariate luminosity function of galaxies:
... star formation rate (hereafter SFR) has been of central importance to an understanding of the formation and evolution of galaxies. However, this has been a difficult task for a long time because of dust extinction. Active star formation (SF) is always accompanied by dust production through various d ...
... star formation rate (hereafter SFR) has been of central importance to an understanding of the formation and evolution of galaxies. However, this has been a difficult task for a long time because of dust extinction. Active star formation (SF) is always accompanied by dust production through various d ...
Molecular Gas in Late-stage Merging Galaxies
... and the total far-infrared luminosity. This suggests that the physical activities that are responsible for increasing luminosity, namely starburst/AGN, are related to the formation of the extended molecular gas disks. The molecular gas disks in the merger remnants show various properties, and we co ...
... and the total far-infrared luminosity. This suggests that the physical activities that are responsible for increasing luminosity, namely starburst/AGN, are related to the formation of the extended molecular gas disks. The molecular gas disks in the merger remnants show various properties, and we co ...
Article PDF - IOPscience
... A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and modelindependent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural ...
... A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and modelindependent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural ...
(if any) Galaxy Properties Depend on Environment at High Redshift?
... – How does the SF-density relation evolve? – Is environmental quenching efficiency invariant with galaxy mass? – What drives these relations? Gain insight by: – testing for galaxy properties that vary with environment? – When (at what epoch) do they manifest? – over what timescale(s) do the effects ...
... – How does the SF-density relation evolve? – Is environmental quenching efficiency invariant with galaxy mass? – What drives these relations? Gain insight by: – testing for galaxy properties that vary with environment? – When (at what epoch) do they manifest? – over what timescale(s) do the effects ...
Lecture 1 - Kavli IPMU
... if the source of the light is in motion towards or away from the observer, spectral lines become blue- or red-shifted: ...
... if the source of the light is in motion towards or away from the observer, spectral lines become blue- or red-shifted: ...
Hubble`s Law
... velocity of the Andromeda galaxy (M31), and found it moving towards us at 300 kilometres per second. ...
... velocity of the Andromeda galaxy (M31), and found it moving towards us at 300 kilometres per second. ...
studies - European Southern Observatory
... sample of the redshift-stellar mass-star formation rate, parameter space for log(M*/M)>9.7 star-forming galaxies (see Methods and Extended Data Figure 1). Star-forming galaxies over the entire mass range of the parent sample enter the stack (Extended Data Figure 1). Within the uncertainties, the st ...
... sample of the redshift-stellar mass-star formation rate, parameter space for log(M*/M)>9.7 star-forming galaxies (see Methods and Extended Data Figure 1). Star-forming galaxies over the entire mass range of the parent sample enter the stack (Extended Data Figure 1). Within the uncertainties, the st ...
Lifetime of merger features of equal
... a single stellar population using population synthesis models. This method is effective because of its simplicity and applicability. Several studies have examined the observable properties of merger remnants by assuming the total amount of dust extinction from empirical data (Kaviraj et al. 2009; Ga ...
... a single stellar population using population synthesis models. This method is effective because of its simplicity and applicability. Several studies have examined the observable properties of merger remnants by assuming the total amount of dust extinction from empirical data (Kaviraj et al. 2009; Ga ...
CUSPS AND CORES IN GALAXIES:PROBLEMS AND - Cosmo-ufes
... the gas density and temperature. Top Left.Chandra image of Abell 2029. Top Right.Radial gas density profile of Abell 2029 (large circles) fit to several standard parameterizations. This parameterized fit is then fed into equation for M(r), along with the temperature profile to calculate the enclosed ...
... the gas density and temperature. Top Left.Chandra image of Abell 2029. Top Right.Radial gas density profile of Abell 2029 (large circles) fit to several standard parameterizations. This parameterized fit is then fed into equation for M(r), along with the temperature profile to calculate the enclosed ...
Stellar Populations of Dwarf Elliptical Galaxies: UBVRI Photometry
... low mass versions of elliptical galaxies (e.g., Lin & Faber 1983; Kormendy 1985; Ichikawa, Wakamatsu, & Okamura 1986; Caldwell & Bothun 1987; Binggeli & Cameron 1991). Unlike their giant counterparts, gas-poor dwarf elliptical galaxies and gas-rich dwarf irregular galaxies have similar stellar distr ...
... low mass versions of elliptical galaxies (e.g., Lin & Faber 1983; Kormendy 1985; Ichikawa, Wakamatsu, & Okamura 1986; Caldwell & Bothun 1987; Binggeli & Cameron 1991). Unlike their giant counterparts, gas-poor dwarf elliptical galaxies and gas-rich dwarf irregular galaxies have similar stellar distr ...
The Milky Way - Cobb Learning
... ones) => Look for very young clusters or associations containing O and B stars: O/B Associations=one of the star groupings; bright high mass stars; 10-200 stars ...
... ones) => Look for very young clusters or associations containing O and B stars: O/B Associations=one of the star groupings; bright high mass stars; 10-200 stars ...
No Slide Title
... The WLM galaxy has one GC, [Fe/H] = –1.52 age = 14.8 Gyrs (Hodge et al. 1999). ...
... The WLM galaxy has one GC, [Fe/H] = –1.52 age = 14.8 Gyrs (Hodge et al. 1999). ...
Gas Mass Fractions and the Evolution of Spiral Galaxies
... The data have been selected to be as inclusive as possible given the demands placed on information content. We make no claim that these data are complete in any volume limited sense. For our present purposes, this is less important than having data representative of all morphological types, luminosi ...
... The data have been selected to be as inclusive as possible given the demands placed on information content. We make no claim that these data are complete in any volume limited sense. For our present purposes, this is less important than having data representative of all morphological types, luminosi ...
active galactic nuclei (AGNs) between two BOSS
... insensitive to the local environment. In addition, I note that in the LOWZ sample, stellar mass and stellar velocity dispersion distributions of star forming galaxies and AGNs are nearly same. Keywords Galaxies: active-- galaxies: statistics 1. INTRODUCTION In the past, some issues of active galacti ...
... insensitive to the local environment. In addition, I note that in the LOWZ sample, stellar mass and stellar velocity dispersion distributions of star forming galaxies and AGNs are nearly same. Keywords Galaxies: active-- galaxies: statistics 1. INTRODUCTION In the past, some issues of active galacti ...
Universe 8e Lecture Chapter 23 Our Galaxy
... According to the density-wave theory, spiral arms are created by density waves that sweep around the Galaxy. The gravitational field of this spiral pattern compresses the interstellar clouds through which it passes, thereby triggering the formation of the OB associations and H II regions that illumi ...
... According to the density-wave theory, spiral arms are created by density waves that sweep around the Galaxy. The gravitational field of this spiral pattern compresses the interstellar clouds through which it passes, thereby triggering the formation of the OB associations and H II regions that illumi ...
A Spectroscopically Confirmed Excess of 24 micron Sources in a
... Also, instead of focusing on massive clusters, the key to understanding the interplay between galaxy evolution and environment is to study galaxy groups because: 1) most galaxies in the local universe are in groups (e.g. Geller & Huchra 1983); and 2) hierarchical structure formation predicts that ga ...
... Also, instead of focusing on massive clusters, the key to understanding the interplay between galaxy evolution and environment is to study galaxy groups because: 1) most galaxies in the local universe are in groups (e.g. Geller & Huchra 1983); and 2) hierarchical structure formation predicts that ga ...
Chapter 5 The Evolutionary Paths Of Nearby Galaxies
... not (see Figure 5.1 middle and bottom rows). A comparison of the cluster and ‘field’ colour-mass diagrams clearly shows that very few disk galaxies have their star formation suppressed outside the cluster environment. The vast majority of transition spirals are in fact composed of Hi deficient clust ...
... not (see Figure 5.1 middle and bottom rows). A comparison of the cluster and ‘field’ colour-mass diagrams clearly shows that very few disk galaxies have their star formation suppressed outside the cluster environment. The vast majority of transition spirals are in fact composed of Hi deficient clust ...
Galactic Thin Disk - Caltech Astronomy
... remarkably constant at 21.6 B magnitudes arcsec−2 . In the meantime, many galaxies with fainter central surface brightnesses have been found, but these are mostly small dwarf galaxies or a minority of so-called low-surfacebrightness galaxies (constituting a small fraction of the mass in stars in the ...
... remarkably constant at 21.6 B magnitudes arcsec−2 . In the meantime, many galaxies with fainter central surface brightnesses have been found, but these are mostly small dwarf galaxies or a minority of so-called low-surfacebrightness galaxies (constituting a small fraction of the mass in stars in the ...
Accreting Supermassive Black Holes and their
... Solid and long-dashed curves are for T_i with M_{accr} (a) = 10^(-4) , (b) = 10^(-3) (c) = 10^(-2) & (d) = 10^(-2). short-dashed and dotted curves are for T_e with same parameters. M_BH = 10^9 solar mass. M_{accr} in Edd unit. (Ghosh 2015b ) ...
... Solid and long-dashed curves are for T_i with M_{accr} (a) = 10^(-4) , (b) = 10^(-3) (c) = 10^(-2) & (d) = 10^(-2). short-dashed and dotted curves are for T_e with same parameters. M_BH = 10^9 solar mass. M_{accr} in Edd unit. (Ghosh 2015b ) ...
Galaxies - hwchemistry
... • Also, searches for white dwarfs and brown dwarfs in the halo of Milky Way have been successful. – Nevertheless, the searches have not turned up enough of these low-luminosity objects to make up all the dark matter. ...
... • Also, searches for white dwarfs and brown dwarfs in the halo of Milky Way have been successful. – Nevertheless, the searches have not turned up enough of these low-luminosity objects to make up all the dark matter. ...
Galaxy Formation, Reionization, the First Stars and Quasars
... using the 21cm line. Several experiments are now being constructed or planned to do this, e.g., the Mileura Wide-Field Array in Australia, or the Square Kilometer Array (SKA) ...
... using the 21cm line. Several experiments are now being constructed or planned to do this, e.g., the Mileura Wide-Field Array in Australia, or the Square Kilometer Array (SKA) ...
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).