Recent Star Formation in Nearby Early-type Galaxies
... we could reach down to a detection limit of just 0.1 Å for the equivalent width (EW) of the emission lines and detect extended ionized gas emission in 75% of the early-type galaxies in the sauron representative sample, confirming that these systems contain gas more often than not. Although the limit ...
... we could reach down to a detection limit of just 0.1 Å for the equivalent width (EW) of the emission lines and detect extended ionized gas emission in 75% of the early-type galaxies in the sauron representative sample, confirming that these systems contain gas more often than not. Although the limit ...
The Co-evolution of Galaxies and their Supermassive Black Holes
... 1) No evidence of any enhancement due to the presence of a close companion. 2) More weakly clustered than control galaxies on “intermediate” scales (100 kpc-1 Mpc) 3) In dark matter halos with masses ~10^12 M_solar ...
... 1) No evidence of any enhancement due to the presence of a close companion. 2) More weakly clustered than control galaxies on “intermediate” scales (100 kpc-1 Mpc) 3) In dark matter halos with masses ~10^12 M_solar ...
Galaxy properties
... They contain dust (sometimes visible as dusty lanes), and gas. They contain young stars, but also old stellar populations are present (Roberts & Haynes, 1994). As mentioned above, a separate intermediate type are lenticular galaxies: S0 (L). They are characterized by the ellipse axis ratio b/a < 0.3 ...
... They contain dust (sometimes visible as dusty lanes), and gas. They contain young stars, but also old stellar populations are present (Roberts & Haynes, 1994). As mentioned above, a separate intermediate type are lenticular galaxies: S0 (L). They are characterized by the ellipse axis ratio b/a < 0.3 ...
A Physical Model for the Anisotropies of Cosmic Far-infrared Background
... from MgII absorber provides lower limit ...
... from MgII absorber provides lower limit ...
The Hubble Law - Department of Astronomy
... There are a couple of features you should especially note when trying to decipher these spectra: 1. Not all of the "jiggly" lines come from the light of the galaxy. Each spectrum contains noise; we just cannot get away from it. You should notice that some of the spectra are much "noisier" than othe ...
... There are a couple of features you should especially note when trying to decipher these spectra: 1. Not all of the "jiggly" lines come from the light of the galaxy. Each spectrum contains noise; we just cannot get away from it. You should notice that some of the spectra are much "noisier" than othe ...
Galaxies
... Elliptical Galaxies Elliptical galaxies come in many sizes, from giant ellipticals of trillions of stars, down to dwarf ellipticals of less than a million stars Ellipticals also contain very little, if any, cool gas and dust, and they show no evidence of ongoing star formation Many do, however, hav ...
... Elliptical Galaxies Elliptical galaxies come in many sizes, from giant ellipticals of trillions of stars, down to dwarf ellipticals of less than a million stars Ellipticals also contain very little, if any, cool gas and dust, and they show no evidence of ongoing star formation Many do, however, hav ...
The Host Galaxies of the Brightest Quasars: Gas
... quasar and its host, and the small angular size of the host are the main limitations to a spectroscopic study. Quasar host galaxies are typically 2–3 magnitudes fainter than their central quasar. Their angular size is only a few arcseconds at low redshift (z ~ 0.1–0.3). Figure 1 gives an example of ...
... quasar and its host, and the small angular size of the host are the main limitations to a spectroscopic study. Quasar host galaxies are typically 2–3 magnitudes fainter than their central quasar. Their angular size is only a few arcseconds at low redshift (z ~ 0.1–0.3). Figure 1 gives an example of ...
spatially resolved properties of the stellar populations
... assembled their mass through dissipative processes and in-situ star formation. The star formation is induced by cold flow accretion or by gas-rich mergers. Then, ex-situ star formation formed by minor mergers of galaxies with the central more massive one. Because the central core of these ETG have e ...
... assembled their mass through dissipative processes and in-situ star formation. The star formation is induced by cold flow accretion or by gas-rich mergers. Then, ex-situ star formation formed by minor mergers of galaxies with the central more massive one. Because the central core of these ETG have e ...
CMB-Wed-Crittenden
... We can calculate the amplitude of the signal for size estimator for convergence, using Euclid-like observations. For such a deep survey, the intrinsic-intrinsic correlations are suppressed. However, the cross correlation between lensing and intrinsic signals is still significant, as large as 30% on ...
... We can calculate the amplitude of the signal for size estimator for convergence, using Euclid-like observations. For such a deep survey, the intrinsic-intrinsic correlations are suppressed. However, the cross correlation between lensing and intrinsic signals is still significant, as large as 30% on ...
Dark Matter: Observational Constraints
... • Since Dark Matter is by definition, dark, its observational constraints are generally of a dynamical nature. What this means is that there are only two equations of importance: ...
... • Since Dark Matter is by definition, dark, its observational constraints are generally of a dynamical nature. What this means is that there are only two equations of importance: ...
Document
... • Construct and operate many (>30) 0.4 meter telescopes around the globe for education and outreach. • Remote operations, data management, and instrument construction based in Santa Barbara. • Strong connection to UC-Santa Barbara. Tim Brown is LCOGT Scientific Director and Adjunct Professor of Phys ...
... • Construct and operate many (>30) 0.4 meter telescopes around the globe for education and outreach. • Remote operations, data management, and instrument construction based in Santa Barbara. • Strong connection to UC-Santa Barbara. Tim Brown is LCOGT Scientific Director and Adjunct Professor of Phys ...
PowerPoint Lecture - UCSD Department of Physics
... Other, familiar naked-eye stars are Sirius and Procyon, each on the left edge of the disk. ...
... Other, familiar naked-eye stars are Sirius and Procyon, each on the left edge of the disk. ...
Expansion of the Universe
... 1. Draw nine galaxies (dots) on the balloon (away from the valve on the inflatable part of the balloon). Mark one of these galaxies as the “home” galaxy, number the remaining galaxies 1 through 8. The “home” galaxy will be the galaxy that you live in and are making your measurements from. 2. Blow up ...
... 1. Draw nine galaxies (dots) on the balloon (away from the valve on the inflatable part of the balloon). Mark one of these galaxies as the “home” galaxy, number the remaining galaxies 1 through 8. The “home” galaxy will be the galaxy that you live in and are making your measurements from. 2. Blow up ...
The Milky Way`s Collision with the Andromeda Galaxy
... continue to draw closer, their speeds will increase. In time, both galaxies will distort due to the tidal pull of gravity, and some of their stars will be thrown into long, streamer-like tails. These features are commonly seen in other colliding galaxies. As the merger progresses, both galaxies will ...
... continue to draw closer, their speeds will increase. In time, both galaxies will distort due to the tidal pull of gravity, and some of their stars will be thrown into long, streamer-like tails. These features are commonly seen in other colliding galaxies. As the merger progresses, both galaxies will ...
8-4.9 - S2TEM Centers SC
... 2. Ask them to share what they know about it. 3. Make sure they are aware that a galaxy is a very large collection of stars, dust, and gas held together by the force of gravity. They should also be aware that not all galaxies look the same. 4. Provide students with copies of the activity sheet and t ...
... 2. Ask them to share what they know about it. 3. Make sure they are aware that a galaxy is a very large collection of stars, dust, and gas held together by the force of gravity. They should also be aware that not all galaxies look the same. 4. Provide students with copies of the activity sheet and t ...
Word version - GyVe
... galaxy clusters. The format expected for each of these files is below. Each file is white space delimited (tabs or space). An example of these formats can be found in the documentation section of the sourceforge site for this project. It should also be noted that GyVe actually only uses the RA decim ...
... galaxy clusters. The format expected for each of these files is below. Each file is white space delimited (tabs or space). An example of these formats can be found in the documentation section of the sourceforge site for this project. It should also be noted that GyVe actually only uses the RA decim ...
GALAXY ZOO Backwards Faded Scaffolding Inquiry Lab constructed
... Imagine your team has been assigned the task of designing a scientific observation plan for your favorite news blog about galaxies that collide and merge into a single, larger galaxy. Describe precisely what evidence you would need to collect in order to answer the research question of, “What fracti ...
... Imagine your team has been assigned the task of designing a scientific observation plan for your favorite news blog about galaxies that collide and merge into a single, larger galaxy. Describe precisely what evidence you would need to collect in order to answer the research question of, “What fracti ...
Power Point
... publish results • once published Subaru results may go back to GMRT TAC for another sample of field galaxies • other possibilities: - obtain more redshifts for coadding particularly on the outskirts of the clusters - stellar mass measurements using redshifts and additional near-infrared imaging ...
... publish results • once published Subaru results may go back to GMRT TAC for another sample of field galaxies • other possibilities: - obtain more redshifts for coadding particularly on the outskirts of the clusters - stellar mass measurements using redshifts and additional near-infrared imaging ...
bennerttucson.win
... The Nature of QSO Host Galaxies Dunlop et al. (2003): 33 AGNs (RQQs, RLQs, RGs, 0.1
... The Nature of QSO Host Galaxies Dunlop et al. (2003): 33 AGNs (RQQs, RLQs, RGs, 0.1
Nbody
... Simulation of star cluster(6500 stars) orbiting the galactic center for 0.75 Myr. Initial density profile is a King model. Cluster starts at 4pc from galactic center but spirals in. 1 orbit = 105 yrs. Notice the star colors in the tidal tails; these researchers include stellar evolution with dynami ...
... Simulation of star cluster(6500 stars) orbiting the galactic center for 0.75 Myr. Initial density profile is a King model. Cluster starts at 4pc from galactic center but spirals in. 1 orbit = 105 yrs. Notice the star colors in the tidal tails; these researchers include stellar evolution with dynami ...
Absolute vs. relative distance measures
... ,3DE Q: H;8 5 WFG654:9 ;H `3D aQ:O ;4 9F6R98 GFW9 ;H 6R9 WFGP :946893 ...
... ,3DE Q: H;8 5 WFG654:9 ;H `3D aQ:O ;4 9F6R98 GFW9 ;H 6R9 WFGP :946893 ...
Building galaxies Hunt, Leslie Kipp
... plates, the Hubble sequence is in fact a physical one. Several quantifiable parameters vary significantly with Hubble type. Already from photographic material it was known that optical colors (U −B, B −V ) and surface brightness depend on morphological type with later type spirals tending to have fa ...
... plates, the Hubble sequence is in fact a physical one. Several quantifiable parameters vary significantly with Hubble type. Already from photographic material it was known that optical colors (U −B, B −V ) and surface brightness depend on morphological type with later type spirals tending to have fa ...
Chapter 15 THE MILKY WAY IN RELATION TO OTHER GALAXIES
... size is difficult. Although studies on photographic plates are available from the earliest days of photometry (de Vaucouleurs (1957) observed the LMC very early on in his studies and determined the exponential nature of its disk), the prime method today is the use of CCD’s behind small telescopes (o ...
... size is difficult. Although studies on photographic plates are available from the earliest days of photometry (de Vaucouleurs (1957) observed the LMC very early on in his studies and determined the exponential nature of its disk), the prime method today is the use of CCD’s behind small telescopes (o ...
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).