Galaxies - University of Iowa Astrophysics
... • One can examine how galaxies within a cluster orbit each other. Again, the orbital speeds are higher than expected if only visible matter (including gas visible in X-rays) is taken into account. Thus, clusters of galaxies have dark matter. ...
... • One can examine how galaxies within a cluster orbit each other. Again, the orbital speeds are higher than expected if only visible matter (including gas visible in X-rays) is taken into account. Thus, clusters of galaxies have dark matter. ...
How to kill a galaxy - University of Waterloo
... Galaxy clusters: the end of star formation? • “Dead” galaxies (i.e. little gas or star formation) found in rich clusters • Hierarchical formation models predict number of clusters increases with time. • So perhaps dense environments are responsible for terminating star formation? ...
... Galaxy clusters: the end of star formation? • “Dead” galaxies (i.e. little gas or star formation) found in rich clusters • Hierarchical formation models predict number of clusters increases with time. • So perhaps dense environments are responsible for terminating star formation? ...
Lecture 3 - University of Washington
... determine a, b and n. Sometimes, n is fixed as a function of galaxy’s morphology, and only a and b are fit to the data. Sometimes, de Vaucouleurs profile is expressed as ...
... determine a, b and n. Sometimes, n is fixed as a function of galaxy’s morphology, and only a and b are fit to the data. Sometimes, de Vaucouleurs profile is expressed as ...
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) ...
Lecture notes 18: Galaxies and galaxy clusters
... At scales larger than 100 Mpc the galaxies (matter) seems evenly distributed. Gravitational lenses and dark matter. Galactic cluster dynamics show that there is a great amount of dark matter: there is not enough luminous matter, even when considering the very hot intergalactic gas clouds, to bind ga ...
... At scales larger than 100 Mpc the galaxies (matter) seems evenly distributed. Gravitational lenses and dark matter. Galactic cluster dynamics show that there is a great amount of dark matter: there is not enough luminous matter, even when considering the very hot intergalactic gas clouds, to bind ga ...
Disk Galaxies in the Magneticum Pathfinder Simulations
... physical processes. To distinguish the populations and classify the galaxies, we use a procedure similar to Scannapieco et al. (2008): we align each galaxy along its principal axis of inertia of the stars within 0.1Rvir and subsequently classify it according to the circularity parameter ǫ = jz /jcir ...
... physical processes. To distinguish the populations and classify the galaxies, we use a procedure similar to Scannapieco et al. (2008): we align each galaxy along its principal axis of inertia of the stars within 0.1Rvir and subsequently classify it according to the circularity parameter ǫ = jz /jcir ...
3. Cosmology and the Origin and Evolution of Galaxies
... spectroscopic follow-up at mm wavelengths will place very strong constraints on the evolutionary history of star formation in this important galaxy population, and challenge the currently accepted scenarios for massive-galaxy formation. ...
... spectroscopic follow-up at mm wavelengths will place very strong constraints on the evolutionary history of star formation in this important galaxy population, and challenge the currently accepted scenarios for massive-galaxy formation. ...
Abstract book
... Review/contributions on accretion disk structure and wind and jet launching processes. ADAF, especially at high accretion rate and their relation to emitting regions (continuum and lines) of quasars. Overarching issue: disk (ADAF) structure and its connection to quasar continuum and line emitting re ...
... Review/contributions on accretion disk structure and wind and jet launching processes. ADAF, especially at high accretion rate and their relation to emitting regions (continuum and lines) of quasars. Overarching issue: disk (ADAF) structure and its connection to quasar continuum and line emitting re ...
Word version of Episode 704
... The Andromeda galaxy M31 can just, but only just, be seen with the naked eye. Its light, 2 million years old, is the oldest light you can see with the unaided eye. The Andromeda galaxy, M31, is the nearest neighbour large galaxy to our own Galaxy, the Milky Way. It is about 2.2 million light years a ...
... The Andromeda galaxy M31 can just, but only just, be seen with the naked eye. Its light, 2 million years old, is the oldest light you can see with the unaided eye. The Andromeda galaxy, M31, is the nearest neighbour large galaxy to our own Galaxy, the Milky Way. It is about 2.2 million light years a ...
Lifting the Dusty Veil on the Cradle of Star Birth
... Big Bang; ground-based observations show decline HST, SIRTF, NGST probe the peak and early times ...
... Big Bang; ground-based observations show decline HST, SIRTF, NGST probe the peak and early times ...
The Mystery of the Giant Galactic Blobs
... Dokkum et al 2004) suggests that major star formation ceases in these massive systems very early in their assembly ...
... Dokkum et al 2004) suggests that major star formation ceases in these massive systems very early in their assembly ...
1Cmoles.pdf
... spectroscopic surveys cannot go as deep as the photometric surveys, reaching only I ≈ 24 with the use of large telescopes. The covered fields are necessarily small and cannot cope with the complex variety of objects in the Universe. To get the optimum compromise between large area and depth, good sp ...
... spectroscopic surveys cannot go as deep as the photometric surveys, reaching only I ≈ 24 with the use of large telescopes. The covered fields are necessarily small and cannot cope with the complex variety of objects in the Universe. To get the optimum compromise between large area and depth, good sp ...
Document
... break technique in combination with the new generation of 8- to 10-m telescopes made it possible to identify significant samples of high-redshift objects. Lyman Break Galaxies (LBGs) are color-selected, luminous, star forming galaxies that emitted their light more than 10 billion years ago, e.g., at ...
... break technique in combination with the new generation of 8- to 10-m telescopes made it possible to identify significant samples of high-redshift objects. Lyman Break Galaxies (LBGs) are color-selected, luminous, star forming galaxies that emitted their light more than 10 billion years ago, e.g., at ...
Part2
... o Individual clouds only resolved inside the Local Group by the 30m. o Individual low mass clouds only detectable inside Local Group. o Individual high mass clouds detectable with effort in nearest other groups. o Observing distant galaxies requires averaging many clouds inside a beam (that’s okay, ...
... o Individual clouds only resolved inside the Local Group by the 30m. o Individual low mass clouds only detectable inside Local Group. o Individual high mass clouds detectable with effort in nearest other groups. o Observing distant galaxies requires averaging many clouds inside a beam (that’s okay, ...
Starburst Galaxies Under the Microscope: High
... Starburst galaxies are unique laboratories. Starburst episodes are phases in the evolution of galaxies that are by definition transient, and during which they convert a significant fraction of their gas reservoirs into stars. During a starburst phase a galaxy thus evolves rapidly in stellar, gas, du ...
... Starburst galaxies are unique laboratories. Starburst episodes are phases in the evolution of galaxies that are by definition transient, and during which they convert a significant fraction of their gas reservoirs into stars. During a starburst phase a galaxy thus evolves rapidly in stellar, gas, du ...
2013. CCAT. All Rights Reserved.
... We are developing X-Spec, a multi-object wide-band direct-detection spectrometer for CCAT. X-Spec is designed for rapid full-band (195-510 GHz), moderate resolution (R~700) spectral surveys of galaxies, measuring the bright atomic fine-structure and molecular rotational transitions which cool the in ...
... We are developing X-Spec, a multi-object wide-band direct-detection spectrometer for CCAT. X-Spec is designed for rapid full-band (195-510 GHz), moderate resolution (R~700) spectral surveys of galaxies, measuring the bright atomic fine-structure and molecular rotational transitions which cool the in ...
Stellar-Mass Black Holes and Ultraluminous X
... Most BHXRBs are, however, low-mass x-ray the outburst through Fig. 2, top; a sketch of likely lines (which can be fluorescence lines from neutral binaries, which are almost certainly much older geometries in the soft, intermediate/flaring, and or ionized iron) in this phase. This iron line can than ...
... Most BHXRBs are, however, low-mass x-ray the outburst through Fig. 2, top; a sketch of likely lines (which can be fluorescence lines from neutral binaries, which are almost certainly much older geometries in the soft, intermediate/flaring, and or ionized iron) in this phase. This iron line can than ...
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 answers to five essential questions: ...
... 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 answers to five essential questions: ...
Far-infrared line emission from high
... low-resolution simulations which include all these processes (Baek et al. 2009). Finally, we note that the large gravitational potential of massive galaxies reduces the effects of SN feedback on star formation, as exemplified by fig. 1 of Vallini, Dayal & Ferrara (2012) and related discussion. We in ...
... low-resolution simulations which include all these processes (Baek et al. 2009). Finally, we note that the large gravitational potential of massive galaxies reduces the effects of SN feedback on star formation, as exemplified by fig. 1 of Vallini, Dayal & Ferrara (2012) and related discussion. We in ...
Results from the search for tidal disruption flares in the GALEX Deep
... emission requires excitation by a persistent Seyfert nucleus. ...
... emission requires excitation by a persistent Seyfert nucleus. ...
Wandering in the Redshift Desert
... range coming from the restframe ultraviolet (UV). Just as opportunistic organHRLR RSHKK jMC SGDHQ DBNKNFHB@K MHBGD HM the driest desert, so we currently rely on weak, restframe UV features to explore the redshift desert. In the case of ...
... range coming from the restframe ultraviolet (UV). Just as opportunistic organHRLR RSHKK jMC SGDHQ DBNKNFHB@K MHBGD HM the driest desert, so we currently rely on weak, restframe UV features to explore the redshift desert. In the case of ...
Chapter 31
... • In 1929, Edwin Hubble, by measuring the redshifts and distances of many galaxies, found that the farther away from Earth a galaxy is, the faster it is moving away. • The universe is expanding. • In a medium that is uniformly expanding, all points are moving away from all other points, and no point ...
... • In 1929, Edwin Hubble, by measuring the redshifts and distances of many galaxies, found that the farther away from Earth a galaxy is, the faster it is moving away. • The universe is expanding. • In a medium that is uniformly expanding, all points are moving away from all other points, and no point ...
The Magellan 20 Telescope Science Goals
... in the plane of the sky. A 3D tomographic reconstruction of the mass distribution and kinematics of the IGM becomes possible, mapping tenuous structures with densities down to the mean density of the universe. A combination with a traditional galaxy redshift survey of the same volume sampled by the ...
... in the plane of the sky. A 3D tomographic reconstruction of the mass distribution and kinematics of the IGM becomes possible, mapping tenuous structures with densities down to the mean density of the universe. A combination with a traditional galaxy redshift survey of the same volume sampled by the ...
Diapositiva 1 - Universidad de Guanajuato
... the bar and disc – dwarfs are more frequently E and Irr) the word “normal” for unbarred spirals and lenticulars do not mean that they are more common than barred: about 30% of the spirals and S0s are classified as barred, but this includes only the most extreme examples since this pattern may be u ...
... the bar and disc – dwarfs are more frequently E and Irr) the word “normal” for unbarred spirals and lenticulars do not mean that they are more common than barred: about 30% of the spirals and S0s are classified as barred, but this includes only the most extreme examples since this pattern may be u ...
PHYS3380_113015_bw - The University of Texas at Dallas
... • finally realized that the reason optical spectra were so unusual is that the lines were Doppler shifted by a very large amount, corresponding to velocities away from us that were significant fractions of the speed of light. • objects were thought to be relatively nearby stars, no one had any reaso ...
... • finally realized that the reason optical spectra were so unusual is that the lines were Doppler shifted by a very large amount, corresponding to velocities away from us that were significant fractions of the speed of light. • objects were thought to be relatively nearby stars, no one had any reaso ...
Quasar
Quasars (/ˈkweɪzɑr/) or quasi-stellar radio sources are the most energetic and distant members of a class of objects called active galactic nuclei (AGN). Quasars are extremely luminous and were first identified as being high redshift sources of electromagnetic energy, including radio waves and visible light, that appeared to be similar to stars, rather than extended sources similar to galaxies. Their spectra contain very broad emission lines, unlike any known from stars, hence the name ""quasi-stellar."" Their luminosity can be 100 times greater than that of the Milky Way. Most quasars were formed approximately 12 billion years ago caused by collisions of galaxies and their central black holes merging to form either a supermassive black hole or a Binary black hole system.Although the true nature of these objects was controversial until the early 1980s, there is now a scientific consensus that a quasar is a compact region in the center of a massive galaxy surrounding a central supermassive black hole. Its size is 10–10,000 times the Schwarzschild radius of the black hole. The energy emitted by a quasar derives from mass falling onto the accretion disc around the black hole.