Gas fraction and star formation efficiency at z< 1.0
... main sequence have a morphology intermediate between the MS and quiecent objects (Wuyts et al. 2011). To better clarify the role of each physical process in the SFH decline in the second half of the Universe’s history, it is of prime importance to determine the gas content, spatial extent and surfac ...
... main sequence have a morphology intermediate between the MS and quiecent objects (Wuyts et al. 2011). To better clarify the role of each physical process in the SFH decline in the second half of the Universe’s history, it is of prime importance to determine the gas content, spatial extent and surfac ...
Rest-frame Optical Spectra: A Window into Galaxy Formation at z~2
... • We typically target a small number of Xray and/or IR-selected AGNs on each mask. • Use MOSFIRE spectra to identify additional AGNs. • We will study AGN demographics, distributions of BH accretion rates, methods of AGN detection. • With early sample of AGNs (red X-ray, burgunday IR), we are sta ...
... • We typically target a small number of Xray and/or IR-selected AGNs on each mask. • Use MOSFIRE spectra to identify additional AGNs. • We will study AGN demographics, distributions of BH accretion rates, methods of AGN detection. • With early sample of AGNs (red X-ray, burgunday IR), we are sta ...
Galaxies, Cosmology and Dark Matter - IA
... The Galaxy was built in two phases: 1. In the beginning the gas collapsed within a few hundred million years from a large volume: → metal poor stars (and GCs) with negligible rotation → halo 2. After that a slower, dissipative phase followed: → because of its angular momentum, the gas concentrated m ...
... The Galaxy was built in two phases: 1. In the beginning the gas collapsed within a few hundred million years from a large volume: → metal poor stars (and GCs) with negligible rotation → halo 2. After that a slower, dissipative phase followed: → because of its angular momentum, the gas concentrated m ...
Recent Star Formation in Nearby Early-type Galaxies
... can show substantial amounts of CO emission, which generally traces regularly rotating molecular disks (e.g., Young 2002, 2005). More recently, Combes, Young & Bureau (2007) have followed up with single-dish observations 43 out of the 48 early-type galaxies in the sauron sample, detecting CO emissio ...
... can show substantial amounts of CO emission, which generally traces regularly rotating molecular disks (e.g., Young 2002, 2005). More recently, Combes, Young & Bureau (2007) have followed up with single-dish observations 43 out of the 48 early-type galaxies in the sauron sample, detecting CO emissio ...
Chapter 24
... than possessing a dense central nucleus, they often exhibit little internal structure of any kind. As with spirals, the stellar density increases sharply in the central nucleus. Denoted by the letter E, these systems are subdivided according to how elliptical they appear on the sky. The most circula ...
... than possessing a dense central nucleus, they often exhibit little internal structure of any kind. As with spirals, the stellar density increases sharply in the central nucleus. Denoted by the letter E, these systems are subdivided according to how elliptical they appear on the sky. The most circula ...
EROs and submm galaxies: Expectations for FMOS in the
... Galaxies with S850~8mJy have SFRs ~1000MΘ/yr. This is a sensitive function of the assumed dust temperature (T6 for z<3). Optical spectroscopy gives ~10-20MΘ/yr on average. ...
... Galaxies with S850~8mJy have SFRs ~1000MΘ/yr. This is a sensitive function of the assumed dust temperature (T6 for z<3). Optical spectroscopy gives ~10-20MΘ/yr on average. ...
Introduction to Observational Cosmology
... The basic pillars of our cosmological picture (i.e. we are starting with the answer first) 1. Averaged over sufficiently large scales, the universe is nearly homogeneous and isotropic (=cosmological principle) 2. The universe, i.e. space itself, is expanding so that the distance D between any pairs ...
... The basic pillars of our cosmological picture (i.e. we are starting with the answer first) 1. Averaged over sufficiently large scales, the universe is nearly homogeneous and isotropic (=cosmological principle) 2. The universe, i.e. space itself, is expanding so that the distance D between any pairs ...
File 11 - School of Astronomy, IPM
... • M87 is Super giant galaxy. • Also known as M87, Virgo A or NGC ...
... • M87 is Super giant galaxy. • Also known as M87, Virgo A or NGC ...
Document
... nebulae were merely in our own Galaxy, while others suggested that they were very far away—“island universes” in their own right, so distant that the individual stars appeared blurred together. The distance and nature of the spiral nebulae was the subject of the well-publicized “Shapley-Curtis debat ...
... nebulae were merely in our own Galaxy, while others suggested that they were very far away—“island universes” in their own right, so distant that the individual stars appeared blurred together. The distance and nature of the spiral nebulae was the subject of the well-publicized “Shapley-Curtis debat ...
13.1 Galaxy Evolution: Introduction
... we can look at the diffuse backgrounds, the collective emission of all galaxies ever. Now, that has a drawback of not knowing which source is where until you actually resolve the background. But, it bypasses selection effects, because you get everything, whether or not individual ga ...
... we can look at the diffuse backgrounds, the collective emission of all galaxies ever. Now, that has a drawback of not knowing which source is where until you actually resolve the background. But, it bypasses selection effects, because you get everything, whether or not individual ga ...
Sample pages 1 PDF
... Furthermore, we can observe the local dynamics of stars and gas clouds as well as the properties of satellite galaxies (such the Magellanic Clouds). Finally, the Galactic center at a distance of only 8 kpc gives us the unique opportunity to examine the central region of a galaxy at very high resolut ...
... Furthermore, we can observe the local dynamics of stars and gas clouds as well as the properties of satellite galaxies (such the Magellanic Clouds). Finally, the Galactic center at a distance of only 8 kpc gives us the unique opportunity to examine the central region of a galaxy at very high resolut ...
lecture course
... The entire theoretical framework on which AGNs are based is somewhat less secure than for stars. This is in part due to the extreme conditions near these very massive black holes of 106 to 109 solar masses, which is quite unlike anything we can test in laboratories on Earth (we are in the strong fie ...
... The entire theoretical framework on which AGNs are based is somewhat less secure than for stars. This is in part due to the extreme conditions near these very massive black holes of 106 to 109 solar masses, which is quite unlike anything we can test in laboratories on Earth (we are in the strong fie ...
talk
... Baryonic fraction for NGC 3741 (within the extent of the gas disk) ~ 0.18 ► comparable to other galaxies with less extended HI disk No evidence for baryon loss (measured within the extent of gas disk) in faint dwarf galaxies (contradiction to simulations of galaxy formation !) To reconcile rot ...
... Baryonic fraction for NGC 3741 (within the extent of the gas disk) ~ 0.18 ► comparable to other galaxies with less extended HI disk No evidence for baryon loss (measured within the extent of gas disk) in faint dwarf galaxies (contradiction to simulations of galaxy formation !) To reconcile rot ...
mg_colloq - University of Massachusetts Amherst
... Detection rate of individual sources is about 6% for both compact, 4% for non compact Consistent with the small incidence of AGN among LBG Absence of evidence is NOT evidence of absence, but presence of AGN does not seem obvious ...
... Detection rate of individual sources is about 6% for both compact, 4% for non compact Consistent with the small incidence of AGN among LBG Absence of evidence is NOT evidence of absence, but presence of AGN does not seem obvious ...
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. ...
Stellar populations in the nuclear regions of nearby radio galaxies
... the variations are correlated with the position at which the telescope is pointing. Since flat-fielding is crucial for the reddest wavelengths, where the sky lines are most prominent, after every exposure of 20–30 min we acquired a flat-field in the same position of the telescope as the one for whic ...
... the variations are correlated with the position at which the telescope is pointing. Since flat-fielding is crucial for the reddest wavelengths, where the sky lines are most prominent, after every exposure of 20–30 min we acquired a flat-field in the same position of the telescope as the one for whic ...
The Final Version of the White Paper is available.
... The characterization of exoplanets is one of the outstanding key science cases for HIRES. The focus will be on characterizing exo-planet atmospheres over a wide range of masses, from Neptune-like down to Earth-like including those in the habitable zones, in terms of chemical composition, stratificat ...
... The characterization of exoplanets is one of the outstanding key science cases for HIRES. The focus will be on characterizing exo-planet atmospheres over a wide range of masses, from Neptune-like down to Earth-like including those in the habitable zones, in terms of chemical composition, stratificat ...
Chapter 16
... important object to us but only one of the many billions of galaxies visible in the sky. We can no more understand galaxies by understanding a single example, the Milky Way, than we could understand humanity by understanding a single person. This chapter expands our horizon to discuss the different ...
... important object to us but only one of the many billions of galaxies visible in the sky. We can no more understand galaxies by understanding a single example, the Milky Way, than we could understand humanity by understanding a single person. This chapter expands our horizon to discuss the different ...
Starburst Galaxies Encyclopedia of Astronomy & Astrophysics eaa.iop.org T Heckman
... of interstellar gas in the starburst divided by the present rate of star formation. This is then a rough estimate of how much longer the starburst can be sustained before running out of gas. Gas-depletion times in starbursts are usually of order 108 yr, but they are highly uncertain for many reasons ...
... of interstellar gas in the starburst divided by the present rate of star formation. This is then a rough estimate of how much longer the starburst can be sustained before running out of gas. Gas-depletion times in starbursts are usually of order 108 yr, but they are highly uncertain for many reasons ...
THE DAWN OF X-RAY ASTRONOMY
... From its beginning in 1962 until today, the instrumentation for x-ray astronomical observations has improved in sensitivity by more than 9 orders of magnitude, comparable to the entire improvement from the capability of the naked eye to those of the current generation of 8- or 10-meter telescopes. A ...
... From its beginning in 1962 until today, the instrumentation for x-ray astronomical observations has improved in sensitivity by more than 9 orders of magnitude, comparable to the entire improvement from the capability of the naked eye to those of the current generation of 8- or 10-meter telescopes. A ...
Power Point
... Radio Continuum vs. [OII] Star Formation Rate Average 87 red [OII] emission galaxies 81 blue [OII] emission galaxies line from Bell 2003 ...
... Radio Continuum vs. [OII] Star Formation Rate Average 87 red [OII] emission galaxies 81 blue [OII] emission galaxies line from Bell 2003 ...
The environment of high-redshift AGN OLIMPIA JUDIT FOGASY
... revealed that galaxies come in many different colours and sizes and they undergo cosmic evolution. Studies of the Milky Way and nearby galaxies helped to reveal the basic building blocks of galaxies and understand the underlying physics that connects them. In the most general sense a galaxy is a gra ...
... revealed that galaxies come in many different colours and sizes and they undergo cosmic evolution. Studies of the Milky Way and nearby galaxies helped to reveal the basic building blocks of galaxies and understand the underlying physics that connects them. In the most general sense a galaxy is a gra ...
The evolution of spiral galaxies in clusters Kutdemir, Elif
... some of which will later merge to form large spheroidal galaxies (Baugh et al. 1996). Observations of galaxy mergers and signatures of accretion support this picture. Evidence have been accumulating, mainly from HI studies, on the importance of cold gas accretion in the local universe: A large numbe ...
... some of which will later merge to form large spheroidal galaxies (Baugh et al. 1996). Observations of galaxy mergers and signatures of accretion support this picture. Evidence have been accumulating, mainly from HI studies, on the importance of cold gas accretion in the local universe: A large numbe ...
Chapter 15 Normal and Active Galaxies
... Although short-exposure images can appear starlike, many quasars show jets or other signs of intense activity. Copyright © 2010 Pearson Education, Inc. ...
... Although short-exposure images can appear starlike, many quasars show jets or other signs of intense activity. Copyright © 2010 Pearson Education, Inc. ...
Chapter 1: Introduction to Galaxies File - QMplus
... Spiral galaxies have much gas within their discs, plus some embedded dust, which amounts to 1-20% of their visible mass (the rest of the visible mass is stars). This gas shows active star formation. The discs contain stars having a range of ages as a result of this continuing star formation. Spiral ...
... Spiral galaxies have much gas within their discs, plus some embedded dust, which amounts to 1-20% of their visible mass (the rest of the visible mass is stars). This gas shows active star formation. The discs contain stars having a range of ages as a result of this continuing star formation. Spiral ...
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.