Exploring Neutral Hydrogen and Galaxy Evolution with the SKA
... distribution in galaxies, as well as insight into the relationship between star formation and the interstellar medium, have been limited to the local universe. Ongoing and upcoming H I surveys on SKA pathfinder instruments will extend these measurements beyond the local universe to intermediate reds ...
... distribution in galaxies, as well as insight into the relationship between star formation and the interstellar medium, have been limited to the local universe. Ongoing and upcoming H I surveys on SKA pathfinder instruments will extend these measurements beyond the local universe to intermediate reds ...
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... a very large simulation of the concordance ΛCDM cosmogony. Our procedures follow the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In t ...
... a very large simulation of the concordance ΛCDM cosmogony. Our procedures follow the detailed assembly history of each object and are able to track the evolution of all galaxies more massive than the Small Magellanic Cloud throughout a volume comparable to that of large modern redshift surveys. In t ...
from z=0 to z=1
... 5. The z~0 counterparts of LBGs are a population of compact luminous UV galaxies (UVLG). In terms of Ltot (SFR), UVLGs are more than 10 times fainter than ULIRGs. 6. LBGs and SCUBA galaxies (UV and IR selected galaxies at z~3) do not overlap with each other very much. SCUBA galaxies have significant ...
... 5. The z~0 counterparts of LBGs are a population of compact luminous UV galaxies (UVLG). In terms of Ltot (SFR), UVLGs are more than 10 times fainter than ULIRGs. 6. LBGs and SCUBA galaxies (UV and IR selected galaxies at z~3) do not overlap with each other very much. SCUBA galaxies have significant ...
A new view of galaxy evolution
... the ancestors of the galaxies we that are bright at one filter, but find in the local universe, but are that essentially disappear using just the brightest few that are there. a filter just a bit bluer. This is the These galaxies are very bright and thus traditional way to find distant galaxies easy ...
... the ancestors of the galaxies we that are bright at one filter, but find in the local universe, but are that essentially disappear using just the brightest few that are there. a filter just a bit bluer. This is the These galaxies are very bright and thus traditional way to find distant galaxies easy ...
Galaxy formation in the Planck cosmology - II. Star
... over time. The latter follows only the history of the main component of the galaxy (along the ‘main branch’ of the merger tree) and has been investigated for the Millennium Simulation by Cohn & van de Voort (2015). The difference between the two reflects the merger history of galaxies. The term SFH ...
... over time. The latter follows only the history of the main component of the galaxy (along the ‘main branch’ of the merger tree) and has been investigated for the Millennium Simulation by Cohn & van de Voort (2015). The difference between the two reflects the merger history of galaxies. The term SFH ...
The oxygen abundance deficiency in irregular galaxies
... has been computed. The positions of these models in the Ms /LB versus (B-V) diagram for various values of t0 and for fixed values of other parameters (τ =13 Gyr, n=7, c=0.75) are shown in Fig.1. A similar grid of models with bursting star formation history has also be computed with τ =13 Gyr, n=7, c ...
... has been computed. The positions of these models in the Ms /LB versus (B-V) diagram for various values of t0 and for fixed values of other parameters (τ =13 Gyr, n=7, c=0.75) are shown in Fig.1. A similar grid of models with bursting star formation history has also be computed with τ =13 Gyr, n=7, c ...
Super-solar Metal Abundances in Two Galaxies at ζ ∼ 3.57
... We report on the surprisingly high metallicity measured in two absorption systems at high redshift, detected in the Very Large Telescope spectrum of the afterglow of the gamma-ray burst GRB 090323. The two systems, at redshift z = 3.5673 and z = 3.5774 (separation ∆v ≈ 660 km s−1 ), are dominated by ...
... We report on the surprisingly high metallicity measured in two absorption systems at high redshift, detected in the Very Large Telescope spectrum of the afterglow of the gamma-ray burst GRB 090323. The two systems, at redshift z = 3.5673 and z = 3.5774 (separation ∆v ≈ 660 km s−1 ), are dominated by ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... one tenth the mass of our Sun. The symbol that indicates the mass of the Sun is M ). The relative proportions of stars of a given mass produced during an episode of star formation are, to first approximation, the same everywhere and are described by the so-called initial mass function (IMF). These ...
... one tenth the mass of our Sun. The symbol that indicates the mass of the Sun is M ). The relative proportions of stars of a given mass produced during an episode of star formation are, to first approximation, the same everywhere and are described by the so-called initial mass function (IMF). These ...
Galaxy Evolution
... one tenth the mass of our Sun. The symbol that indicates the mass of the Sun is M ). The relative proportions of stars of a given mass produced during an episode of star formation are, to first approximation, the same everywhere and are described by the so-called initial mass function (IMF). These ...
... one tenth the mass of our Sun. The symbol that indicates the mass of the Sun is M ). The relative proportions of stars of a given mass produced during an episode of star formation are, to first approximation, the same everywhere and are described by the so-called initial mass function (IMF). These ...
AST 346, Galaxies, Part 6
... pc in radius; these are often seen in spiral and dwarf elliptical galaxies. They are fed by the infall of new gas and continued star formation. The nuclear star clusters can hide black holes. H-burning releases 0.7% of the rest mass as energy, but material falling into a black hole can release 10%. ...
... pc in radius; these are often seen in spiral and dwarf elliptical galaxies. They are fed by the infall of new gas and continued star formation. The nuclear star clusters can hide black holes. H-burning releases 0.7% of the rest mass as energy, but material falling into a black hole can release 10%. ...
Galaxies
... These are galaxies with lanes of stars and nebula emanating from a central nucleus Spiral galaxies range from Tightly wound arms and Large central bulge Loosely wound arms and Small central bulge Direct relationship between the tightness of the arms and size of the central bulge Allows classificatio ...
... These are galaxies with lanes of stars and nebula emanating from a central nucleus Spiral galaxies range from Tightly wound arms and Large central bulge Loosely wound arms and Small central bulge Direct relationship between the tightness of the arms and size of the central bulge Allows classificatio ...
Galaxy Sorting
... galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Interstellar ...
... galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Interstellar ...
Star formation and dust extinction properties of local galaxies A. Sakurai
... (SFR) (Takeuchi et al., 2010). Massive stars are known to be good indicators of star formation (SF) activity, since they have a much shorter lifetime (∼106–8 yr) than the age of galaxies and the Universe (∼1010 yr) and therefore are regarded as an “instantaneous” indicator of the SFR in galaxies. Ma ...
... (SFR) (Takeuchi et al., 2010). Massive stars are known to be good indicators of star formation (SF) activity, since they have a much shorter lifetime (∼106–8 yr) than the age of galaxies and the Universe (∼1010 yr) and therefore are regarded as an “instantaneous” indicator of the SFR in galaxies. Ma ...
What Drives the Stellar Mass Growth of Early-Type
... a universal function, partly because of the complexities in obtaining proper observational constraints. The traditional approximation by a single power law (Salpeter 1955) has undergone numerous updates, with more complex functions that include a significant flattening of the slope towards low-mass ...
... a universal function, partly because of the complexities in obtaining proper observational constraints. The traditional approximation by a single power law (Salpeter 1955) has undergone numerous updates, with more complex functions that include a significant flattening of the slope towards low-mass ...
Building galaxies Hunt, Leslie Kipp
... New General Catalogue (NGC) and its successors the First and Second Index Catalogue (IC), published from 1888 to 1908. The combined NGC+IC contains more than 12000 objects, and to this day the brightest extragalactic objects are denoted by their numbers in Dreyer’s catalogue. The nature of these neb ...
... New General Catalogue (NGC) and its successors the First and Second Index Catalogue (IC), published from 1888 to 1908. The combined NGC+IC contains more than 12000 objects, and to this day the brightest extragalactic objects are denoted by their numbers in Dreyer’s catalogue. The nature of these neb ...
20_Testbank
... Answer: The pull of gravity works to slow the expansion rate of the universe. Therefore, in dense regions such as galaxies and clusters of galaxies, gravity is able to overcome the expansion and keep these objects from expanding. However, on larger scales, where the average density is lower, gravity ...
... Answer: The pull of gravity works to slow the expansion rate of the universe. Therefore, in dense regions such as galaxies and clusters of galaxies, gravity is able to overcome the expansion and keep these objects from expanding. However, on larger scales, where the average density is lower, gravity ...
PH607lec08
... • When examined with sufficient resolution, 25% to more than 40% of E galaxies show features due to dust absorption. • The dust lanes seen in E galaxies imply that the absorbing material is distributed in rings or disks. Dust lanes may be aligned with either the major or minor axes, or they may be w ...
... • When examined with sufficient resolution, 25% to more than 40% of E galaxies show features due to dust absorption. • The dust lanes seen in E galaxies imply that the absorbing material is distributed in rings or disks. Dust lanes may be aligned with either the major or minor axes, or they may be w ...
RXTE PCA Contributions to Monitoring Fast Transients
... membership) are just distant, not low luminosity at peak or low average dM/dt . For some orbital periods both persistent and transient binaries exist, with dM/dt probably too high (> 10 -11 Msun yr-1 ) for post-minimum period binaries. During transient decays the disk goes through instabilities (flu ...
... membership) are just distant, not low luminosity at peak or low average dM/dt . For some orbital periods both persistent and transient binaries exist, with dM/dt probably too high (> 10 -11 Msun yr-1 ) for post-minimum period binaries. During transient decays the disk goes through instabilities (flu ...
VLT identifications in the Chandra/XMM
... X-ray background by a mixture of absorbed and unabsorbed AGN, folded with the corresponding luminosity function and its cosmological evolution. According to these models, most AGN spectra are heavily absorbed and about 80% of the light produced by accretion will be absorbed by gas and dust (Fabian e ...
... X-ray background by a mixture of absorbed and unabsorbed AGN, folded with the corresponding luminosity function and its cosmological evolution. According to these models, most AGN spectra are heavily absorbed and about 80% of the light produced by accretion will be absorbed by gas and dust (Fabian e ...
Evolution of galaxy morphology - Lecture 1 - NCRA-TIFR
... they are the basic building blocks of the Universe on large scales they show a broad range in their physical properties Understanding of galaxy formation and evolution is one of the main outstanding problems in modern cosmology there are ∼ 1011 galaxies in the observable universe typical total mass ...
... they are the basic building blocks of the Universe on large scales they show a broad range in their physical properties Understanding of galaxy formation and evolution is one of the main outstanding problems in modern cosmology there are ∼ 1011 galaxies in the observable universe typical total mass ...
2011-GravLens
... Gravitational lenses can be used as gravitational telescopes. The concentrated light from objects seen behind gravitational lenses makes very faint objects appear brighter, larger and therefore more easily studied. One of the most distant object in the universe was discovered by the gravitational le ...
... Gravitational lenses can be used as gravitational telescopes. The concentrated light from objects seen behind gravitational lenses makes very faint objects appear brighter, larger and therefore more easily studied. One of the most distant object in the universe was discovered by the gravitational le ...
Star formation rate in spiral galaxies
... exclusively by O5 stars, which are also very rare, this number can be useful to compare the possible number of young and hot stars in each galaxy. Therefore, among our galaxies, there are some of them that reach only 2400 O5 stars (like object 5 in the table below), while some other galaxies contain ...
... exclusively by O5 stars, which are also very rare, this number can be useful to compare the possible number of young and hot stars in each galaxy. Therefore, among our galaxies, there are some of them that reach only 2400 O5 stars (like object 5 in the table below), while some other galaxies contain ...
Gas fraction and star formation efficiency at z \< 1.0⋆⋆⋆⋆⋆⋆
... weakens the signal by about a factor 5.5 with respect to the previous closer sample, and this outweighs the gain by climbing up the CO ladder. At 0.6 < z < 1.0, the average angular distance is 1550 Mpc; i.e., the beam of 17 corresponds to 127 kpc, so the sources can all be considered as point-like ...
... weakens the signal by about a factor 5.5 with respect to the previous closer sample, and this outweighs the gain by climbing up the CO ladder. At 0.6 < z < 1.0, the average angular distance is 1550 Mpc; i.e., the beam of 17 corresponds to 127 kpc, so the sources can all be considered as point-like ...
THE MORPHOLOGICAL DEMOGRAPHICS OF GALAXIES IN THE
... has been modified from earlier BPZ versions to remove differences between the predicted colors and those of real galaxies, which results in improved BPZ estimates (see Benítez et al. 2004, for details). We note that Coe et al. (2005) have followed a similar approach to estimate the UV-SFR using also ...
... has been modified from earlier BPZ versions to remove differences between the predicted colors and those of real galaxies, which results in improved BPZ estimates (see Benítez et al. 2004, for details). We note that Coe et al. (2005) have followed a similar approach to estimate the UV-SFR using also ...
ULXs: General Properties and Variability - X
... •evidence against beaming (QPOs, broad Fe Lines, eclipses) •At least one object has a break in the PDS at the frequency predicted for M~1000M objects •Associated extended radio sources •General lack of optical Ids (massive stars would be seen) •they lie near, but not in star forming regions Kyoto me ...
... •evidence against beaming (QPOs, broad Fe Lines, eclipses) •At least one object has a break in the PDS at the frequency predicted for M~1000M objects •Associated extended radio sources •General lack of optical Ids (massive stars would be seen) •they lie near, but not in star forming regions Kyoto me ...
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.