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 ...
Jul y 9- 11,
... The early-type galaxy NGC 5044 resides at the center of the X-ray brightest group in the sky. Chandra observations show that the central region of NGC 5044 has been repeatedly perturbed by AGN outbursts. Low frequency radio observations have detected several distinct AGN outbursts and an ALMA observ ...
... The early-type galaxy NGC 5044 resides at the center of the X-ray brightest group in the sky. Chandra observations show that the central region of NGC 5044 has been repeatedly perturbed by AGN outbursts. Low frequency radio observations have detected several distinct AGN outbursts and an ALMA observ ...
Building galaxies Hunt, Leslie Kipp
... that atomic gas mass fraction also varies along the Hubble sequence. On the other hand, the massto-light ratio measured in the B band remains relatively constant with morphology, even toward the very late spiral types (although see Burstein 1982). With data from Roberts & Haynes (1994), Figure 3 sho ...
... that atomic gas mass fraction also varies along the Hubble sequence. On the other hand, the massto-light ratio measured in the B band remains relatively constant with morphology, even toward the very late spiral types (although see Burstein 1982). With data from Roberts & Haynes (1994), Figure 3 sho ...
Evolution of galaxy morphology - Lecture 1 - NCRA-TIFR
... gravitationally bound agglomerations of stars, dust, gas, dark matter. Mass ratio Gas:Stars:Dark Matter - 1:10:100 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 mai ...
... gravitationally bound agglomerations of stars, dust, gas, dark matter. Mass ratio Gas:Stars:Dark Matter - 1:10:100 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 mai ...
Rest-frame Optical Spectra: A Window into Galaxy Formation at z~2
... • It is now possible to obtain robust, unbiased statistical samples of the gaseous and stellar contents of galaxies at z>1. • We are conducting the MOSDEF survey with MOSFIRE on Keck. The survey leverages existing multi-wavelength datasets in the COSMOS, AEGIS, and GOODS-N fields, and will address ...
... • It is now possible to obtain robust, unbiased statistical samples of the gaseous and stellar contents of galaxies at z>1. • We are conducting the MOSDEF survey with MOSFIRE on Keck. The survey leverages existing multi-wavelength datasets in the COSMOS, AEGIS, and GOODS-N fields, and will address ...
Stellar populations in the nuclear regions of nearby radio galaxies
... respectively. This configuration provides the spectral resolution necessary to resolve the Mg b and CaT features and, at the same at 5.1-Å time, offers a wide spectral span: l3350–6000 A at 3.5-Å resolution in resolution in the blue and l7900–9400 A the red. In the 1997 run, in which we assess ...
... respectively. This configuration provides the spectral resolution necessary to resolve the Mg b and CaT features and, at the same at 5.1-Å time, offers a wide spectral span: l3350–6000 A at 3.5-Å resolution in resolution in the blue and l7900–9400 A the red. In the 1997 run, in which we assess ...
here - Ira-Inaf
... coverage of the first galactic quadrant. From these 3 sources, we selected candidates on the basis of distance from the Galactic Center (the farther the object, the more preferable it was), CO(1–0) signal strength, and galactic latitude and sidereal time considerations. Of the 70 GMCs that we observ ...
... coverage of the first galactic quadrant. From these 3 sources, we selected candidates on the basis of distance from the Galactic Center (the farther the object, the more preferable it was), CO(1–0) signal strength, and galactic latitude and sidereal time considerations. Of the 70 GMCs that we observ ...
from z=0 to z=1
... characteristic IR/UV ratios (the means differ by a factor of 10). 2. The morphological and stellar mass distributions of the two populations have good overlaps (> 70%). IR galaxies tend to be more massive and earlier types, with an excess of interacting galaxies, and UV galaxies to be less massive a ...
... characteristic IR/UV ratios (the means differ by a factor of 10). 2. The morphological and stellar mass distributions of the two populations have good overlaps (> 70%). IR galaxies tend to be more massive and earlier types, with an excess of interacting galaxies, and UV galaxies to be less massive a ...
Article PDF - IOPscience
... Received 2009 December 22; accepted 2010 March 11; published 2010 April 5 ...
... Received 2009 December 22; accepted 2010 March 11; published 2010 April 5 ...
Studies of molecular clouds at the Galactic centre Roland Karlsson DECLINATION (B1950)
... and evolution of star-forming complexes, ignition of starbursts as well as the overall kinematic behaviour of the interstellar medium throughout the Galaxy. In spiral galaxies, radial transport of material is considered essential for the build-up of the energy budget and the evolution of the various ...
... and evolution of star-forming complexes, ignition of starbursts as well as the overall kinematic behaviour of the interstellar medium throughout the Galaxy. In spiral galaxies, radial transport of material is considered essential for the build-up of the energy budget and the evolution of the various ...
Star formation in a galactic outflow
... the ratio between ionizing photon flux and gas density; when divided by the speed of light it is the adimensional ionization parameter U) much lower than typically observed in star-forming galaxies. Yet, despite the gas density in the outflow (~600-1,500 cm-3, as inferred from the [SII] doublet) bei ...
... the ratio between ionizing photon flux and gas density; when divided by the speed of light it is the adimensional ionization parameter U) much lower than typically observed in star-forming galaxies. Yet, despite the gas density in the outflow (~600-1,500 cm-3, as inferred from the [SII] doublet) bei ...
sections 23-25 powerpoint
... Elliptical galaxy (E). A spheroidal galaxy containing millions to billions of old low-mass stars and no gas or dust. Spiral Galaxy (S). A galaxy with a spheroidal bulge of several million old low-mass stars and a flattened pancake-like disk of billions of old low-mass and young high-mass stars, alon ...
... Elliptical galaxy (E). A spheroidal galaxy containing millions to billions of old low-mass stars and no gas or dust. Spiral Galaxy (S). A galaxy with a spheroidal bulge of several million old low-mass stars and a flattened pancake-like disk of billions of old low-mass and young high-mass stars, alon ...
instructor notes: weeks 9/10
... bluer in colour than isolated galaxies, presumably because of the presence of recently-created hot young stars. It is believed that a tidal interaction with another galaxy has induced star formation, although the resulting excess luminosity is hidden behind obscuring clouds of gas and dust. Such gal ...
... bluer in colour than isolated galaxies, presumably because of the presence of recently-created hot young stars. It is believed that a tidal interaction with another galaxy has induced star formation, although the resulting excess luminosity is hidden behind obscuring clouds of gas and dust. Such gal ...
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 ...
Luminosity and Mass Functions of Galaxies
... Malmquist Bias: brighter galaxies are easier to detect and are detectable at greater distances. Weight galaxies by 1/Vmax , the maximum volume over which they can be detected. Φ = Σi 1/Vmax,i Accounts for many selection effects: luminosity, redshift, etc. Agrees well with fancier methods. Not strong ...
... Malmquist Bias: brighter galaxies are easier to detect and are detectable at greater distances. Weight galaxies by 1/Vmax , the maximum volume over which they can be detected. Φ = Σi 1/Vmax,i Accounts for many selection effects: luminosity, redshift, etc. Agrees well with fancier methods. Not strong ...
21_Testbank
... 21.3 Short Answer Questions 1) Give examples demonstrating the role of "nature" and "nurture" in galaxy evolution. Answer: Galaxies come in a wide variety of shapes and sizes. Protogalactic clouds that had low angular momentum may have formed spheroidal stellar systems (elliptical galaxies), while ...
... 21.3 Short Answer Questions 1) Give examples demonstrating the role of "nature" and "nurture" in galaxy evolution. Answer: Galaxies come in a wide variety of shapes and sizes. Protogalactic clouds that had low angular momentum may have formed spheroidal stellar systems (elliptical galaxies), while ...
The Extragalactic Group of MPE and USM
... of Massive Galaxies in the FORS Deep and GOODS South fields • Study evolution of galaxies with broadband deep U to K surveys. • LFs, Mass Functions, SFRs do not require spectroscopy but can be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter lumin ...
... of Massive Galaxies in the FORS Deep and GOODS South fields • Study evolution of galaxies with broadband deep U to K surveys. • LFs, Mass Functions, SFRs do not require spectroscopy but can be derived with accurate photometric redshifts. • Advantage of photo z: no color selection bias, fainter lumin ...
mg_colloq - University of Massachusetts Amherst
... compactness require highly dissipative gas process; they may be the telltale of galaxy formation by “cold accretion”. However, current models seem too crude. •They ...
... compactness require highly dissipative gas process; they may be the telltale of galaxy formation by “cold accretion”. However, current models seem too crude. •They ...
Chapter 15 THE MILKY WAY IN RELATION TO OTHER GALAXIES
... radially exponential surface brightness distribution; most bars in spiral galaxies however, have a fairly constant surface brightness. At 2◦.8 a faster decline than the exponential sets in in all colors and this may indicate the onset of a truncation of the stellar distribution caused by the tidal f ...
... radially exponential surface brightness distribution; most bars in spiral galaxies however, have a fairly constant surface brightness. At 2◦.8 a faster decline than the exponential sets in in all colors and this may indicate the onset of a truncation of the stellar distribution caused by the tidal f ...
The evolution of spiral galaxies in clusters Kutdemir, Elif
... precise, it has to be implemented since the former is useless at large distances. Integrated spectra are composite, which means that they have contribution of different types of stars at a given wavelength and this mixture changes with wavelength. Here we will not talk about how this combination pro ...
... precise, it has to be implemented since the former is useless at large distances. Integrated spectra are composite, which means that they have contribution of different types of stars at a given wavelength and this mixture changes with wavelength. Here we will not talk about how this combination pro ...
3. Cosmology and the Origin and Evolution of Galaxies
... These collective results from the continuum extragalactic surveys and the 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 ...
... These collective results from the continuum extragalactic surveys and the 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 ...
Understanding the Astrophysics of Galaxy Evolution: the role of
... Over the past decade and a half, our observational understanding of galaxy evolution has grown enormously. Steidel and collaborators demonstrated that colour selection techniques allow so-called Lyman Break galaxies (LBGs) to be isolated efficiently at redshifts ∼ 3, thus breaking the z = 1 redshift ...
... Over the past decade and a half, our observational understanding of galaxy evolution has grown enormously. Steidel and collaborators demonstrated that colour selection techniques allow so-called Lyman Break galaxies (LBGs) to be isolated efficiently at redshifts ∼ 3, thus breaking the z = 1 redshift ...
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 ...
the Local Group - Simon P Driver
... – in fact, the SMC turns out to be unbound to the LMC so is moving away • smaller galaxies can get torn apart – for example, the Sagittarius dSph is only 15 kpc from the centre of the Milky Way – the MW rotation curve shows that ~1011 Msolar lies within this radius – the Sgr galaxy would need 1 ...
... – in fact, the SMC turns out to be unbound to the LMC so is moving away • smaller galaxies can get torn apart – for example, the Sagittarius dSph is only 15 kpc from the centre of the Milky Way – the MW rotation curve shows that ~1011 Msolar lies within this radius – the Sgr galaxy would need 1 ...
Megamaser
A megamaser is a type of astrophysical maser, which is a naturally occurring source of stimulated spectral line emission. Megamasers are distinguished from astrophysical masers by their large isotropic luminosity. Megamasers have typical luminosities of 103 solar luminosities (L☉), which is 100 million times brighter than masers in the Milky Way, hence the prefix mega. Likewise, the term kilomaser is used to describe masers outside the Milky Way that have luminosities of order L☉, or thousands of times stronger than the average maser in the Milky Way, gigamaser is used to describe masers billions of times stronger than the average maser in the Milky Way, and extragalactic maser encompasses all masers found outside the Milky Way. Most known extragalactic masers are megamasers, and the majority of megamasers are hydroxyl (OH) megamasers, meaning the spectral line being amplified is one due to a transition in the hydroxyl molecule. There are known megamasers for three other molecules: water (H2O), formaldehyde (H2CO), and methine (CH).Water megamasers were the first type of megamaser discovered. The first water megamaser was found in 1979 in NGC 4945, a galaxy in the nearby Centaurus A/M83 Group. The first hydroxyl megamaser was found in 1982 in Arp 220, which is the nearest ultraluminous infrared galaxy to the Milky Way. All subsequent OH megamasers that have been discovered are also in luminous infrared galaxies, and there are a small number of OH kilomasers hosted in galaxies with lower infrared luminosities. Most luminous infrared galaxies have recently merged or interacted with another galaxy, and are undergoing a burst of star formation. Many of the characteristics of the emission in hydroxyl megamasers are distinct from that of hydroxyl masers within the Milky Way, including the amplification of background radiation and the ratio of hydroxyl lines at different frequencies. The population inversion in hydroxyl molecules is produced by far infrared radiation that results from absorption and re-emission of light from forming stars by surrounding interstellar dust. Zeeman splitting of hydroxyl megamaser lines may be used to measure magnetic fields in the masing regions, and this application represents the first detection of Zeeman splitting in a galaxy other than the Milky Way.Water megamasers and kilomasers are found primarily associated with active galactic nuclei, while galactic and weaker extragalactic water masers are found in star forming regions. Despite different environments, the circumstances that produce extragalactic water masers do not seem to be very different from those that produce galactic water masers. Observations of water megamasers have been used to make accurate measurements of distances to galaxies in order to provide constraints on the Hubble constant.