Chapter 24
... somewhat larger than dwarf ellipticals. They typically contain between 108 and 1010 stars. The smallest such galaxies are called dwarf irregulars. As with elliptical galaxies, the dwarf type is the most common irregular. Dwarf ellipticals and dwarf irregulars occur in approximately equal numbers and ...
... somewhat larger than dwarf ellipticals. They typically contain between 108 and 1010 stars. The smallest such galaxies are called dwarf irregulars. As with elliptical galaxies, the dwarf type is the most common irregular. Dwarf ellipticals and dwarf irregulars occur in approximately equal numbers and ...
Evolution of the atomic and molecular gas content of galaxies
... Hi and H2 in radial bins in each galaxy, using both the metallicity-dependent recipes of Krumholz, McKee & Tumlinson (2009, hereafter KMT) and the pressure-based recipe of BR, and self-consistently implemented a H2 -based star formation recipe, within the established semi-analytic modeling framework ...
... Hi and H2 in radial bins in each galaxy, using both the metallicity-dependent recipes of Krumholz, McKee & Tumlinson (2009, hereafter KMT) and the pressure-based recipe of BR, and self-consistently implemented a H2 -based star formation recipe, within the established semi-analytic modeling framework ...
Evolution of the atomic and molecular gas content of galaxies
... Hi and H2 content of galaxies in the Millennium simulations (De Lucia & Blaizot 2007). Power, Baugh & Lacey (2010) carried out a similar project based on postprocessing. Fu et al. (2010, 2012) modeled the partitioning of gas into Hi and H2 in radial bins in each galaxy, using both the metallicity-de ...
... Hi and H2 content of galaxies in the Millennium simulations (De Lucia & Blaizot 2007). Power, Baugh & Lacey (2010) carried out a similar project based on postprocessing. Fu et al. (2010, 2012) modeled the partitioning of gas into Hi and H2 in radial bins in each galaxy, using both the metallicity-de ...
VLT identifications in the Chandra/XMM
... lower flux levels seems to be the dominant population in these samples too (Barger et al., 2001; Rosati et al., 2002; Stern et al., 2002; Szokoly et al., 2002; see below). Interestingly, first examples of the long-sought class of high-redshift, high-luminosity, heavily obscured active galactic nucle ...
... lower flux levels seems to be the dominant population in these samples too (Barger et al., 2001; Rosati et al., 2002; Stern et al., 2002; Szokoly et al., 2002; see below). Interestingly, first examples of the long-sought class of high-redshift, high-luminosity, heavily obscured active galactic nucle ...
Galaxies
... e. the stars in the spiral arms emit most of their energy at radio wavelengths. If the spiral density wave were the only thing producing spiral arms, it would be expected that a. all spiral arms would be dust free. b. all galaxies would have only two smooth spiral arms. c. the Milky Way would be mor ...
... e. the stars in the spiral arms emit most of their energy at radio wavelengths. If the spiral density wave were the only thing producing spiral arms, it would be expected that a. all spiral arms would be dust free. b. all galaxies would have only two smooth spiral arms. c. the Milky Way would be mor ...
Dynamical properties of a large young disk galaxy at z=2.03⋆
... (K= 19.7 − 21.1) and have large stellar masses (M > 1011 M⊙ ). They constitute half of the most rest-frame luminous galaxies (LV > 6 × 1010 h−2 70 L⊙ ) and their number density exceeds model predictions (e.g., Mo et al., 1998) by a factor of two. Obviously, the first and foremost question that needs ...
... (K= 19.7 − 21.1) and have large stellar masses (M > 1011 M⊙ ). They constitute half of the most rest-frame luminous galaxies (LV > 6 × 1010 h−2 70 L⊙ ) and their number density exceeds model predictions (e.g., Mo et al., 1998) by a factor of two. Obviously, the first and foremost question that needs ...
Galaxies
... that they can overlap with each other and with foreground stars. The LSST object catalog will be a compromise, intended to enable a broad spectrum of scientific programs without returning to the original image data. Perhaps the most challenging aspect of constructing a galaxy catalog is the issue of ...
... that they can overlap with each other and with foreground stars. The LSST object catalog will be a compromise, intended to enable a broad spectrum of scientific programs without returning to the original image data. Perhaps the most challenging aspect of constructing a galaxy catalog is the issue of ...
Galaxies - WordPress.com
... A one which shows a circular disk containing only old stars B one which shows a line of stars, gas, and dust passing through a bulbous c C one which shows a cigar-like distribution of yellow, orange, and red stars only D an amorphous concentration of young stars and glowing interstellar gas ...
... A one which shows a circular disk containing only old stars B one which shows a line of stars, gas, and dust passing through a bulbous c C one which shows a cigar-like distribution of yellow, orange, and red stars only D an amorphous concentration of young stars and glowing interstellar gas ...
PPT presentation
... Arnaboldi et al. (1998) have measured the rotation curve and velocity dispersions along two axes of the early type galaxy NGC 1316 (Fornax A) from RV measurements of 43 PNe. The total galactic mass inside 16 kpc radius was derived to be 2.9x1011 solar masses. ...
... Arnaboldi et al. (1998) have measured the rotation curve and velocity dispersions along two axes of the early type galaxy NGC 1316 (Fornax A) from RV measurements of 43 PNe. The total galactic mass inside 16 kpc radius was derived to be 2.9x1011 solar masses. ...
distance
... Or the universe has changed over time so that we can’t see an infinite number of stars ...
... Or the universe has changed over time so that we can’t see an infinite number of stars ...
Superbubble Activity in Star-Forming Galaxies M. S. Oey
... Superbubbles around OB associations are more prominent than singlestar bubbles, and thus have been studied more extensively. Soft X-ray emission has been detected within many objects, which is qualitatively consistent with the adiabatic evolution model. Two classes of X-ray emission have been identi ...
... Superbubbles around OB associations are more prominent than singlestar bubbles, and thus have been studied more extensively. Soft X-ray emission has been detected within many objects, which is qualitatively consistent with the adiabatic evolution model. Two classes of X-ray emission have been identi ...
ALFALFA H-alpha: The Star-Formation-Rate Density
... For astronomers studying past star-formation rates (SFRs), distances play the role of a time machine. Light travels at a finite speed; it travels slowly enough that astronomers can still view light from the Big Bang. Light emitted by the Sun takes more than eight minutes to reach Earth, roughly five ...
... For astronomers studying past star-formation rates (SFRs), distances play the role of a time machine. Light travels at a finite speed; it travels slowly enough that astronomers can still view light from the Big Bang. Light emitted by the Sun takes more than eight minutes to reach Earth, roughly five ...
The Jansky Very Large Array – New Capabilities, New Science
... • Three of the four prior examples employed mm (PdBI) interferometer observations as well as VLA. • The rise of ALMA will strengthen this complementarity, with stellar scientific results. • New example – Wagg and Carilli combine VLA and ALMA for early forming galaxies: – Massive galaxies at z~2 must ...
... • Three of the four prior examples employed mm (PdBI) interferometer observations as well as VLA. • The rise of ALMA will strengthen this complementarity, with stellar scientific results. • New example – Wagg and Carilli combine VLA and ALMA for early forming galaxies: – Massive galaxies at z~2 must ...
STELLAR AGE VERSUS MASS OF EARLY
... ago. Similar results were obtained at higher redshifts, for which the rest-frame UV can be probed with optical surveys: Kaviraj et al. (2007b) found “compelling evidence that early-types of all luminosities form stars over the lifetime of the Universe”. Again, less massive objects were found to have ...
... ago. Similar results were obtained at higher redshifts, for which the rest-frame UV can be probed with optical surveys: Kaviraj et al. (2007b) found “compelling evidence that early-types of all luminosities form stars over the lifetime of the Universe”. Again, less massive objects were found to have ...
SUB-KILOPARSEC IMAGING OF COOL MOLECULAR GAS IN
... these galaxies in low-J CO (either CO(1–0) or CO(2–1)). In this paper, we present high-resolution observations of low-J CO emission in two DSFGs from the SPT sample performed with the Australia Telescope Compact Array (ATCA). Both objects have been observed at comparable (∼0.5”) resolution by ALMA a ...
... these galaxies in low-J CO (either CO(1–0) or CO(2–1)). In this paper, we present high-resolution observations of low-J CO emission in two DSFGs from the SPT sample performed with the Australia Telescope Compact Array (ATCA). Both objects have been observed at comparable (∼0.5”) resolution by ALMA a ...
The Origin and Evolution of Dust in Galaxies
... Lower metallicities do not hamper dust formation in AGB stars Origins of dust in high-z galaxies are still open question. Dust mass in high-z galaxies may be explained, if both SNe and AGB stars contribute dust formation The orign and evolution of dust in galaxies ...
... Lower metallicities do not hamper dust formation in AGB stars Origins of dust in high-z galaxies are still open question. Dust mass in high-z galaxies may be explained, if both SNe and AGB stars contribute dust formation The orign and evolution of dust in galaxies ...
The 2008 RBSE Journal - National Optical Astronomy Observatory
... The star formations within the galaxy that ends up creating most of the stars are known as ultra-luminous clusters. They are about 10-20 light-years across and can have luminosities up to 100 million times that of the Sun. These clusters are the densest starforming environments known. The thing that ...
... The star formations within the galaxy that ends up creating most of the stars are known as ultra-luminous clusters. They are about 10-20 light-years across and can have luminosities up to 100 million times that of the Sun. These clusters are the densest starforming environments known. The thing that ...
Constraining the star formation histories of spiral bulges
... gradients are observed in line strengths, similar to those exhibited by elliptical galaxies. The bulge data are also consistent with correlations between Mg2, Mg2 gradient and central velocity dispersion observed in elliptical galaxies. In contrast to elliptical galaxies, central line strengths lie ...
... gradients are observed in line strengths, similar to those exhibited by elliptical galaxies. The bulge data are also consistent with correlations between Mg2, Mg2 gradient and central velocity dispersion observed in elliptical galaxies. In contrast to elliptical galaxies, central line strengths lie ...
Chapter 15 Stars, Galaxies, and Universe
... in a spiral galaxy called the Milky Way. From the side, the Milky Way appears to be a narrow disk with a bulge in the middle. The galaxy’s spiral structure is visible only from above or below. Center is 25,000 light years away from Earth ...
... in a spiral galaxy called the Milky Way. From the side, the Milky Way appears to be a narrow disk with a bulge in the middle. The galaxy’s spiral structure is visible only from above or below. Center is 25,000 light years away from Earth ...
EROs and submm galaxies: Expectations for FMOS in the
... These were selected to have R-K>5.5 from the optical/infrared data of T. Haynes et al. (2002). ...
... These were selected to have R-K>5.5 from the optical/infrared data of T. Haynes et al. (2002). ...
– 1 – 1. Emission Lines in Nearby Galaxies 1.1.
... all forbidden lines, which means they have low transition probabilities. When the 4363 Å line is too weak to be detected, one can use strong-line ratios as first laid out by Pagel et al (1979). R23 = ([OII]3727 + [OIII]4959, 5007)/Hβ is the most common such ratio. The problem is that R23 is not mon ...
... all forbidden lines, which means they have low transition probabilities. When the 4363 Å line is too weak to be detected, one can use strong-line ratios as first laid out by Pagel et al (1979). R23 = ([OII]3727 + [OIII]4959, 5007)/Hβ is the most common such ratio. The problem is that R23 is not mon ...
A GMOS dissection of the line-of
... Our observations show that there is no large cluster in front of the quasar, but rather several smaller groups at different redshifts. Hard to tell if there is strong magnification present from current data. Statistical properties of high-z radio quasars may be more useful in determining importance ...
... Our observations show that there is no large cluster in front of the quasar, but rather several smaller groups at different redshifts. Hard to tell if there is strong magnification present from current data. Statistical properties of high-z radio quasars may be more useful in determining importance ...
Summary of Talks at Growing Black Holes 2004 in Garching
... z objects -> implication : rapid chemical enrichment near the quasar itself (although not necessarily in the galaxy farther out). NV emission implies multiple generations of star formation. Fe II emission might be from metal-free Pop III stars. BH mass estimates. Work of Vestergaard and Dietrich/H ...
... z objects -> implication : rapid chemical enrichment near the quasar itself (although not necessarily in the galaxy farther out). NV emission implies multiple generations of star formation. Fe II emission might be from metal-free Pop III stars. BH mass estimates. Work of Vestergaard and Dietrich/H ...
The Formation and Evolution of Massive Black Holes - Ira-Inaf
... disrupt an unlucky star passing too close by (20). The gravitational potential energy of the accreted mass is converted to radiation, making the black hole luminous. Luminous, accreting MBHs are generally referred to as active galactic nuclei, and the most powerful among them are known as quasars. Q ...
... disrupt an unlucky star passing too close by (20). The gravitational potential energy of the accreted mass is converted to radiation, making the black hole luminous. Luminous, accreting MBHs are generally referred to as active galactic nuclei, and the most powerful among them are known as quasars. Q ...
Pea galaxy
A Pea galaxy, also referred to as a Pea or Green Pea, might be a type of Luminous Blue Compact Galaxy which is undergoing very high rates of star formation. Pea galaxies are so-named because of their small size and greenish appearance in the images taken by the Sloan Digital Sky Survey (SDSS).Pea Galaxies were first discovered in 2007 by the volunteer users within the forum section of the online astronomy project Galaxy Zoo (GZ).