![Probing nuclear activity versus star formation at z ∼ 0.8 using near](http://s1.studyres.com/store/data/014762860_1-b30eb7364e81ecb5b6ea23510307b20f-300x300.png)
Probing nuclear activity versus star formation at z ∼ 0.8 using near
... as X-ray-selected AGN with no evidence for nuclear accretion activity in optical spectroscopy, showing stellar emission-dominated or obscured optical-to-infrared (IR) SEDs instead, practically indistinguishable from those of spiral/starburst galaxies (Alonso-Herrero et al. 2004, 2008; Rigby et al. 2 ...
... as X-ray-selected AGN with no evidence for nuclear accretion activity in optical spectroscopy, showing stellar emission-dominated or obscured optical-to-infrared (IR) SEDs instead, practically indistinguishable from those of spiral/starburst galaxies (Alonso-Herrero et al. 2004, 2008; Rigby et al. 2 ...
Carbon-enhanced metal-poor stars in dwarf galaxies
... Iwamoto et al. 2005; Joggerst et al. 2009; Marassi et al. 2014; Tominaga et al. 2014). A reatively good agreement with observations is also obtained by models of zero- (or very low-) metallicity massive “spinstars”, which experience mixing and mass loss because of their very high-rotational velociti ...
... Iwamoto et al. 2005; Joggerst et al. 2009; Marassi et al. 2014; Tominaga et al. 2014). A reatively good agreement with observations is also obtained by models of zero- (or very low-) metallicity massive “spinstars”, which experience mixing and mass loss because of their very high-rotational velociti ...
Unravelling the Origin and Evolution of Our Galaxy
... Solar System predicted that they would not form so close to the central star, where temperatures are high, and where the amount of protoplanetary disc matter was believed to be small. A transit across the face of the parent star has been observed for one system, and this leads to estimates of the ra ...
... Solar System predicted that they would not form so close to the central star, where temperatures are high, and where the amount of protoplanetary disc matter was believed to be small. A transit across the face of the parent star has been observed for one system, and this leads to estimates of the ra ...
Article PDF - IOPscience
... ^ 0.09(random) ^ 0.16(systematic), which agrees well with previous determinations via Cepheid variables. Dolphin (1999b) has studied the star formation history in two Ðelds in the LMC. His results, which are summarized in Table 1, appear to show (1) a steady rise of the metallicity index [Fe/H] with ...
... ^ 0.09(random) ^ 0.16(systematic), which agrees well with previous determinations via Cepheid variables. Dolphin (1999b) has studied the star formation history in two Ðelds in the LMC. His results, which are summarized in Table 1, appear to show (1) a steady rise of the metallicity index [Fe/H] with ...
Image filtering
... Optimizing SExtractor performance • Execution speed Current rule of thumb: ~1Mpix/s per GHz at high galactic latitude • Turns out to be I/O-limited in some cases: might be useful to use different devices for reading and writing data • In crowded fields, limited by source-density: 500+ extractions ...
... Optimizing SExtractor performance • Execution speed Current rule of thumb: ~1Mpix/s per GHz at high galactic latitude • Turns out to be I/O-limited in some cases: might be useful to use different devices for reading and writing data • In crowded fields, limited by source-density: 500+ extractions ...
File
... This unusual long arm shows lots of young blue star clusters. But NGC 772 also possesses many weak, tightly coiled arms which, although well formed, are relatively smooth, indicating only a small current rate of star formation. The relatively smooth multiple arms on the opposite side from the promin ...
... This unusual long arm shows lots of young blue star clusters. But NGC 772 also possesses many weak, tightly coiled arms which, although well formed, are relatively smooth, indicating only a small current rate of star formation. The relatively smooth multiple arms on the opposite side from the promin ...
A Budget and Accounting of Metals at z~ 0: Results from the COS
... of oxygen in their ISM. COS-Halos has specifically addressed the metal content of diffuse halo gas. The current study aims to place these findings on highly ionized oxygen into the larger context of metal masses contained within all galactic and circumgalactic components: stars, dust, and the other ...
... of oxygen in their ISM. COS-Halos has specifically addressed the metal content of diffuse halo gas. The current study aims to place these findings on highly ionized oxygen into the larger context of metal masses contained within all galactic and circumgalactic components: stars, dust, and the other ...
Plotting the Rotation Curve of M31
... Answer: large collections of stars. They vary in their morphology and stellar composition i.e. ellipticals are red and contain older stars than spirals which are predominantly blue/white in colour and younger. What is a spectrum? Answer: a ‘fingerprint’ of an object made of light. The spectrum of vis ...
... Answer: large collections of stars. They vary in their morphology and stellar composition i.e. ellipticals are red and contain older stars than spirals which are predominantly blue/white in colour and younger. What is a spectrum? Answer: a ‘fingerprint’ of an object made of light. The spectrum of vis ...
Order of Magnitude Icebreaker
... ★ Use your physical intuition, not google! ★ Remember: Multiple approaches possible! ...
... ★ Use your physical intuition, not google! ★ Remember: Multiple approaches possible! ...
THE UV-OPTICAL COLOR MAGNITUDE DIAGRAM. II. PHYSICAL
... GALEX data were obtained as part of the GALEX Medium Imaging Survey (MIS; Martin et al. 2005), cataloged as part of an internal data release 1.1 (IR1.1) and processed using standard GALEX pipeline processing (Morrissey et al. 2005, 2007). The MIS reaches a limiting UV magnitude of 23 through single ...
... GALEX data were obtained as part of the GALEX Medium Imaging Survey (MIS; Martin et al. 2005), cataloged as part of an internal data release 1.1 (IR1.1) and processed using standard GALEX pipeline processing (Morrissey et al. 2005, 2007). The MIS reaches a limiting UV magnitude of 23 through single ...
PPT presentation
... • Two point sources bright in the on-band and fainter but visible in the offband. Could be high-z quasars or star forming regions or even a PN within a globular cluster in NGC 4697, as reported recently in the case of NGC 5128 by Minniti and Rejkuba. Again no confusion is possible since the continuu ...
... • Two point sources bright in the on-band and fainter but visible in the offband. Could be high-z quasars or star forming regions or even a PN within a globular cluster in NGC 4697, as reported recently in the case of NGC 5128 by Minniti and Rejkuba. Again no confusion is possible since the continuu ...
argo and other tidal structures around the milky way
... should be more or less symmetrically distributed, two methods were used to identify asymmetries in the (l, b) distribution of 2MASS M giants that may be the signature of stellar overdensities: (1) direct symmetry checking in fields reflected across various hypothesized Galactic symmetric great circl ...
... should be more or less symmetrically distributed, two methods were used to identify asymmetries in the (l, b) distribution of 2MASS M giants that may be the signature of stellar overdensities: (1) direct symmetry checking in fields reflected across various hypothesized Galactic symmetric great circl ...
FLARE SWG theme 3: high
... hosts… but less great if lose shorter wavelength (<1.5um), which are required for the rest-frame UV lines. (3) Very few (~5-10) spec-ID’d z>6 quasars from FLARE unless quasars drive the spectroscopic programme (galaxies ...
... hosts… but less great if lose shorter wavelength (<1.5um), which are required for the rest-frame UV lines. (3) Very few (~5-10) spec-ID’d z>6 quasars from FLARE unless quasars drive the spectroscopic programme (galaxies ...
- MNASSA Page
... more than 30 arc minutes. It is a very nice object to study through binoculars. The Magellanic Cloud is home to NGC 2070, also known as Bennett 35, the great looped nebula situated in the south-eastern part of the Cloud and probably one of the most amazing objects in the southern night sky. Known as ...
... more than 30 arc minutes. It is a very nice object to study through binoculars. The Magellanic Cloud is home to NGC 2070, also known as Bennett 35, the great looped nebula situated in the south-eastern part of the Cloud and probably one of the most amazing objects in the southern night sky. Known as ...
Eye in the sky - Academy of Science of South Africa
... Later in history there was massive exchange of knowledge between West Africa and the Islamic world that probably started over a thousand years ago when Muslim North Africa started trading with West Africa during the Ghana empire. The Ghana empire covered parts of Mauritania, Mali and Senegal and col ...
... Later in history there was massive exchange of knowledge between West Africa and the Islamic world that probably started over a thousand years ago when Muslim North Africa started trading with West Africa during the Ghana empire. The Ghana empire covered parts of Mauritania, Mali and Senegal and col ...
The correlation between galaxy morphology and star
... appear more common, and traditional Hubble types do not appear to be present at these epochs (Giavalisco et al. 1996a,b; Steidel et al. 1996; Lowenthal et al. 1997; Lotz et al. 2004; Papovich et al. 2005; Lotz et al. 2006; Ravindranath et al. 2006; Law et al. 2007; Conselice et al. 2008). This is ge ...
... appear more common, and traditional Hubble types do not appear to be present at these epochs (Giavalisco et al. 1996a,b; Steidel et al. 1996; Lowenthal et al. 1997; Lotz et al. 2004; Papovich et al. 2005; Lotz et al. 2006; Ravindranath et al. 2006; Law et al. 2007; Conselice et al. 2008). This is ge ...
The local spiral structure of the Milky Way
... some spiral arm segments in the solar neighborhood were clearly identified (2, 3). Since then, many models have been proposed (4) and debated (5). Popular models (6, 7) suggest a grand design morphology with two- or four-armed spiral structure (8), such as M 51 or NGC 1232 (Fig. 1). Still, today, th ...
... some spiral arm segments in the solar neighborhood were clearly identified (2, 3). Since then, many models have been proposed (4) and debated (5). Popular models (6, 7) suggest a grand design morphology with two- or four-armed spiral structure (8), such as M 51 or NGC 1232 (Fig. 1). Still, today, th ...
Stars, Galaxies, Superuniverses and the Urantia Book, by Frederick
... stars in our Milky Way galaxy is estimated to be around 200 to 400 billion. This is pretty good agreement with our average number since our galaxy is the second largest in our local cluster of about 30 galaxies, and thus may be considered to be an exceptionally large galaxy. There are many more smal ...
... stars in our Milky Way galaxy is estimated to be around 200 to 400 billion. This is pretty good agreement with our average number since our galaxy is the second largest in our local cluster of about 30 galaxies, and thus may be considered to be an exceptionally large galaxy. There are many more smal ...
2_ISM - UCT Astronomy Department
... Why? The history review of history of determining shape and size of galaxies have shown the importance of dust absorption and scattering, and Rayleigh scattering in the determination of the true size of the Galaxy • distances to object in the Galaxy • mapping distances to other galaxies • determinat ...
... Why? The history review of history of determining shape and size of galaxies have shown the importance of dust absorption and scattering, and Rayleigh scattering in the determination of the true size of the Galaxy • distances to object in the Galaxy • mapping distances to other galaxies • determinat ...
SUB-KILOPARSEC IMAGING OF COOL MOLECULAR GAS IN
... galaxy, these CO observations confirm that the background source is undergoing a major merger, while the velocity field of the other source is more complex. We use the ATCA CO observations and comparable resolution Atacama Large Millimeter/submillimeter Array dust continuum imaging of the same objec ...
... galaxy, these CO observations confirm that the background source is undergoing a major merger, while the velocity field of the other source is more complex. We use the ATCA CO observations and comparable resolution Atacama Large Millimeter/submillimeter Array dust continuum imaging of the same objec ...
Chapter 14 Black Holes as Central Engines
... appeared to be points with no obvious spatial extension, just as one would expect for stars. • These were often called “radio stars”, but they had very strange characteristics for stars. • In 1963, the first two of these radio stars were associated with the radio sources 3C48 and 3C273, respectively ...
... appeared to be points with no obvious spatial extension, just as one would expect for stars. • These were often called “radio stars”, but they had very strange characteristics for stars. • In 1963, the first two of these radio stars were associated with the radio sources 3C48 and 3C273, respectively ...
The HERMES GALAH survey: overview
... For large spirals like the Milky Way, the thick disk mass is typically about 10% of the thin disk, and its vertical scale height is about 1000 pc; the scale height of the thin disk is typically about 300 pc. Near the sun, the thick disk is more metal poor, although the abundance ranges of the thick ...
... For large spirals like the Milky Way, the thick disk mass is typically about 10% of the thin disk, and its vertical scale height is about 1000 pc; the scale height of the thin disk is typically about 300 pc. Near the sun, the thick disk is more metal poor, although the abundance ranges of the thick ...
Chapter 19 Stars Galaxies and the Universe
... a black hole. Even though they are called holes, black holes aren’t really empty spaces. A black hole is an object so dense that even light cannot escape its gravity. Because black holes do not give off light, it can be hard for scientists to locate them. Gas and dust from a nearby star may fall int ...
... a black hole. Even though they are called holes, black holes aren’t really empty spaces. A black hole is an object so dense that even light cannot escape its gravity. Because black holes do not give off light, it can be hard for scientists to locate them. Gas and dust from a nearby star may fall int ...
Gamma Ray Burst Afterglows and Host Galaxies
... Deaths of Massive Stars Afterglow data suggests that GRBs occur… • in galaxies with active star formation, • often in regions with a lot of gas, which is where new stars form and where the most massive stars spend their entire brief lives. However, GRBs are so rare that only a tiny fraction of massi ...
... Deaths of Massive Stars Afterglow data suggests that GRBs occur… • in galaxies with active star formation, • often in regions with a lot of gas, which is where new stars form and where the most massive stars spend their entire brief lives. However, GRBs are so rare that only a tiny fraction of massi ...
Galaxy Zoo
![](https://commons.wikimedia.org/wiki/Special:FilePath/Galaxyzoo.jpg?width=300)
Galaxy Zoo is a crowdsourced astronomy project which invites people to assist in the morphological classification of large numbers of galaxies. (e.g.) It is an example of citizen science as it enlists the help of members of the public to help in scientific research. There have been seven versions up to July 2014, which are outlined in this article. Galaxy Zoo is part of the Zooniverse, a group of citizen science projects.