Magnetic Fields in Lensing Elliptical Galaxies D. Narasimha1, S. M.
... will establish that the observed magnetic field is in the Intervening Medium rather than at the Source. ...
... will establish that the observed magnetic field is in the Intervening Medium rather than at the Source. ...
Worksheet - Science4Inquiry.com
... amount of air added to the balloons. 1. What did you notice about the measurements in your data? (Answers will vary but students should be able to see that the measurements keep getting larger and larger) 2. Can you devise an explanation of your data based on your observations? (Students should be a ...
... amount of air added to the balloons. 1. What did you notice about the measurements in your data? (Answers will vary but students should be able to see that the measurements keep getting larger and larger) 2. Can you devise an explanation of your data based on your observations? (Students should be a ...
Where are the First Stars now?
... A first striking effect is the bias towards earlier formation for stars which end up inside the cluster. Thus half the stars which lie within the final virial radius form before z = 4 while half the stars outside this radius form after z = 2. The first 1.5% of stars in cluster galaxies have already ...
... A first striking effect is the bias towards earlier formation for stars which end up inside the cluster. Thus half the stars which lie within the final virial radius form before z = 4 while half the stars outside this radius form after z = 2. The first 1.5% of stars in cluster galaxies have already ...
StructForm
... this is also the epoch of highest quasar activity; galaxy clusters are forming. In LCDM growth of structure on large (linear) scales has nearly stopped, but smaller non-linear scales continue to evolve. z=0 -Small galaxies continue to get merged to form larger ones; in an open and lambda universes l ...
... this is also the epoch of highest quasar activity; galaxy clusters are forming. In LCDM growth of structure on large (linear) scales has nearly stopped, but smaller non-linear scales continue to evolve. z=0 -Small galaxies continue to get merged to form larger ones; in an open and lambda universes l ...
High-z Universe – cont`d
... High-z Universe – cont’d Both the low and high z ends are unique to WFC3. The redshift interval z = 1-3 is unexplored because a systematic study requires high sensitivity below 3000 A over a large FOV. The figure illustrates a color selection criterion to isolate low redshift objects through the Ly ...
... High-z Universe – cont’d Both the low and high z ends are unique to WFC3. The redshift interval z = 1-3 is unexplored because a systematic study requires high sensitivity below 3000 A over a large FOV. The figure illustrates a color selection criterion to isolate low redshift objects through the Ly ...
Formation of Galaxies
... Minimum fragment mass ~ g mp ~ 0.01 M a robust but wrong result! Resolution: continuing accretion of cold gas, eventually halted by feedback that taps stellar energy via MHD turbulence3 vs Ý M gas ~ G first stars were massive ...
... Minimum fragment mass ~ g mp ~ 0.01 M a robust but wrong result! Resolution: continuing accretion of cold gas, eventually halted by feedback that taps stellar energy via MHD turbulence3 vs Ý M gas ~ G first stars were massive ...
ASTRO-114--Lecture 49-
... merge and they turn into one giant galaxy. If we look down in the center of that galaxy, if we take a long exposure photograph just of that galaxy and look down in the center, we find more than one nucleus. We find four or five nuclei of different galaxies. So this is a merged galaxy. It’s not an or ...
... merge and they turn into one giant galaxy. If we look down in the center of that galaxy, if we take a long exposure photograph just of that galaxy and look down in the center, we find more than one nucleus. We find four or five nuclei of different galaxies. So this is a merged galaxy. It’s not an or ...
Spectro-Morphology of Galaxies.
... types of galaxies. Star-forming regions and young blue stars are prominent in rest-frame (RF) UV whereas older stellar population are observed in RF visible. Consequently, the morphology of galaxies at these two wavelengths could extremely change in the case of two-component stellar population galax ...
... types of galaxies. Star-forming regions and young blue stars are prominent in rest-frame (RF) UV whereas older stellar population are observed in RF visible. Consequently, the morphology of galaxies at these two wavelengths could extremely change in the case of two-component stellar population galax ...
The properties and evolution of low surface brightness galaxies de
... (Zwaan et al. 1995). Here, we confirm this with rotation curve decompositions of two galaxies selected for their nearly identical location in the TF plane, but with very different surface brightnesses. This choice is made to isolate galaxies whose gross properties are similar, so that differences in ...
... (Zwaan et al. 1995). Here, we confirm this with rotation curve decompositions of two galaxies selected for their nearly identical location in the TF plane, but with very different surface brightnesses. This choice is made to isolate galaxies whose gross properties are similar, so that differences in ...
The Thickness of Stellar Disks in Early
... Meanwhile, the average thickness of galactic disks has no more value than the mean temperature in a hospital. Galactic disks can display very different dynamic evolution, due primarily to the density of the environment, as well as the prominence and structure of the spheroidal components of the galax ...
... Meanwhile, the average thickness of galactic disks has no more value than the mean temperature in a hospital. Galactic disks can display very different dynamic evolution, due primarily to the density of the environment, as well as the prominence and structure of the spheroidal components of the galax ...
H I in Early-Type Galaxies. II. Mass Loss and Galactic Winds
... the look-back time. Finally, in view of the similarity in morphology between NGC 4472 and other ellipticals, the larger discrepancy for NGC 4472 may well be typical for the class of elliptical galaxies as a whole. For all these reasons, we feel the discrepancy is real, although more stringent upper ...
... the look-back time. Finally, in view of the similarity in morphology between NGC 4472 and other ellipticals, the larger discrepancy for NGC 4472 may well be typical for the class of elliptical galaxies as a whole. For all these reasons, we feel the discrepancy is real, although more stringent upper ...
NGC 1569 A Dwarf galaxy with a Giant Starburst Stefanie Mhhle1,2
... We have studied the distribution and kinematics of the neutral atomic hydrogen in NGC 1569 using a high-resolution HI data cube complemented with single-dish observations. The velocity structure is ...
... We have studied the distribution and kinematics of the neutral atomic hydrogen in NGC 1569 using a high-resolution HI data cube complemented with single-dish observations. The velocity structure is ...
bennerttucson.win
... accretion onto BH more common, triggering mechanism more common ULIRGs: close connection between mergers and QSO activity (e.g. Canalizo & Stockton 2001) Most QSOs: begin life as mergers (e.g. Sanders et al. 1988)? reside in old ellipticals (e.g. Dunlop et al. 2003)? ...
... accretion onto BH more common, triggering mechanism more common ULIRGs: close connection between mergers and QSO activity (e.g. Canalizo & Stockton 2001) Most QSOs: begin life as mergers (e.g. Sanders et al. 1988)? reside in old ellipticals (e.g. Dunlop et al. 2003)? ...
The Milky Way Galaxy
... The Milky Way Galaxy The infinitude of creation is great enough to make a world, or a Milky Way of worlds, look in comparison with it what a flower or an insect does in comparison with the Earth. ...
... The Milky Way Galaxy The infinitude of creation is great enough to make a world, or a Milky Way of worlds, look in comparison with it what a flower or an insect does in comparison with the Earth. ...
Star formation and dust extinction properties of local galaxies A. Sakurai
... order to have a secure sample of galaxies with redshift data, we made a cross-match of AKARI sources with the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), a redshift catalog recently published by Wang and Rowan-Robinson (2009). The IIFSCz is based on the IRAS Faint Source Catalog (FSC). In the IRA ...
... order to have a secure sample of galaxies with redshift data, we made a cross-match of AKARI sources with the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), a redshift catalog recently published by Wang and Rowan-Robinson (2009). The IIFSCz is based on the IRAS Faint Source Catalog (FSC). In the IRA ...
Clustering of far-infrared galaxies in the AKARI All-Sky Survey North
... Then, given our selection criteria, we expect the contamination of both Galactic and extragalactic groups classified by our algorithm, to be of the order of 2–4%. This result is supported by tests based on a sample of AKARI All-Sky Survey sources identified in public databases, in a similar way as u ...
... Then, given our selection criteria, we expect the contamination of both Galactic and extragalactic groups classified by our algorithm, to be of the order of 2–4%. This result is supported by tests based on a sample of AKARI All-Sky Survey sources identified in public databases, in a similar way as u ...
Exam # 3 – Tue 12/06/2011
... E. all of the above 31. Globular clusters are: A. clusters of stars located in the disks of galaxies B. clusters of stars located in the bulges of galaxies C. clusters of the youngest stars in a galaxy D. clusters of stars located in the haloes of galaxies E. clusters of the most metal rich stars in ...
... E. all of the above 31. Globular clusters are: A. clusters of stars located in the disks of galaxies B. clusters of stars located in the bulges of galaxies C. clusters of the youngest stars in a galaxy D. clusters of stars located in the haloes of galaxies E. clusters of the most metal rich stars in ...
Do non-relativistic neutrinos constitute the dark matter
... Two galaxy clusters crossed each other. And so did their dark matter. ...
... Two galaxy clusters crossed each other. And so did their dark matter. ...
The SZ effect in nearby galaxies
... • assuming that non-baryonic DM scales like dark baryons, this constrains the total DM content of halo ...
... • assuming that non-baryonic DM scales like dark baryons, this constrains the total DM content of halo ...
Unit 3 EM Spectrum and Doppler Effect powerpoint
... What else can the light from distant stars and galaxies tell us? When an object such as a star or galaxy is moving towards us the the wavelengths of the light it emits are shifted towards the blue end of the spectrum (frequency is shifted higher). This is called blue shift. If the object is moving ...
... What else can the light from distant stars and galaxies tell us? When an object such as a star or galaxy is moving towards us the the wavelengths of the light it emits are shifted towards the blue end of the spectrum (frequency is shifted higher). This is called blue shift. If the object is moving ...
THE SPATIALLY RESOLVED [Cii] COOLING LINE DEFICIT IN
... deficits, the advent of [C II] surveys at redshifts z1 has completely altered this viewpoint. In the nearby universe, to good approximation, global luminosity serves as a reliable parameterization of the strongly varying local heating conditions in the ISM, which must underly the deficit, perhaps d ...
... deficits, the advent of [C II] surveys at redshifts z1 has completely altered this viewpoint. In the nearby universe, to good approximation, global luminosity serves as a reliable parameterization of the strongly varying local heating conditions in the ISM, which must underly the deficit, perhaps d ...
Common BH/SFR Evolution
... • Critical stage of BH-galaxy connection. • Occurs when galaxies form most of their stars. • Can represent up to 50% of matter accretion onto the central black hole. ...
... • Critical stage of BH-galaxy connection. • Occurs when galaxies form most of their stars. • Can represent up to 50% of matter accretion onto the central black hole. ...
02 Observing the Universe I - Jodrell Bank Centre for Astrophysics
... many furthest galaxies detected this way • Microwaves: CMB as BB at 2.725 K, astonishingly uniform, best evidence of cosmological principle, tiny anisotropies at 10-5 level • Infrared: surveys spotting different galaxy population: ‘young’ galaxies; useful to look through dust close to galactic plane ...
... many furthest galaxies detected this way • Microwaves: CMB as BB at 2.725 K, astonishingly uniform, best evidence of cosmological principle, tiny anisotropies at 10-5 level • Infrared: surveys spotting different galaxy population: ‘young’ galaxies; useful to look through dust close to galactic plane ...
Star formation rate in spiral galaxies
... We have calculated the star formation rate, the number of solar masses annually formed, in 20 spiral galaxies. Moreover it has been possible to establish the number of ionizing photons and the theoretical number of O5 stars needed to produce these emissions. The twenty galaxies have been selected fr ...
... We have calculated the star formation rate, the number of solar masses annually formed, in 20 spiral galaxies. Moreover it has been possible to establish the number of ionizing photons and the theoretical number of O5 stars needed to produce these emissions. The twenty galaxies have been selected fr ...
Seyfert galaxy
Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei (very luminous, distant and bright sources of electromagnetic radiation) with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.Seyfert galaxies account for about 10% of all galaxies and are some of the most intensely studied objects in astronomy, as they are thought to be powered by the same phenomena that occur in quasars, although they are closer and less luminous than quasars. These galaxies have supermassive black holes at their centers which are surrounded by accretion discs of in-falling material. The accretion discs are believed to be the source of the observed ultraviolet radiation. Ultraviolet emission and absorption lines provide the best diagnostics for the composition of the surrounding material.Seen in visible light, most Seyfert galaxies look like normal spiral galaxies, but when studied under other wavelengths, it becomes clear that the luminosity of their cores is of comparable intensity to the luminosity of whole galaxies the size of the Milky Way.Seyfert galaxies are named after Carl Seyfert, who first described this class in 1943.