instructor notes: weeks 9/10
... tied to overall dimensions: cD galaxies. Huge elliptical galaxies dominating some clusters of galaxies. “cD” stands for “cluster dominating” galaxy. Some are incredibly large, massive, and luminous. Normal ellipticals. Standard E galaxies comparable in luminosity to supergiant spiral galaxies. Dwarf ...
... tied to overall dimensions: cD galaxies. Huge elliptical galaxies dominating some clusters of galaxies. “cD” stands for “cluster dominating” galaxy. Some are incredibly large, massive, and luminous. Normal ellipticals. Standard E galaxies comparable in luminosity to supergiant spiral galaxies. Dwarf ...
PH607lec09-3gal1
... • 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 ...
PH607lec10-3gal1
... • 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 ...
... • 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 ...
sections 23-25 powerpoint
... There is an entire class of galaxies that appears to have something peculiar about their nuclei. Some are called Seyfert galaxies, after their discoverer, others are referred to as AGN = Active Galactic Nuclei, others still display oppositely-directed radio jets. Quasars are considered to be extrem ...
... There is an entire class of galaxies that appears to have something peculiar about their nuclei. Some are called Seyfert galaxies, after their discoverer, others are referred to as AGN = Active Galactic Nuclei, others still display oppositely-directed radio jets. Quasars are considered to be extrem ...
Building` a Galaxy SED
... Practical problem: galaxies are biased tracers of underlying mass distribution. In order to use galaxies to measure underlying mass distribution, we must understand galaxies. ...
... Practical problem: galaxies are biased tracers of underlying mass distribution. In order to use galaxies to measure underlying mass distribution, we must understand galaxies. ...
Module 5: To the Galaxies and Beyond!
... Trying to understand the scale of distances and sizes in the universe is really hard. Things are just so big and far away that we really need new words to describe them. However, we are going to try to get a feel for things by using our imagination to take a little trip out to the edge of the Observ ...
... Trying to understand the scale of distances and sizes in the universe is really hard. Things are just so big and far away that we really need new words to describe them. However, we are going to try to get a feel for things by using our imagination to take a little trip out to the edge of the Observ ...
Next Generation VLA Science White Paper
... Radio telescopes are essential to our understanding of “galaxy ecosytems,” here meaning the complex interplay of gas, stars, black holes, and dark matter in and around galaxies. They provide a main tool to study almost all phases of gas in galaxies: cool and cold gas (via emission and absorption lin ...
... Radio telescopes are essential to our understanding of “galaxy ecosytems,” here meaning the complex interplay of gas, stars, black holes, and dark matter in and around galaxies. They provide a main tool to study almost all phases of gas in galaxies: cool and cold gas (via emission and absorption lin ...
The Hubble Law - Department of Astronomy
... The next step is to determine the distances to galaxies. For nearby galaxies, we can use standard candles such as Cepheid variables or white-dwarf supernovae. But, for very distant galaxies, we must rely on more indirect methods. The key assumption for this lab is that we are measuring galaxies of s ...
... The next step is to determine the distances to galaxies. For nearby galaxies, we can use standard candles such as Cepheid variables or white-dwarf supernovae. But, for very distant galaxies, we must rely on more indirect methods. The key assumption for this lab is that we are measuring galaxies of s ...
The National Centre for Radio Astrophysics
... linked to the end stages of massive stars. Thus the major thrust in this direction is towards understanding stellar deaths involving massive progenitors. The study of environments of the progenitor stars that lead to supernovae and GRB explosions is the main focus of my research, which mainly uses t ...
... linked to the end stages of massive stars. Thus the major thrust in this direction is towards understanding stellar deaths involving massive progenitors. The study of environments of the progenitor stars that lead to supernovae and GRB explosions is the main focus of my research, which mainly uses t ...
SPACETIME SINGULARITIES: The STORY of BLACK HOLES
... Before we discuss exactly what a Black Hole looks like, it is useful to know how and why they form in the first place (in fact, since black holes are objects in spacetime, we can’t actually separate their behaviour in time from their behaviour in space). Let’s start with why black holes can form. As ...
... Before we discuss exactly what a Black Hole looks like, it is useful to know how and why they form in the first place (in fact, since black holes are objects in spacetime, we can’t actually separate their behaviour in time from their behaviour in space). Let’s start with why black holes can form. As ...
Practical cosmology with the Local Volume galaxies
... HI mass density, as well as the star formation rate density. ...
... HI mass density, as well as the star formation rate density. ...
Curriculum Vitae - Centre for Astrophysics and Supercomputing
... Research Interests • Modelling spectral energy distributions of galaxies • Stellar population synthesis models • Statistical interpretation of spectroscopic and photometric galaxy surveys • The formation and evolution of galaxies, comparison between theory/models and observations • The connections b ...
... Research Interests • Modelling spectral energy distributions of galaxies • Stellar population synthesis models • Statistical interpretation of spectroscopic and photometric galaxy surveys • The formation and evolution of galaxies, comparison between theory/models and observations • The connections b ...
the Local Group - Simon P Driver
... • to turn a map of the sky into a 3-D picture of the Local Group, we need galaxy distances – Hubble’s law does not apply within the Group because expansion has halted • need to remember that the uncertainty in the distance is ~10% even for bright galaxies – e.g. for the LMC, the range found for ...
... • to turn a map of the sky into a 3-D picture of the Local Group, we need galaxy distances – Hubble’s law does not apply within the Group because expansion has halted • need to remember that the uncertainty in the distance is ~10% even for bright galaxies – e.g. for the LMC, the range found for ...
LET`S MAKE A PORTRAIT OF A GALAXY Abstract
... As the name suggests, “irregular” galaxies are those galaxies which have no specific form, and so the group contains a very diverse selection of objects. In fact, there are two types of irregular galaxies. Type I are usually single galaxies of peculiar appearance. They contain a large fraction of yo ...
... As the name suggests, “irregular” galaxies are those galaxies which have no specific form, and so the group contains a very diverse selection of objects. In fact, there are two types of irregular galaxies. Type I are usually single galaxies of peculiar appearance. They contain a large fraction of yo ...
Galaxies
... All stars you can see by eye or with small telescopes are in Milky Way ‣ as are stellar remains: white dwarfs, neutron stars, black holes and planetary nebulae ...
... All stars you can see by eye or with small telescopes are in Milky Way ‣ as are stellar remains: white dwarfs, neutron stars, black holes and planetary nebulae ...
Document
... 2. Microlensing on isolated stellar mass BHs • There are several good candidates • But it is necessary to find the black hole ITSELF! 3. Exotic emission mechanisms • As all other exotics: interesting, but not very probable • If it works, then GLAST will show us isolated BHs 4. Runaway stars • A rare ...
... 2. Microlensing on isolated stellar mass BHs • There are several good candidates • But it is necessary to find the black hole ITSELF! 3. Exotic emission mechanisms • As all other exotics: interesting, but not very probable • If it works, then GLAST will show us isolated BHs 4. Runaway stars • A rare ...
Document
... 2. Microlensing on isolated stellar mass BHs • There are several good candidates • But it is necessary to find the black hole ITSELF! 3. Exotic emission mechanisms • As all other exotics: interesting, but not very probable • If it works, then GLAST will show us isolated BHs 4. Runaway stars • A rare ...
... 2. Microlensing on isolated stellar mass BHs • There are several good candidates • But it is necessary to find the black hole ITSELF! 3. Exotic emission mechanisms • As all other exotics: interesting, but not very probable • If it works, then GLAST will show us isolated BHs 4. Runaway stars • A rare ...
3D Tour of the Universe Template
... regions, resulting in the formation of new young stars. As is common in these kinds of encounters, spiral structure was induced in the more massive galaxy. M51 is an easily found astronomical showpiece if the sky is dark, where suggestions of its spiral arms may be visible. As is also common with th ...
... regions, resulting in the formation of new young stars. As is common in these kinds of encounters, spiral structure was induced in the more massive galaxy. M51 is an easily found astronomical showpiece if the sky is dark, where suggestions of its spiral arms may be visible. As is also common with th ...
The new X-ray universe
... which turned out to be highly variable (indicating that it was a single object, not a close group of sources) and at the known distance of M82 this implied that it was “ultraluminous” (Lx >1039 erg s–1; the source in M82 varies up 1041 erg s–1). While the existence of such objects was hinted at by e ...
... which turned out to be highly variable (indicating that it was a single object, not a close group of sources) and at the known distance of M82 this implied that it was “ultraluminous” (Lx >1039 erg s–1; the source in M82 varies up 1041 erg s–1). While the existence of such objects was hinted at by e ...
The Diverse Galaxies
... If the Universe is expanding uniformly today, then galaxies must have been closer in the past. At sometime in the past everything must Expansion have been contained at one point and Of universe that everthing came into being at a single moment – the Big Bang The cosmological principle is the idea th ...
... If the Universe is expanding uniformly today, then galaxies must have been closer in the past. At sometime in the past everything must Expansion have been contained at one point and Of universe that everthing came into being at a single moment – the Big Bang The cosmological principle is the idea th ...
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 ...
Clusters
... ICM in the centres of galaxy clusters should be rapidly cooling at the rate of tens to thousands of solar masses per year this should happen as the ICM is quickly losing its energy by the emission of X-rays X-ray brightness of the ICM is proportional to the square of its density, which rises steeply ...
... ICM in the centres of galaxy clusters should be rapidly cooling at the rate of tens to thousands of solar masses per year this should happen as the ICM is quickly losing its energy by the emission of X-rays X-ray brightness of the ICM is proportional to the square of its density, which rises steeply ...
Starburst Galaxies - Beck-Shop
... The young stars, that can now be seen directly, have masses ranging from 0.08 solar masses (the brown dwarf limit) to slightly over 100 solar masses (beyond which stars become unstable). By far the majority of stars though are at the low-mass end of this range – 80% have masses less than that of the ...
... The young stars, that can now be seen directly, have masses ranging from 0.08 solar masses (the brown dwarf limit) to slightly over 100 solar masses (beyond which stars become unstable). By far the majority of stars though are at the low-mass end of this range – 80% have masses less than that of the ...
AGN surveys to study galaxy evolution along cosmic times
... of galaxies. We also know that they are deeply connected, as shown by the so-called Magorrian relation (Magorrian et al. 1998). We want to know the full cosmic history of energy generation by stars (star formation) and AGNs (black hole accretion). These energy production rates correspond to built up ...
... of galaxies. We also know that they are deeply connected, as shown by the so-called Magorrian relation (Magorrian et al. 1998). We want to know the full cosmic history of energy generation by stars (star formation) and AGNs (black hole accretion). These energy production rates correspond to built up ...
Black Holes - Gresham College
... Though no one has ever seen a Black Hole directly, it is, at least in principle, possible to “see” one if one could get near enough. This is due to the fact that its mass distorts the space-time around it forming a gravitational lens which distorts what we see beyond it. The “lens” acts rather like ...
... Though no one has ever seen a Black Hole directly, it is, at least in principle, possible to “see” one if one could get near enough. This is due to the fact that its mass distorts the space-time around it forming a gravitational lens which distorts what we see beyond it. The “lens” acts rather like ...
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.