Program_files/40 Years of Microquasarsembed
... • Do all galactic XRBs have radio emission at some level? Need much better sensitivity to bring the 20% detections up! • Microquasars in other galaxies e.g. M31 (Middleton et al 2013), IC10 (Bernard et al 2008), NGC300 (Crowther et al. 2010) – should be lots, especially in star forming galaxies. • E ...
... • Do all galactic XRBs have radio emission at some level? Need much better sensitivity to bring the 20% detections up! • Microquasars in other galaxies e.g. M31 (Middleton et al 2013), IC10 (Bernard et al 2008), NGC300 (Crowther et al. 2010) – should be lots, especially in star forming galaxies. • E ...
Feedback - Cambridge University Press
... Recent observations constrain both the abundance of dark matter galaxy halos and the luminosity function of galaxies with a fair amount of precision. The result shows that star formation efficiency, defined as the ratio of stellar mass to halo mass, has a fairly sharp peak at a halo mass slightly below ...
... Recent observations constrain both the abundance of dark matter galaxy halos and the luminosity function of galaxies with a fair amount of precision. The result shows that star formation efficiency, defined as the ratio of stellar mass to halo mass, has a fairly sharp peak at a halo mass slightly below ...
Formation of z~6 Quasars from Hierarchical Galaxy Mergers
... ¥ Find target halo by performing a N-body simulation in large volume. ¥ Largest halo reaches M ~ 5.4x1012 h-1 Gpc3 through 7 major mergers between Z ~14.4 and Z~6.5 ¥ Quasar host galaxy build rapidly through gas rich mergers. ¥ SFR up to 104 Msun /year ¥ Reaching stellar mass of 1012Msun at Z~6.5 ¥ ...
... ¥ Find target halo by performing a N-body simulation in large volume. ¥ Largest halo reaches M ~ 5.4x1012 h-1 Gpc3 through 7 major mergers between Z ~14.4 and Z~6.5 ¥ Quasar host galaxy build rapidly through gas rich mergers. ¥ SFR up to 104 Msun /year ¥ Reaching stellar mass of 1012Msun at Z~6.5 ¥ ...
Characteristics of Stars
... absolute brightness. A star’s apparent brightness is its brightness as seen from Earth. Astronomers can measure apparent brightness fairly easily using electronic devices. A star’s absolute brightness is the brightness the star would have if it were at a standard distance from Earth. Distances on Ea ...
... absolute brightness. A star’s apparent brightness is its brightness as seen from Earth. Astronomers can measure apparent brightness fairly easily using electronic devices. A star’s absolute brightness is the brightness the star would have if it were at a standard distance from Earth. Distances on Ea ...
01_test_bank
... later, we take it out and the distances between raisins are 3 cm. If you lived in one of the raisins and watched the other raisins as the cake expanded, which of the following would you conclude? A) All raisins would be moving away from you at the same speed. B) More distant raisins would be moving ...
... later, we take it out and the distances between raisins are 3 cm. If you lived in one of the raisins and watched the other raisins as the cake expanded, which of the following would you conclude? A) All raisins would be moving away from you at the same speed. B) More distant raisins would be moving ...
Chapter 1 Introduction
... The challenging part is to disentangle evolutionary differences between a number of objects from intrinsic differences because of the degeneracies between the two. An example of this is the stellar mass. One could think of using the stellar mass as tracer of evolution, assuming that the mass of the ...
... The challenging part is to disentangle evolutionary differences between a number of objects from intrinsic differences because of the degeneracies between the two. An example of this is the stellar mass. One could think of using the stellar mass as tracer of evolution, assuming that the mass of the ...
telescopes - NPZ Optics
... Observations When using higher magnification not only the visible image size appears larger in the telescope, but also blurring and distortion of the image, star twinkle, caused by atmosphere become more significant. To achieve maximum stability ...
... Observations When using higher magnification not only the visible image size appears larger in the telescope, but also blurring and distortion of the image, star twinkle, caused by atmosphere become more significant. To achieve maximum stability ...
Summary of Talks at Growing Black Holes 2004 in Garching
... 3C184, a monster radio galaxy at z-0.994, is one example of a high-z radio galaxy. It is very faint, but there is evidence for the [NeV], [NeIII] lines, which are signatures of an AGN. They have also observed a high-z quasar that is gravitationally lensed and shows the redshift Paschen alpha and ...
... 3C184, a monster radio galaxy at z-0.994, is one example of a high-z radio galaxy. It is very faint, but there is evidence for the [NeV], [NeIII] lines, which are signatures of an AGN. They have also observed a high-z quasar that is gravitationally lensed and shows the redshift Paschen alpha and ...
PPT presentation
... The main contaminants are background sources with emission lines redshifted into the on-band filter: [O II] 3727 at z=0.35 or Ly alpha at z=3.1. The contamination increases as the surface density of PNs decreases. Negligible near the galaxy’s center, the contamination may become a problem in the int ...
... The main contaminants are background sources with emission lines redshifted into the on-band filter: [O II] 3727 at z=0.35 or Ly alpha at z=3.1. The contamination increases as the surface density of PNs decreases. Negligible near the galaxy’s center, the contamination may become a problem in the int ...
Chapter-by-Chapter Guide
... Yourself Questions The Think About It and See It For Yourself questions are not numbered in the book, so we list them in the order in which they appear, keyed by section number. ...
... Yourself Questions The Think About It and See It For Yourself questions are not numbered in the book, so we list them in the order in which they appear, keyed by section number. ...
The population of young stars in Orion A: X-rays and... Ignazio Pillitteri , S. J. Wolk , L. Allen
... emit in X-rays out of 1060 X-ray sources. By assuming the same fraction of X-ray detection of WTT stars and CTT stars we estimate a population of ∼ 1850 PMS stars, for an overall detection efficiency of ∼ 38% among PMS stars and a mean density of PMS stars of ∼750 stars deg−2. Our sensitivity limit ...
... emit in X-rays out of 1060 X-ray sources. By assuming the same fraction of X-ray detection of WTT stars and CTT stars we estimate a population of ∼ 1850 PMS stars, for an overall detection efficiency of ∼ 38% among PMS stars and a mean density of PMS stars of ∼750 stars deg−2. Our sensitivity limit ...
HD 140283: A Star in the Solar Neighborhood that Formed Shortly
... N(p, γ)15O reaction that occurred ...
... N(p, γ)15O reaction that occurred ...
Signals from the Beginnings of the World - Max-Planck
... of a cosmic mass swallower: a black hole is born. Astrophysicists are working on the theoretical details of this scenario. What causes gas to stream into a central compact object at high velocity and thus convert its surroundings into a source of high-energy light and plasma jets? If you want to und ...
... of a cosmic mass swallower: a black hole is born. Astrophysicists are working on the theoretical details of this scenario. What causes gas to stream into a central compact object at high velocity and thus convert its surroundings into a source of high-energy light and plasma jets? If you want to und ...
Essential physics of early galaxy formation
... medium (IGM) or to be brought in by mergers to re-ignite further star formation. As halos build-up mass with time, their DM potential well can sustain much larger star formation rates (SFR) without losing gas. This naturally implies that, at any given time, there is a limiting star formation efficie ...
... medium (IGM) or to be brought in by mergers to re-ignite further star formation. As halos build-up mass with time, their DM potential well can sustain much larger star formation rates (SFR) without losing gas. This naturally implies that, at any given time, there is a limiting star formation efficie ...
doc - Jnoodle
... The constant in Wien's displacement law is usually called "the constant in Wien's displacement law" or sometimes for short "Wien's constant" and should be assigned units: 2.90 x 103 Km (kelvinmeters). It is rarely given any symbol, but one can be assigned to it at will. This law means that the hotte ...
... The constant in Wien's displacement law is usually called "the constant in Wien's displacement law" or sometimes for short "Wien's constant" and should be assigned units: 2.90 x 103 Km (kelvinmeters). It is rarely given any symbol, but one can be assigned to it at will. This law means that the hotte ...
hanson.pdf
... actual animation scale to match the user’s observable scale in such a way that inappropriately large or small numbers do not occur. For example, in an initial test, we had difficulties when trying to animate the Earth’s rotation with the animation scale corresponding to the rotation speed of the ent ...
... actual animation scale to match the user’s observable scale in such a way that inappropriately large or small numbers do not occur. For example, in an initial test, we had difficulties when trying to animate the Earth’s rotation with the animation scale corresponding to the rotation speed of the ent ...
Chapter-by-Chapter Guide - We can offer most test bank and
... were on top of everything else. This suggests that the universe may have been very tiny and dense at some point in the distant past and has been expanding ever since. This beginning is what we call the Big Bang. Based on observations of the expansion rate, the Big Bang must have occurred about 14 bi ...
... were on top of everything else. This suggests that the universe may have been very tiny and dense at some point in the distant past and has been expanding ever since. This beginning is what we call the Big Bang. Based on observations of the expansion rate, the Big Bang must have occurred about 14 bi ...
FREE Sample Here
... were on top of everything else. This suggests that the universe may have been very tiny and dense at some point in the distant past and has been expanding ever since. This beginning is what we call the Big Bang. Based on observations of the expansion rate, the Big Bang must have occurred about 14 bi ...
... were on top of everything else. This suggests that the universe may have been very tiny and dense at some point in the distant past and has been expanding ever since. This beginning is what we call the Big Bang. Based on observations of the expansion rate, the Big Bang must have occurred about 14 bi ...
FREE Sample Here
... were on top of everything else. This suggests that the universe may have been very tiny and dense at some point in the distant past and has been expanding ever since. This beginning is what we call the Big Bang. Based on observations of the expansion rate, the Big Bang must have occurred about 14 bi ...
... were on top of everything else. This suggests that the universe may have been very tiny and dense at some point in the distant past and has been expanding ever since. This beginning is what we call the Big Bang. Based on observations of the expansion rate, the Big Bang must have occurred about 14 bi ...
Hubble Deep Field
The Hubble Deep Field (HDF) is an image of a small region in the constellation Ursa Major, constructed from a series of observations by the Hubble Space Telescope. It covers an area 2.5 arcminutes across, about one 24-millionth of the whole sky, which is equivalent in angular size to a 65 mm tennis ball at a distance of 100 metres. The image was assembled from 342 separate exposures taken with the Space Telescope's Wide Field and Planetary Camera 2 over ten consecutive days between December 18 and December 28, 1995.The field is so small that only a few foreground stars in the Milky Way lie within it; thus, almost all of the 3,000 objects in the image are galaxies, some of which are among the youngest and most distant known. By revealing such large numbers of very young galaxies, the HDF has become a landmark image in the study of the early universe, with the associated scientific paper having received over 900 citations by the end of 2014.Three years after the HDF observations were taken, a region in the south celestial hemisphere was imaged in a similar way and named the Hubble Deep Field South. The similarities between the two regions strengthened the belief that the universe is uniform over large scales and that the Earth occupies a typical region in the Universe (the cosmological principle). A wider but shallower survey was also made as part of the Great Observatories Origins Deep Survey. In 2004 a deeper image, known as the Hubble Ultra-Deep Field (HUDF), was constructed from a few months of light exposure. The HUDF image was at the time the most sensitive astronomical image ever made at visible wavelengths, and it remained so until the Hubble Extreme Deep Field (XDF) was released in 2012.