Niraj D. Welikala Thesis - D-Scholarship@Pitt
... and on these scales the density fluctuations are small in size (rms fluctuations of the order ∼ 0.1 at 1 Gpc). However, on scales of the order of 10 Mpc, the density fluctuations are large (∼ 1). The most apparent overdensities are therefore on small scales, less than 10 Mpc which are the typical sc ...
... and on these scales the density fluctuations are small in size (rms fluctuations of the order ∼ 0.1 at 1 Gpc). However, on scales of the order of 10 Mpc, the density fluctuations are large (∼ 1). The most apparent overdensities are therefore on small scales, less than 10 Mpc which are the typical sc ...
Galaxies - hwchemistry
... of galaxies, however, they find that the measured masses are much larger than expected from the luminosities of the galaxies. • This seems to be true of most galaxies. – Measured masses of galaxies amount to 10 to 100 times more mass than you would expect from the appearance of galaxies. ...
... of galaxies, however, they find that the measured masses are much larger than expected from the luminosities of the galaxies. • This seems to be true of most galaxies. – Measured masses of galaxies amount to 10 to 100 times more mass than you would expect from the appearance of galaxies. ...
Preliminary Talk Abstract Book - MoCA
... Clusters of galaxies are the most massive virialised cosmic structures. The diversity of their environmental conditions, from the dense cores to the sparse outskirts, allows them to be used as observational laboratories for the study of the environmental drivers of galaxy evolution. Furthermore, the ...
... Clusters of galaxies are the most massive virialised cosmic structures. The diversity of their environmental conditions, from the dense cores to the sparse outskirts, allows them to be used as observational laboratories for the study of the environmental drivers of galaxy evolution. Furthermore, the ...
Galaxies
... The past decade of research has given us confidence that it is possible to construct a self-consistent model of galaxy evolution and cosmology based on the paradigm that galaxies form hierarchically around peaks in the dark matter density distribution. Within this framework, astronomers have made gr ...
... The past decade of research has given us confidence that it is possible to construct a self-consistent model of galaxy evolution and cosmology based on the paradigm that galaxies form hierarchically around peaks in the dark matter density distribution. Within this framework, astronomers have made gr ...
Observational evidence for AGN feedback in early
... strength of the Balmer lines that is at least what expected by recombination theory. From the fit to the stellar continuum and absorption features, we measure the line-of-sight velocity dispersions. From subtraction of the emission-line spectrum from the observed one, we get the clean absorption lin ...
... strength of the Balmer lines that is at least what expected by recombination theory. From the fit to the stellar continuum and absorption features, we measure the line-of-sight velocity dispersions. From subtraction of the emission-line spectrum from the observed one, we get the clean absorption lin ...
Mapping the Pathways of Galaxy Transformation Across Time and
... early-types, and represent a clear path for galaxies to transform from star-forming to quiescence. Many show signs of a recent galaxy-galaxy merger and a newly-evolved stellar bulge, and most have LINER-like emission, which may indicate low luminosity AGN activity. Thus, the study of this short-live ...
... early-types, and represent a clear path for galaxies to transform from star-forming to quiescence. Many show signs of a recent galaxy-galaxy merger and a newly-evolved stellar bulge, and most have LINER-like emission, which may indicate low luminosity AGN activity. Thus, the study of this short-live ...
THE MORPHOLOGICAL DEMOGRAPHICS OF GALAXIES IN THE
... based on the 1600Å UV flux. The inset panel shows the relation between the BPZ photometric redshifts estimates and the spectroscopic ones from our ground-based observations. ...
... based on the 1600Å UV flux. The inset panel shows the relation between the BPZ photometric redshifts estimates and the spectroscopic ones from our ground-based observations. ...
2. The X-ray-Radio correlation for bulgeless galaxies
... Correlations between the X-ray and Radio emissions are observed for both galaxies with Active Galactic Nuclei (AGN) and in Star Forming galaxies. For the first case, the Xray/Radio correlation seems to present different slopes for Radio-loud and Radio-quiet AGN and may be used to estimate the mass o ...
... Correlations between the X-ray and Radio emissions are observed for both galaxies with Active Galactic Nuclei (AGN) and in Star Forming galaxies. For the first case, the Xray/Radio correlation seems to present different slopes for Radio-loud and Radio-quiet AGN and may be used to estimate the mass o ...
Evolution of galaxy morphology - Lecture 1 - NCRA-TIFR
... and ask questions if you don’t understand something. Some of the slides will cite papers which you are encouraged to read to know more. A number of excellent online courses are available. I will use material from these as appropriate. I particularly like the Galaxies and Cosmology course by S. G. Dj ...
... and ask questions if you don’t understand something. Some of the slides will cite papers which you are encouraged to read to know more. A number of excellent online courses are available. I will use material from these as appropriate. I particularly like the Galaxies and Cosmology course by S. G. Dj ...
Article PDF - IOPscience
... play a role. In addition to this we have the issue of projection, that is, we view galaxies as two-dimensional ‘‘ pictures ’’ when in fact stars are distributed in a galaxy in three-dimensional space. When trying to understand a galaxy from its stellar light distributions, and what it means physical ...
... play a role. In addition to this we have the issue of projection, that is, we view galaxies as two-dimensional ‘‘ pictures ’’ when in fact stars are distributed in a galaxy in three-dimensional space. When trying to understand a galaxy from its stellar light distributions, and what it means physical ...
The environment of high-redshift AGN OLIMPIA JUDIT FOGASY
... contribution of the two modes, the hot mode accreation onto haloes becomes more important at higher mass haloes (Mhalo ≥ 1011 M ). However, the hot fraction of the gas accreted onto galaxies does not depend on the halo mass. Moreover, while the accretion onto haloes is insensitive to metal-line coo ...
... contribution of the two modes, the hot mode accreation onto haloes becomes more important at higher mass haloes (Mhalo ≥ 1011 M ). However, the hot fraction of the gas accreted onto galaxies does not depend on the halo mass. Moreover, while the accretion onto haloes is insensitive to metal-line coo ...
X. Nuclear star clusters in low-mass early-type galaxies
... that the evolution of NSCs and SMBHs may possibly somehow be linked. Likely there is some interaction between NSCs and SMBHs, such that one may prevent the growth of the other or even destroy it (McLaughlin, King & Nayakshin 2006; Merritt 2009; Nayakshin, Wilkinson & King 2009). The Milky Way was th ...
... that the evolution of NSCs and SMBHs may possibly somehow be linked. Likely there is some interaction between NSCs and SMBHs, such that one may prevent the growth of the other or even destroy it (McLaughlin, King & Nayakshin 2006; Merritt 2009; Nayakshin, Wilkinson & King 2009). The Milky Way was th ...
Spectacular Evidence of the Greatness of Almighty Allah
... contain many multiple star systems, star clusters, and various interstellar clouds. Most galaxies are 1,000 to 100,000 parsecs in diameter. The parsec measurement unit is used in astronomy. The parsec is a unit of length, equal to just under 31 trillion kilometers (about 19 trillion miles), or about ...
... contain many multiple star systems, star clusters, and various interstellar clouds. Most galaxies are 1,000 to 100,000 parsecs in diameter. The parsec measurement unit is used in astronomy. The parsec is a unit of length, equal to just under 31 trillion kilometers (about 19 trillion miles), or about ...
SPICA Yellow Book
... through the investigation of the cold and obscured parts of the Universe, where the basic processes of formation and evolution occur. Deep exploration of the cold Universe using high spatial resolution observations in the Far Infrared (FIR) and sub-mm started in 2009 with the launch of the Herschel ...
... through the investigation of the cold and obscured parts of the Universe, where the basic processes of formation and evolution occur. Deep exploration of the cold Universe using high spatial resolution observations in the Far Infrared (FIR) and sub-mm started in 2009 with the launch of the Herschel ...
Local Group Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mario L Mateo
... dust) in only a few million years. The implication is that unless it started out with an astoundingly large reservoir of gas from which to form stars, IC 10 has probably been caught during a particularly active—but short-lived— phase in its star-formation history. Such galaxies that appear to form s ...
... dust) in only a few million years. The implication is that unless it started out with an astoundingly large reservoir of gas from which to form stars, IC 10 has probably been caught during a particularly active—but short-lived— phase in its star-formation history. Such galaxies that appear to form s ...
the stebbins galaxy: the origins of interstellar medium studies
... Abstract: The development of photoelectric photometry as an observational technique by Joel Stebbins and his colleagues at the University of Wisconsin‘s Washburn Observatory made possible, in the early 1930s, a new approach to the effects, extent, and nature of interstellar matter. In a series of pa ...
... Abstract: The development of photoelectric photometry as an observational technique by Joel Stebbins and his colleagues at the University of Wisconsin‘s Washburn Observatory made possible, in the early 1930s, a new approach to the effects, extent, and nature of interstellar matter. In a series of pa ...
A Spectroscopically Confirmed Excess of 24 micron Sources in a
... and a diet Salpeter initial mass function (IMF) is assumed. We use the diet Salpeter IMF defined in Bell & de Jong (2001) as having x = 0 below 0.6M⊙ and so the stellar mass using a diet Salpeter IMF is 70% of that for a regular Salpeter IMF (Salpeter 1955). Using an absolute magnitude for the sun o ...
... and a diet Salpeter initial mass function (IMF) is assumed. We use the diet Salpeter IMF defined in Bell & de Jong (2001) as having x = 0 below 0.6M⊙ and so the stellar mass using a diet Salpeter IMF is 70% of that for a regular Salpeter IMF (Salpeter 1955). Using an absolute magnitude for the sun o ...
Chapter 24
... Figure 24.1 shows a vast expanse of space lying about 100 million pc from Earth. Almost every patch or point of light in this figure is a separate galaxy— hundreds can be seen in just this one photograph. Over the years, astronomers have accumulated similar images of many millions of galaxies. We be ...
... Figure 24.1 shows a vast expanse of space lying about 100 million pc from Earth. Almost every patch or point of light in this figure is a separate galaxy— hundreds can be seen in just this one photograph. Over the years, astronomers have accumulated similar images of many millions of galaxies. We be ...
ABSTRACT Exoplanet Habitability and an Analysis of Gliese 436 b
... are not abundant in abiotic processes.13 However, it should be noted that, on Earth, these molecules are not highly abundant in the atmosphere.13 As such, it can be very difficult to even observe the presence of these molecules on a spectroscopy readout.13 Even if this class of molecules were discov ...
... are not abundant in abiotic processes.13 However, it should be noted that, on Earth, these molecules are not highly abundant in the atmosphere.13 As such, it can be very difficult to even observe the presence of these molecules on a spectroscopy readout.13 Even if this class of molecules were discov ...
Lab 14 Galaxy Morphology
... Some of these fuzzy nebulae, however, did not break-up into stars no matter how big a telescope was used to look at them. While many of these nebulae are clouds of glowing hydrogen gas within the Milky Way galaxy (HII regions), others (some of which resembled pinwheels) were true galaxies–similar to ...
... Some of these fuzzy nebulae, however, did not break-up into stars no matter how big a telescope was used to look at them. While many of these nebulae are clouds of glowing hydrogen gas within the Milky Way galaxy (HII regions), others (some of which resembled pinwheels) were true galaxies–similar to ...
The Milky Way - The Independent School
... As you begin studying galaxies, you will discover they are classified into different types, and that will lead you to insights into how galaxies form and evolve. In the next chapter, you will discover that some galaxies are violently active, and that will give you more clues to the evolution of gala ...
... As you begin studying galaxies, you will discover they are classified into different types, and that will lead you to insights into how galaxies form and evolve. In the next chapter, you will discover that some galaxies are violently active, and that will give you more clues to the evolution of gala ...
Galaxy Evolution
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
Lecture notes 18: Galaxies and galaxy clusters
... first to recocnize the possibility that the Milky Way was indeed a stellar disk where the Sun was but one of many. Kant went on to propose that if the Milky Way were limited then perhaps the diffuse “elliptical nebulae” seen in the night sky may also be distant disklike systems similar to our own but ...
... first to recocnize the possibility that the Milky Way was indeed a stellar disk where the Sun was but one of many. Kant went on to propose that if the Milky Way were limited then perhaps the diffuse “elliptical nebulae” seen in the night sky may also be distant disklike systems similar to our own but ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
Fermi paradox
The Fermi paradox (or Fermi's paradox) is the apparent contradiction between high estimates of the probability of the existence of extraterrestrial civilizations, such as in the Drake equation, and the lack of evidence for such civilizations. The basic points of the argument, made by physicists Enrico Fermi and Michael H. Hart, are: The Sun is a typical star, and there are billions of stars in the galaxy that are billions of years older. With high probability, some of these stars will have Earth-like planets, and if the earth is typical, some might develop intelligent life. Some of these civilizations might develop interstellar travel, a step the Earth is investigating now. Even at the slow pace of currently envisioned interstellar travel, the Milky Way galaxy could be completely traversed in about a million years.According to this line of thinking, the Earth should already have been visited by extraterrestrial aliens though Fermi saw no convincing evidence of this, nor any signs of alien intelligence anywhere in the observable universe, leading him to ask, ""Where is everybody?""