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 ...
my dissertation (PhD. Thesis) - Argelander
... To gain access to information about galaxies one has an enormous amount of objects at hand, galaxies of all sizes and distances ranging from our “backyard”, namely the Milky Way itself and the Local Group to galaxies at a redshift of z ' 11 and higher. Each approach can deliver different information ...
... To gain access to information about galaxies one has an enormous amount of objects at hand, galaxies of all sizes and distances ranging from our “backyard”, namely the Milky Way itself and the Local Group to galaxies at a redshift of z ' 11 and higher. Each approach can deliver different information ...
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
... Star formation and its associated feedbacks take place at very small, sub-pc scales, yet they extend their influence on very large scales, shaping the host galaxies and leading to the ejection of gas and metals from dark matter halos to the Inter-Galactic Medium. I will first review the microphysics ...
... Star formation and its associated feedbacks take place at very small, sub-pc scales, yet they extend their influence on very large scales, shaping the host galaxies and leading to the ejection of gas and metals from dark matter halos to the Inter-Galactic Medium. I will first review the microphysics ...
Mapping the Pathways of Galaxy Transformation Across Time and
... Is “quenching” the termination of star formation or the compression of star formation histories (SFHs)? I discuss the deep implications this reframing has for what we see as and how we study core processes shaping galaxy life-cycles. As a lens, I use two outcomes from the IMACS Cluster-Building Surv ...
... Is “quenching” the termination of star formation or the compression of star formation histories (SFHs)? I discuss the deep implications this reframing has for what we see as and how we study core processes shaping galaxy life-cycles. As a lens, I use two outcomes from the IMACS Cluster-Building Surv ...
Annual Report 2011 - Max Planck Institute for Astrophysics
... quickly repaired by a complete exchange of the computer. In addition to the desktop systems, which, are almost all younger than 5 years and which (in 2011) amount to more than 160 fully equipped working places, users have access to central number crunchers (about 20 machines, all 64-bit architecture ...
... quickly repaired by a complete exchange of the computer. In addition to the desktop systems, which, are almost all younger than 5 years and which (in 2011) amount to more than 160 fully equipped working places, users have access to central number crunchers (about 20 machines, all 64-bit architecture ...
Star Formation in the Milky Way and Nearby Galaxies Further
... The immense expansion of this subject, in terms of both the volume of results and the range of physical scales explored, may help to explain one of its idiosyncrasies, namely the relative isolation between the community studying individual star-forming regions and stars in the Milky Way (MW; also so ...
... The immense expansion of this subject, in terms of both the volume of results and the range of physical scales explored, may help to explain one of its idiosyncrasies, namely the relative isolation between the community studying individual star-forming regions and stars in the Milky Way (MW; also so ...
Gaia 1 and 2. A pair of new satellites of the Galaxy
... Accepted XXX. Received YYY; in original form ZZZ ...
... Accepted XXX. Received YYY; in original form ZZZ ...
Multiplicity in Early Stellar Evolution - Astronomy Group
... number of brown dwarfs formed (e.g., Bonnell et al., 2008; Bate, 2009a,b; Attwood et al., 2009). Three-dimensional HD SPH calculations by Bate (2009a) made predictions of the frequency of single, binary, triple, and quadruple star systems formed during the collapse of a highly unstable cloud with an ...
... number of brown dwarfs formed (e.g., Bonnell et al., 2008; Bate, 2009a,b; Attwood et al., 2009). Three-dimensional HD SPH calculations by Bate (2009a) made predictions of the frequency of single, binary, triple, and quadruple star systems formed during the collapse of a highly unstable cloud with an ...
environmental effects on galaxy evolution in nearby clusters
... The environmental effects on galaxy evolution in nearby clusters are investigated using a multiwavelength dataset. The present analysis is focused on the properties of three (Abell 1367, Virgo and Coma) among the best studied clusters in the local Universe. Due to the variety of their environmental ...
... The environmental effects on galaxy evolution in nearby clusters are investigated using a multiwavelength dataset. The present analysis is focused on the properties of three (Abell 1367, Virgo and Coma) among the best studied clusters in the local Universe. Due to the variety of their environmental ...
Science Case for the Chinese Participation of TMT
... Telescope (TMT). The Chinese participation in the TMT will place China in the forefront of astronomy for many decades to come; it can be a transformational experience for Chinese astronomy in terms of science, management and technology through international collaborations. The TMT partnership will f ...
... Telescope (TMT). The Chinese participation in the TMT will place China in the forefront of astronomy for many decades to come; it can be a transformational experience for Chinese astronomy in terms of science, management and technology through international collaborations. The TMT partnership will f ...
- Isaac Newton Group of Telescopes
... 1996 we had the additional distraction of the Prior Options process the then UK Governments requirement for public services to be subject to competitive tendering, in this case the management of the telescopes and delivery of the instrumentation programme. So my main emotion on reading this annua ...
... 1996 we had the additional distraction of the Prior Options process the then UK Governments requirement for public services to be subject to competitive tendering, in this case the management of the telescopes and delivery of the instrumentation programme. So my main emotion on reading this annua ...
Observations and Theory of Dynamical Triggers for Star Formation
... distant sources, such as supernovae or stellar winds, or perhaps from older HII regions that have already expanded. These make comet shapes when the pressure is one-sided. Catalogs of such cometary globules are in Hawarden & Brand (1976), Sandqvist (1976), Reipurth (1983), and Zealey et al. (1983). ...
... distant sources, such as supernovae or stellar winds, or perhaps from older HII regions that have already expanded. These make comet shapes when the pressure is one-sided. Catalogs of such cometary globules are in Hawarden & Brand (1976), Sandqvist (1976), Reipurth (1983), and Zealey et al. (1983). ...
harlow shapley - National Academy of Sciences
... variables found in these clusters. Curtis favored much reduced distances for these stars, based on intrinsically very much fainter absolute brightnesses. Shapley clearly came out the winner in the first part of the debate; however, there was a second side. Shapley and Curtis each discussed their vie ...
... variables found in these clusters. Curtis favored much reduced distances for these stars, based on intrinsically very much fainter absolute brightnesses. Shapley clearly came out the winner in the first part of the debate; however, there was a second side. Shapley and Curtis each discussed their vie ...
Elliptical Galaxies
... found in de Zeeuw and Franx (1992). Dark haloes: mass at large radius Spiral galaxy rotation curves have been used to show that they are embedded in dark haloes that contain three to ten times as much mass as is visible in stars, gas and dust. Can dark haloes be detected in elliptical galaxies? The ...
... found in de Zeeuw and Franx (1992). Dark haloes: mass at large radius Spiral galaxy rotation curves have been used to show that they are embedded in dark haloes that contain three to ten times as much mass as is visible in stars, gas and dust. Can dark haloes be detected in elliptical galaxies? The ...
Astronomy Astrophysics Gaia-ESO Survey: The analysis of high-resolution The
... E(B − V). The targets selected before April 2012 had a brightest cut on J = 11 instead of 12. When there were not enough targets, the red edge was extended. When there were too many potential targets an algorithm selected roughly the same number of stars per magnitude bin with the rest being marked ...
... E(B − V). The targets selected before April 2012 had a brightest cut on J = 11 instead of 12. When there were not enough targets, the red edge was extended. When there were too many potential targets an algorithm selected roughly the same number of stars per magnitude bin with the rest being marked ...
LACEwING: A New Moving Group Analysis Code
... The groups have ages between ∼5 Myr old (ò Cha) and 600–800 Myr old (Hyades). The fundamental assumption about these NYMGs and open clusters is that they are the products of single bursts of star formation. This means that every constituent member should be roughly the same age (with attendant const ...
... The groups have ages between ∼5 Myr old (ò Cha) and 600–800 Myr old (Hyades). The fundamental assumption about these NYMGs and open clusters is that they are the products of single bursts of star formation. This means that every constituent member should be roughly the same age (with attendant const ...
the PDF program book
... Welcome to Cool Stars 19 On behalf of the Cool Stars 19 LOC, the SOC, and Uppsala universitet, we welcome you to Uppsala, home to the oldest university in Scandinavia and the home of Carl Linnaeus, Anders Celsius and Anders Jonas Ångström. It is our goal to provide you with a relaxed and comfortabl ...
... Welcome to Cool Stars 19 On behalf of the Cool Stars 19 LOC, the SOC, and Uppsala universitet, we welcome you to Uppsala, home to the oldest university in Scandinavia and the home of Carl Linnaeus, Anders Celsius and Anders Jonas Ångström. It is our goal to provide you with a relaxed and comfortabl ...
Formation of Molecular Clouds and Global Conditions for Star
... have revised estimates of magnetic field strengths downwards, and new simulations and theoretical models that suggest that clouds may in fact be turbulence-supported, or that they may be entirely transient objects that are not supported against collapse at all. These questions are all under active d ...
... have revised estimates of magnetic field strengths downwards, and new simulations and theoretical models that suggest that clouds may in fact be turbulence-supported, or that they may be entirely transient objects that are not supported against collapse at all. These questions are all under active d ...
Evolution of low mass stars
... the chief assistant of the Royal Greenwich Observatory. In 1926 Eddington offered the first stellar model able to explain the physics behind the HRD, in his book “The Internal Constitution of the Stars” (Eddington, 1926). This model, almost entirely based on the theory of radiative transfer, describ ...
... the chief assistant of the Royal Greenwich Observatory. In 1926 Eddington offered the first stellar model able to explain the physics behind the HRD, in his book “The Internal Constitution of the Stars” (Eddington, 1926). This model, almost entirely based on the theory of radiative transfer, describ ...
A Universal Stellar Initial Mass Function? A Critical Look Further
... Way! Elmegreen & Scalo (2006) provide a detailed exploration of the degeneracies involved in inferring a stellar population’s IMF from its measured PDMF and adopted SFH. It is somewhat disconcerting that the break from the Salpeter law identified in many IMF studies needs to be invoked near the plac ...
... Way! Elmegreen & Scalo (2006) provide a detailed exploration of the degeneracies involved in inferring a stellar population’s IMF from its measured PDMF and adopted SFH. It is somewhat disconcerting that the break from the Salpeter law identified in many IMF studies needs to be invoked near the plac ...
Digital Universe Guide - American Museum of Natural History
... may want to do this slowly in case the graphics demand is pushed too high for your machine (at which point your computer will grind to a halt). If your machine freezes, either shrink the window or close it (press ESC) and wait for your computer to catch up. ...
... may want to do this slowly in case the graphics demand is pushed too high for your machine (at which point your computer will grind to a halt). If your machine freezes, either shrink the window or close it (press ESC) and wait for your computer to catch up. ...
Physical Properties of the Gas and Dust in the Orion B Molecular
... 1990). What else are then the actual birthplaces of stars in a molecular cloud and how can one find them? Progress in this field has been made by using the millimetre dust continuum emission as a tracer which was only possible after the development of very sensitive broadband bolometer systems (see ...
... 1990). What else are then the actual birthplaces of stars in a molecular cloud and how can one find them? Progress in this field has been made by using the millimetre dust continuum emission as a tracer which was only possible after the development of very sensitive broadband bolometer systems (see ...
Multiplicity in Early Stellar Evolution
... population of stars and brown dwarfs (1250) so as to provide an excellent basis for comparison with observed multiple systems. It is remarkable that this simulation – which clearly omits important physical ingredients such as magnetic fields and radiative feedback – nevertheless results in a reasona ...
... population of stars and brown dwarfs (1250) so as to provide an excellent basis for comparison with observed multiple systems. It is remarkable that this simulation – which clearly omits important physical ingredients such as magnetic fields and radiative feedback – nevertheless results in a reasona ...
Introduction
... a dataset of multiwavelength observations for a new sample of galaxies. The sample is volume and mass limited, and includes galaxies of all morphological types inhabiting a range of different environments, from galaxies in the dense core of the Virgo cluster to relatively isolated systems. As such, ...
... a dataset of multiwavelength observations for a new sample of galaxies. The sample is volume and mass limited, and includes galaxies of all morphological types inhabiting a range of different environments, from galaxies in the dense core of the Virgo cluster to relatively isolated systems. As such, ...
Open cluster
An open cluster, also known as galactic cluster, is a group of up to a few thousand stars that were formed from the same giant molecular cloud and have roughly the same age. More than 1,100 open clusters have been discovered within the Milky Way Galaxy, and many more are thought to exist. They are loosely bound by mutual gravitational attraction and become disrupted by close encounters with other clusters and clouds of gas as they orbit the galactic center, resulting in a migration to the main body of the galaxy as well as a loss of cluster members through internal close encounters. Open clusters generally survive for a few hundred million years, with the most massive ones surviving for a few billion years. In contrast, the more massive globular clusters of stars exert a stronger gravitational attraction on their members, and can survive for longer. Open clusters have been found only in spiral and irregular galaxies, in which active star formation is occurring.Young open clusters may still be contained within the molecular cloud from which they formed, illuminating it to create an H II region. Over time, radiation pressure from the cluster will disperse the molecular cloud. Typically, about 10% of the mass of a gas cloud will coalesce into stars before radiation pressure drives the rest of the gas away.Open clusters are key objects in the study of stellar evolution. Because the cluster members are of similar age and chemical composition, their properties (such as distance, age, metallicity and extinction) are more easily determined than they are for isolated stars. A number of open clusters, such as the Pleiades, Hyades or the Alpha Persei Cluster are visible with the naked eye. Some others, such as the Double Cluster, are barely perceptible without instruments, while many more can be seen using binoculars or telescopes. The Wild Duck Cluster, M11, is an example.