Gamma-Ray Bursts and Puzzles of Core
... First 21 GRB hosts: The Hubble diagram for GRB host galaxies with known (before June 2002) observable stellar magnitudes (or with upper R limits) and spectroscopic red shifts against the background of results of the photometric measurement of z applied to galaxies from the Hubble Deep Field (HDF) b ...
... First 21 GRB hosts: The Hubble diagram for GRB host galaxies with known (before June 2002) observable stellar magnitudes (or with upper R limits) and spectroscopic red shifts against the background of results of the photometric measurement of z applied to galaxies from the Hubble Deep Field (HDF) b ...
SPICA Yellow Book
... Progress in mid- and far-infrared astronomy has been slow because instruments and telescopes must be cooled to cryogenic temperatures to achieve high sensitivity and, for most of the frequency range, the observations can only be made from space. Only four small space observatories have operated in t ...
... Progress in mid- and far-infrared astronomy has been slow because instruments and telescopes must be cooled to cryogenic temperatures to achieve high sensitivity and, for most of the frequency range, the observations can only be made from space. Only four small space observatories have operated in t ...
Stellar Structure and Evolution
... our Galaxy, depends on stellar evolution calculations. Furthermore, since the synthesis of almost all chemical elements is supposed to take place inside stars, an understanding of the chemical history of the Universe (and of our own origins) requires that one understands stellar evolution. However, ...
... our Galaxy, depends on stellar evolution calculations. Furthermore, since the synthesis of almost all chemical elements is supposed to take place inside stars, an understanding of the chemical history of the Universe (and of our own origins) requires that one understands stellar evolution. However, ...
Probing nuclear activity versus star formation at z ∼ 0.8 using near
... We present near-infrared (NIR) spectroscopic observations of 28 X-ray and mid-infrared selected sources at a median redshift of z ∼ 0.8 in the Extended Groth Strip (EGS). To date this is the largest compilation of NIR spectra of active galactic nuclei (AGN) at this redshift. The data were obtained u ...
... We present near-infrared (NIR) spectroscopic observations of 28 X-ray and mid-infrared selected sources at a median redshift of z ∼ 0.8 in the Extended Groth Strip (EGS). To date this is the largest compilation of NIR spectra of active galactic nuclei (AGN) at this redshift. The data were obtained u ...
Prospects for asteroseismic inference on the envelope helium
... ticularly true close to the frequency at which the amplitude of the oscillations is a maximum (ν max ), where the trend is approximately flat with frequency. In this paper we have restricted our analysis to modes with frequencies close to ν max and therefore satisfactory results can be obtained simp ...
... ticularly true close to the frequency at which the amplitude of the oscillations is a maximum (ν max ), where the trend is approximately flat with frequency. In this paper we have restricted our analysis to modes with frequencies close to ν max and therefore satisfactory results can be obtained simp ...
The correlation between galaxy morphology and star
... than local ones with similar mass (Cassata et al. 2011, 2013). Recent works have suggested, however, that a large fraction of, and possibly even all, massive, quiscent galaxies at z ∼ 2 are disk dominated (van der Wel et al. 2011). While the observation of such disks at z > 2 is based on morphologic ...
... than local ones with similar mass (Cassata et al. 2011, 2013). Recent works have suggested, however, that a large fraction of, and possibly even all, massive, quiscent galaxies at z ∼ 2 are disk dominated (van der Wel et al. 2011). While the observation of such disks at z > 2 is based on morphologic ...
Preliminary Talk Abstract Book - MoCA
... Massive early-type galaxies (ETGs) are on average more compact (smaller size and higher velocity dispersion) at higher redshift. Galaxy mergers are believed to contribute substantially to this cosmological galaxy growth. I will present the results of theoretical models for the joint evolution of mas ...
... Massive early-type galaxies (ETGs) are on average more compact (smaller size and higher velocity dispersion) at higher redshift. Galaxy mergers are believed to contribute substantially to this cosmological galaxy growth. I will present the results of theoretical models for the joint evolution of mas ...
Mapping the Pathways of Galaxy Transformation Across Time and
... that accelerate evolution. They led to a paradigm in which the decline in activity of SF galaxies since z∼2; the removal of systems from that population; and the correlations between environment, SFR, and morphology all reflect the same underlying phenomenon: the initial configuration of the matter ...
... that accelerate evolution. They led to a paradigm in which the decline in activity of SF galaxies since z∼2; the removal of systems from that population; and the correlations between environment, SFR, and morphology all reflect the same underlying phenomenon: the initial configuration of the matter ...
Annual Report 2006/2007
... Stars form in galaxies from interstellar material, and at the end of their lives return chemicallyenriched material to the interstellar medium from which new generations of stars and planets form. The most massive and luminous stars evolve fastest, and leave neutron stars and black holes. This life ...
... Stars form in galaxies from interstellar material, and at the end of their lives return chemicallyenriched material to the interstellar medium from which new generations of stars and planets form. The most massive and luminous stars evolve fastest, and leave neutron stars and black holes. This life ...
Towards the understanding of the deepest layers of solar
... of the model that best represents the internal structure of a star are shifted in relation to the observed ones. The empirical formulation that has been suggested in the literature to correct for this shift was considered and its successfulness is discussed. Chapter 4 concerns the study of small con ...
... of the model that best represents the internal structure of a star are shifted in relation to the observed ones. The empirical formulation that has been suggested in the literature to correct for this shift was considered and its successfulness is discussed. Chapter 4 concerns the study of small con ...
A Budget and Accounting of Metals at z~ 0: Results from the COS
... galaxies over a range of stellar mass and star formation properties. The rationale and design for COS-Halos are described in Tumlinson et al. (2013); the key findings on metal lines are found in Tumlinson et al. (2011) for high-ionization gas and in Werk et al. (2013) for lowionization gas. Tumlinso ...
... galaxies over a range of stellar mass and star formation properties. The rationale and design for COS-Halos are described in Tumlinson et al. (2013); the key findings on metal lines are found in Tumlinson et al. (2011) for high-ionization gas and in Werk et al. (2013) for lowionization gas. Tumlinso ...
Astronomy 201 Cosmology
... First test: bending of light • Star light should be bend as it passes through the gravitational field of the Sun, i.e., it should be possible to see a star behind the Sun • General relativity predicts an angle of 1.75”, twice as big as that predicted by Newtonian gravity • measured by Arthur Edding ...
... First test: bending of light • Star light should be bend as it passes through the gravitational field of the Sun, i.e., it should be possible to see a star behind the Sun • General relativity predicts an angle of 1.75”, twice as big as that predicted by Newtonian gravity • measured by Arthur Edding ...
Galaxy evolution: A new version of the Besançon Maria A. Czekaj
... The Besançon Galaxy Model is a stellar population synthesis model, built over the last two decades in Besançon (Robin and Crézé (1986); Robin et al. (2003)). Until now the star production process in that model was based on the drawing from the so called Hess diagrams. Each Galaxy population had ...
... The Besançon Galaxy Model is a stellar population synthesis model, built over the last two decades in Besançon (Robin and Crézé (1986); Robin et al. (2003)). Until now the star production process in that model was based on the drawing from the so called Hess diagrams. Each Galaxy population had ...
Chapter 5 The Evolutionary Paths Of Nearby Galaxies
... of a small random sample of the massive late-types residing across the blue cloud and transition region, demonstrating the visible reddening at optical wavelengths. Therefore, in the rest of this section I focus on the properties of late-type galaxies to try to understand the mechanisms behind the q ...
... of a small random sample of the massive late-types residing across the blue cloud and transition region, demonstrating the visible reddening at optical wavelengths. Therefore, in the rest of this section I focus on the properties of late-type galaxies to try to understand the mechanisms behind the q ...
THE STAR FORMATION AND NUCLEAR ACCRETION HISTORIES OF NORMAL GALAXIES
... dominated by star formation, while that from early-type galaxies is dominated by a combination of hot gas and active galactic nucleus (AGN) emission. We find that the mean star formation and supermassive black hole accretion rate densities evolve like ∼ (1+z)3±1 , in agreement with the trends found ...
... dominated by star formation, while that from early-type galaxies is dominated by a combination of hot gas and active galactic nucleus (AGN) emission. We find that the mean star formation and supermassive black hole accretion rate densities evolve like ∼ (1+z)3±1 , in agreement with the trends found ...
Discovery of a Dusty Ring in the Coalsack - Harvard
... tions to thousands of stars behind the cloud. These measurements enable an examination of the structure of the globule to be made in a degree of detail considerably greater than that obtained by previous studies and comparable to that acheived earlier for B 68. The high angular resolution achieved b ...
... tions to thousands of stars behind the cloud. These measurements enable an examination of the structure of the globule to be made in a degree of detail considerably greater than that obtained by previous studies and comparable to that acheived earlier for B 68. The high angular resolution achieved b ...
Sample syllabus 2 - Johns Hopkins Center for Talented Youth
... Course Description: When the sun runs out of fuel, will it explode in a giant supernova or fade out into a white dwarf? Does every galaxy revolve around a super-massive black hole? Will the universe continue to expand, or will it eventually collapse back upon itself in a reversal of the Big Bang? As ...
... Course Description: When the sun runs out of fuel, will it explode in a giant supernova or fade out into a white dwarf? Does every galaxy revolve around a super-massive black hole? Will the universe continue to expand, or will it eventually collapse back upon itself in a reversal of the Big Bang? As ...
Formation of Molecular Clouds and Global Conditions for Star
... regions and along the Galactic Plane revealed the unexpectedly large spatial extent of giant molecular clouds (GMCs Kutner et al. 1977; Lada 1976; Blair et al. 1978; Blitz and Thaddeus 1980), and their substantial contribution to the mass budget of the ISM (Scoville 1975; Gordon and Burton 1976; Bur ...
... regions and along the Galactic Plane revealed the unexpectedly large spatial extent of giant molecular clouds (GMCs Kutner et al. 1977; Lada 1976; Blair et al. 1978; Blitz and Thaddeus 1980), and their substantial contribution to the mass budget of the ISM (Scoville 1975; Gordon and Burton 1976; Bur ...
A catalogue of the Chandra Deep Field South with multi
... Baade et al. 1999) at the MPG/ESO 2.2m-telescope on La Silla, Chile. This camera covers an area of more than 0 5 0 5 , which is larger than the field initially observed from space by GOODS. The footprint of this larger WFI-based image is occasionally called Extended CDFS or E-CDFS, but we just call ...
... Baade et al. 1999) at the MPG/ESO 2.2m-telescope on La Silla, Chile. This camera covers an area of more than 0 5 0 5 , which is larger than the field initially observed from space by GOODS. The footprint of this larger WFI-based image is occasionally called Extended CDFS or E-CDFS, but we just call ...
X. Nuclear star clusters in low-mass early-type galaxies
... sizes of the NSCs, although not without some uncertainty, since also a widely accepted theory for the formation of GCs is still lacking. Bekki et al. (2004) present scaling relations for the sizes of NSCs based on N-body simulations of the merging of equal-mass star clusters; however, they do not pr ...
... sizes of the NSCs, although not without some uncertainty, since also a widely accepted theory for the formation of GCs is still lacking. Bekki et al. (2004) present scaling relations for the sizes of NSCs based on N-body simulations of the merging of equal-mass star clusters; however, they do not pr ...
Lambda-CDM model
The ΛCDM (Lambda cold dark matter) or Lambda-CDM model is a parametrization of the Big Bang cosmological model in which the universe contains a cosmological constant, denoted by Lambda (Greek Λ), associated with dark energy, and cold dark matter (abbreviated CDM). It is frequently referred to as the standard model of Big Bang cosmology, because it is the simplest model that provides a reasonably good account of the following properties of the cosmos: the existence and structure of the cosmic microwave background the large-scale structure in the distribution of galaxies the abundances of hydrogen (including deuterium), helium, and lithium the accelerating expansion of the universe observed in the light from distant galaxies and supernovaeThe model assumes that general relativity is the correct theory of gravity on cosmological scales.It emerged in the late 1990s as a concordance cosmology, after a period of time when disparate observed properties of the universe appeared mutually inconsistent, and there was no consensus on the makeup of the energy density of the universe.The ΛCDM model can be extended by adding cosmological inflation, quintessence and other elements that are current areas of speculation and research in cosmology.Some alternative models challenge the assumptions of the ΛCDM model. Examples of these are modified Newtonian dynamics, modified gravity and theories of large-scale variations in the matter density of the universe.