The visibility of Lyman Alpha Emitters: constraining reionization
... through the IGM and reach the observer. As expected, this transmission sensitively depends on the IGM H I ionization state and it has been shown that only galaxies residing in over-lapping H II regions would be observed as LAEs in the initial stages of reionization, i.e. reionization increases the o ...
... through the IGM and reach the observer. As expected, this transmission sensitively depends on the IGM H I ionization state and it has been shown that only galaxies residing in over-lapping H II regions would be observed as LAEs in the initial stages of reionization, i.e. reionization increases the o ...
Abstract The Star Formation History of Low Surface Brightness Galaxies
... The star formation histories of low surface brightness galaxies are interesting but poorly constrained. These objects tend to be rather blue, contradicting the initial impression that they may simply be faded remnants of higher surface brightness galaxies whose star formation has finished. Other sce ...
... The star formation histories of low surface brightness galaxies are interesting but poorly constrained. These objects tend to be rather blue, contradicting the initial impression that they may simply be faded remnants of higher surface brightness galaxies whose star formation has finished. Other sce ...
A Universal Stellar Initial Mass Function? A Critical Look Further
... 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 place where the correction becomes important (around 1 M% ). Knowledge of the SFH of the Galaxy i ...
... 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 place where the correction becomes important (around 1 M% ). Knowledge of the SFH of the Galaxy i ...
Astronomy Astrophysics Gaia-ESO Survey: The analysis of high-resolution The
... Aims. These UVES spectra are analyzed in parallel by several state-of-the-art methodologies. Our aim is to present how these analyses were implemented, to discuss their results, and to describe how a final recommended parameter scale is defined. We also discuss the precision (method-tomethod dispers ...
... Aims. These UVES spectra are analyzed in parallel by several state-of-the-art methodologies. Our aim is to present how these analyses were implemented, to discuss their results, and to describe how a final recommended parameter scale is defined. We also discuss the precision (method-tomethod dispers ...
from z=0 to z=1
... 10 times fainter than ULIRGs. 6. LBGs and SCUBA galaxies (UV and IR selected galaxies at z~3) do not overlap with each other very much. SCUBA galaxies have significantly higher SFR, higher attenuation, higher stellar mass, and higher correlation length than LBGs. 7. At intermediate redshifts of z~0. ...
... 10 times fainter than ULIRGs. 6. LBGs and SCUBA galaxies (UV and IR selected galaxies at z~3) do not overlap with each other very much. SCUBA galaxies have significantly higher SFR, higher attenuation, higher stellar mass, and higher correlation length than LBGs. 7. At intermediate redshifts of z~0. ...
Here - NASA/IPAC Extragalactic Database
... the morphology of H ii regions is generally rather complex on all scales. Typical hydrogen densities n are 103 – 104 cm−3 for compact H ii regions. The average densities in giant extragalactic H ii regions are lower, typically 102 cm−3 since giant H ii regions encompass also zones of diffuse materia ...
... the morphology of H ii regions is generally rather complex on all scales. Typical hydrogen densities n are 103 – 104 cm−3 for compact H ii regions. The average densities in giant extragalactic H ii regions are lower, typically 102 cm−3 since giant H ii regions encompass also zones of diffuse materia ...
Observational evidence for AGN feedback in early
... activity, black hole activity, the composite of the two and quiescence. We find that emission is mostly LINER (low ionization nuclear emission line region) like in high-mass galaxies (σ > 200 km s−1 ) and roughly evenly distributed between star formation and AGN at intermediate and low (σ < 100 km s ...
... activity, black hole activity, the composite of the two and quiescence. We find that emission is mostly LINER (low ionization nuclear emission line region) like in high-mass galaxies (σ > 200 km s−1 ) and roughly evenly distributed between star formation and AGN at intermediate and low (σ < 100 km s ...
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 ...
JENAM-2011 Book of abstracts
... probability for a massive star to become an accretion powered X-ray source once upon its lifetime. This explains the unexpectedly high contribution of accreting compact objects of stellar mass to the Cosmic X-ray background, ∼7-10%. Underneath bright X-ray binaries, unresolved emission is present in ...
... probability for a massive star to become an accretion powered X-ray source once upon its lifetime. This explains the unexpectedly high contribution of accreting compact objects of stellar mass to the Cosmic X-ray background, ∼7-10%. Underneath bright X-ray binaries, unresolved emission is present in ...
2 Justification and benefits in joining TMT
... reveal that the Universe is dominated by dark matter and dark energy. The nature of these two dark components is the most fundamental question in (astro-)physics today. The discovery of more than 400 extrasolar planet systems indicates that our solar system may be the exception rather than the norm; ...
... reveal that the Universe is dominated by dark matter and dark energy. The nature of these two dark components is the most fundamental question in (astro-)physics today. The discovery of more than 400 extrasolar planet systems indicates that our solar system may be the exception rather than the norm; ...
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 ...
Astronomy
... originate outside the Earth's atmosphere (such as the cosmic background radiation). It is concerned with the evolution, physics, chemistry, meteorology, and motion of celestial objects, as well as the formation and development of the universe. Astronomy is one of the oldest sciences. Prehistoric cul ...
... originate outside the Earth's atmosphere (such as the cosmic background radiation). It is concerned with the evolution, physics, chemistry, meteorology, and motion of celestial objects, as well as the formation and development of the universe. Astronomy is one of the oldest sciences. Prehistoric cul ...
Carbon, nitrogen and oxygen abundances in
... stars are selected according to their effective temperatures Teff and surface gravities log g, namely: Teff is between 15 300 and 24 100 K and log g is mostly greater than 3.75; therefore, stars with medium masses of 5–11 M are selected. Theory predicts for the stars with such parameters that the C ...
... stars are selected according to their effective temperatures Teff and surface gravities log g, namely: Teff is between 15 300 and 24 100 K and log g is mostly greater than 3.75; therefore, stars with medium masses of 5–11 M are selected. Theory predicts for the stars with such parameters that the C ...
Stellarium User Guide
... scipting facility is Stellarium’s version of a “Presentation”, a feature that may be used to run an astronomical or other presentation for instruction or entertainment from within the Stellarium program. The original Stratoscript was quite limited in what it could do so a new Stellarium Scripting Sy ...
... scipting facility is Stellarium’s version of a “Presentation”, a feature that may be used to run an astronomical or other presentation for instruction or entertainment from within the Stellarium program. The original Stratoscript was quite limited in what it could do so a new Stellarium Scripting Sy ...
Science Case for the Chinese Participation of TMT
... reveal that the Universe is dominated by dark matter and dark energy. The nature of these two dark components is the most fundamental question in (astro-)physics today. The discovery of more than 400 extrasolar planet systems indicates that our solar system may be the exception rather than the norm; ...
... reveal that the Universe is dominated by dark matter and dark energy. The nature of these two dark components is the most fundamental question in (astro-)physics today. The discovery of more than 400 extrasolar planet systems indicates that our solar system may be the exception rather than the norm; ...
The Formation of Population III Stars in Gas Accretion Stage: Effects
... a collapsing primordial cloud with a simple initial setting and showed fragmentation before protostar formation (see also Machida et al. 2008, 2009a,b). Recently, starting from the cosmological setting, Turk et al. (2009) also showed the possibility of fragmentation during the gas collapsing phase. ...
... a collapsing primordial cloud with a simple initial setting and showed fragmentation before protostar formation (see also Machida et al. 2008, 2009a,b). Recently, starting from the cosmological setting, Turk et al. (2009) also showed the possibility of fragmentation during the gas collapsing phase. ...
THE UV-OPTICAL COLOR MAGNITUDE DIAGRAM. II. PHYSICAL
... quite clearly how the NUV r color covers a much wider magnitude range than g r. In addition, the g r color starts to saturate for red galaxies, while NUV r varies by more than 2 magnitudes. We see indications from these plots that rest-frame UV-optical colors correlate with Sersic index (and ...
... quite clearly how the NUV r color covers a much wider magnitude range than g r. In addition, the g r color starts to saturate for red galaxies, while NUV r varies by more than 2 magnitudes. We see indications from these plots that rest-frame UV-optical colors correlate with Sersic index (and ...
Mass Functions in Fractal Clouds: The Role of Cloud Structure in the
... M 3/(2η−3) ∼ M −1.3 when η = 1/3, which is close to the Salpeter IMF, dN/d log M ∝ M −1.35 . The final IMF was assumed to be this clump mass function multiplied by the probability that a clump of mass M exceeds the thermal Jeans mass; the pdf for thermal Jeans masses comes from the pdf for density a ...
... M 3/(2η−3) ∼ M −1.3 when η = 1/3, which is close to the Salpeter IMF, dN/d log M ∝ M −1.35 . The final IMF was assumed to be this clump mass function multiplied by the probability that a clump of mass M exceeds the thermal Jeans mass; the pdf for thermal Jeans masses comes from the pdf for density a ...
IK Pegasi
IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 150 light years from the Solar System.The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day. Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.44 solar masses (M☉), it may explode as a Type Ia supernova.