Recipes for ULX formation: necessary ingredients and garnishments
... evolution, when its protostars are still surrounded by large, optically-thick envelopes, and are still accreting from neutral intra-cluster gas. Collapsing molecular clumps with masses ∼ 104 M are large enough to enable the formation of stars with masses > 100M via accretion and coalescence, and a ...
... evolution, when its protostars are still surrounded by large, optically-thick envelopes, and are still accreting from neutral intra-cluster gas. Collapsing molecular clumps with masses ∼ 104 M are large enough to enable the formation of stars with masses > 100M via accretion and coalescence, and a ...
Active Galactic Nuclei
... • Early radio telescopes found radio emission from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like stars. ...
... • Early radio telescopes found radio emission from stars, nebulae, and some galaxies. • There were also point-like, or star-like, radio sources which varied rapidly these are the `quasi-stellar’ radio sources or quasars. • In visible light quasars appear as points, like stars. ...
Project Descriptions - UCI Physics and Astronomy
... binary are very close together and much farther away from us in comparison, the two stars appears to be one single object, but the light you observe will be the combined light of both stars. As the one star in the system passes in front of the other, occulting part of its surface, the combined color ...
... binary are very close together and much farther away from us in comparison, the two stars appears to be one single object, but the light you observe will be the combined light of both stars. As the one star in the system passes in front of the other, occulting part of its surface, the combined color ...
4 Distances in Astronomy
... reliably. The best ground-based telescopes can achieve a resolution of about 0:500 , which can sometimes be reduced to about 0:0100 by averaging over many measurements. This corresponds to a distance of about 300 ly. Spacebased telescopes can do better (see the discussion of Hipparcos below), but so ...
... reliably. The best ground-based telescopes can achieve a resolution of about 0:500 , which can sometimes be reduced to about 0:0100 by averaging over many measurements. This corresponds to a distance of about 300 ly. Spacebased telescopes can do better (see the discussion of Hipparcos below), but so ...
A dozen new galaxies caught in the act: Gas stripping and extended
... (60×2 kpc) Hα emitting region associated with a galaxy of the Coma cluster. Sun, Donahue & Voit (2007) found a ∼ 40 kpc Hα tail of a galaxy in Abell 3627. The galaxy also had a ∼ 70 kpc X-ray tail. Sun et al. (2010) investigated the galaxy to show two of ∼ 80 kpc tails, and also reported one more ga ...
... (60×2 kpc) Hα emitting region associated with a galaxy of the Coma cluster. Sun, Donahue & Voit (2007) found a ∼ 40 kpc Hα tail of a galaxy in Abell 3627. The galaxy also had a ∼ 70 kpc X-ray tail. Sun et al. (2010) investigated the galaxy to show two of ∼ 80 kpc tails, and also reported one more ga ...
Chemo-spectrophotometric evolution of spiral galaxies ± II. Main
... Evolution of spiral galaxies ± II the simple scaling relations for galactic discs (established in the framework of SAMs; see Section 2.2) in order to derive initial gaseous profiles. They subsequently calculate the full chemical and spectrophotometric evolution of such discs for the case of low sur ...
... Evolution of spiral galaxies ± II the simple scaling relations for galactic discs (established in the framework of SAMs; see Section 2.2) in order to derive initial gaseous profiles. They subsequently calculate the full chemical and spectrophotometric evolution of such discs for the case of low sur ...
First Light Sources at the End of the Dark Ages: Direct
... helium, the very first stars were metal-free (Population III). Their formation and evolution hold key clues that can establish how the Universe was subsequently enriched with metals, and how and when massive galaxies containing Population II stars formed. There is an apparent chemical enrichment “fl ...
... helium, the very first stars were metal-free (Population III). Their formation and evolution hold key clues that can establish how the Universe was subsequently enriched with metals, and how and when massive galaxies containing Population II stars formed. There is an apparent chemical enrichment “fl ...
Lyman-α observations of astrospheres
... ejections (CMEs) that are seen on the Sun but not yet detected on stars. Drake et al. (2013) argued that CMEs in active stars could dominate the mass-loss rate based on an extrapolation of solar data, but this process must be tested in realistic models and against stellar CME measurements when they ...
... ejections (CMEs) that are seen on the Sun but not yet detected on stars. Drake et al. (2013) argued that CMEs in active stars could dominate the mass-loss rate based on an extrapolation of solar data, but this process must be tested in realistic models and against stellar CME measurements when they ...
Importance of the bonus lines (depends on excitation)
... Thin (1 mag) and dense (5 105 cm-3) expanding layer Traced by high-J CO rotational lines and water (Herschel data). Reasonably well explained by gas phase PDR chemical models Thin (10mag) and dense (< 106 cm-3) molecular layer Traced by IRAM and Herschel data. Partially explained by gas phase PDR ch ...
... Thin (1 mag) and dense (5 105 cm-3) expanding layer Traced by high-J CO rotational lines and water (Herschel data). Reasonably well explained by gas phase PDR chemical models Thin (10mag) and dense (< 106 cm-3) molecular layer Traced by IRAM and Herschel data. Partially explained by gas phase PDR ch ...
Galaxy Cosmological Mass Function
... Aims. This paper studies the galaxy cosmological mass function (GCMF) in a semi-empirical relativistic approach that uses observational data provided by recent galaxy redshift surveys. Methods. Starting from a previously presented relation between the mass-to-light ratio, the selection function obta ...
... Aims. This paper studies the galaxy cosmological mass function (GCMF) in a semi-empirical relativistic approach that uses observational data provided by recent galaxy redshift surveys. Methods. Starting from a previously presented relation between the mass-to-light ratio, the selection function obta ...
Evidence for a signature of the galactic bar in the solar neighbourhood
... a mean asymmetrical drift hSi ≈ 20 - 30 km s−1 . Nevertheless, a quantitative interpretation of the origin of this phenomenon has never been given until now. Two new facts allow to go more deeply into this question. At first, after the de Vaucouleurs (1964) presumption, a series of more or less dire ...
... a mean asymmetrical drift hSi ≈ 20 - 30 km s−1 . Nevertheless, a quantitative interpretation of the origin of this phenomenon has never been given until now. Two new facts allow to go more deeply into this question. At first, after the de Vaucouleurs (1964) presumption, a series of more or less dire ...
Self-similarity in the chemical evolution of galaxies and the delay
... It is also important to note exactly which sample we are using. Indeed, to the basic set of model ellipticals from Section 6.3 of Y13 we impose an overall lower-mass limit of log(M*)=10.0, in order to roughly match that of the W15 sample. Here, we did not impose the additional cut based on the 1σ sc ...
... It is also important to note exactly which sample we are using. Indeed, to the basic set of model ellipticals from Section 6.3 of Y13 we impose an overall lower-mass limit of log(M*)=10.0, in order to roughly match that of the W15 sample. Here, we did not impose the additional cut based on the 1σ sc ...
Article PDF - IOPscience
... (60 × 2 kpc) Hα emitting region associated with a galaxy of the Coma cluster. Sun et al. (2007) found a ∼40 kpc Hα tail of a galaxy in Abell 3627. The galaxy also had a ∼70 kpc X-ray tail. Sun et al. (2010) investigated the galaxy to show two ∼80 kpc tails, and also reported one more galaxy with a > ...
... (60 × 2 kpc) Hα emitting region associated with a galaxy of the Coma cluster. Sun et al. (2007) found a ∼40 kpc Hα tail of a galaxy in Abell 3627. The galaxy also had a ∼70 kpc X-ray tail. Sun et al. (2010) investigated the galaxy to show two ∼80 kpc tails, and also reported one more galaxy with a > ...
Carolina Kehrig
... WR features are not seen whenever narrow HeII is observed IFS spatial offset between nebular HeII-emitting zone and WR stars can be a possible explanation for the non-detection of WR features in some galaxy spectra Nearby narrow HeII emitters, specially metal-poor ones, are fundamental to be ...
... WR features are not seen whenever narrow HeII is observed IFS spatial offset between nebular HeII-emitting zone and WR stars can be a possible explanation for the non-detection of WR features in some galaxy spectra Nearby narrow HeII emitters, specially metal-poor ones, are fundamental to be ...
Absolute magnitude of type Ia supernovae
... Research on the Relation between Type Ia Supernova’s Brightness and Galaxy’s Distance 1 Supernovae are violent phenomena in which runaway of thermonuclear fusion causes whole star’s explosion. In spite of calling a supernova as “a new star”, this phenomenon occurs at the last stage of a star’s evolu ...
... Research on the Relation between Type Ia Supernova’s Brightness and Galaxy’s Distance 1 Supernovae are violent phenomena in which runaway of thermonuclear fusion causes whole star’s explosion. In spite of calling a supernova as “a new star”, this phenomenon occurs at the last stage of a star’s evolu ...
Probing the Dark Matter Content of Local Group Dwarf Spheroidal
... As this was significantly higher than the values typical of globular star clusters, this provided the first hint that the dSphs were a class of stellar system distinct from the globular clusters, despite the fact that in many cases their stellar mass was similar. Subsequent observations have borne o ...
... As this was significantly higher than the values typical of globular star clusters, this provided the first hint that the dSphs were a class of stellar system distinct from the globular clusters, despite the fact that in many cases their stellar mass was similar. Subsequent observations have borne o ...
N-body Simulations and Galaxy Formation
... galaxies, the basic building blocks of our universe. You learn how particle models for disk galaxies are set up and how their dynamical evolution can be simulated using simulations. In the astrophysical context this is particularly important to understand galaxy interactions which are observed in th ...
... galaxies, the basic building blocks of our universe. You learn how particle models for disk galaxies are set up and how their dynamical evolution can be simulated using simulations. In the astrophysical context this is particularly important to understand galaxy interactions which are observed in th ...
H I observations of three compact high
... HVCs are distributed throughout the Local Group, but this theory has been disproven several times by searching for HVCs around other galaxies: all these observations have either failed to find any HVCs (Pisano et al. 2004, 2007) or located them very close to their host galaxies (Thilker et al. 2004) ...
... HVCs are distributed throughout the Local Group, but this theory has been disproven several times by searching for HVCs around other galaxies: all these observations have either failed to find any HVCs (Pisano et al. 2004, 2007) or located them very close to their host galaxies (Thilker et al. 2004) ...
FROM MOLECULAR CLOUDS TO STARS 1 Star formation and the
... clouds. CO is the best tracer of the diffuse medium because it is very abundant ([CO]/[ H2], ~ 10-4), it has a relatively high dissociation energy (11.09 eV) and it can be excited from millimetre wavelengths (few Kelvin) to the near infrared (~ 3000 K) in a variety of different physical environments ...
... clouds. CO is the best tracer of the diffuse medium because it is very abundant ([CO]/[ H2], ~ 10-4), it has a relatively high dissociation energy (11.09 eV) and it can be excited from millimetre wavelengths (few Kelvin) to the near infrared (~ 3000 K) in a variety of different physical environments ...
UV Spectroscopy of Star-Grazing Comets within the 49 Ceti Debris
... We present analysis of time-variable, Doppler-shifted absorption features in far-UV spectra of the unusual 49 Ceti debris disk. This nearly edge-on disk is one of the brightest known, and is one of the very few containing detectable amounts of circumstellar gas as well as dust. In our two visits of ...
... We present analysis of time-variable, Doppler-shifted absorption features in far-UV spectra of the unusual 49 Ceti debris disk. This nearly edge-on disk is one of the brightest known, and is one of the very few containing detectable amounts of circumstellar gas as well as dust. In our two visits of ...
here - ISAS/JAXA
... Christopher Fuller Galaxy Evolution in Coma, Fornax and Virgo nearby and Clusters as seen by Herschel Yusei Koyama SPICA distant cluster survey: unveiling the dust-obscured star formation activity triggered by young cluster environments Kazumi Murata Environmental dependence of galaxy properties rev ...
... Christopher Fuller Galaxy Evolution in Coma, Fornax and Virgo nearby and Clusters as seen by Herschel Yusei Koyama SPICA distant cluster survey: unveiling the dust-obscured star formation activity triggered by young cluster environments Kazumi Murata Environmental dependence of galaxy properties rev ...
MICROQUASARS
... Particle energy in QSOs and mQSOs are comparable (blazar-microblazar analogy) The kinetic power in mQSOs is equal or larger than the radiated power Electrons in the jets are accelerated up to TeV energies LS 5039: jets are steady, two-sided, seem to have bulk motions of 0.2-0.3c as compact mQSO jets ...
... Particle energy in QSOs and mQSOs are comparable (blazar-microblazar analogy) The kinetic power in mQSOs is equal or larger than the radiated power Electrons in the jets are accelerated up to TeV energies LS 5039: jets are steady, two-sided, seem to have bulk motions of 0.2-0.3c as compact mQSO jets ...
Description of Pictures In the Dome
... The Orion Nebula (also known as Messier 42, M42, or NGC 1976) is a diffuse nebula situated south of Orion's Belt. It is one of the brightest nebulae, and is visible to the naked eye in the night sky. M42 is located at a distance of 1,344 ± 20 light years and is the closest region of massive star for ...
... The Orion Nebula (also known as Messier 42, M42, or NGC 1976) is a diffuse nebula situated south of Orion's Belt. It is one of the brightest nebulae, and is visible to the naked eye in the night sky. M42 is located at a distance of 1,344 ± 20 light years and is the closest region of massive star for ...
File - Mr. Gray`s Class
... base would cover the entire state of Arizona. Nearby there begins the Mariner Valley, a "grand canyon" system so vast that on Earth it would stretch from Los Angeles to Washington, D.C. Between Venus and Mars is our own Earth, whose thick atmosphere contains oxygen and allows us to survive. Its surf ...
... base would cover the entire state of Arizona. Nearby there begins the Mariner Valley, a "grand canyon" system so vast that on Earth it would stretch from Los Angeles to Washington, D.C. Between Venus and Mars is our own Earth, whose thick atmosphere contains oxygen and allows us to survive. Its surf ...
Building` a Galaxy SED
... Practical problem: galaxies are biased tracers of underlying mass distribution. In order to use galaxies to measure underlying mass distribution, we must understand galaxies. ...
... Practical problem: galaxies are biased tracers of underlying mass distribution. In order to use galaxies to measure underlying mass distribution, we must understand galaxies. ...