Super-Eddington outburst in a binary system: V4641 Sgr Mikhail Revnivtsev, Marat Gilfanov
... ∆mV ∼ 5 during the outburst! Factor of 100 increase of the optical luminosity! What is the reason for that? Is it common/normal or ...
... ∆mV ∼ 5 during the outburst! Factor of 100 increase of the optical luminosity! What is the reason for that? Is it common/normal or ...
Candidate star clusters toward the inner Milky Way discovered on
... Methods. We applied an automated two-step procedure to the point-source catalog derived from the deep KS images: first, we identified overdensities of stars, and then we selected only candidate clusters with probable member stars that match an isochrone with a certain age, distance, and extinction o ...
... Methods. We applied an automated two-step procedure to the point-source catalog derived from the deep KS images: first, we identified overdensities of stars, and then we selected only candidate clusters with probable member stars that match an isochrone with a certain age, distance, and extinction o ...
Hidden57_rf
... of images using three different wavebands of light. Infrared data from the Spitzer Space Telescope are coloured red; visible data from the Hubble Space Telescope are yellow; and X-ray data from the Chandra X-ray Observatory are green and blue. Located 10,000 light-years away in the constellation Cas ...
... of images using three different wavebands of light. Infrared data from the Spitzer Space Telescope are coloured red; visible data from the Hubble Space Telescope are yellow; and X-ray data from the Chandra X-ray Observatory are green and blue. Located 10,000 light-years away in the constellation Cas ...
ASPEN WORKSHOP 2003
... interaction, as in half of ULIRGS [as long as they are identified as “single galaxy”!] Simulations show that AI stays above 0.35 for about 700 Myears, but NOT for face-on HDF application: rest frame B morphologies, NICMOS extends out to z=3 Correcting for selection effects by simulating 38 nearer ga ...
... interaction, as in half of ULIRGS [as long as they are identified as “single galaxy”!] Simulations show that AI stays above 0.35 for about 700 Myears, but NOT for face-on HDF application: rest frame B morphologies, NICMOS extends out to z=3 Correcting for selection effects by simulating 38 nearer ga ...
PP Chapter 28 Text
... We see the Sun’s luminosity as LSun. If we were on a spaceship twice as far away from the Sun, its apparent brightness would appear A. B. C. D. ...
... We see the Sun’s luminosity as LSun. If we were on a spaceship twice as far away from the Sun, its apparent brightness would appear A. B. C. D. ...
CONSTELLATION PERSEUS The constellation
... and thirsty. A fisherman, Dictys, broke the chest open and found the mother and child. Dictys brought up Perseus as his own son. The brother of Dictys was King Polydectes, who coveted Danaë as a wife. But Danaë was reluctant and Perseus, now grown to manhood, defended her from the king’s advances. B ...
... and thirsty. A fisherman, Dictys, broke the chest open and found the mother and child. Dictys brought up Perseus as his own son. The brother of Dictys was King Polydectes, who coveted Danaë as a wife. But Danaë was reluctant and Perseus, now grown to manhood, defended her from the king’s advances. B ...
IXO as an observatory in the large telescopes era
... 1024 cm-2). This bias may explain the apparently very small fraction of Compton thick AGNs in the Swift/BAT sample (Tueller et al. 2009). At higher redshifts (z~2), it has been suggested from deep multi-wavelengths surveys that Comptonthick AGN at z~2 may be hiding among infrared bright, optically f ...
... 1024 cm-2). This bias may explain the apparently very small fraction of Compton thick AGNs in the Swift/BAT sample (Tueller et al. 2009). At higher redshifts (z~2), it has been suggested from deep multi-wavelengths surveys that Comptonthick AGN at z~2 may be hiding among infrared bright, optically f ...
![arXiv:1502.03605v2 [astro-ph.EP] 24 Apr 2015](http://s1.studyres.com/store/data/017598977_1-7182fa8223b5ceaded332d6412cd3a07-300x300.png)
arXiv:1502.03605v2 [astro-ph.EP] 24 Apr 2015
... the hydrostatic equilibrium equation coupled with a thermodynamic approach based on Gibbs free-energy minimization and Equation-of-State (EoS) modeling. In this regard, our work is similar to earlier studies (Valencia et al. 2007b; Sotin et al. 2007; Seager et al. 2007; Fortney et al. 2007), except ...
... the hydrostatic equilibrium equation coupled with a thermodynamic approach based on Gibbs free-energy minimization and Equation-of-State (EoS) modeling. In this regard, our work is similar to earlier studies (Valencia et al. 2007b; Sotin et al. 2007; Seager et al. 2007; Fortney et al. 2007), except ...
PH607lec08
... In barred S0 galaxies the bar is often the only structure visible in the disk. In types SBa and later the bar often connects to a spiral pattern extending to larger radii (e.g. NGC 1300). Viewed face-on, bars typically appear to have axial ratios of 2. The surface brightness within the bar is often ...
... In barred S0 galaxies the bar is often the only structure visible in the disk. In types SBa and later the bar often connects to a spiral pattern extending to larger radii (e.g. NGC 1300). Viewed face-on, bars typically appear to have axial ratios of 2. The surface brightness within the bar is often ...
The GL 569 Multiple System
... The proper motion of GL 569 A is µα = 275.95 and µδ = −122.12 mas yr−1 (HIPPARCOS). Thus, in the ∼20 years since the discovery by Forrest et al. (1988) of GL 569 B, the A component has moved ∼6′′ on the sky. Our February, 2005 NIRC-2 H- and K-band images showed the photocenter of GL 569 B 4.′′ 18 ± ...
... The proper motion of GL 569 A is µα = 275.95 and µδ = −122.12 mas yr−1 (HIPPARCOS). Thus, in the ∼20 years since the discovery by Forrest et al. (1988) of GL 569 B, the A component has moved ∼6′′ on the sky. Our February, 2005 NIRC-2 H- and K-band images showed the photocenter of GL 569 B 4.′′ 18 ± ...
Constraining the star formation histories of spiral bulges
... attained on either side of the galaxy. This results in a small q 2000 RAS, MNRAS 311, 37±49 ...
... attained on either side of the galaxy. This results in a small q 2000 RAS, MNRAS 311, 37±49 ...
Collisions and Encounters of Stellar Systems
... between two such galaxies is Σ ≈ π(2R)2 . If the positions and velocities of the galaxies are uncorrelated, the rate at which an L! galaxy suffers collisions with similar galaxies is then expected to be of order nΣvp ≈ 10−6 Gyr−1 , so only about one galaxy in 105 would suffer a collision during the ...
... between two such galaxies is Σ ≈ π(2R)2 . If the positions and velocities of the galaxies are uncorrelated, the rate at which an L! galaxy suffers collisions with similar galaxies is then expected to be of order nΣvp ≈ 10−6 Gyr−1 , so only about one galaxy in 105 would suffer a collision during the ...
Gas fraction and star formation efficiency at z \< 1.0⋆⋆⋆⋆⋆⋆
... After new observations of 39 galaxies at z ∼ 0.6–1.0 obtained at the IRAM 30-m telescope, we present our full CO line survey covering the redshift range 0.2 < z < 1. Our aim is to determine the driving factors accounting for the steep decline in the star formation rate during this epoch. We study bo ...
... After new observations of 39 galaxies at z ∼ 0.6–1.0 obtained at the IRAM 30-m telescope, we present our full CO line survey covering the redshift range 0.2 < z < 1. Our aim is to determine the driving factors accounting for the steep decline in the star formation rate during this epoch. We study bo ...
Satellite galaxies in hydrodynamical simulations of Milky Way sized
... them being so far undetected because of their low surface brightness. In this scenario, the ‘common mass scale’ inferred for the observed satellites may in fact just arise from a selection bias. The first high-resolution hydrodynamic simulation able to directly resolve the satellite population has re ...
... them being so far undetected because of their low surface brightness. In this scenario, the ‘common mass scale’ inferred for the observed satellites may in fact just arise from a selection bias. The first high-resolution hydrodynamic simulation able to directly resolve the satellite population has re ...
Distance to VY Canis Majoris with VERA
... (Kovalev et al. 2007). Because these offsets are constant at all epochs, it dose not affect the parallax measurements. Also, when the reference source is not a point source, the positional errors of the target source could occur due to the structure and its variation of the reference source. However ...
... (Kovalev et al. 2007). Because these offsets are constant at all epochs, it dose not affect the parallax measurements. Also, when the reference source is not a point source, the positional errors of the target source could occur due to the structure and its variation of the reference source. However ...
Simulations of the galaxy population constrained by observations
... the regions of parameter space consistent with the data and to obtain robust best-fit parameter estimates with associated confidence ranges. This can yield new insight into how the data constrain galaxy formation physics. We start by investigating the uniqueness of the parameter choices of G11, find ...
... the regions of parameter space consistent with the data and to obtain robust best-fit parameter estimates with associated confidence ranges. This can yield new insight into how the data constrain galaxy formation physics. We start by investigating the uniqueness of the parameter choices of G11, find ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... contribute very little to the luminosity of the event. This is because high-mass stars are much more luminous than low-mass ones. A star of 100 M is about 1000 000 times brighter than the Sun. Even if there is only one star of 100 M every 500 stars of 1 M , it alone outshines all of them, whose c ...
... contribute very little to the luminosity of the event. This is because high-mass stars are much more luminous than low-mass ones. A star of 100 M is about 1000 000 times brighter than the Sun. Even if there is only one star of 100 M every 500 stars of 1 M , it alone outshines all of them, whose c ...
Quiescent and flaring X-ray emission from the nearby M/T dwarf
... Spectrometer) detectors is rather weak; while we clearly see a few photons from prominent emission lines, e.g. O viii at 19 Å and O vii at 21.6–22.1 Å, the RGS spectra are not suitable for a quantitative analysis. Thus we considered only X-ray data taken with the EPIC (European Photon Imaging Camera ...
... Spectrometer) detectors is rather weak; while we clearly see a few photons from prominent emission lines, e.g. O viii at 19 Å and O vii at 21.6–22.1 Å, the RGS spectra are not suitable for a quantitative analysis. Thus we considered only X-ray data taken with the EPIC (European Photon Imaging Camera ...
R136a1
RMC 136a1 (usually abbreviated to R136a1) is a Wolf-Rayet star located at the center of R136, the central condensation of stars of the large NGC 2070 open cluster in the Tarantula Nebula. It lies at a distance of about 50 kiloparsecs (163,000 light-years) in the Large Magellanic Cloud. It has the highest mass and luminosity of any known star, at 265 M☉ and 8.7 million L☉, and also one of the hottest at over 50,000 K.