... of Pennsylvania, 209 South 33rd St., Philadelphia, PA 191046396, inr@morales.physics.upenn.edu 3 Division of Physics, M/S 10333, California Institute of Technology, Pasadena CA 91125, diver@cco.caltech.edu 4 Infrared Processing and Analysis Center ...
... A 3 scaling would favor retentions of IMBHs with M~102-103 Min globular clusters, but the fraction of large kicks would still be high enough, compared to earlier estimates using PN/EOB (calibrated with NR) [Schnittman & Buonanno'07] BBCKMC · Very large ...
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Ссылки http://www.stsci.edu/institute/itsd/information/streaming/archive/OSBHM2009/ManuelaCampanelli033009Hi_supporting/ManuelaCampanelli033009C -- 2649.5 Кб -- 02.04.2009 Похожие документы
... This limit corresp onds to the maximum star formation rate of 103M yr-1 of a gas-rich spheroid undergoing a monolithic collapse on a dynamical time scale. ...
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Ссылки http://www.stsci.edu/science/starburst/Preprints/LaPalma2001.pdf -- 768.4 Кб -- 12.08.2003 Похожие документы
... and Lin Simulations Gaia 104 Known RV-Discovered Planets Solar System Planets Radial Velocity 1 m/s Planet Mass Sensitivity, M103 Jupiter 102 SIM Lite Farthest Star 101 Saturn Neptune Uranus Habitable Worlds for Best 60 SIM Lite Target Stars SIM Lite ...
... As an example, the expected luminosity of [OIV](25.9 micron) in a 103M_sun cluster in M51a is about 3-5 10-20 erg/s/cm2, implying that S/N=10 can be achieved for this line with MIRI, at R=1000, in 100,000 seconds. ...
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Ссылки http://www.stsci.edu/jwst/doc-archive/technical-reports/JWST-STScI-000703.pdf -- 366.8 Кб -- 05.02.2013 Похожие документы