Submm Observations of Massive Star Formation in the Giant
... the Galaxy at a distance of 1.7 kpc. It is aimed to trace the gas velocities in the filamentary, massive star-forming region NGC 6334 at several scales and to explain its dynamics. For that purpose, different scales are examined from 0.01–10 pc to collect information about the density, molecular abu ...
... the Galaxy at a distance of 1.7 kpc. It is aimed to trace the gas velocities in the filamentary, massive star-forming region NGC 6334 at several scales and to explain its dynamics. For that purpose, different scales are examined from 0.01–10 pc to collect information about the density, molecular abu ...
PowerPoint
... Since there are so few of them, in order to make it possible to find calibrators at more times/elevations, a number of other sources are observed along with the primary sources, and their flux density is bootstrapped from the primary (secondary calibration sources). We would like to have some 10’s o ...
... Since there are so few of them, in order to make it possible to find calibrators at more times/elevations, a number of other sources are observed along with the primary sources, and their flux density is bootstrapped from the primary (secondary calibration sources). We would like to have some 10’s o ...
Global structure and kinematics of stellar haloes in cosmological
... Mpc in radius) extracted from the Millennium Simulation (Springel et al. 2005). The regions were picked to have overdensities at z = 1.5 of (+2, +1, 0, −1, −2)σ, where σ is the root-mean-square deviation from the mean on this spatial scale. The 5 spheres are therefore environmentally diverse in term ...
... Mpc in radius) extracted from the Millennium Simulation (Springel et al. 2005). The regions were picked to have overdensities at z = 1.5 of (+2, +1, 0, −1, −2)σ, where σ is the root-mean-square deviation from the mean on this spatial scale. The 5 spheres are therefore environmentally diverse in term ...
Dark matter scaling relations and the assembly epoch of Coma early
... K2000 galaxies are brighter (and have higher stellar mass) than Coma early-types with a similar halo. Can this be an artifact related to differences in the dynamical models? Many of the K2000 models are based on B-band photometry, while we used RC -band images for the Coma galaxies. Elliptical galax ...
... K2000 galaxies are brighter (and have higher stellar mass) than Coma early-types with a similar halo. Can this be an artifact related to differences in the dynamical models? Many of the K2000 models are based on B-band photometry, while we used RC -band images for the Coma galaxies. Elliptical galax ...
Ultra-luminous Quasars with the Most Massive Black Holes at
... The first low-resolution optical spectrum of this source was obtained with the Lijiang 2.4 m telescope using the YFOSC on 2013 November 25 (UT), then follow-up by Magellan. ...
... The first low-resolution optical spectrum of this source was obtained with the Lijiang 2.4 m telescope using the YFOSC on 2013 November 25 (UT), then follow-up by Magellan. ...
CHARACTERIZING THE COOL KOIs. III. KOI 961: A SMALL STAR
... of low-mass KOIs. The spectrum confirmed that it is a dwarf and not a giant based on the shallowness of the CO absorption band, and we reported an effective temperature of 3200 ± 50 K and an overall metallicity ([M/H]) of −0.33 ± 0.12 using the spectroscopic indices and calibrations of Rojas-Ayala e ...
... of low-mass KOIs. The spectrum confirmed that it is a dwarf and not a giant based on the shallowness of the CO absorption band, and we reported an effective temperature of 3200 ± 50 K and an overall metallicity ([M/H]) of −0.33 ± 0.12 using the spectroscopic indices and calibrations of Rojas-Ayala e ...
Annual Report 2014 - Max Planck Institute for Astrophysics
... particles, and the calculation of transition probThe Max-Planck-Institut für Astrophysik, usually abilities and cross–sections for astrophysical procalled MPA for short, was founded in 1958 under cesses in rarefied media. From its inception the the directorship of Ludwig Biermann. It was estab- MPA h ...
... particles, and the calculation of transition probThe Max-Planck-Institut für Astrophysik, usually abilities and cross–sections for astrophysical procalled MPA for short, was founded in 1958 under cesses in rarefied media. From its inception the the directorship of Ludwig Biermann. It was estab- MPA h ...
PPT
... Additionally, a distance modulus of 13.46±0.1 has been recently derived for NGC 6791 using eclipsing binaries, a totally independent and reliable method that does not make use of theoretical models. Thus, a large error in the distance modulus is quite implausible. The only possibility left to ...
... Additionally, a distance modulus of 13.46±0.1 has been recently derived for NGC 6791 using eclipsing binaries, a totally independent and reliable method that does not make use of theoretical models. Thus, a large error in the distance modulus is quite implausible. The only possibility left to ...
Grosdidier et al. 1998
... • Wolf-Rayet stars are believed to be evolved, very massive (M > 30 M) and metal-rich (> 1/3 Z). • Extreme mass loss (dM/dt up to 10-4 M /yr) at high velocities (up to 2000 km/s). Total mass loss can be a significant fraction of the ZAMS mass. • Occurs during He-core burning, so later burning sta ...
... • Wolf-Rayet stars are believed to be evolved, very massive (M > 30 M) and metal-rich (> 1/3 Z). • Extreme mass loss (dM/dt up to 10-4 M /yr) at high velocities (up to 2000 km/s). Total mass loss can be a significant fraction of the ZAMS mass. • Occurs during He-core burning, so later burning sta ...
Catalogs of Hot White Dwarfs in the Milky Way from GALEX`s
... sequence phase is fairly well understood and observationally constrained, the hot-WD population is hitherto quite elusive, owing to their small radius, hence low optical luminosity, and extremely hot temperatures, to which optical colors are insensitive (see e.g. Bianchi (2007), Bianchi et al. (2007 ...
... sequence phase is fairly well understood and observationally constrained, the hot-WD population is hitherto quite elusive, owing to their small radius, hence low optical luminosity, and extremely hot temperatures, to which optical colors are insensitive (see e.g. Bianchi (2007), Bianchi et al. (2007 ...
Theory of Motion of Matter on the Formation of Galaxy and Star
... matter unable to move rapidly towards nebula center. It produced relative motion between matter moving outwards primordial galaxy nebula center high density nuclear zone and dispersed matter, which has changed the motion direction of dispersed matter and made it move towards nebula center. Energy ch ...
... matter unable to move rapidly towards nebula center. It produced relative motion between matter moving outwards primordial galaxy nebula center high density nuclear zone and dispersed matter, which has changed the motion direction of dispersed matter and made it move towards nebula center. Energy ch ...
Core formation in giant planets formed through
... compared with the core-accretion model is that it need no core to explain the formation of a planet and that it does not predict the formation of a core. This means that the new formed giant gaseous protoplanet has the same abundance of elements as the protoplanetary disc which has a solar compositi ...
... compared with the core-accretion model is that it need no core to explain the formation of a planet and that it does not predict the formation of a core. This means that the new formed giant gaseous protoplanet has the same abundance of elements as the protoplanetary disc which has a solar compositi ...