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A Direct Measurement of the Total Gas Column Density in Orion KL
Comito, C.; Schilke, P.; Lis, D. C. +7 more
The large number of high-J lines of C18O available via the Herschel Space Observatory provide an unprecedented ability to model the total CO column density in hot cores. Using the emission from all the observed lines (up to J = 15-14), we sum the column densities in each individual level to obtain the total column after correcting for t…
Galaxy alignments in very X-ray luminous clusters at z > 0.5
Hung, Chao-Ling; Ebeling, Harald
We present the results of a search for galaxy alignments in 12 galaxy clusters at z > 0.5, a statistically complete subset of the very X-ray luminous clusters from the MAssive Cluster Survey (MACS). Using high-quality images taken with the Hubble Space Telescope (HST) that render measurement errors negligible, we find no radial galaxy alignment…
Supergranules as Probes of Solar Convection Zone Dynamics
Hathaway, David H.
Supergranules are convection cells seen at the Sun's surface as a space filling pattern of horizontal flows. While typical supergranules have diameters of about 35 Mm, they exhibit a broad spectrum of sizes from ~10 Mm to ~100 Mm. Here we show that supergranules of different sizes can be used to probe the rotation rate in the Sun's outer convectio…
Estimating distance, pressure, and dust opacity using submillimeter observations of self-gravitating filaments
Martin, P. G.; Fischera, J.
We present a detailed study of the surface brightness profiles of dense filaments in
Astrometric confirmation of young low-mass binaries and multiple systems in the Chamaeleon star-forming regions
Neuhäuser, R.; Schmidt, T. O. B.; Mugrauer, M. +4 more
Context. The star-forming regions in Chamaeleon (Cha) are one of the nearest (distance ~ 165 pc) and youngest (age ~ 2 Myr) conglomerates of recently formed stars and the ideal target for population studies of star formation.
Aims: We investigate a total of 16 Cha targets that have been suggested, but not confirmed, to be binaries or multiple…
Detection of Mg spinel lithologies on central peak of crater Theophilus using Moon Mineralogy Mapper (M3) data from Chandrayaan-1
Bhattacharya, S.; Kiran Kumar, A. S.; Chauhan, P. +3 more
Spectral reflectance data derived from Moon Mineralogy Mapper (M3) onboard India's Chandrayaan-1 has revealed Fe bearing Mg-spinel-rich lithology on central peaks of the crater Theophilus. These newly identified Fe bearing Mg-spinel-rich rock types are defined by their strong 2-µm absorption and lack of 1-µm absorptions in s…
Dissociative recombination of nitrile ions with implications for Titan's upper atmosphere
Vigren, E.; Semaniak, J.; Hamberg, M. +6 more
Nitrile ions are abundant in Titan's upper atmosphere and are expected to be lost mainly via dissociative recombination with free electrons. We review in this paper a series of experimental results on the dissociative recombination reactions of nitrile ions known/expected to be present in Titan's upper atmosphere. The experiments were all performe…
Warm absorber energetics in broad-line radio galaxies
Costantini, E.; Grandi, P.; Torresi, E. +1 more
We review the soft X-ray properties of 3C 390.3, 3C 120, 3C 382 and 3C 445, the only broad-line radio galaxies (BLRGs) for which good quality gratings data are currently available. The XMM-Newton/Reflection Grating Spectrometer data of 3C 390.3 and 3C 120 were re-analysed searching for warm absorbers, already discovered in 3C 382 and 3C 445. We co…
The growth of wind-waves in Titan's hydrocarbon seas
Lorenz, Ralph D.; Hayes, Alexander G.
Ocean wave growth on Titan is considered. The classic Sverdrup-Munk theory for terrestrial wave growth is applied to Titan, and is compared with a simple energy balance model that exposes the effect of Titan's environmental parameters (air density, gravity, and fluid density). These approaches are compared with the only previously-published (semi-…
η Carinae: linelist for the emission spectrum of the Weigelt blobs in the 1700 to 10 400 Å wavelength region
Gull, T. R.; Johansson, S.; Hartman, H. +1 more
Aims: We present line identifications in the 1700 to 10 400 Å region for the Weigelt blobs B and D, located 0″.1 to 0″.3 NNW of