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Simultaneous Velocity-Intensity Spectral and Cross-Spectral Fitting of Helioseismic Data
Hill, F.; Barban, C.; Kras, S.
Solar oscillation parameters, such as the frequency, are usually estimated by fitting the mode profile in the velocity (V) power spectrum. In this paper, the solar oscillation parameters are derived by simultaneously fitting four observational spectra: V and I (intensity) power, I-V phase difference, and I-V coherence using the model of Severino e…
Observation of continuum radiations from the Cluster fleet: first results from direction finding
Buckley, A.; Canu, P.; Décréau, P. +9 more
Available from http://www.copernicus.org/site/EGU/annales/22/7/2607.htm?FrameEngine=false;
Detection of Saturnian X-ray emission with XMM-Newton
Schmitt, J. H. M. M.; Ness, J. -U.; Robrade, J.
The giant planet Saturn was observed by XMM-Newton in September 2002. We present and analyse these XMM-Newton observations and compare our findings to the Chandra observations of Saturn. Contamination of the XMM-Newton data by optical light is found to be severe in the medium and thin filters, but with the thick filter all optical light is suffici…
STIS observations of FLIERs in NGC 7662
Balick, B.; Corradi, R. L. M.; Patriarchi, P. +1 more
We observed the planetary nebula NGC 7662 with STIS on board the HST to investigate the physical conditions in the microstructures within the nebula at high spatial resolution and to closely examine the physical conditions in FLIERs. We aim to reveal spectroscopic differences in small scale structures moving at about the same velocity as the surro…
The Ofpe/WN9 Stars in M33
Massey, Philip; Bianchi, Luciana; Bohlin, Ralph
We present Hubble Space Telescope/STIS Ultraviolet spectra of the six known Ofpe/WN9 stars (``slash stars'') in M33. These stars were selected for showing the characteristics of the Ofpe/WN9 class from previous optical ground-based spectroscopy. The UV spectra are rich in wind lines whose strength and terminal velocity vary greatly across our targ…
The nearest extreme starburst: bubbles, young star clusters and outflow in the merger NGC 3256
Taniguchi, Y.; Terlevich, R.; Díaz, R. J. +6 more
We have studied the extreme starburst in the infrared merger NGC 3256. We detect four galactic bubbles (using ESO New Technology Telescope and Hubble Space Telescope WFPC2 Hα images). These shells would be associated with previous supernova explosions.
The first analysis of the spatial distribution of young star cluster candidates shows that …NGC 6543. II. Understanding the Dilation of the Cat's Eye
Balick, Bruce; Hajian, Arsen R.
Hubble Space Telescope images of NGC 6543 taken in 1994.7 and 2000.7 reveal a pattern of overall expansion of its core over 6 years. Spatial scale changes of the sharp edges of filamentary structures are consistent with purely radial motions. One prolate ellipsoid, E25, lies along the overall symmetry axis of the core. We find that it expands unif…
Dynamics of the fast solar tachocline. II. Migrating field
Forgács-Dajka, E.
We present detailed numerical calculations of the fast solar tachocline based on the assumption that the dynamo field dominates over the dynamics of the tachocline. In the present paper of the series, we focus on three shortfalls of the earlier models. First, instead of the simple oscillating dipole poloidal field we study the more general magneti…
The field surrounding NGC 7603: Cosmological or non-cosmological redshifts?
López-Corredoira, M.; Gutiérrez, C. M.
We present new observations of the field surrounding the Seyfert galaxy NGC 7603, where four galaxies with different redshifts - NGC 7603 (z=0.029), NGC 7603B (z=0.057) and two fainter emission line galaxies (z=0.245 and z=0.394) - are apparently connected by a narrow filament, leading to a possible case of anomalous redshift. The observations com…
Keck Spectroscopy of Two Young Globular Clusters in the Merger Remnant NGC 3921
Brodie, Jean P.; Seitzer, Patrick; Schweizer, François
Low-resolution, ultraviolet-to-visual spectra of two candidate globular clusters in the merger remnant NGC 3921 (czLG=6021 km s-1) are presented. These two clusters of apparent magnitude V~22.2 (MV~-12.5) lie at projected distances of about 5 kpc (0.9 Reff) from the center and move with halo-type radial …