Computer Science
Scientific paper
Feb 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990phdt........20m&link_type=abstract
Ph.D. Thesis California Univ., Berkeley.
Computer Science
1
High Resolution, Milky Way Galaxy, Molecular Spectra, Spatial Resolution, Spectral Resolution, Stellar Envelopes, Very Long Base Interferometry, Emission Spectra, Hydrocyanic Acid, Ionized Gases, Line Spectra
Scientific paper
Radio studies of the parsec-scale structure in the centers of NGC 1275 and the Milky Way galaxy are presented. The nucleus of NGC 1275 was observed with Very Long Baseline Interferometry (VLBI) at 1.3 cm twice per year for three years, with a resolution of 0.3 milliarcseconds, corresponding to approximately 0.1 pc. The galactic center was observed in the J = 1 approaches 0 transition lines of H-13(CN) and HCO(+) with the Berkeley-Illinois-Maryland Array (BIMA) at the Hat Creek Radio Observatory, with a spatial resolution that corresponded to 0.2 pc, and spectral resolution of 4 km s-1. The H-13(CN) and HCO(+) data, which were seen in emission from the 2 pc galactocentric ring and in absorption from galactic line-of-sight features, were compared with published H-12(CN) observations. The VLBI maps of NGC 1275 reveal that intensity flares are associated with the ejection of knots of emission moving at velocities approximately 0.5 h-1 c, while a slowly evolving outburst is associated with the emergence of diffuse emission expanding in a cone at a velocity approximately 0.33 h-1 pc. The core emission has a roughly constant and complex morphology with a number of ridges extending out radially from the emission peak and an inner jet at PA 210 deg. The galactic center observations are also used to study previously identified foreground features that appear in absorption by HCO(+) and HCN. Opacity maps suggest either that Sgr A* is at least 3 pc in front of the ionized gas bar or that 'the high velocity gas' is very clumpy and has a window at the position of Sgr A*.
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