The Nuclei of Normal Galaxies: Lessons from the Galactic by Roland Diehl (auth.), R. Genzel, A. I. Harris (eds.)

By Roland Diehl (auth.), R. Genzel, A. I. Harris (eds.)

Our Galactic center's proximity permits astronomers to check actual professional­ cesses inside galactic nuclei at a degree of aspect that would by no means be attainable within the extra far away, yet frequently additionally extra fabulous, extragalactic structures. fresh advances in instrumentation from the radio, in the course of the submillime­ ter and infrared wavebands, and out to the X- and "'(-ray bands now let observations of the Galactic heart over 13 orders of importance in wave­ size. Our wisdom in regards to the primary few hundred parsecs of our Galaxy has for that reason elevated greatly during the last decade. a similar new instru­ ments offer excessive solution, prime quality measurements of within sight ''normal'' galactic nuclei; that's, nuclei whose modest strength output is analogous to that of our personal (and such a lot different) galaxies. Theorists, spurred partially through the hot observations, were capable of refine types of the energetics, dynam­ ics, and evolution of the gasoline and stellar structures deep inside galactic nuclei.

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Rieke et al. (1988) proposed a significantly shorter duration (10 6 - 10 7 yr) for this phase of the nuclear starburst in NGC 253 from other reasons making the nuclear superwind origin of the halo emission questionable. Further indications that the ongoing nuclear starburst is not supporting the extended X-ray halo emission in NGC 253 can be drawn from the ROSAT HRI and the VLA radio observations. f. Fig. 3) and does not connect to the hot halo gas (observed in the ROSAT PSPC). Similarly, the radio spur and prominence starting in the north-east part of the NGC 253 disk argue for an origin of the halo gas from areas outside the nucleus (Carilli et al.

In this case. 75·10 MeV) (Bloemen el 01 .. 1993) observe in other parts of the Galaxy; as a rough estimate. this demands - 108 Mo or - 1000 clouds of the 'p Oph' type. if no cosmic ray anomalies are assumed. There is some indication of variability of this source. which would j 0 -10 11 favour the compact source interpretation. Further observations are beeing performed to put statistically significant constraints on the GC source variability on the timescale of weeks to months. 150 - 5. Summary 300 MeV Recent observational data from spacebom telescopes have the potential to provide a substantially more detailed of the picture Galactic Centre region in the light 160 140 120 IOU eo GO 4u 20 a )40 320 JOO 280 260 240 220 200 Ie of gamma-rays.

No. 330, pp. , and Lesch, H. 1992: 'Anatomy of the Sagittarius A complex', Astron. B Astrophys. Vol. no. 261, pp. H. Townes (left), P. Mezger (middle), and M. Morris (right) R. Hildebrand (left) and J. Storey (right) in front of Schlo6 Ringberg THE 511 keY LINE AND THE GREAT ANNIHILATOR M. LEVENTIIAL Department of Astronomy University of Maryland College Park, Maryland 20742 ABSTRACT. The history of Galactic Center 511 keY electron/positron line observations is reviewed with an emphasis on current observations.

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