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Astron. Astrophys. 323, L17-L20 (1997)

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4. Future possibilities

The successful detection of 8 out of 9 active galactic nuclei in 1.4 mm VLBI observations between Pico Veleta and Plateau de Bure, and the fact that the sources probably show complex intrinsic source structures on micro-arcsecond scales, stimulate further and more extensive 1 mm VLBI observations. In order to increase the sensitivity, it is highly desirable to use the existing millimeter interferometers as phased arrays (eg. Plateau de Bure, BIMA, OVRO, Nobeyema) and to combine them with existing other mm-/sub-mm telescopes (eg. Pico Veleta, Kitt Peak, Sest). For the present station characteristics (as taken from the literature) and VLBI-observations with 112 MHz bandwidth and an array detection threshold of 3 [FORMULA] (adopting global fringe fitting, eg. Alef & Porcas 1986), we formally derive detection limits between Pico Veleta and other phased arrays of [FORMULA] mJy. This allows the investigation of some 50 Active Galactic Nuclei and compact galactic objects. For the near future 1 mm VLBI experiments also with longer baselines should be envisaged. 215 GHz VLBI interferometry on a 8000 km baseline (eg. Pico-BIMA or BURE-OVRO) would yield an angular resolution of [FORMULA] as, corresponding to a spatial resolution of 54 lightdays for a source at redshift [FORMULA] ([FORMULA] km s-1 Mpc-1, [FORMULA]). This corresponds to [FORMULA] Schwarzschild radii of a black hole of [FORMULA] solar masses.

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© European Southern Observatory (ESO) 1997

Online publication: June 5, 1998

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