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28 July 2008 Extragalactic reference targets for PRIMA
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The VLTI's PRIMA (Phase-Referenced Imaging and Microarcsecond Astrometry) instrument is designed to provide tens of microarcseond astrometry and faint-object imaging for the interferometer facility. Astrometry is to be enabled by PRIMA between object pairs that are separated on the sky by one isoplanatic patch (roughly 60 seconds of arc at Cerro Paranal in the K band), with at least one of the two objects being bright (K <10), and a second fainter object (ΔK < 7) that is nominally a 'stable' astrometric reference. The original expectation was for star-star pairs to be observed by PRIMA in its astrometric mode; however, we are exploring the possibility of also utilizing background galaxies in this role. Advantages of such source selection is eliminating the need to solve for dim object parallax and proper motion before obtaining similar values for the bright foreground star. Additionally, data from the galaxy may be of scientific interest as well, potentially leading to characterizations of object morphology at milliarcsecond scales. Towards that end, we have begun observations with ESO's NTT to explore the suitability of qualifying star-galaxy asterisms as potential PRIMA targets. Commissioning observations for PRIMA are slated to begin in Fall of 2008.
© (2008) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Gerard T. van Belle, Roberto Abuter, Judith Ngoumou, Francoise Delplancke, and Johannes Sahlmann "Extragalactic reference targets for PRIMA", Proc. SPIE 7013, Optical and Infrared Interferometry, 70133W (28 July 2008); doi: 10.1117/12.789257;


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