An Investigation of the Performance of CCD Stellar Photometry with a 1.5-mu M Diffraction-Limited 8-m Next Generation Space Telescope

Details An Investigation of the Performance of CCD Stellar Photometry with a 1.5-mu M Diffraction-Limited 8-m Next Generation Space Telescope An Investigation of the Performance of CCD Stellar Photometry with a 1.5-mu M Diffraction-Limited 8-m Next Generation Space Telescope

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...193.3507m&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #35.07; Bulletin of the American Astronomical Society, Vol. 30, p.1296

Computer Science

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Scientific paper

I present the results of an investigation of the performance of CCD stellar photometry with a 1.5-mu m diffraction-limited 8-m Next Generation Space Telescope. These simulations used artificial Point Spread Functions for three different 8-m NGST design concepts which were kindly provided by John Krist. Assuming that the 8-m NGST primary mirror has 1/13 wave RMS errors at 1.5 mu m, I demonstrate that 90% of the light from a star falls within an aperture radius of 0.1 arcsec --- the size of one WF pixel of the {Hubble Space Telescope} WFPC2 instrument. The three NGST design concepts have nearly identical V-band encircled-energy functions; the degradation caused by the differences between the different design concepts is quite negligible when state-of-the-art digital-PSF photometric reduction software is used to analyze uncrowded stellar fields. All the V-band PSFs used in these simulations were sampled at 0.0064 arcsec pixel(-1) which is the critical V-band sampling rate of a perfect 0.5-mu m diffraction-limited 8-m NGST. Better photometric performance for all three NGST design concepts could be obtained by using larger CCD pixels: a pixel size of ~ 0.013 (~ 2x0.0064) arcsec pixel(-1) should provide an optimal pixel sampling when the 8-m primary mirror is diffraction-limited at 1.5 mu m.

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