1994/07/20 by E. L. Wright, Wright, E. L., P. Eisenhardt +4
Engineering · Physics and Astronomy · #Adaptive optics and wavefront sensing #Astronomical Observations and Instrumentation #Astrophysics (astro-ph) #CCD and CMOS Imaging Sensors #FOS: Physical sciences #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9407055
poster paper presented at the June 1994 AAS meeting, 3 pages LaTex using aaspp.sty with appended color Postscript, GIF and JPEG figures, (330 kbytes) UCLA-ASTRO-ELW-94-03
openalex publication_date 1994/07/20 · arxiv created 1994/07/21 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Starlight from distant galaxies (z > 3) is redshifted into the near infrared band with observed wavelengths from 2-8 μm. Most of the light is emitted by stars that have a peak emission at the 1.6 μm wavelength of the minimum of the H- opacity. We present simulated images of galaxy and star fields at 3, 4.7 and 8 μm, using the expected performance of the infrared camera on the Space InfraRed Telescope Facility (SIRTF). Standard astronomical image processing tools are used to locate sources, distinguish stars from galaxies, and create color-magnitude and color-color diagrams for the galaxies.