Abstract
ABSTRACT The profiles of stellar images near the zenith are measured on 57 random nights between 1975 and 1979, by employing a sequence of Coude slit widths and an exposure meter that measures the profiles in one dimension to an average internal standard error of plus or minus 0.06 arcsec. The advantages and disadvantages of this method are discussed, together with questions of seasonal variations in seeing for Kitt Peak. The results are examined, and it is determined that directional (seeing) differences occur due to local topography or to the wind direction.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callMore From: Publications of the Astronomical Society of the Pacific
Disclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
