Publications of the Astronomical Society of the Pacific
Description:Publications of the Astronomical Society of the Pacific, the technical journal of the Astronomical Society of the Pacific (ASP), has been published regularly since 1889, as part of the ASP’s mission to advance the science of astronomy and disseminate astronomical information. The journal provides an outlet for astronomical results of a scientific nature and serves to keep readers in touch with current astronomical research. It contains refereed research and
instrumentation papers, invited reviews, and dissertation summaries.
The "moving wall" represents the time period between the last issue
available in JSTOR and the most recently published issue of a journal.
Moving walls are generally represented in years. In rare instances, a
publisher has elected to have a "zero" moving wall, so their current
issues are available in JSTOR shortly after publication.
Note: In calculating the moving wall, the current year is not counted.
For example, if the current year is 2008 and a journal has a 5 year
moving wall, articles from the year 2002 are available.
Terms Related to the Moving Wall
Fixed walls: Journals with no new volumes being added to the archive.
Absorbed: Journals that are combined with another title.
Complete: Journals that are no longer published or that have been
combined with another title.
Science & Mathematics,
Arts & Sciences X Collection,
Corporate & For-Profit Access Initiative Collection
ABSTRACT Using what is known about the physical and chemical structure of the CCD detector on the Space Telescope Imaging Spectrograph (STIS) and over 50 calibration images taken with different wavelength mappings onto the detector, we have devised a model function that allows us to predict the fringing of any spectral image taken with the STIS CCD. This function is especially useful for spectra taken without a slit with the G750L grating. The STIS parallel observing program uses this “slitless spectroscopy” mode extensively. The arbitrary mapping of wavelength versus position that results from each source's chance position in the field renders direct calibration of the fringe amplitudes in this mode impossible. However, we find that correcting observed data using our semiempirical fringing model produces a substantial reduction in the fringe amplitudes. Tests using the flux calibration white dwarf standard G191‐B2B show that we can reduce the fringe amplitude in the 9000–10000 Å region from about 20% peak to peak (10% rms) to about 4% peak to peak (2% rms) using the model, while a standard calibration using a “fringe flat” reduces the fringe amplitudes to 3.3% peak to peak (1.7% rms). The same technique is applicable to other astronomical CCDs.
Notes and References
This item contains 9 references.
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['Pickles, A. J. 1998, PASP, 110, 863']
['Silva, D. R., & Cornell, M. E. 1992, ApJS, 81, 865']