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The McMath Solar-Stellar Program (1Jun92) (from NSO, NOAO Newsletter No. 30, 1 June 1992) Some of you may not be familiar with the unique opportunities available to conduct both synoptic and visitor programs of high-resolution spectroscopy in the general area of solar-stellar physics at the NSO McMath telescope on Kitt Peak. The next deadline for proposals for programs beginning in the fourth quarter (October-December) is 15 July 1992. You may submit proposals via e-mail in care of: bartlome@noao.edu (INTERNET) or, NOAO::BARTLOME (SPAN). You may fax any figures to accompany the e-mail version of your proposal to 602-325-9278. TeX and Unix roff templates of the NSO observing proposal form are available for your convenience from the above e-mail addresses. The NSO operates a program of solar-stellar spectroscopy at the McMath telescope which is open to the entire astronomical community. We operate on a "six on-six off" schedule where our resident observer (Paul Avellar) obtains spectra for approved programs during six consecutive nights. The six nights immediately after a `synoptic run' are available for visitor programs. During `visitor time,' the PI is expected to travel to Kitt Peak to obtain his or her own observations. These programs are usually of a short-term nature, though a PI is welcome to use visitor time to extend a synoptic program. `Visitor time' is usually allocated in three- or six- night blocks. A PI may apply for both synoptic and visitor time during any quarter. Proposals, either synoptic or visitor, are approved for up to four consecutive quarters. Thereafter, the PI must reapply with a progress report if more time is desired. It is not necessary to apply for time each quarter once your program is approved. Besides proposals for visitor or synoptic time, PIs may apply for `targets of opportunity' pending, for example, the scheduling of approved spacecraft observing time. This allows the possibility of obtaining coordinated observations with current missions such as IUE, HST, and ROSAT. The quarterly scheduling generally permits the kind of flexibility that is needed to operate joint McMath/ spacecraft programs, and programs coordinated with other ground-based facilities. The instrument complement that comprises the solar-stellar spectrograph currently includes a TI 800 x 800 UV-enhanced CCD array along with both conventional (Milton and Roy) and echelle gratings. The echelle is not yet cross-dispersed; individual orders are isolated using interference filters. We plan to install a large-format array (1024 x 3072 SAIC/Ford Aerospace CCD) and a cross-dispersing element during the next year. The output of the spectrograph is imaged onto the CCD with a Nikon transfer lens. At Ha, resolutions in the range of R = 42,000 to R = 122,000 can be achieved. The broad range available across the visible spectrum is R = 22,000-122,000. The principal transfer lenses that are used include the 180 mm lens (for the highest resolution programs) and the 105 mm lens (for lower resolutions). We also have a Kinoptic (130 mm) lens available that yields superior throughput in the blue, which is especially useful for programs that emphasize the Ca II H and K lines. For those of you who are familiar with the KPNO Coude Feed, the McMath solar-stellar spectrograph has at least twice the throughput of the feed. As an example, a recent observation of a dK8 star (V = 9.66) at Ha with the 105 mm lens and Milton and Roy grating 1 in second order yielded S/N = 29 in the continuum in 25 minutes. We can work to a practical faint limit of about V = 12. This limit is mainly determined by the sensitivity of our present TV and guider system which will be upgraded during the next year. If you have any questions concerning the performance of the system or the McMath solar-stellar program, please contact the program scientist, Mark Giampapa: (giampapa@noao.edu or NOAO::giampapa) or our technical support staff member, Dave Jaksha (jaksha@noao.edu or NOAO::jaksha). Mark Giampapa
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