Scientific and Technical Aerospace Reports Volume 38 July 28, 2000

operation, and troubleshooting. Recent AIT exercise scenarios highlighted the need for training programs at all levels from aerial
port personnel to commanders. Furthermore, it does not appear that the application of AIT will reduce manning requirements.
Despite these disadvantages, AIT could improve ITV at remote locations. Given that past attempts to collect ITV data at remote
or austere locations have been manpower and time intensive, AIT could eliminate these problems in the future. Consequently,
AMC should plan to use AIT to improve ITV at remote locations.
DTIC
Visibility; Information Systems; Identifying
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ASTRONOMY
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20000062311 Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA USA
High-Resolution Optical and Near-Infrared Imaging of Young Circumstellar Disks
McCaughrean, Mark, Astrophysikalisches Inst., Germany; Stapelfeldt, Karl, Jet Propulsion Lab., California Inst. of Tech., USA;
Close, Laird, Hawaii Univ., USA; [2000]; 20p; In English; No Copyright; Avail: CASI; A03, Hardcopy; A01, Microfiche
In the past five years, observations at optical and near-infrared wavelengths obtained with the Hubble Space Telescope and
ground-based adaptive optics have provided the first well-resolved images of young circumstellar disks which may form planetary
systems. We review these two observational techniques and highlight their results by presenting prototype examples of disks
imaged in the Taurus-Auriga and Orion star-forming regions. As appropriate, we discuss the disk parameters that may be typically
derived from the observations, as well as the implications that the observations may have on our understanding of, for example,
the role of the ambient environment in shaping the disk evolution. We end with a brief summary of the prospects for future
improvements in space- and ground-based optical/IR imaging techniques, and how they may impact disk studies.
Author
Adaptive Optics; Imaging Techniques; Image Resolution; Stellar Envelopes
20000062359 National Optical Astronomy Observatories, Tucson, AZ USA
A Spectroscopic Study of Field BHB Star Candidates
Kinman, T., Kitt Peak National Observatory, USA; Castelli, F., Osservatorio Astronomico, Italy; Cacciari, C., Osservatorio
Astronomico, Italy; Bragaglia, A., Osservatorio Astronomico, Italy; Harmer, D., Kitt Peak National Observatory, USA; Valdes,
F., Kitt Peak National Observatory, USA; June 2000; 48p; In English
Report No.(s): NOAO-Preprint-879; No Copyright; Avail: CASI; A03, Hardcopy; A01, Microfiche
New spectroscopic observations are presented for a sample of thirty-one blue horizontal branch (BHB) star candidates that
are sufficiently nearby to have reliable proper motions. Comments are given on a further twenty-five stars that have previously
been suggested as BHB star candidates but which were not included in our sample. Moderately high-resolution spectra (lambda/
Delta(lambda) approx. = 15 000) of twenty five of our program stars were taken with the coude feed spectrograph at Kitt Peak.
Twelve of the program stars were also observed with the CAT spectrograph at ESO. Six of these program stars were observed from
both hemispheres. IUE low-resolution spectra are available for most of our candidates and were used, in addition to other methods,
in the determination of their T(sub ff) and reddening. A compilation of the visual photometry for these stars (including new photometry
obtained at Kitt Peak) is also given. Abundances were obtained from these spectra using models computed by Castelli
with an updated version of the ATLAS9 code.
Author
Spectroscopy; Research; Blue Stars; IUE; Spectra; Stellar Evolution
20000062461 National Optical Astronomy Observatories, Tucson, AZ USA
WFPC2 Stellar Photometry with HSTphot
Dolphin, Andrew E., National Optical Astronomy Observatories, USA; June 2000; 18p; In English
Contract(s)/Grant(s): GO-02227.06-A; GO-07696
Report No.(s): NOAO-Preprint-881; No Copyright; Avail: CASI; A03, Hardcopy; A01, Microfiche
HSTphot, a photometry package designed to handle the undersampled PSFs found in WFPC2 images, is introduced and
described, as well as some of the considerations that have to be made in order to obtain accurate PSF-fitting stellar photometry