TY - JOUR
T1 - Ultraviolet sky surveys
T2 - Instruments, findings, and prospects
AU - Brosch, Noah
N1 - Funding Information:
The TAUVEX (Tel Aviv University UV Explorer) payload (Brosch et al., 1994) represents the most advanced attempt to design, build and operate a flexible instrument for observations in the entire UV band. The experiment is built for Tel Aviv University by El-Op, Electro-Optical Industries, Ltd., with the largest part of the funding from the Government of Israel through the Ministry of Science and Arts and the Israel Space Agency. TAUVEX images the same 0◦.9 FOV with three co-aligned telescopes and with an image quality of about 10′′. It was originally conceived for a small satellite of the OFEQ or SMEX class, but is now part of the scientific complement of the SRG spacecraft scheduled to launch in late-1999 or in 2000.
Funding Information:
UV research at Tel Aviv University is supported by special grants from the Government of Israel, the Ministry of Science and Arts, through the Israel Space Agency, and from the Austrian Friends of Tel Aviv University, as well as by a Center of Excellence Award from the Israel Science Foundation. I acknowledge support from a US-Israel Binational Award to study UV sources imaged by the FAUST experiment, and the hospitality of NORDITA, the Danish Space Research Institute, and the Space Telescope Science Institute, where parts of this review were prepared. I am grateful for the help of many individuals in producing this review. Benny Bilenko calculated sky models, Liliana Formiggini recalculated the optical-to-UV transformation and compared the predicted and actual UV brightness for Virgo, Hrant Tovmassian explained intricacies of the GLAZAR series, and Jeff Bloch from the ALEXIS team supplied sky charts and information. Bruno Milliard from LAS Marseille clarified a number of points related to FOCA observations and allowed me to look at a FOCA UV image and optical spectra of a few galaxies in it, Michael Lampton from the Berkeley’s SSL/CEA explained intricacies of the EUVE source count, Jesse Hill from the UIT team explained UIT results, David Bersier from the Observatoire de Génève added information on M51 and supplied its calibrated FOCA UV image, Jayant Murthy added information about UVISI, Luciana Bianch provided GALEX details in advance of publication, and David Israel from GSFC explained the TDRSS-balloon connection; for these I am very grateful. Mark Hurwitz supplied information and a list of publications from the ORFEUS flights; Bill Waller did the same for UIT, read an early version of the paper, and provided some useful remarks. I thank Alan Dressler for some information on his committee’s report, Marie Treyer for calculating the contribution to the UV background from FOCA galaxies, and Prab Gondhalekar for constructive remarks upon reading one of the final drafts. Boris Shustov kindly supplied details about the Spectrum-UV mission. I am grateful to the referee for very constructive remarks.
PY - 1999
Y1 - 1999
N2 - I review the development of UV and EUV astronomy, covering the spectral range from 5 to 300 nm, with emphasis on sky surveys for discrete sources. I discuss studies which resulted in lists of sources observed by imaging and deliberately omit most spectroscopic studies. Technical issues, such as detector and telescope developments, are treated separately from descriptions of specific missions and their results, which contributed to the understanding of the UV sky. The missions are compared in terms of their 'survey power', a variable which combines sky coverage and survey depth. I use the existing knowledge of UV sources to predict views of the UV sky, which I then compare with those actually detected. Finally, UV missions which will detect fainter sources and will fly in the near future are described, and a wish list for low-cost ventures, which could considerably advance our knowledge of the UV sky, is presented.
AB - I review the development of UV and EUV astronomy, covering the spectral range from 5 to 300 nm, with emphasis on sky surveys for discrete sources. I discuss studies which resulted in lists of sources observed by imaging and deliberately omit most spectroscopic studies. Technical issues, such as detector and telescope developments, are treated separately from descriptions of specific missions and their results, which contributed to the understanding of the UV sky. The missions are compared in terms of their 'survey power', a variable which combines sky coverage and survey depth. I use the existing knowledge of UV sources to predict views of the UV sky, which I then compare with those actually detected. Finally, UV missions which will detect fainter sources and will fly in the near future are described, and a wish list for low-cost ventures, which could considerably advance our knowledge of the UV sky, is presented.
KW - Instrumentation
KW - Sky surveys
KW - Ultraviolet
UR - http://www.scopus.com/inward/record.url?scp=0042639093&partnerID=8YFLogxK
U2 - 10.1023/A:1008134215736
DO - 10.1023/A:1008134215736
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AN - SCOPUS:0042639093
SN - 0922-6435
VL - 9
SP - 119
EP - 187
JO - Experimental Astronomy
JF - Experimental Astronomy
IS - 3
ER -