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Tohoku-Hiroshima-Nagoya planetary spectra library: a method for characterizing planets in the visible to near infrared
Context: A comprehensive framework for comparing spectral data fromdifferent planets has yet to be established. This framework is neededfor the study of extrasolar planets and objects within the solarsystem. Aims: We completed observations to compile a libraryof planet spectra for all planets, some moons, and some dwarf planets inthe solar system to study their general spectroscopic and photometricnatures. Methods: During May and November of 2008, weacquired spectra for the planets using TRISPEC, which is capable ofsimultaneous three-band spectroscopy across a wide wavelength range of0.45-2.5 ?m with low resolving power (?/?? ~140-360). Results: Patterns emerge when comparing thespectra. By analyzing their general spectroscopic and photometricnatures, we show that it is possible to distinguish between gas planets,soil planets, and ice planets. These methods can be applied toextrasolar observations acquired using low resolution spectrography orbroad-band filters. Conclusions: The present planet spectrallibrary is the first library to contain observational spectra for all ofthe solar system planets, based on simultaneous observations at visibleand near infrared wavelengths. This library will be a useful referencefor analyzing extrasolar planet spectra and calibrating planetary datasets.THN Planet spectra library is only available in electronic form at theCDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/507/1649
| The Spacelab-1 Very Wide Field Survey of UV-excess objects. IV. The performance of the instrument in combination with optical photometry as a means of identifying stars with peculiar properties.
UV (195 nm) and Stroemgren uvby photometry of a 110 square degree fieldat high southern galactic latitudes are analyzed through a comparison ofi) UV magnitudes for 57 stars of various types common to the publishedTD1 catalogue and the Very Wide Field Camera (VWFC); and ii) observedand theoretical two-colour diagrams. The higher sensitivity of the VWFC(=~0.5magnitude) and its more complete survey are exemplified by thedetection and UV measurement of a series of objects with moderateUV-excess in addition to detection of some very blue objects of variousnature down to fainter than 12th magnitude in the optical domain. Adeeper survey with a VWFC-type instrument could provide a completesample for studies of the group properties of faint blue stars. Duringthe uvby reductions it was found that the usual procedure of plottingresiduals as functions of declination, hour angle and airmass can be apowerful and diagnostic test of photometer rigidity.
| Observations of occultations of stars by the moon
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1974A&AS...13..395H&db_key=AST
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Gözlemler ve gökölçümü verileri
| Takýmyýldýz: | Oglak |
| Sað Açýklýk: | 21h27m23.23s |
| Yükselim: | -13°35'15.3" |
| Görünürdeki Parlaklýk: | 7.09 |
| Uzaklýk: | 458.716 parsek |
| özdevim Sað Açýklýk: | 14.3 |
| özdevim Yükselim: | 2.6 |
| B-T magnitude: | 7 |
| V-T magnitude: | 7.083 |
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