STIS UV Atlas of the Red Giant Arcturus(1)

Details STIS UV Atlas of the Red Giant Arcturus(1) STIS UV Atlas of the Red Giant Arcturus(1)

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...194.6701a&link_type=abstract

American Astronomical Society, 194th AAS Meeting, #67.01; Bulletin of the American Astronomical Society, Vol. 31, p.930

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The Space Telescope Imaging Spectrograph (STIS) conducted a series of observations of the archetype ``noncoronal'' red giant Arcturus (HD 124897; alpha Boo; K1 III) on 24 August 1998, 17--23 UT. The STIS program was the result of a failed cycle 5 pointing, which could not be rescheduled during the abbreviated cycle 6, and was carried over to cycle 7. Three grating settings---E230H (t_exp= 1340 s), E230M (2493 s), and E140M (5208 s)---covered the ultraviolet spectrum from 1150--2850 Angstroms, at resolutions between R ~ 4*E(4) - 1*E(5) , with essentially no gaps. The resulting spectrograms are stunning. The resolution is very high, as is the S/N; the spectral coverage is broad and comprehensive. The far-UV interval (1150--1700 Angstroms) is a rich emission line spectrum, dominated by the broad resonance transitions of atomic hydrogen (lambda 1215) and oxygen (lambda 1305 triplet). There are numerous narrow emissions, mostly from low-excitation species such as Si I, Fe II, and fluoresced bands of carbon monoxide. Surprisingly, high-excitation species---Si IV (lambda 1393: 6*E(4) K) and C IV (lambda 1548: 1*E(5) K)---are present as well (as seen in the earlier ``failed'' GHRS spectra). The mid-UV (1700--2600 Angstroms) shows additional emission lines, particularly [C II] and [Si II] in the 2325 Angstroms region; the photospheric continuum rises strongly toward the longer wavelengths. The 2600--2850 Angstroms interval is mostly a photospheric absorption spectrum, although the bright chromospheric emission doublet of Mg II lords over the 2800 Angstroms region. We present a comprehensive spectral atlas based on our reductions of the STIS echellograms. We discuss the processing strategies, line identifications, and some of the preliminary results from our analysis of this windy, noncoronal giant. (1) This work was supported by grants GO-06066.01-94A from STScI, and NAG5-3226 from NASA. Observations were from the NASA/ESA HST, collected at the STScI, operated by AURA, under contract NAS5-26555.

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