Observations of Diffuse EUV Emission with the Cosmic Hot Interstellar Plasma Spectrometer (CHIPS)

Details Observations of Diffuse EUV Emission with the Cosmic Hot Interstellar Plasma Spectrometer (CHIPS) Observations of Diffuse EUV Emission with the Cosmic Hot Interstellar Plasma Spectrometer (CHIPS)

2004-11-04

arxiv.org/abs/astro-ph/0411121v1

Astrophys.J. 623 (2005) 911-916

Astronomy and Astrophysics

Astrophysics

13 pages, 4 figures, 1 table

Scientific paper

10.1086/428446

The Cosmic Hot Interstellar Plasma Spectrometer (CHIPS) was designed to study diffuse emission from hot gas in the local interstellar cavity in the wavelength range 90 - 265 A. Between launch in January 2003 and early 2004, the instrument was operated in narrow-slit mode, achieving a peak spectral resolution of about 1.4 A FWHM. Observations were carried out preferentially at high galactic latitudes; weighted by observing time, the mean absolute value of the galactic latitude for all narrow-slit observations combined is about 45 degrees. The total integration time is about 13.2 Msec (74% day, 26% night). In the context of a standard collisional ionization equilibrium plasma model, the CHIPS data set tight constraints on the emission measure at temperatures between 10^{5.55} K and 10^{6.4} K. At 10^{6.0} K, the 95% upper limit on the emission measure is about 0.0004 cm^{-6} pc for solar abundance plasma with foreground neutral hydrogen column of 2 x 10^{18} cm^{-2}. This constraint, derived primarily from limits on the extreme ultraviolet emission lines of highly ionized iron, is well below the range for the local hot bubble estimated previously from soft X-ray studies. To support the emission measures inferred previously from X-ray data would require depletions much higher than the moderate values reported previously for hot gas.

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