Observations of OviEmission from the Diffuse Interstellar Medium | Zendy

R. L. Shelton | Zendy; J. W. Kruk | Zendy; E. M. Murphy | Zendy; B. G. Andersson | Zendy; William P. Blair | Zendy; W. V. Dixon | Zendy; Jerry Edelstein | Zendy; A. W. Fullerton | Zendy; C. Gry | Zendy; J. Christopher Howk | Zendy; E. B. Jenkins | Zendy; Jeffrey L. Linsky | Zendy; H. W. Moos | Zendy; W. R. Oegerle | Zendy; M. S. Oey | Zendy; Katherine C. Roth | Zendy; David J. Sahnow | Zendy; Ravi Sankrit | Zendy; Blair D. Savage | Zendy; Kenneth R. Sembach | Zendy; J. Michael Shull | Zendy; Oswald H. W. Siegmund | Zendy; A. VidalMadjar | Zendy; Barry Y. Welsh | Zendy; Donald G. York | Zendy

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Observations of OviEmission from the Diffuse Interstellar Medium

Author(s) -

R. L. Shelton,

J. W. Kruk,

E. M. Murphy,

B. G. Andersson,

William P. Blair,

W. V. Dixon,

Jerry Edelstein,

A. W. Fullerton,

C. Gry,

J. Christopher Howk,

E. B. Jenkins,

Jeffrey L. Linsky,

H. W. Moos,

W. R. Oegerle,

M. S. Oey,

Katherine C. Roth,

David J. Sahnow,

Ravi Sankrit,

Blair D. Savage,

Kenneth R. Sembach,

J. Michael Shull,

Oswald H. W. Siegmund,

A. VidalMadjar,

Barry Y. Welsh,

Donald G. York

Publication year - 2001

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/322478

Subject(s) - physics , interstellar medium , astrophysics , supernova , intensity (physics) , halo , line (geometry) , photon , sky , ultraviolet , atomic physics , galaxy , optics , geometry , mathematics

We report the first Far Ultraviolet Spectroscopic Explorer (FUSE)measurements of diffuse O VI (lambda,lambda 1032,1038) emission from thegeneral diffuse interstellar medium outside of supernova remnants orsuperbubbles. We observed a 30arcsec x 30arcsec region of the sky centered at l= 315 and b = -41. From the observed intensities(2930+/-290(random)+/-410(systematic) and 1790+/-260(random)+/-250(systematic)photons/cm/cm/s/sr in the 1032 and 1038 Angstrom emission lines, respectively),derived equations, and assumptions about the source location, we calculate theintrinsic intensity, electron density, thermal pressure, and emitting depth.The intensities are too large for the emission to originate solely in the LocalBubble. Thus, we conclude that the Galactic thick disk and lower halo alsocontribute. High velocity clouds are ruled out because there are none near thepointing direction. The calculated emitting depth is small, indicating that theO VI-bearing gas fills a small volume. The observations can also be used toestimate the cooling rate of the hot interstellar medium and constrain models.The data also yield the first intensity measurement of the C II 3s2 S1/2 to 2p2P3/2 emission line at 1037 Angstroms and place upper limits on the intensitiesof ultraviolet line emission from C I, C III, Si II, S III, S IV, S VI, and FeIII.Comment: 30 pages including 5 figures and 5 tables; submitted to ApJ, October 2000; accepted by ApJ, May 200

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