OVI Gas as an Indicator of the Diffuse Web of Baryons

Details OVI Gas as an Indicator of the Diffuse Web of Baryons OVI Gas as an Indicator of the Diffuse Web of Baryons

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9158m&link_type=abstract

HST Proposal ID #9158

Physics

Hst Proposal Id #9158 Quasar Absorption Lines And Igm

Scientific paper

Most of the baryons in the local universe are expected to be in a hot phase {10^5-10^7 K}, yet direct detection of this material is challenging. The most suitable way of detecting this gas in the UV is through the high-ionization OVI doublet at 1035 Angstrom, which traces collisionally ionized gas at 3x10^5 K. However, OVI can also be produced through photoionization in cooler gas {< 5x10^4 K}, which is not part of the web of hot baryons. Tripp & Savage {2000} suggest that they have finally detected the hot baryonic gas in an OVI absorption system without measurable NV, although this combination occurs often in photoionized systems. We propose to resolve this ambiguity by measuring the CIV line, which for the photoionized case occurs at about the same equivalent width as the OVI line.

Affiliated with

Also associated with

No associations

Rating

OVI Gas as an Indicator of the Diffuse Web of Baryons does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with OVI Gas as an Indicator of the Diffuse Web of Baryons, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and OVI Gas as an Indicator of the Diffuse Web of Baryons will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1200607