Intergalactic O VI absorption at redshift <0.004

Details Intergalactic O VI absorption at redshift <0.004 Intergalactic O VI absorption at redshift <0.004

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9754w&link_type=abstract

HST Proposal ID #9754

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Hst Proposal Id #9754 Quasar Absorption Lines And Igm

Scientific paper

Simulations of the formation of large-scale structure in the universe predict that at the present time a large fraction of the baryons in the intergalactic medium {IGM} is in a warm/hot phase, with T=10^5-10^7 K. The warm phase has been detected with HST in absorption through the OVI 1031.926, 1037.671 doublet at redshifts 0.15-0.3. In a sample of 100 extra-galactic objects observed with FUSE, we find 12 detections of OVI at redshifts z=0.0008-0.004 {v=250 to 1200 km/s}. Many of these occur within 400 kpc and 50 km/s of a nearby galaxy, making it much easier to understand the relation between the OVI absorbers and galaxies. Our sample allows a comparison of the properties of nearby vs more distant OVI absorbers. However, modeling the physical conditions in the gas requires measurements of HI, OVI, CIV, NV and CIII. High velocity resolution is required to resolve the HI, CIV and NV lines in order to discriminate between collisional and photoionization. We propose to obtain improved HI data, as well as the CIV and NV measurements for two absorbers at z<0.004. One appears to represent collisional ionization {Mrk 876}, while the other probably represents a case of a photoionized system {Ton S180}. Understanding the ionization of the warm IGM is essential for determining elemental abundance and the baryonic content of the gas.

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