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Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003assl..281..283g&link_type=abstract
The IGM/Galaxy Connection: The Distribution of Baryons at z=0, ASSL Conference Proceedings Vol. 281. Edited by Jessica L. Rosenb
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1
Scientific paper
3C 273 and RX J1230.8+0115 are fortuitously separated by only 54' on the sky. Their sight lines pass through the Virgo Southern Extension, allowing a direct comparison of the absorption lines produced by gas (separated by 300 kpc) in the Virgo Cluster. Tripp et al. (2002) have recently presented a high S/N HST/STIS spectrum of 3C 273. Based on the detection of neutral (HI) and low ionization absorption (CII, SiII, & SiIII) species at z = 0.00530, they constrain the physical conditions of the absorber to: [C/H] = -1.2+0.3-0.2, [Si/C] = 0.2 +/- 0.1, log nH = -2.8 +/- 0.3, and an absorber thickness ~70 pc. In these proceedings, we present spectra from a 27.2 ks HST/STIS-E140M exposure and a 4 ks FUSE snapshot of absorption features at z = 0.00577 toward RX J1230. From an inspection of Figure 1, marked differences in these two sight lines, are readily apparent. (1) Absorption over a wide range of ionization stages is detected toward RX J1230, and all ions show stronger absorption. This implies that the RX J1230 sight line intercepts more gas than the 3C 273 sight line. (2) The absorption along the two sight lines is offset by a mere 140 km/s. This may indicate a common sheet-like structure intercepting both sight lines. (3) Overlays of the absorption profiles toward the two sight lines reveal that an additional structure may exist at v < -50 km/s. This component is prevalent in the RX J1230 sight line. In the 3C 273 sight line, there is a hint of it in HI, but it is not apparent in any other species.
Charlton Jane C.
Ganguly Rajib
Sembach Kenneth Russell
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