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The Heavy Element Enrichment of Lyman alpha Clouds in the Virgo Supercluster | | T.M. Tripp
; E.B. Jenkins
; G.M. Williger
; S.R. Heap
; C.W. Bowers
; A.C. Danks
; R. Dave’
; R.F. Green
; T.R. Gull
; C.L. Joseph
; M.E. Kaiser
; D. Lindler
; R.J. Weymann
; B.E. Woodgate
; | | Date: |
11 Apr 2002 | | Journal: | Astrophys.J. 575 (2002) 697-711 | | Subject: | astro-ph | | Affiliation: | 2,3,4), S.R. Heap , C.W. Bowers , A.C. Danks , R. Dave’ , R.F. Green , T.R. Gull , C.L. Joseph , M.E. Kaiser , D. Lindler , R.J. Weymann , and B.E. Woodgate ( Princeton, NASA-Goddard, NOAO, JHU, Arizona, Rutgers, Carnegie Obs. | | Abstract: | Using high S/N STIS echelle spectra (FWHM=7 km/s) of 3C 273, we constrain the metallicities of two Lya clouds in the vicinity of the Virgo cluster. We detect C II, Si II, and Si III absorption lines in the Lya absorber at z = 0.00530. Previous observations with FUSE have revealed Ly beta - Ly theta lines at this redshift, thereby accurately constraining N(H I). We model the ionization of the gas and derive [C/H] = -1.2^{+0.3}_{-0.2}, [Si/C] = 0.2+/-0.1, and log n_{H} = -2.8+/-0.3. The model implies a small absorber thickness, ~70 pc, and thermal pressure p/k ~ 40 cm^{-3} K. It is most likely that the absorber is pressure confined by an external medium because gravitational confinement would require a very high ratio of dark matter to baryonic matter. Based on Milky Way sight lines in which carbon and silicon abundances have been reliably measured in the same interstellar cloud (including new measurements presented herein), we argue that the overabundance of Si relative to C is not due to dust depletion. Instead, this probably indicates that the gas has been predominately enriched by Type II supernovae. Such enrichment is most plausibly provided by an unbound galactic wind, given the absence of galaxies within a projected distance of 100 kpc and the presence of galaxies capable of driving a wind at larger distances. We also constrain the metallicity and physical conditions of the Virgo absorber at z = 0.00337 based on detections of O VI and H I and an upper limit on C IV. If this absorber is collisionally ionized, the O VI/C IV limit requires T > 10^{5.3} K. For either collisional ionization or photoionization, we find that [O/H] > -2.0 at z = 0.00337. | | Source: | arXiv, astro-ph/0204204 | | Services: | Forum | Review | PDF | Favorites | |
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