Search Swinburne Research Bank
Please use this identifier to cite or link to this item: http://hdl.handle.net/1959.3/42762
 Download PDF (Accepted manuscript) (Adobe Acrobat PDF, -1 bytes) |
- Title
- The clustering of luminous red galaxies around MgII absorbers
- Author(s)
- Bouche, Nicolas; Murphy, Michael T.; Peroux, Celine
- Abstract
- We study the cross-correlation between 212 Mg ii quasar absorption systems and ∼20 000 luminous red galaxies (LRGs) selected from the Sloan Digital Sky Survey Data Release 1 in the redshift range 0.4 ≤z≤ 0.8 . The Mg ii systems were selected to have λλ 2796 and 2803 rest-frame equivalent widths ≥1.0 Å and identifications confirmed by the Fe iiλ2600 or Mg iλ2852 lines. Over comoving scales 0.05–13 h−1 Mpc , the Mg ii–LRG cross-correlation has an amplitude 0.67 ± 0.09 times that of the LRG–LRG auto-correlation. Since LRGs have halo masses greater than 3.5 × 1012 M⊙ for MR≲−21 , this relative amplitude implies that the absorber host galaxies have halo masses greater than ∼2–8 × 1011 M⊙ . For 1013-M⊙ LRGs, the absorber host galaxies have halo masses ∼0.5–2.5 × 1012 M⊙ . Our results appear consistent with those of Steidel, Dickinson & Persson (1994) who found that Mg ii absorbers with WMg IIr≥ 0.3 Å are associated with ∼ 0.7L*B galaxies.
- Publication type
- Journal article
- Source
- Monthly Notices of the Royal Astronomical Society, Vol. 354, no. 2 (Oct 2004), pp. L25-L29
- Publication year
- 2004
- Keyword(s)
- Absorption systems; Cosmology; Digital sky survey; Evolution; Galaxies; Haloes; High-redshift; Observations; Photometric redshifts; Quasar absorption lines; Spectroscopic target selection; Stellar mass density
- Publisher
- Wiley-Blackwell Publishing
- ISSN
- 0035-8711
- Publisher URL
- http://dx.doi.org/10.1111/j.1365-2966.2004.08348.x
- Copyright
- Copyright © 2004 the authors. Journal compilation copyright © 2004 Royal Astronomical Society. The accepted manuscript of the paper is reproduced here in accordance with the copyright policy of the publisher. The definitive publication is available at www.interscience.wiley.com.
- Full text
- Peer reviewed
