{
  "id": "astro-ph/0407237",
  "version": "v1",
  "published": "2004-07-12T16:12:36.000Z",
  "updated": "2004-07-12T16:12:36.000Z",
  "title": "The Number Density of 0.6 < z < 1.7 MgII Systems from CORALS: Observational Biases at Intermediate Redshift",
  "authors": [
    "Sara L. Ellison",
    "Chris W. Churchill",
    "Samantha A. Rix",
    "Max Pettini"
  ],
  "comment": "Accepted for publication in the ApJ",
  "journal": "Astrophys.J. 615 (2004) 118-129",
  "doi": "10.1086/424375",
  "categories": [
    "astro-ph"
  ],
  "abstract": "The goal of the Complete Optical and Radio Absorption Line System (CORALS) survey is to quantify the potential impact on QSO absorber statistics from dust in intervening galaxies. Dust may introduce a selection bias in surveys which are based on magnitude limited QSO samples, leading to an underestimate of absorber number density, n(z). Here we present the results of the second phase of the CORALS survey which extends our previous work on z > 1.8 damped Lyman alpha systems (DLAs) to search for strong metal line systems (candidate DLAs) in the range 0.6 < z < 1.7. We have identified 47 MgII systems with rest frame equivalent widths EW(MgII lambda 2796) > 0.3 A in our sample of 75 radio-selected quasars. Our principal and most robust result is that the n(z) of low redshift MgII systems determined for the CORALS survey is in excellent agreement with that of optically-selected, magnitude limited QSO samples. The statistically inferred number density of DLAs, n(z)=0.16^+0.08_-0.06, is consistent with other low redshift samples, although the large 1 sigma error bars permit up to a factor of 2.5 more DLAs in CORALS. However, confirmation of the DLA candidates, precise evaluation of their n(z) and measurement of their HI column densities awaits UV observations with the Hubble Space Telescope. Finally, we report an excess of intermediate redshift MgII systems observed towards bright QSOs which could be due to a lensing amplification bias. However, there is also evidence that this excess could simply be due to more sensitive EW detection limits towards brighter QSOs. We also emphasize that absorber statistics determined from magnitude limited surveys reach a steady value if the completeness limit is significantly fainter than the fiducial value of the quasar luminosity function. (Abridged).",
  "revisions": [
    {
      "version": "v1",
      "updated": "2004-07-12T16:12:36.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "number density",
      "intermediate redshift",
      "densities awaits uv observations",
      "observational biases",
      "column densities awaits uv"
    ],
    "tags": [
      "journal article"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 654161
    }
  }
}