### Abstract

We present the results of a survey of the analogs of weak Mg II absorbers [rest-frame equivalent width W_{r}(2796) < 0.3 Å] at 0 < z < 0.3. Our sample consisted of 25 HST STIS echelle quasar spectra (R = 45,000), which covered Si II λ1260 and C II λ1335 over this redshift range. Using those similar transitions as tracers of Mg II facilitates a much larger survey, covering a redshift path length of g(z) = 5.3 for an equivalent width limit of Mg II corresponding to W_{r}(2796) > 0.02 Å, with 30% completeness for the weakest lines. Correcting for incompleteness, we find the number of weak Mg II absorber analogs with 0.02 Å < W_{r},(2796) < 0.3 Å to be dN/dz = 1.00 ±0.20 for 0 < z < 0.3. This compares to a value of dN/dz = 1.74 ± 0.10 found by Churchill et al. for the higher redshift range, 0.4 < z < 1.4, and is consistent with cosmological evolution of the population. We consider the expected effect on observability of weak Mg II absorbers of the decreasing intensity of the extragalactic background radiation field from z ∼ 1 to ∼0. Assuming that all the objects that produce absorption at z ∼ 1 are stable on a cosmological timescale and that no new objects are created, we would expect dN/dz ∼ 2-3 at z ∼ 0. About 30%-50% of this z ∼ 0 population would be descendants of the parsec-scale structures that produce single-cloud, weak Mg n absorbers at z ∼ 1. The other 50%-70% would be lower density, kiloparsec-scale structures that produce C IV absorption, but not detectable low-ionization absorption, at z ∼ 1. We conclude that at least one, and perhaps some fraction of both, of these populations has evolved away since z ∼ 1, in order to match the z ∼ 0 value of dN/dz measured in our survey. This would follow naturally for a population of transient structures whose generation is related to star-forming processes, whose rate has decreased since z ∼ 1.

Original language | English (US) |
---|---|

Pages (from-to) | 92-109 |

Number of pages | 18 |

Journal | Astrophysical Journal |

Volume | 632 |

Issue number | 1 I |

DOIs | |

State | Published - Oct 10 2005 |

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### All Science Journal Classification (ASJC) codes

- Astronomy and Astrophysics
- Space and Planetary Science

### Cite this

*Astrophysical Journal*,

*632*(1 I), 92-109. https://doi.org/10.1086/432750

}

*Astrophysical Journal*, vol. 632, no. 1 I, pp. 92-109. https://doi.org/10.1086/432750

**A survey of analogs to weak Mg II absorbers in the present.** / Narayanan, Anand; Charlton, Jane C.; Masiero, Joe R.; Lynch, Ryan.

Research output: Contribution to journal › Review article

TY - JOUR

T1 - A survey of analogs to weak Mg II absorbers in the present

AU - Narayanan, Anand

AU - Charlton, Jane C.

AU - Masiero, Joe R.

AU - Lynch, Ryan

PY - 2005/10/10

Y1 - 2005/10/10

N2 - We present the results of a survey of the analogs of weak Mg II absorbers [rest-frame equivalent width Wr(2796) < 0.3 Å] at 0 < z < 0.3. Our sample consisted of 25 HST STIS echelle quasar spectra (R = 45,000), which covered Si II λ1260 and C II λ1335 over this redshift range. Using those similar transitions as tracers of Mg II facilitates a much larger survey, covering a redshift path length of g(z) = 5.3 for an equivalent width limit of Mg II corresponding to Wr(2796) > 0.02 Å, with 30% completeness for the weakest lines. Correcting for incompleteness, we find the number of weak Mg II absorber analogs with 0.02 Å < Wr,(2796) < 0.3 Å to be dN/dz = 1.00 ±0.20 for 0 < z < 0.3. This compares to a value of dN/dz = 1.74 ± 0.10 found by Churchill et al. for the higher redshift range, 0.4 < z < 1.4, and is consistent with cosmological evolution of the population. We consider the expected effect on observability of weak Mg II absorbers of the decreasing intensity of the extragalactic background radiation field from z ∼ 1 to ∼0. Assuming that all the objects that produce absorption at z ∼ 1 are stable on a cosmological timescale and that no new objects are created, we would expect dN/dz ∼ 2-3 at z ∼ 0. About 30%-50% of this z ∼ 0 population would be descendants of the parsec-scale structures that produce single-cloud, weak Mg n absorbers at z ∼ 1. The other 50%-70% would be lower density, kiloparsec-scale structures that produce C IV absorption, but not detectable low-ionization absorption, at z ∼ 1. We conclude that at least one, and perhaps some fraction of both, of these populations has evolved away since z ∼ 1, in order to match the z ∼ 0 value of dN/dz measured in our survey. This would follow naturally for a population of transient structures whose generation is related to star-forming processes, whose rate has decreased since z ∼ 1.

AB - We present the results of a survey of the analogs of weak Mg II absorbers [rest-frame equivalent width Wr(2796) < 0.3 Å] at 0 < z < 0.3. Our sample consisted of 25 HST STIS echelle quasar spectra (R = 45,000), which covered Si II λ1260 and C II λ1335 over this redshift range. Using those similar transitions as tracers of Mg II facilitates a much larger survey, covering a redshift path length of g(z) = 5.3 for an equivalent width limit of Mg II corresponding to Wr(2796) > 0.02 Å, with 30% completeness for the weakest lines. Correcting for incompleteness, we find the number of weak Mg II absorber analogs with 0.02 Å < Wr,(2796) < 0.3 Å to be dN/dz = 1.00 ±0.20 for 0 < z < 0.3. This compares to a value of dN/dz = 1.74 ± 0.10 found by Churchill et al. for the higher redshift range, 0.4 < z < 1.4, and is consistent with cosmological evolution of the population. We consider the expected effect on observability of weak Mg II absorbers of the decreasing intensity of the extragalactic background radiation field from z ∼ 1 to ∼0. Assuming that all the objects that produce absorption at z ∼ 1 are stable on a cosmological timescale and that no new objects are created, we would expect dN/dz ∼ 2-3 at z ∼ 0. About 30%-50% of this z ∼ 0 population would be descendants of the parsec-scale structures that produce single-cloud, weak Mg n absorbers at z ∼ 1. The other 50%-70% would be lower density, kiloparsec-scale structures that produce C IV absorption, but not detectable low-ionization absorption, at z ∼ 1. We conclude that at least one, and perhaps some fraction of both, of these populations has evolved away since z ∼ 1, in order to match the z ∼ 0 value of dN/dz measured in our survey. This would follow naturally for a population of transient structures whose generation is related to star-forming processes, whose rate has decreased since z ∼ 1.

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U2 - 10.1086/432750

DO - 10.1086/432750

M3 - Review article

AN - SCOPUS:28044460531

VL - 632

SP - 92

EP - 109

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1 I

ER -