2013A&A...552A..77K


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.07CET12:32:32

2013A&A...552A..77K - Astronomy and Astrophysics, volume 552A, 77-77 (2013/4-1)

The evolution of HI and CIV quasar absorption line systems at 1.9 < z < 3.2.

KIM T.-S., PARTL A.M., CARSWELL R.F. and MUELLER V.

Abstract (from CDS):

We have investigated the distribution and evolution of ∼3100 intergalactic neutral hydrogen (HI) absorbers with HI column densities log NHI=[12.75, 17.0] at 1.9<z<3.2, using 18 high resolution, high signal-to-noise quasar spectra obtained from the ESO VLT/UVES archive. We used two sets of Voigt profile fitting analysis, one including all the available high-order Lyman lines to obtain reliable HI column densities of saturated lines, and another using only the Lyα transition. There is no significant difference between the Lyα-only fit and the high-order Lyman fit results. Combining our Lyα-only fit results at 1.7<z<3.6 with high-quality literature data, the mean number density at 0<z<4 is not well described by a single power law and strongly suggests that its evolution slows down at z≤1.5 at the high and low column density ranges. We also divided our entire HI absorbers at 1.9<z<3.2 into two samples, the unenriched forest and the CIV-enriched forest, depending on whether HI lines are associated with CIV at log NCIV≥12.2 within a given velocity range. The entire HI column density distribution function (CDDF) can be described as the combination of these two well-characterised populations which overlap at log NHI∼15. At log NHI≤15, the unenriched forest dominates, showing a similar power-law distribution to the entire forest. The CIV-enriched forest dominates at log NHI≥15, with its distribution function as ∝ NHI~–1.45. However, it starts to flatten out at lower NHI, since the enriched forest fraction decreases with decreasing NHI. The deviation from the power law at log NHI=[14, 17] shown in the CDDF for the entire HI sample is a result of combining two different HI populations with a different CDDF shape. The total HI mass density relative to the critical density is ΩHI∼1.6x10–6h–1, where the enriched forest accounts for ∼40% of ΩHI.

Abstract Copyright:

Journal keyword(s): quasars: absorption lines - cosmology: observations - large-scale structure of Universe

Simbad objects: 18

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Number of rows : 18

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 QSO B0002-422 QSO 00 04 48.2718823544 -41 57 28.150311306   17.44 17.21     ~ 154 0
2 QSO B0055-26 QSO 00 57 58.0249885733 -26 43 14.753717865   17.90 17.47 17.99   ~ 132 1
3 QSO B0109-353 QSO 01 11 43.6321355926 -35 03 00.586979841   16.6 16.9     ~ 72 0
4 QSO B0122-379 QSO 01 24 17.3723276055 -37 44 22.919153842     17.1     ~ 113 0
5 QSO B0237-2322 QSO 02 40 08.1742481040 -23 09 15.727160394   16.78 16.63     ~ 467 0
6 QSO B0329-385 QSO 03 31 06.3780192488 -38 24 04.653743031   17.63 16.92     ~ 75 0
7 PHL 4444 QSO 03 31 08.9205312901 -25 24 43.264751845   17.82 17.51 18.2   ~ 90 1
8 PKS 0405-123 Sy1 04 07 48.4309594137 -12 11 36.660481492   15.09 14.86 14.7   ~ 461 1
9 QSO J0422-3844 BLL 04 22 14.7829518039 -38 44 52.824921025   17.70 16.92 16.3   ~ 189 1
10 QSO J0455-4216 QSO 04 55 23.0623318803 -42 16 17.398158654   17.77 17.06     ~ 133 0
11 QSO B0940-1050 QSO 09 42 53.5076745009 -11 04 25.929146122   16.96 16.6 16.6   ~ 82 0
12 PG 1101-264 QSO 11 03 25.2992132616 -26 45 15.809136362   16.08 16.02     ~ 238 0
13 QSO B1122-168 QSO 11 24 42.8660012281 -17 05 17.386970324   16.5 16.5 16.1   ~ 118 1
14 QSO B1448-232 QSO 14 51 02.5094965667 -23 29 31.105639377   17.13 16.96     ~ 118 2
15 QSO B2126-15 QSO 21 29 12.17589777 -15 38 41.0413097   17.61 17.3 17.3   ~ 456 1
16 QSO J2220-2803 QSO 22 20 06.7586653848 -28 03 23.466203761     16.0 16.10   ~ 88 0
17 QSO J2233-606 QSO 22 33 37.5814904803 -60 33 29.146578276 16.90 17.39 17.16 16.93 16.51 ~ 84 0
18 QSO B2347-4342 QSO 23 50 34.2595236845 -43 25 59.680334378   16.3 16.3     ~ 159 0

    Equat.    Gal    SGal    Ecl

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2019.12.07-12:32:32

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