1998ApJ...506....1W


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.17CEST03:43:15

1998ApJ...506....1W - Astrophys. J., 506, 1-18 (1998/October-2)

The Hubble space telescope quasar absorption line key project. XIV. The evolution of Lyα absorption lines in the redshift interval z = 0-1.5.

WEYMANN R.J., JANNUZI B.T., LU L., BAHCALL J.N., BERGERON J., BOKSENBERG A., HARTIG G.F., KIRHAKOS S., SARGENT W.L.W., SAVAGE B.D., SCHNEIDER D.P., TURNSHEK D.A. and WOLFE A.M.

Abstract (from CDS):

We present the results of an analysis of the rate of evolution of the Lyα absorption lines in the redshift interval 0.0 to ∼1.5 based upon a sample of 987 Lyα absorption lines identified in the spectra of 63 QSOs obtained with the Faint Object Spectrograph (FOS) of the Hubble Space Telescope (HST). These spectra were obtained as part of the QSO Absorption Line Survey, an HST Key Project during the first four years of observations with the telescope. Fits to the evolution of the number of absorbers per unit redshift (dN/dz) of the form dN/dz = Ax(1 + z)γ continue to yield values of γ in the range 0.1-0.3, decidedly flatter than results from ground-based data pertaining to the redshift range z > 1.7. These results are consistent with our previous results based on a much smaller sample of lines, but the uncertainties in the fit have been greatly reduced. The combination of the HST and ground-based data suggest a marked transition in the rate of evolution of the Lyα lines at a redshift of about 1.7. The 19 Lyα lines from an additional higher redshift QSO from our sample for which tentative line identifications are available (UM 18; zem = 1.89) support the suggestion of a rapid increase at around this redshift. We derive the cumulative distribution of the full sample of Lyα lines and show that the distribution in redshift can indeed be well represented by a power law of the form (1 + z)γ. For this same sample, the distribution of equivalent widths of the Lyα absorbers above a rest equivalent width of 0.1 Å is fit quite well by an exponential. Comparing samples of Lyα lines, one set of which has redshifts the same as, or very near to, the redshifts of ions from heavy elements and another set in which no ions from heavy elements have been identified, we find that the Lyα systems with heavy element detections have a much steeper slope than the high rest equivalent width portion of the Lyman-only sample. We argue that this result is not likely to be due to either line misidentification or incomplete spectral coverage. Considering the insensitivity of the equivalent width to large changes in the column density for saturated lines, we suggest that this result is probably attributable to rapid evolution of the very highest column density systems, rather than real differences in metallicity. We find evidence that the rate of evolution increases with increasing equivalent width. We compare our results for the variation of line density with redshift to recent numerical simulations of Lyα absorbers, in particular, to those of Riediger, Petitjean, & Mucket, which extend to zero redshift. We find fairly good agreement between these simulations and our results, though the rapid evolution we find in the Lyα systems containing heavy element ions is not predicted in their models. We speculate that these heavy element-containing Lyα systems involve those clouds closely associated with galaxies, whose column densities are too high and whose sizes are too small to be included in the Riediger et al. simulations. Our results for Lyα lines at the high end of our equivalent width distribution are compatible with the recent analysis of the absorber-galaxy correlation by Chen et al. For the weaker lines, however, our results suggest that whatever association exists between absorbers and galaxies is different from that for the stronger lines. We conclude with some suggestions for further observations.

Abstract Copyright:

Journal keyword(s): Cosmology: Observations - Galaxies: Intergalactic Medium - Galaxies: Quasars: Absorption Lines

Simbad objects: 65

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Number of rows : 65

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 QSO B0002+0507 BLL 00 05 20.2154926286 +05 24 10.802553926   16.56 16.21 16.26   ~ 175 1
2 2E 12 Sy1 00 05 59.2379634379 +16 09 49.023089304   16.51 16.40     ~ 270 1
3 QSO J0027+2241 QSO 00 27 15.3715607 +22 41 58.067394   16.90 16.57 15.60   ~ 83 1
4 QSO B0043+0354 Sy1 00 45 47.2230875166 +04 10 23.385233220   15.88 16.00     ~ 151 0
5 2E 177 Sy1 00 47 05.9186400186 +03 19 54.785770057   16.2 16.37     ~ 140 1
6 QSO B0117+2118 QSO 01 20 17.2644311878 +21 33 46.196835922     16.1     ~ 122 0
7 QSO J0125-0005 QSO 01 25 28.8436590768 -00 05 55.930666802   16.92 16.64 16.30   ~ 266 1
8 ICRF J020157.1-113233 Sy1 02 01 57.1798202842 -11 32 33.436998341   16.54 16.40 16.073   ~ 197 1
9 4C -04.06 QSO 02 35 07.3417120791 -04 02 05.319157399   16.61 16.46 16.2   ~ 190 1
10 2MASS J03512857-1429082 Sy1 03 51 28.5672281753 -14 29 08.258414299 15.62 16.55 16.22     ~ 178 1
11 PKS 0405-123 Sy1 04 07 48.4309594137 -12 11 36.660481492   15.09 14.86 14.7   ~ 478 1
12 2E 962 Sy1 04 17 16.7842860907 -05 53 45.608565853   16.24 15.94 15.7   ~ 165 1
13 QSO J0441-4313 QSO 04 41 17.3385473794 -43 13 45.487081188   16.64 16.36 16.54 16.26 ~ 96 1
14 QSO B0624+6907 QSO 06 30 02.5049167075 +69 05 03.912553984   14.64 14.16     ~ 89 0
15 QSO J0635-7516 QSO 06 35 46.5080299 -75 16 16.815501   15.96 15.75 15.82   ~ 522 1
16 QSO J0743-6726 QSO 07 43 31.61163970 -67 26 25.5464081   16.71 16.37     ~ 139 1
17 ICRF J074541.6+314256 Sy1 07 45 41.6716759025 +31 42 56.614085210   16.10 15.97     ~ 246 1
18 2MASS J08533423+4349023 Sy1 08 53 34.2441726669 +43 49 02.333804505   17.15 16.91     ~ 92 0
19 QSO B0916+512 QSO 09 19 57.6063095883 +51 06 09.546161591   16.47 16.41     ~ 55 0
20 PG 0953+414 Sy1 09 56 52.3930851607 +41 15 22.212153978 14.710 15.611 15.546 15.294 14.720 ~ 423 0
21 Ton 469 Sy1 09 58 20.9495949602 +32 24 02.209578357   15.88 15.78 15.51   ~ 405 1
22 QSO B0959+6827 QSO 10 03 06.767826 +68 13 16.81100   16.28 15.92 15.3   ~ 52 0
23 Ton 28 Sy1 10 04 02.6101006271 +28 55 35.330362166   16.17 15.7     ~ 151 0
24 7C 100725.89+414711.00 Sy1 10 10 27.5276512902 +41 32 39.052946433   16.72 16.67     ~ 171 1
25 QSO B1008+1319 QSO 10 11 10.8548473346 +13 04 12.188098478   17.00 16.76     ~ 86 0
26 4C 06.41 BLL 10 41 17.16249895 +06 10 16.9236835   16.86 16.70 16.14   ~ 279 1
27 PG 1049-005 Sy1 10 51 51.4474876950 -00 51 17.709169017   15.98 15.78     ~ 155 0
28 2E 2389 Sy1 11 04 13.8613944317 +76 58 58.192391742   15.70 15.72 15.40   ~ 515 1
29 ICRF J110715.0+162802 Sy1 11 07 15.0473675622 +16 28 02.244815202   15.91 15.70     ~ 151 1
30 Ton 1388 Sy1 11 19 08.6786143504 +21 19 17.986556889   14.91 14.80     ~ 424 0
31 QSO B1130+111 QSO 11 33 30.2984529835 +10 52 23.351466688   16.52 16.45     ~ 51 0
32 NAME Crt A Sy1 11 39 10.7024704226 -13 50 43.638984127   16.38 16.17 16.4   ~ 249 1
33 2E 2503 Sy1 11 39 57.0253396181 +65 47 49.482487703   16.50 16.32     ~ 493 1
34 PG 1216+069 Sy1 12 19 20.9316038223 +06 38 38.467864632   15.68 15.65     ~ 261 0
35 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5436 1
36 QSO J1244+1721 QSO 12 44 10.8248623367 +17 21 04.509382201   16.40 16.09     ~ 137 1
37 QSO B1248+401 QSO 12 50 48.3268849448 +39 51 39.459453541   16.62 16.19     ~ 131 0
38 QSO B1252+119 QSO 12 54 38.25561161 +11 41 05.8951798   16.99 16.64 16.76   ~ 248 1
39 NVSS J125953+335653 Rad 12 59 54.0 +33 56 54   20.9       ~ 17 1
40 LB 2522 Sy1 13 01 12.9251198286 +59 02 06.693745440   16.04 15.89     ~ 253 0
41 ICRF J130533.0-103319 Sy1 13 05 33.0149111397 -10 33 19.430590671   15.18 15.23 14.46   ~ 515 1
42 Ton 153 QSO 13 19 56.2318070927 +27 28 08.187007779   16.12 15.98     ~ 144 0
43 PB 4007 Sy1 13 36 02.0094221124 +17 25 13.090293838   16.50 16.33     ~ 82 0
44 QSO J1341+4123 QSO 13 41 00.7893963759 +41 23 14.131471417   17.04 16.76     ~ 118 0
45 QSO B1352+0106 QSO 13 54 58.6803586876 +00 52 10.902911679     16.0     ~ 75 0
46 ICRF J135704.4+191907 Sy1 13 57 04.43665381 +19 19 07.3724675   16.33 16.03 15.3   ~ 418 2
47 QSO J1409+2618 QSO 14 09 23.9086975485 +26 18 21.053512073   16.07 15.74     ~ 181 0
48 QSO J1427-1203 QSO 14 27 38.1268921544 -12 03 49.947875383   16.91 16.49 17.19   ~ 71 1
49 4C 37.43 Sy1 15 14 43.0682940988 +36 50 50.355363752   17.11 17.01 15.83   ~ 379 1
50 PG 1538+47 Sy1 15 39 34.8103282209 +47 35 31.265171935   16.01 15.81     ~ 89 1
51 2E 3648 Sy1 16 20 21.8184966430 +17 36 23.952696503   16.53 16.41 20.5   ~ 392 2
52 QSO B1634+7037 QSO 16 34 28.9917493918 +70 31 32.394595988   14.90 14.66     ~ 261 0
53 2A 1705+609 Sy1 17 04 41.3742389551 +60 44 30.522600868   15.65 15.40 15.30   ~ 728 1
54 ClG 1821+64 ClG 18 21 56.7276 +64 20 55.841           ~ 494 1
55 2E 4066 Sy1 18 21 57.2365 +64 20 36.226   14.23 14.24     ~ 548 1
56 QSO B2128-123 BLL 21 31 35.26175 -12 07 04.7961   16.33 16.11 15.87   ~ 427 1
57 4C 06.69 QSO 21 48 05.4585565234 +06 57 38.605396596   16.85 16.47 15.06   ~ 608 1
58 QSO J2246-1206 QSO 22 46 18.2318680462 -12 06 51.276150444   16.63 16.45 15.99   ~ 266 1
59 3C 454.3 Bla 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2571 2
60 4C 11.72 BLL 22 54 10.4213843099 +11 36 38.745749268   16.02 15.82     ~ 323 1
61 ICRF J230343.5-680737 Sy1 23 03 43.5650270994 -68 07 37.443084908   16.26 16.38 17.68   ~ 79 1
62 PB 5235 QSO 23 04 44.9533458555 +03 11 45.918742912   15.44 15.8     ~ 102 0
63 QSO B2340-0339 QSO 23 42 56.6002737186 -03 22 26.268440951   16.53 16.02 16.28   ~ 81 1
64 ICRF J234636.8+093045 Sy1 23 46 36.83854476 +09 30 45.5148840   16.23 15.97 15.99   ~ 312 2
65 QSO J2355-3357 QSO 23 55 25.7958797721 -33 57 55.213455767   18.32 16.4 17.10   ~ 57 1

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2021.05.17-03:43:15

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