2006MNRAS.371..431C


Query : 2006MNRAS.371..431C

2006MNRAS.371..431C - Mon. Not. R. Astron. Soc., 371, 431-443 (2006/September-1)

A survey for redshifted molecular and atomic absorption lines - I. The Parkes half-Jansky flat-spectrum red quasar sample.

CURRAN S.J., WHITING M.T., MURPHY M.T., WEBB J.K., LONGMORE S.N., PIHLSTROM Y.M., ATHREYA R. and BLAKE C.

Abstract (from CDS):

We are currently undertaking a large survey for redshifted atomic and molecular absorption lines at radio frequencies. In this paper, we present the results from the first phase of this survey: the search for Hi 21-cm and OH 18-cm absorption lines in the hosts of reddened quasars and radio galaxies. Although we observed each source for up to several hours with two of the world's most sensitive radio telescopes, the Giant Metrewave Radio Telescope (GMRT) and Westerbork Synthesis Radio Telescope (WSRT), only one clear and one tentative detection were obtained: Hi absorption at z = 0.097 in PKS 1555-140 and OH absorption at z = 0.126 in PKS 2300-189, respectively, with the Australia Telescope Compact Array (ATCA). For the latter, no Hi absorption was detected at the same redshift as the borderline OH detection. In order to determine why no clear molecular absorption was detected in any of the 13 sources searched, we investigate the properties of the five redshifted systems currently known to exhibit OH absorption. In four of these, molecules were first detected via millimetre-wave transitions, and the flat radio spectra indicate compact background continuum sources, which may suggest a high degree of coverage of the background source by the molecular clouds in the absorber. Furthermore, for these systems we find a relationship between the molecular line strength and red optical-near-infrared (V - K) colours, thus supporting the notion that the reddening of these sources is due to dust, which provides an environment conducive to the formation of molecules. Upon comparison with the V - K colours of our sample, this relationship suggests that, presuming the reddening occurs at the host galaxy redshift at least in some of the targets, many of our observations still fall short of the sensitivity required to detect OH absorption, although a confirmation of the `detection' of OH in 2300-189 could contravene this.

Abstract Copyright: 2006 The Authors. Journal compilation © 2006 RAS

Journal keyword(s): galaxies: abundances - galaxies: high-redshift - quasars: absorption lines - cosmology: observations - cosmology: early Universe - radio lines: galaxies

Simbad objects: 36

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Number of rows : 36
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 QSO B0003-066 BLL 00 06 13.89288482 -06 23 35.3353584   19.1 18.50 17.14   ~ 329 1
2 QSO B0023-263 BLL 00 25 49.15629900 -26 02 12.6141092   20.30 19.5 18.084   ~ 161 1
3 QSO B0108+388 Bla 01 11 37.31680 +39 06 28.1039     22 22.000   ~ 254 1
4 QSO B0114+074 QSO 01 17 26.1665163120 +07 42 17.441318664     18.37     ~ 28 2
5 QSO B0131-001 QSO 01 34 12.70415461 +00 03 45.1386194   23.34 22.50 20.780   ~ 39 1
6 QSO B0132-097 QSO 01 34 35.6657627616 -09 31 02.903742300   24.52 22.70 20.80   ~ 110 1
7 3C 48 QSO 01 37 41.2996631208 +33 09 35.080388820   16.62 16.20     ~ 2815 2
8 ICRF J015537.0-404842 Sy2 01 55 37.05930363 -40 48 42.3570102   18.5       ~ 51 1
9 PKS 0201-44 rG 02 03 40.7595537000 -43 49 51.138331176     19.0     ~ 35 1
10 4C 15.05 Bla 02 04 50.41389294 +15 14 11.0436097   21.9 21.00 21.00   ~ 413 1
11 6C 021803+354230 BLL 02 21 05.4920852208 +35 56 13.848581904   20.0 20.0 19.60   ~ 560 3
12 ICRF J045707.7+064507 Sy2 04 57 07.70994002 +06 45 07.2605778   19.2   18.14   ~ 95 1
13 ICRF J050321.1+020304 Sy2 05 03 21.19716454 +02 03 04.6765714   22.500 21.350 20.682   ~ 188 1
14 ICRF J054236.1+495107 Sy1 05 42 36.13789710 +49 51 07.2337139   18.45 17.80 17.210   ~ 1494 1
15 3C 190 QSO 08 01 33.5525166480 +14 14 42.813906612   21.07 20.26 18.972   ~ 242 2
16 NVSS J090530+340756 rG 09 05 30.1 +34 07 57   24.0 23.800 23.500   ~ 160 1
17 QSO B1107-187 QSO 11 10 00.40688649 -18 58 48.7427831   22.44 21.10     ~ 39 0
18 [DG2000] 12107+3157 Mas 12 13 19.5 +31 40 55           ~ 2 0
19 IRAS 12108+3157 G 12 13 19.6 +31 40 55           ~ 7 0
20 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4342 2
21 ICRF J135605.3-342110 Sy2 13 56 05.38656310 -34 21 10.8588959   19.4   18.50   ~ 46 1
22 NVSS J135740+435400 rG 13 57 40.5870 +43 53 59.772     22.708 20.951   ~ 47 1
23 ICRF J141558.8+132023 Sy2 14 15 58.81751033 +13 20 23.7128587   21.055 20.000 18.461   ~ 438 1
24 QSO B1450-338 QSO 14 54 02.47333400 -34 00 57.2105112   22.520 20.400 19.390   ~ 26 1
25 ICRF J150609.5+373051 Sy2 15 06 09.52997529 +37 30 51.1325012   21.2 21.2 20.60   ~ 192 1
26 QSO B1535+004 QSO 15 38 15.95309209 +00 19 05.3239262     18.80 18.8   ~ 37 1
27 ICRF J155821.9-140959 Sy2 15 58 21.94812 -14 09 59.0519   19.0   12.15   ~ 74 1
28 QSO B1830-211 Bla 18 33 39.9399138048 -21 03 39.368838780     18.70 21   ~ 673 1
29 [DG2000] 19154+2704 Cld 19 17 31.1 +27 10 00           ~ 2 1
30 IRAS 19154+2704 PN? 19 17 31.3817643330 +27 10 05.487277656           ~ 7 0
31 ICRF J193925.0-634245 Sy2 19 39 25.0245304992 -63 42 45.640373400   18.87 18.37 17.64   ~ 1229 1
32 [VV98] J225504.2-084404 QSO 22 55 04.23979 -08 44 04.0213       20.5   ~ 50 1
33 ICRF J230302.9-184125 Sy1 23 03 02.9760289032 -18 41 25.823118480   18.29 17.82 16.569   ~ 133 1
34 [VV2006] J233954.5-331018 QSO 23 39 54.53514547 -33 10 16.8813229     22.50 20.8   ~ 43 0
35 [WKK2003] Gal-N G ~ ~           ~ 9 1
36 [WKK2003] Gal-S G ~ ~           ~ 9 1

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