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Date and Time of the Query: 2019-06-19 T14:49:53 PDT
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For refcode 2010MNRAS.408..849G:
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NED Abstract

Copyright by Royal Astronomical Society. 2010MNRAS.408..849G GMRT mini-survey to search for 21-cm absorption in quasar-galaxy pairs at z ~ 0.1 Gupta, N.; Srianand, R.; Bowen, D. V.; York, D. G.; Wadadekar, Y. Abstract. We present the results from our 21-cm absorption survey of a sample of five quasar-galaxy pairs (QGPs), with the redshift of the galaxies in the range 0.03 <= z_g_ <= 0.18, selected from the Sloan Digital Sky Survey (SDSS). The HI 21-cm absorption was searched towards the nine sightlines with impact parameters ranging from ~10 to ~55 kpc using the Giant Metrewave Radio Telescope (GMRT). 21-cm absorption was detected only in one case, i.e. towards the quasar (z_q_ = 2.625 SDSS J124157.54+633241.6)-galaxy (z_g_ = 0.143 SDSS J124157.26+633237.6) pair with the impact parameter ~11 kpc. The quasar sightline in this case pierces through the stellar disc of a galaxy having near solar metallicity [i.e. (O/H)+12 = 8.7] and star formation rate uncorrected for dust attenuation of 0.1 M_sun_ yr^-1^. The quasar spectrum reddened by the foreground galaxy is well fitted with the Milky Way extinction curve (with an A_V_ of 0.44) and the estimated HI column density is similar to the value obtained from 21-cm absorption assuming a spin temperature (T_S_) of 100 K. In the remaining cases, our GMRT spectra provide upper limit on N(HI) in the range (10^17^-10^18^) x T_S_ cm^-2^. Combining our sample with the z <= 0.1 data available in the literature, we find the detectability of 21-cm absorption with integrated optical depth greater than 0.1 km s^-1^ to be 50 per cent for the impact parameter less than 20 kpc. Using the surface brightness profiles and a well-established relationship between the optical size and extent of the HI disc known for nearby galaxies, we conclude that in most of the cases of 21-cm absorption non-detection, the sightlines may not be passing through the HI gas (1{sigma} column density of a few times 10^19^ cm^-2^). We also find that in comparison to the absorption systems associated with these QGPs, z < 1 damped Lyman-{alpha} absorbers (DLAs) with 21-cm absorption detections have lower CaII equivalent widths despite having higher 21-cm optical depths and smaller impact parameters. This suggests that the current sample of DLAs may be a biased population that avoids sightlines through dusty star-forming galaxies. A systematic survey of QGPs over a wider redshift range using a large sample is needed to confirm these findings and understand the nature of 21-cm absorbers. Key words: galaxies: evolution, galaxies: ISM, quasars: absorption lines
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