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A Search for the Damped Lyα Absorber at z = 1.86 toward QSO 1244+3443 with NICMOS

Kulkarni, Varsha P. and Hill, John M. and Schneider, Glenn and Weymann, Ray J. and Storrie-Lombardi, Lisa J. and Rieke, Marcia J. and Thompson, Rodger I. and Jannuzi, Buell T. (2001) A Search for the Damped Lyα Absorber at z = 1.86 toward QSO 1244+3443 with NICMOS. Astrophysical Journal, 551 (1). pp. 37-47. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20170328-092024251

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Abstract

We have carried out a high-resolution imaging search for the galaxy associated with the damped Lyα absorber (DLA) at z = 1.859 toward the z_(em) = 2.48 quasar QSO 1244+3443, using the Hubble Space Telescope (HST) and the near-infrared camera and multiobject spectrometer (NICMOS). Images were obtained in the broad filter F160W and the narrow filter F187N with camera 2 on NICMOS with the goal of detecting the rest-frame optical continuum and the Hα line emission from the DLA. After point-spread function (PSF) subtraction, two weak features are seen at projected separations of 0farcs16-0farcs24 from the quasar. Parts of these features may be associated with the DLA, although we cannot completely rule out that they could be artifacts of the PSF. If associated with the DLA, the objects would be ≈1-2 h^(-1)__(70) kpc in size with integrated flux densities of 2.5 and 3.3 μJy in the F160W filter, implying luminosities at λ_(central) = 5600 Å in the DLA rest frame of 4.4-5.9 × 10^9 h^(-2)__(70) L_☉ at z = 1.86, for q_0 = 0.5. However, no significant Hα line emission is seen from these objects, suggesting low star formation rates (SFRs). Our 3 σ upper limit on the SFR in the DLA is 1.3 h^(-2)_(70) M_☉ yr^(-1) for q_0 = 0.5 (2.4 h^(-2)_(70) M_☉ yr^(-1) for q_0 = 0.1). This together with our earlier result for LBQS 1210 + 1731 mark a significant improvement over previous constraints on the star formation rates of DLAs. Dust within the DLA could extinguish Hα emission, but this would require the dust content in the DLA to be much higher than that inferred from previous DLA observations. A combination of low star formation rate and some dust extinction is likely to be responsible for the lack of Hα emission. Alternatively, the objects, if real, may be associated with the host galaxy of the quasar rather than with the DLA. In any case, our observations suggest that the DLA is not a large bright protodisk, but a compact object or a low surface brightness galaxy. If the two features are PSF artifacts or associated with the quasar host, then the constraints on the size and luminosity of the DLA are even more severe.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1086/320079DOIArticle
http://iopscience.iop.org/article/10.1086/320079PublisherArticle
https://arxiv.org/abs/astro-ph/0012140arXivDiscussion Paper
ORCID:
AuthorORCID
Schneider, Glenn0000-0002-4511-5966
Storrie-Lombardi, Lisa J.0000-0002-5987-5210
Rieke, Marcia J.0000-0002-7893-6170
Jannuzi, Buell T.0000-0002-1578-6582
Additional Information:© 2001. The American Astronomical Society. Received 2000 September 7; accepted 2000 December 12. This project was supported by NASA grant NAG 5-3042 to the NICMOS Instrument Definition Team. It is a pleasure to thank Nicholas Bernstein and Keith Noll for their assistance in the scheduling of our observations. We thank E. Stobie, D. Lytle, E. O'Neil, I. Barg, and A. Ferro for software and computer support.
Funders:
Funding AgencyGrant Number
NASANAG 5-3042
Subject Keywords:cosmology: observations; galaxies: evolution; galaxies: high-redshift; infrared: galaxies; intergalactic medium; quasars: absorption lines
Issue or Number:1
Record Number:CaltechAUTHORS:20170328-092024251
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170328-092024251
Official Citation:Varsha P. Kulkarni et al 2001 ApJ 551 37
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:75465
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:28 Mar 2017 16:31
Last Modified:06 Nov 2019 04:37

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