Damped Lyalpha Absorption Associated with an Early-Type Galaxy at Redshift z=0.16377.

Lanzetta, Kenneth M.; Wolfe, Arthur M.; Altan, Hakan; Barcons, X.; Chen, Hsiao‐Wen; Fernández-Soto, A.; Meyer, D.I.; Ortiz-Gil, A.; Savaglio, S.; Webb, John R.; Yahata, Noriaki

doi:10.1086/118567

Cited by 38 publications

(39 citation statements)

References 15 publications

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“…Object À2.56+2.01 is unresolved. We do not detect object À00023+00043 identified in Lanzetta et al (1997).…”

Section: Q0850+440contrasting

confidence: 72%

“…The near-infrared emission appears to extend toward the quasar. We find an apparent H magnitude of 24.7 for this diffuse emission, while Lanzetta et al (1997) find an apparent AB magnitude of m F702W ¼ 22:5 mag. The F702W H color of À2.2 is extremely blue.…”

Section: Q0850+440mentioning

confidence: 55%

“…Object À9.04+1.53 is the galaxy designated ''G1'' by Lanzetta et al (1997). We find that it is a disklike galaxy with a bulge-to-disk ratio of $0.3 and scale lengths of r e $ 0:7 and r d $ 1:0 kpc.…”

Section: Q0850+440mentioning

confidence: 78%

“…This section describes the QSO-subtraction techniques we used. Lane et al 1998; (7) Lanzetta et al 1997;(8) Bechtold et al 2002. First, during the observation we observed stars as PSF calibrations.…”

Section: Subtraction Of the Quasar Point-spread Functionmentioning

confidence: 99%

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Adaptive Optics Imaging of Low-Redshift Damped Lyα Quasar Absorbers

et al. 2006

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We have carried out a high angular resolution near-infrared imaging study of the fields of six quasars with seven strong absorption-line systems at z < 0:5, using the Hokupa'a adaptive optics system and the Quick Infrared Camera on the Gemini North telescope. These absorption systems include four classical damped Ly absorbers ( DLAs), two sub-DLAs, and one Lyman limit system. Images were obtained in the H or K 0 filters with FWHM between 0B2 and 0B5 with the goal of detecting the absorbing galaxies and identifying their morphologies. Features are seen at projected separations of 0B5-16B0 from the quasars, and all the fields show features at less than 2 00 separation. We find candidate absorbers in all seven systems. With the assumption that some of these are associated with the absorbers, the absorbers are low-luminosity 0:1L Ã H or L Ã K ; we do not find any large, bright candidate absorbers in any of our fields. Some fields show compact features that are too faint for quantitative morphology but could arise in dwarf galaxies.

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“…Object À2.56+2.01 is unresolved. We do not detect object À00023+00043 identified in Lanzetta et al (1997).…”

Section: Q0850+440contrasting

confidence: 72%

Section: Q0850+440mentioning

confidence: 55%

Section: Q0850+440mentioning

confidence: 78%

Section: Subtraction Of the Quasar Point-spread Functionmentioning

confidence: 99%

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Adaptive Optics Imaging of Low-Redshift Damped Lyα Quasar Absorbers

et al. 2006

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“…To date, the answer to this question has been surprisingly ambiguous for a wide range of absorber types. Despite initial detections of Mg IIÈabsorbing galaxies that seemed to Ðrmly establish the existence of D40 h~1 kpc radii halos6 for bright galaxies (Bergeron 1986 ;Bergeron & Boisse 1991 ;Steidel, Dickinson, & Persson 1994), it remains unclear whether individual galaxies are responsible for Lya lines (Lanzetta et al 1995 ;Chen et al 1998 ;Morris et al 1993 ;Stocke et al 1995 ;Bowen et al 1996Bowen et al , 1998Le Brun, Bergeron, & Boisse 1996 ;Shull, Stocke, & Penton 1996 ;van Gorkom et al 1996 ;Tripp, Lu, & Savage 1998), while the diversity of galaxy types associated with damped Lya systems has been a surprise (Le Brun et al 1997 ;Lanzetta et al 1997 ;Rao & Turnshek 1998). Establishing whether O VI absorption is linked to galaxies is important for establishing whether absorption is indeed due to violent processes within the ISM of individual galaxies or the consequence of the growth of large-scale structure in the universe.…”

Section: Introductionmentioning

confidence: 99%

Where Are the Absorbers toward Q2302+029?

Bowen

Jiménez

Jenkins

2001

ApJ

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We present images and spectroscopy of objects close to the sight line of Q2302]029 in order to search for galaxies responsible for the remarkable z \ 0.7 high-ionization absorption-line system found by Jannuzi et al. This system shows "" normal ÏÏ narrow O VI, N V, and C IV lines superimposed on broader (3000È5000 km s~1 wide), unsaturated absorption troughs some 56,000 km s~1 away from the QSO emission redshift Despite reaching sensitivities sufficient to detect 1/10L* galaxies in (z em \ 1.052). the optical and 1/20L* in the infrared, we are unable to detect any obvious bright galaxies that might be responsible for the absorption beyond B6 h~1 kpc of the sight line. This supports the hypotheses that the absorption is either intrinsic to the QSO or arises in intracluster gas. Adopting either explanation is problematic : in the Ðrst case, "" associated ÏÏ absorption at such high ejection velocities is difficult to understand, and challenges the conventional discrimination between intrinsic and extrinsic absorbers ; in the second case, the gas must reside in a D40 h~1 Mpc long Ðlament aligned along the line of sight in order to reproduce the broad absorption. Since the absorption system is unusual, such a chance alignment might not be unreasonable. Spectroscopy of objects beyond the immediate vicinity of the QSO sight line reveals a galaxy cluster at z \ 0.59, which coincides with strong Lya and more narrow highionization lines in the quasar spectrum. Here, too, the lack of galaxies at distances comparable to those found for, e.g., Lya-absorbing galaxies, suggests that the absorption may arise from intracluster gas unassociated with any individual galaxies. Subject headings : large-scale structure of universe È quasars : absorption lines È quasars : individual (Q2302]029)

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Element Abundances at High Redshifts

Pettini

1999

Chemical Evolution From Zero to High Redshift

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I review measurements of element abundances in different components of the high redshift universe, including the Lyman alpha forest, damped Lyman alpha systems, and Lyman break galaxies. Although progress is being made in all three areas, recent work has also produced some surprises and shown that established ideas about the nature of the damped Lyα systems in particular may be too simplistic. Overall, our knowledge of metal abundances at high z is still very sketchy. Most significantly, there seems to be an order of magnitude shortfall in the comoving density of metals which have been measured up to now compared with those produced by the star formation activity seen in Lyman break galaxies. At least some of the missing metals are likely to be in hot gas in galactic halos and proto-clusters.

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Damped Lyalpha Absorption Associated with an Early-Type Galaxy at Redshift z=0.16377.

Abstract: 2 Based on observations made with the William Herschel Telescope operated on the island of La Palma by the

Cited by 38 publications

References 15 publications

Adaptive Optics Imaging of Low-Redshift Damped Lyα Quasar Absorbers

Adaptive Optics Imaging of Low-Redshift Damped Lyα Quasar Absorbers

Where Are the Absorbers toward Q2302+029?

Element Abundances at High Redshifts

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