4.7. Current Redshift Record Breakers With Ly Emission or Absorption Breaks
In Table 3 we list published or otherwise secure "record redshifts" for galaxies; most have prominent Ly emission lines or at least a strong Ly forest absorption.
z | Source | Reference | NB | LBG | ser | other | lens |
6.578 | SDFJ 132418.3 | Kodaira et al. | x | ||||
6.56 | HCM 6A | Hu etal. | x | x | |||
6.541 | SDFJ 132415.7 | Kodaira et al. | x | ||||
5.869 | BDF1:19 | Lehnert and Bremer | x | ||||
5.83 | CDFS 5144 | GOODS | x | ||||
5.783 | CDFS SBM03#3 | Bunker et al. 2003 | x | ||||
5.746 | LALA5 1-03 | Rhoads et al. | x | ||||
5.744 | BDF1:10 | Lehnert and Bremer | x | ||||
5.74 | SSA22-HCMI | Hu etal. | x | x | |||
5.700 | LALA5 1-06 | Rhoads et al. | x | ||||
5.69 | LAE J1044-0130 | Ajiki et al. 2002 | x | ||||
5.674 | LALA5 1-5 | Rhoads et al. 2002 | x | ||||
5.655 | LAE J1044-0123 | Taniguchi et al. | x | ||||
5.649 | BDF2:19 | Lehnert and Bremer | x | ||||
5.631 | HDFF 36246-1511 | Dawson et al. 2001 | x | ||||
5.621 | Lynx R-drop | Stern et al. in prep | x | x | |||
5.60 | HDF 4-473 | Weymann et al. 1998 | x | ||||
5.576 | Abell 2218 lens | Ellis et al. 2001 | x | x | |||
5.46 | NDFWS R-drop | Dey et al., in prep. | x | ||||
5.34 | HDF 3-951.0 | Spinrad et al. 1998 | x | ||||
5.34 | RD1 | Dey et al. 1998 | x | ||||
5.190 | HDFF ES1 | Dawson et al. 2001 | x | ||||
5.19 | TN J0924-2201 | van Breugel et al. 1999 | x | ||||
5.19 | ES1 | Dawson et al. 2001 | x | ||||
5.186 | HDFF Chandra source | Barger et al. 2002 | x | ||||
5.12 | A1689 lens | Frye et al. 2002 | x | x | |||
5.056 | BDF1:26 | Lehnert et al. 2002 | x | ||||
5.018 | BDF1:18 | Lehnert et al. 2002 | x | ||||
4.99 | Cetus R-drop | Stern et al. in prep | x | ||||
Notes on the initial discovery techniques - NB = narrow-band selected; LBG = continuum Lyman-break/Lyman-forest break selected; ser = serendipitously identified; other = selected in other manner (e.g., radio-selected, X-ray selected); lens = known gravitational lens. |
We note that since 1999 astronomers have added at least 25 galaxies with z 5. This is an impressive and useful score; however, a more physical analysis of several aspects of the pioneering effort is now an obvious and desired second approach. Also, the morphologies of the continuum and Ly lines may provide useful information on the environs of very early galactic systems. The cut-off date for entries in Table 8.3 was 2003 February.