Table 4
Galaxy counterpart candidates of the intervening absorption line systems.
| GRB 050730 (GRB: z = 3.969, DLA: z = 3.56439, sub-DLA: z = 3.02209, Mg ii absorbers: z = 2.25313, 1.7731) | |||||||||||
| Candidate | Remark | θ (″) | R (mag) | F775W (mag) | Ks (mag) | 3.6 μm (mag) | 5.8 μm (mag) | ||||
|
|
|||||||||||
| A1 | star | 12.8 | 23.46 ± 0.03 | 23.08 ± 0.01 | 22.51 ± 0.25 | 23.30 ± 0.20 | |||||
| A2 | 12.3 | 28.50 ± 0.26 | |||||||||
| A3 | 10.6 | 26.53 ± 0.12 | 26.60 ± 0.09 | ||||||||
| A4 | star | 7.3 | 23.88 ± 0.03 | 23.71 ± 0.02 | |||||||
| A5a | 2.5 | 27.20 ± 0.27 | 27.98 ± 0.18 | ||||||||
| A5ba | 2.1 | 28.16 ± 0.19 | |||||||||
| A5ca | 2.0 | 28.43 ± 0.22 | |||||||||
| A5d | 1.8 | 28.84 ± 0.30 | |||||||||
| A6a | 1.0 | 28.64 ± 0.26 | |||||||||
| A6b | 0.7 | 28.37 ± 0.24 | |||||||||
| A6c | 0.4 | 28.11 ± 0.19 | |||||||||
| A6d | 1.4 | 28.64 ± 0.26 | |||||||||
| A6e | 0.9 | 28.64 ± 0.26 | |||||||||
| A6f | 1.5 | 28.29 ± 0.20 | |||||||||
| A7 | star | 4.2 | 23.38 ± 0.03 | 22.84 ± 0.01 | 22.28 ± 0.15 | 22.78 ± 0.15 | |||||
| A8 | 6.3 | 27.49 ± 0.12 | |||||||||
| A9 | 9.8 | 27.38 ± 0.12 | |||||||||
| A10 | 11.5 | 27.10 ± 0.13 | |||||||||
| A11 b | z ~ 0.16?; z < 2.81 | 13.3 | |||||||||
| QSO c | z = 3.022 | 17.5 | 20.87 ± 0.05 | ~20.58 | |||||||
| Star c | star | 18.3 | 18.20 ± 0.04 | ||||||||
|
|
|||||||||||
| GRB 050820A (GRB: z = 2.615, DLA: z = 2.3598, Mg ii absorbers: z = 1.4288, 0.6915) | |||||||||||
| Candidate | Remark | θ (″) | g (mag) | F625W (mag) | R (mag) | F775W (mag) | F850LP (mag) | H (mag) | Ks (mag) | 3.6 μm (mag) | 5.8 μm (mag) |
|
|
|||||||||||
| B1d | 11.8 | 25.18 ± 0.04 | 24.87 ± 0.03 | 24.90 ± 0.06 | 23.45 ± 0.30 | ||||||
| B2 | z = 0.693 | 12.3 | 25.41 ± 0.07 | 23.59 ± 0.03 | 23.20 ± 0.03 | 22.35 ± 0.01 | 21.81 ± 0.05 | 20.81 ± 0.10 | 20.47 ± 0.05 | 20.59 ± 0.05 | 21.40 ± 0.20 |
| B3 |
|
5.2 | 25.24 ± 0.06 | 23.90 ± 0.04 | 23.65 ± 0.04 | 23.01 ± 0.02 | 22.57 ± 0.05 | 21.41 ± 0.14 | 21.05 ± 0.07 | 20.94 ± 0.06 | 21.04 ± 0.18 |
| B4 | star | 2.8 | 23.39 ± 0.05 | 22.11 ± 0.01 | 21.97 ± 0.03 | 21.68 ± 0.01 | 21.34 ± 0.01 | 20.94 ± 0.11 | 21.19 ± 0.07 | 21.65 ± 0.10 | 21.68 ± 0.32 |
| B5 | z = 0.9 ± 0.1 | 3.7 | 26.68 ± 0.14 | 26.36 ± 0.09 | 26.48 ± 0.26 | 25.58 ± 0.06 | 25.36 ± 0.06 | ||||
| B6 |
|
4.9 | 25.23 ± 0.06 | 24.94 ± 0.09 | 24.80 ± 0.09 | 24.32 ± 0.04 | 23.67 ± 0.05 | 22.28 ± 0.21 | 22.20 ± 0.15 | 21.81 ± 0.10 | |
| B7 a | z = 2.615 | 1.6 | 25.75 ± 0.08 | 25.99 ± 0.07 | 25.66 ± 0.10 | 25.90 ± 0.06 | 25.83 ± 0.08 | ||||
| B8N a | z = 2.615 | 0.3 | 26.16 ± 0.08 | 25.83 ± 0.08 | 26.18 ± 0.06 | ||||||
| B8S a | 0.1 | 26.19 ± 0.08 | 25.72 ± 0.07 | 25.82 ± 0.05 | |||||||
| B9 | z = 0.428 | 3.4 | 25.49 ± 0.07 | 24.94 ± 0.05 | 24.45 ± 0.07 | 24.76 ± 0.03 | 24.57 ± 0.04 | ||||
| B10 | star | 3.6 | 22.11 ± 0.05 | 20.58 ± 0.00 | 20.31 ± 0.03 | 19.69 ± 0.00 | 19.16 ± 0.00 | 18.60 ± 0.05 | 18.81 ± 0.04 | 19.51 ± 0.03 | 20.29 ± 0.09 |
Notes. Observed magnitudes are given in the AB system (not corrected
for Galactic extinction). VLT and Magellan Vega-magnitudes were
converted into the AB system by adding VLT/R 0.21 mag (Blanton & Roweis 2007),
VLT/Ks 1.895 mag (ESO), and
Magellan/H 1.34 mag. Selective Galactic
extinctions, E(B − V), are 0.051
and 0.044 mag, for GRBs 050730 and 050820A, respectively. Impact parameters were
derived from the HST images, if available, otherwise from R-band
images. The uncertainty in the impact parameter is
. Spectra were extracted
for boldfaced objects. Based on the spectrum, the SED or the shape and colour of an
object, we report in the column “remark” if it is a star or at which redshift the
galaxy is. The 3σ limiting magnitudes are GRB 050730:
R = 27.1, F775W = 28.6,
Ks = 22.8, 3.6 μm = 23.5,
5.8 μm = 21.5 mag, GRB 050820A: g′ = 27.6,
F625W = 27.8, R = 26.1,
F775W = 28.1,
F850LP = 28.0, H = 23.0,
Ks = 23.0, 3.6 μm = 23.5,
5.8 μm = 21.7 mag.
Blended object. The magnitude is only an estimate. The spectrum can be the integrated spectrum of the blended objects.
The object consists of at least two galaxies and is detected in all filters. We do not report any magnitude of the individual objects or the compound in this work. We detect the continuum down to 4630 Å. If this break is caused by Lyα absorption, the redshift is z = 2.81; alternatively if this is the redshifted 4000 Å feature, the redshift is z = 0.16.
The R-band brightness of the quasar and the star were obtained from an afterglow image taken on 23 February 2007 using PSF photometry (Sect. 2.2.1). The blended star is saturated in the HST image. The PSF was subtracted with the tool Tiny Tim (Krist 1993) assuming a FWHM of 5″. While the wings of the star were partly removed, the residuals in the core are quite strong. The measurement of the QSO magnitude is only an estimate.
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