Table 5
Summary of the properties of the objects found in the XRT error circles.
| # | GRB | Object | R-band size | Ks-band size | Comment | (R − K)AB | (R − K)Vega | XRTpos | p | p ERO |
|
|
||||||||||
| 1 | 050717 | •A | 2.1 × 3.9 | not visible | G | <2.08 | <3.70 | 2 | 0.05 ± 0.01 | |
| •B | 1.2 × 1.3 | not visible | <2.93 | <4.55 | 1 | 0.03 ± 0.01 | ||||
| 2 | 050922B | no candidates | ||||||||
| 3 | 060211A | •A | 1.1 × 1.2 | not visible | G | <2.53 | <4.16 | 1 | 0.03 ± 0.01 | |
| B | 3.8 × 2.2 | 3 sources | G | 1.21 | 2.84 ± 0.21 | 3 | 0.07 ± 0.01 | |||
| •C | only in J | – | G | – | – | 1 | – | |||
| •D | only in J | – | – | – | – | 2 | – | |||
| 4 | 060805A | •A | 1.5 × 1.1 | not visible | G | <4.3 | <5.9 | 1 | 0.09 ± 0.04 | |
| •B | 2.7 × 1.3 | not visible | G | <2.5 | <4.1 | 2 | 0.09 ± 0.01 | |||
| 5 | 060919 | •A | 1.5 × 1.4 | not visible | <2.60 | <4.23 | 1 | 0.15 ± 0.03 | ||
| 6 | 060923B | •A | 2.1 × 2.2 | 2.2 × 1.8 | G | 1.05 | 2.68 ± 0.14 | 2 | 0.06 ± 0.01 | |
| B | 2.0 × 2.0 | 1.9 × 1.9 | S | 2.43 | 4.06 ± 0.04 | 2 | – | |||
| •C | 1.1 × 1.0 | 0.8 × 0.8 | 1.33 | 2.96 ± 0.16 | 1 | 0.04 ± 0.01 | ||||
| •D | 1.3 × 1.3 | 0.8 × 0.8 | 3.82 | 5.45 ± 0.13 | 2 | 0.37 ± 0.03 | 0.04 ± 0.01 | |||
| •E | blended with A | blended with A | 1 | – | ||||||
| 7 | 061102 | •A | 2.5 × 1.5 | not visible | G | <1.22 | <2.85 | 2 | 0.34 ± 0.01 | |
| •B | 1.8 × 1.9 | not visible | G | <1.08 | <2.71 | 2 | 0.31 ± 0.01 | |||
| 8 | 070429A | A | 3.8 × 1.4 | 1.9 × 1.1 | G | 2.10 | 3.73 ± 0.32 | 3 | 0.54 ± 0.05 | |
| •B | 2.8 × 1.4 | blended with C | G | 1.41 | 3.04 ± 0.23 | 1 | 0.04 ± 0.01 | |||
| •C | 1.7 × 1.5 | 1.5 × 1.0 | G | 2.09 | 3.72 ± 0.16 | 1 | 0.05 ± 0.01 | |||
| •D | not visible | 1.6 × 1.0 | G | >3.2 | >4.8 | 2 | – | 0.07 ± 0.01 | ||
| 9 | 070517 | •A | 1.6 × 1.3 | not visible | G | <1.69 | <3.32 | 1 | 0.07 ± 0.03 | |
| 10 | 080207 | A | 2.4 × 1.3 | not visible | G | 2.08 | 3.71 ± 0.43 | 2 | 0.20 ± 0.02 | |
| •B | 2.1 × 1.1 | 1.6 × 0.9 | G | 4.66 | 6.29 ± 0.40 | 1 | 0.14 ± 0.04 | 0.01 ± 0.01 | ||
| 11 | 080218B | •A | 2.5 × 1.1 | 1.4 × 0.7 | G | 4.15 | 5.78 ± 0.16 | 1 | 0.12 ± 0.01 | 0.01 |
| B | 1.6 × 1.5 | 0.8 × 0.8 | 1.54 | 3.17 ± 0.24 | 3 | 0.28 ± 0.01 | ||||
| 12 | 080602 | •A | 2.6 × 2.0 | 1.2 × 0.8 | G | 0.34 | 1.97 ± 0.05 | 1 | 0.01 ± 0.01 | |
| B | 2.0 × 1.8 | not visible | G | <0.44 | <2.07 | 2 | 0.13 ± 0.01 | |||
| •C | not visible | 1.2 × 0.8 | G | >4.35 | >5.98 | 2 | – | 0.04 ± 0.01 | ||
| 13 | 080727A | no candidates | ||||||||
| 14 | 080915A | A | 3.5 × 3.5 | 1.2 × 1.2 | S | 1.11 | 2.74 ± 0.02 | 1 | – | |
| B | 5.6 × 4.5 | 3.4 × 1.8 | G | 1.99 | 3.62 ± 0.01 | 3 | 0.16 ± 0.01 | |||
| •C | 1.2 × 1.2 | not visible | G | <1.21 | <2.83 | 1 | 0.23 ± 0.02 | |||
| •D | 1.2 × 1.2 | not visible | G | <1.07 | <2.69 | 2 | 0.61 ± 0.02 | |||
| •E | 1.5 × 1.5 | not visible | <1.94 | <3.57 | 1 | 0.37 ± 0.04 | ||||
| 15 | 081012 | •A | 1.8 × 1.5 | not visible | G | <1.21 | <2.84 | 2 | 0.31 ± 0.03 | |
| 16 | 081105 | A | 1.2 × 1.2 | 1.0 × 1.0 | G | 0.89 | 2.51 ± 0.20 | 1 | 0.19 ± 0.01 | |
| B | 1.1 × 1.1 | 0.8 × 0.8 | 2.15 | 3.78 ± 0.19 | 1 | 0.29 ± 0.02 | ||||
| •C | not visible | 0.8 × 0.5 | G | >3.50 | >5.13 | 1 | – | 0.08 ± 0.01 | ||
| 17 | 081204 | A | 2.1 × 1.4 | 0.9 × 0.5 | G | 0.78 | 2.40 ± 0.16 | 1 | 0.16 ± 0.01 | |
| B | 2.7 × 1.4 | 1.1 × 0.8 | G | 1.81 | 3.43 ± 0.09 | 1 | 0.19 ± 0.01 | |||
| C | 2.2 × 1.7 | 0.9 × 0.6 | G | 1.04 | 2.66 ± 0.13 | 2 | 0.49 ± 0.02 | |||
| D | 1.2 × 1.2 | 0.5 × 0.5 | 1.97 | 3.59 ± 0.18 | 2 | 0.78 ± 0.03 | ||||
| E | 1.2 × 1.2 | not visible | <−0.04 | <1.59 | 2 | 0.81 ± 0.03 | ||||
| •F | ~1 | 0.6 × 0.6 | G | 3.1 | 4.7 ± 0.50 | 1 | 0.43 ± 0.12 | 0.09 ± 0.01 | ||
| G | blended with a star | 1.5 × 1.5 | – | – | 2 | – | ||||
Notes. (1) A bullet (•) in Col. #2 indicates the most likely GRB host candidate. If more than one candidate is marked then we cannot determine which is the best. For details about the selection, see Sect. 3.3. GRBs that are truly dark according to J04 and V09 are highlighted in boldface. (2) Angular sizes are given in units of arcsec. (3) Magnitude errors in (R − K)AB are identical to the corresponding errors for (R − K)Vega. Colors are corrected for Galactic extinction. (4) The last two columns gives the chance probability p of finding a galaxy of the corresponding extinction-corrected (Vega) R-band magnitude on the sky in a region with the size of the corresponding X-ray error circle with a radius r = XRTpos × r0 (Eq. (1)). Thereby, the first column refers to number counts of galaxies of all kinds. If the object is for sure a star, then no value is given. The second column refers to number counts of EROs only (see Sect. 4.8). (5) Comment “G” stands for galaxy, “S” for star; if no letter is given then we could not determine if this is a star or a galaxy. (6) In case of GRB 070517, the probability p is based on the distance between the afterglow and galaxy A (
; Sect. 3.3). GRB 070429A/object D, and GRB 081204/object F are EROs within the large 1σ photometric error (see Table 3).
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