Table 2
Summary of the darkness properties of our sample.
| # | GRB | Time (s) | UL | Filter | ULR | Ref. | β OX | β X | Δmin | Comments |
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) |
|
|
||||||||||
| 1 | 050717 | 420 | 19.0 | v | 18.2 | [1] | < 0.40 |
|
−0.20 | a; b |
| 2 | 050922B | 49 000 | 22.5 | r ′ | 22.3 | [2] | < 0.39 |
|
0.61 | c |
| 3 | 060211A | 19 980 | 22.0 | R C | 21.8 | [3] | < 0.71 |
|
−0.18 | – |
| 4 | 060805A | 63 000 | 22.9 | r ′ | 22.7 | [4] | < 1.00 |
|
−0.63 | – |
| 5 | 060919 | 918 | 20.2 | v | 19.8 | [5] | < 0.68 |
|
−0.70 | a |
| 6 | 060923B | 295 | 18.5 | v | 17.9 | [6] | < 0.62 |
|
−0.37 | b |
| 7 | 061102 | 1480 | 20.5 | v | 20.1 | [7] | < 1.10 |
|
−1.50 | d |
| 8 | 070429A | 44 064 | 24.0 | R C | 23.8 | [8] | < 0.42 |
|
0.14 | •; g |
| 9 | 070517 | 57 600 | 24.5 | i ′ | 24.3 | [9] | < 0.56 | 1.27 |
−0.09 | f |
| 10 | 080207 | 5364 | 20.3 | R C | 20.5 | [10] | < 0.26 |
|
0.56 | • |
| 11 | 080218B | 11 520 | 24.7 | r ′ | 24.3 | Table A.3 | < 0.18 |
|
0.46 | • |
| 12 | 080602 | 504 | 20.3 | v | 20.2 | [11] | < 0.05 |
|
0.34 | e |
| 13 | 080727A | 2268 | 19.8 | K | 22.8 | [12] | < 0.85 |
|
−0.05 | – |
| 14 | 080915A | 6840 | 22.1 | I C | 22.1 | [13] | < 0.62 |
|
0.08 | d |
| 15 | 081012 | 69 660 | 23.5 | r ′ | 23.4 | Table A.3 | < 0.83 |
|
−1.11 | – |
| 16 | 081105 | 46 224 | 23.0 | r ′ | 22.8 | Table A.3 | < 0.61 |
|
−0.21 | d |
| 17 | 081204 | 34 560 | 24.1 | r ′ | 23.9 | Table A.3 | < 0.55 |
|
0.11 | d |
Notes. Columns: (3 to 5) Time after the burst and reported upper limits (UL) of the afterglow (observed magnitudes); r′-band magnitudes are given in the AB system, all others in the Vega/UVOT system. (6) Deduced UL in the RC band (AB system) after correcting for Galactic extinction and shifting from the native filter wavelength (Col. 5) to the RC band using the upper limit to βOX. (8) If βOX < 0.5, then a burst is dark according to J04. (10) The minimum value (based on the 90% confidence error of βX) of the quantity Δ = βX − βOX − 0.5. If Δmin > 0, then a burst is dark according to V09. (11) (a) During the time of the observed UL the SED in the X-ray band is not constant. (b) The observed UL lies close to the end of the prompt GRB phase. (c) No X-ray data exist for the time when the UL was obtained. (d) Very faint X-ray flux; no well-defined X-ray light curve. (e) Flat X-ray light curve during the time when the UL was obtained. (f) The optical afterglow was detected; see Sect. 3.3. (g) No UL is reported in the corresponding GCN (Price 2007). We used RC = 24.0 based on the original data, which are available in the Gemini archive. A bullet (•) indicates that the burst is truly dark according to J04 and V09 (Sect. 2.3). Column (7; references): 1) Blustin et al. (2005); 2) Guziy et al. (2005); 3) Sharapov et al. (2006); 4) Rol & Page (2006); 5) Breeveld & Guidorzi (2006); 6) Holland & Cucchiara (2006); 7) Holland (2006); 8) Price (2007); 9) Fox et al. (2007); 10) Andreev et al. (2008); 11) Beardmore et al. (2008e); 12) Levan & Wiersema (2008); 13) Rossi et al. (2008c).
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