Table 2
grasil fitting results.
| GRB host | SFR(UV)a | SFR(IR)a | A V | log | Herschel | log | log | log | T dust | Modified blackbody fits |
| galaxy | (M⊙ yr-1) | (M⊙ yr-1) | (mag) | L IR | detected? |
|
|
M dust | (grasil) | log(Mdust) |
| (L⊙) | (M⊙) | (M⊙) | (M⊙) | (K) | (M⊙) | |||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) |
|
|
||||||||||
| 970828 | 0.3 | 14.4 | 2.38 | 11.18 | No | 9.80 | 8.96 | − | 38.7 | <8.21 |
| 980613 | 1.5 | 39.5 | 1.94 | 11.62 | Yes | 9.31 | 9.28 | 7.53 | 71.5 | − |
| 980703 | 2.7 | 86.4 | 1.94 | 11.96 | No | 9.98 | 9.60 | − | 38.7 | <8.65 |
| 990705 | 2.3 | 6.6 | 0.16 | 10.84 | No | 10.50 | − | − | 28.5 | <8.18 |
| 020127 | 2.7 | 56.3 | 0.39 | 11.77 | No | 11.51 | 9.54 | − | 61.3 | <9.01 |
| 020819B | 3.5 | 13.0 | 0.54 | 11.13 | Yes | 10.52 | − | 8.99 | 24.4 | − |
| 030115 | 1.6 | 159.1 | 1.95 | 12.22 | No | 10.87 | 9.85 | − | 33.2 | <9.53 |
| 050219A | <0.1 | <0.1 | 0.00 | 8.29 | No | 9.91 | − | − | 47.2 | <6.37 |
| 050223 | 1.9 | 1.7 | 0.21 | 10.25 | No | 10.02 | − | − | 21.0 | <7.87 |
| 051022 | 4.8 | 17.9 | 0.56 | 11.27 | Yes | 10.29 | 9.28 | 7.27 | 52.6 | − |
| 060904A | 1.1 | 303.9 | 4.17 | 12.50 | No | 10.18 | 10.17 | <8.41 | 132.0 | − |
| 070306 | 9.6 | 144.1 | 1.65 | 12.18 | Yes | 10.05 | 9.97 | 8.29 | 52.6 | − |
| 071021 | 2.6 | 288.2 | 1.72 | 12.48 | No | 11.40 | 10.15 | − | 33.2 | <9.50 |
| 080207 | 1.0 | 170.1 | 1.69 | 12.25 | Yes | 11.17 | 10.16 | 8.15 | 61.3 | − |
| 080325 | 1.2 | 66.5 | 1.03 | 11.84 | Yes | 11.09 | 9.62 | 8.06 | 52.6 | − |
| 090404 | 3.1 | 380.8 | 2.28 | 12.60 | No | 11.10 | 10.30 | − | 52.6 | <9.93 |
| 090417B | 0.2 | 1.7 | 0.54 | 10.25 | Yes | 9.73 | − | 8.18 | 21.0 | − |
Notes.
The SFRs and stellar masses have been converted to a Chabrier (2003) IMF by dividing by a factor of 1.8. Column (2): SFR inferred from SED fitting and rest-frame UV, uncorrected for extinction; Col. (3): SFR inferred from the IR emission from radiation reprocessed by dust; Col. (4): total AV obtained by considering the total attenuation in both the diffuse ISM and the dense molecular cloud components as described in the text; Col. (5): total IR luminosity from dust emission; Col. (7): total stellar mass of the galaxy; Col. (8): stellar mass of the burst episode assumed to have onset 50 Myr ago; Col. (9): total dust mass of the galaxy; Col. (10): luminosity-weighted mean dust temperature as given by grasil; Col. (11): the fixed-temperature (T = 35 ± 1 K) fixed-emissivity (β = 2.0) MBB fits are given when the grasil fit does not give a realistic upper limit.
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