Table B.1.
Long-duration GRB host galaxies detected in radio so far.
| GRB | z | ν | Fν | Lν | SFR | Ref. |
|---|---|---|---|---|---|---|
| (GHz) | (μJy beam−1) | (erg s−1 Hz−1) | M⊙ yr−1 | |||
| 980425 | 0.0085 | 1.38 | 840±160 | (1.4±0.3) × 1027 | 0.08±0.02 | Michałowski et al. (2012) |
| 980703 | 0.967 | 1.43 | 76±10 | (3.2±0.4) × 1030 | 206±27 | Berger et al. (2001) |
| 000418 | 1.119 | 1.43 | 69±15 | (4.1±0.9) × 1030 | 264±57 | Berger et al. (2003) |
| 020819B | 0.41 | 3.0 | 31±8 | (1.7±0.4) × 1029 | 20±5 | Greiner et al. (2016) |
| 021211 | 1.006 | 1.43 | 330±31 | (1.5±0.1) × 1031 | 982±82 | Michałowski et al. (2012) |
| 031203a | 0.105 | 1.39 | 254±46 | (7±1) × 1028 | 4.5±0.8 | Michałowski et al. (2012) |
| 050223 | 0.591 | 5.5 | 90±30 | (1.2±0.4) × 1030 | 210±70 | Stanway et al. (2014) |
| 051006 | 1.059 | 3.0 | 9±3 | (5±2) × 1029 | 53±18 | Perley et al. (2015) |
| 051022 | 0.809 | 5.23 | 13±4 | (4±1) × 1029 | 61±19 | Perley & Perley (2013) |
| 060505 | 0.089 | 1.38 | 76±35 | 1.5±0.7×1028 | 0.9±0.4 | Michałowski et al. (2015) |
| 060729b | 0.54 | 5.5 | 65±28 | (7±3) × 1029 | 123±53 | Stanway et al. (2014) |
| 060814 | 1.92 | 3.0 | 11±3 | (2.3±0.6) × 1030 | 258±70 | Perley et al. (2015) |
| 061121 | 1.314 | 3.0 | 17±5 | (1.5±0.4) × 1030 | 165±48 | Perley et al. (2015) |
| 070306 | 1.496 | 3.0 | 11±3 | (1.3±0.4) × 1030 | 145±39 | Perley et al. (2015) |
| 080207 | 2.086 | 5.23 | 17±2 | (4.3±0.5) × 1030 | 731±86 | Perley & Perley (2013) |
| 080517 | 0.089 | 4.5 | 220±40 | (4.4±0.8) × 1028 | 7±1 | Stanway et al. (2015) |
| 090404d | 3.0 | 5.23 | 11±3 | (6±2) × 1030 | 1074±293 | Perley & Perley (2013) |
| 100316D | 0.059 | 1.38 | 657±21 | (5.5±0.2) × 1028 | 3.5±0.1 | Michałowski et al. (2015) |
| 100621Ac | 0.542 | 5.5 | 120±32 | (1.3±0.3) × 1030 | 229±61 | Stanway et al. (2014) |
| 111005A | 0.013 | 1.38 | 245±30 | (9±1) × 1026 | 0.06±0.01 | Michałowski et al. (2015) |
| 200716C | 0.341 | 1.4 | 1380±40 | (5.1±0.2) × 1030 | 324±61 | This work |
Notes.Column 1: GRB name. Column 2: redshift. Column 3: observing frequency (GHz). Column 4: Flux density (μJy beam−1) referred to the observing frequency. Column 5: monochromatic luminosity (erg s−1 Hz−1). Column 6: SFR calculated with the formula provided by Greiner et al. (2016). Column 7: References. The uncertainties on the monochromatic luminosity and the SFR are derived with the standard formula for the propagation of errors. a We used the flux density measurement at 1.39 GHz from Michałowski et al. (2012), while the SFR from Greiner et al. (2016) is derived from the flux density at 5.5 GHz. b We used the flux density value from Stanway et al. (2014) at 5.5 GHz, while Greiner et al. (2016) derived an upper limit for the SFR using the upper limit for the flux density at 1.39 GHz from Michałowski et al. (2012). c We used the flux density at from Stanway et al. (2014), while Greiner et al. (2016) used an upper limit for the flux density at 2.1 GHz. d Even though the host galaxy of GRB 090404 was detected by Perley & Perley (2013), the authors stated that an afterglow origin for the observed detection could not be ruled out.
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