Table 1
Existing radio follow-up observations of TDF candidates that were discovered at optical to soft X-ray frequencies (our new observations are shown in Table 2).
| Name | tD | Fν | ν | Δt |
| (yr) | (mJy) | (GHz) | (yr) | |
|
|
||||
| NGC 59051 | 1990.5 | <0.15 | 8.5 | 6.0 |
| D3−132 | 2004.5 | <0.15 | 1.4 | 1.8 |
| TDE23 | 2007.8 | <0.10 | 8.4 | 1.1 |
| CSS1002174 | 2010.2 | 0.50 ± 0.03 | 7.9 | 0.3 |
| SDSS J1201+305 | 2010.4 | <0.22 | 4.8 | 1.4 |
|
|
||||
| RX J1624+75546 | 1990.8 | <0.085 | 3.0 | 21.8 |
| IC 35997 | 1990.9 | 0.19 ± 0.03 | 3.0 | 21.6 |
| RX J1420+53348 | 1990.9 | 0.11 ± 0.02 | 3.0 | 21.6 |
| RX J1242−11199 | 1992.5 | <0.090 | 3.0 | 20.0 |
| SDSS J1323+4810 | 2003.9 | <0.170 | 3.0 | 8.6 |
| SDSS J1311−0111 | 2004.1 | <0.095 | 3.0 | 8.4 |
Notes.In the third column we show 5-σ upper limits on the radio flux or the detected flux and 1-σ uncertainty. Δt denotes the time of the radio observation with respect to the estimated time of disruption (tD). The radio observation of the first five candidates were published before mid-2012, the last six are taken from Bower et al. (2013). We note that most of the TDF candidates that were discovered in the nineties also have post disruption radio upper limits from large radio surveys (e.g., NVSS, Condon et al. 1998), these are listed in Komossa (2002).
Reference. 1) Bade et al. (1996), Komossa (2002), 2) Gezari et al. (2008), Bower (2011), 3) van Velzen et al. (2011a), 4) Drake et al. (2011), 5) Saxton et al. (2012), 6) Grupe et al. (1999), 7) Komossa & Bade (1999), 8) Komossa & Greiner (1999), 9) Komossa & Greiner (1999), 10) Esquej et al. (2007), 11) Maksym et al. (2010).
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