Table 3.
Multi-wavelength properties of the TDEs in our sample.
| TDE | Class | X-ray | Infrared | Radio | Notes | Ref. |
|---|---|---|---|---|---|---|
| OGLE16aaa | H + He | ✓(delayed) | ✗ | ? | • X-ray bright while polarised | [1][*] |
| Sw 1644+57 | ✓(early) | ✗ | ✓ | • Relativistic / jetted TDE | [2][*][3] | |
| Sw 2058+05 | ✓(early) | ✗ | ✓ | • Relativistic / jetted TDE | [4][*][5] | |
| AT 2018dyb | H + He | ✗ | ✓ | ✓ | • Polarisation decreases with time, | [6][7,8][9] |
| line depolarisation | ||||||
| AT 2018hyz | H + He | ✓(early) | ✓ | ✓ | • Double-peaked emission lines | [10][7][11] |
| AT 2019azh | H + He | ✓(delayed) | ✓ | ✓ | • Line depolarisation | [12][7,8][13,14] |
| AT 2019dsg | H + He | ✓(delayed) | ✓ | ✓ | • Polarisation decreases with time, | [15][8,16] |
| line depolarisation | [17,18] | |||||
| AT 2019lwu | H | ✗ | ✗ | ✗ | [†][*][13] | |
| AT 2019qiz | H + He | ✓(delayed) | ✓ | ✓ | • Polarisation increases with time, | [19][16][13] |
| line depolarisation | ||||||
| AT 2020mot | H + He | ✗ | ✓ | ✗ | • ∼25% polarisation | [20][21][13] |
| AT 2020zso | H + He | ✗ | ✗ | ✗ | • Polarisation decreases with time, | [22][*][13] |
| double-peaked emission lines | ||||||
| AT 2021blz | H + He | ✓(delayed) | ✗ | ✗ | • Roughly constant polarisation, | [23][*][13] |
| line depolarisation | ||||||
| AT 2022cmc | ✓(early) | ✗ | ✓ | • Relativistic / jetted TDE | [24,25][*] | |
| AT 2022bdw | H + He | ✗ | ✗ | ✗ | • Low polarisation at peak light | [†][*][13] |
| AT 2022dsb | H + He | ✓(early) | ✗ | ✗ | • Polarisation decreases with time, | [26][*][13] |
| line depolarisation | ||||||
| AT 2022exr | H | ✓(delayed) | ✗ | ? | • Double-peaked optical light curve | [27][*][13] |
| AT 2022hvp | He | ✗ | ✗ | ? | [†][*] | |
| AT 2023clx | H + He | ✓(delayed) | ✗ | ✓ | • Line depolarisation, dust | [28][*][29] |
| polarisation via light echo | ||||||
| AT 2023mhs | H | ✓(delayed) | ✗ | ? | • Roughly constant polarisation, | [†][*] |
| wavelength-dependent continuum |
Notes. The second column provides the spectroscopic subtype. In columns 3–5, a tick mark indicates the TDEs in our sample were detected in X-rays, mid-infrared, or radio, whereas a cross indicates non-detections. The information in this table is based on publicly available data, provided by the references in the final column. In some cases, it is unknown whether there are any observations of a TDE, in which case we put down a question mark. For the X-ray detections, we specify whether the X-rays peaked before or during the optical peak (‘early’) or after (‘delayed’). Swift J164449.3+573451 and Swift J2058+0516 have been abbreviated to Sw 1644+57 and Sw 2058+05. [1] Kajava et al. (2020), [2] Mangano et al. (2016), [3] Cendes et al. (2021b), [4] Cenko et al. (2012), [5] Pasham et al. (2015), [6] Holoien et al. (2020), [7] Jiang et al. (2021), [8] Leloudas et al. (2022), [9] Cendes et al. (2024), [10] Gomez et al. (2020), [11] Cendes et al. (2022), [12] Hinkle et al. (2020), [13] Anumarlapudi et al. (2024), [14] Goodwin et al. (2022), [15] Cannizzaro et al. (2021), [16] van Velzen et al. (2024), [17] Cendes et al. (2021a), [18] Stein & Velzen (2021), [19] Nicholl et al. (2024), [20] Liodakis et al. (2023), [21] Newsome et al. (2024), [22] Wevers et al. (2022), [23] Liu et al. (2021), [24] Andreoni et al. (2022), [25] Pasham et al. (2023), [26] Malyali et al. (2024), [27] Guolo et al. (2022), [28] Zhu et al. (2023), [29] Sfaradi et al. (2023). †X-ray observations analysed in this work; see Table D.1. *NEOWISE IR light curve inspected in this work.
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