Table 1.
Perseus cluster jellyfish galaxies.
| Name | RA (a) | Dec (a) | Redshift (a) | Mstar (b) | SFR (b) | R/R500 (c) | Δv (d) | f144 MHz (e) | fHα + [NII] |
|---|---|---|---|---|---|---|---|---|---|
| [deg] | [deg] | [109 M⊙] | [M⊙ yr−1] | [km s−1] | [mJy] | [10−13 erg s−1 cm2] | |||
| LEDA 2191078 | 49.14133 | 42.02572 | 0.0136 |
 |
 |
0.80 | 1289 | 19.8 ± 3.6 | 0.82 ± 0.08 |
| MCG +07-07-070 | 50.09175 | 41.64072 | 0.0125 |
 |
 |
0.17 | 1618 | 40.8 ± 5.7 | 1.92 ± 0.19 |
| UGC 2654 | 49.67958 | 42.30058 | 0.0193 |
 |
 |
0.82 | 427 | 109.4 ± 12.7 | 1.48 ± 0.16 |
| UGC 2665 | 49.86404 | 41.63531 | 0.0260 |
 |
 |
0.14 | 2441 | 21.5 ± 5.6 | 2.09 ± 0.21 |
Notes.
Computed using calibrations from Leroy et al. (2019). Stellar masses are determined from a combination of WISE1 luminosity with a mass-to-light ratio set according to WISE1-WISE4 color. SFRs are determined from WISE4 luminosity.
Projected offset from NGC 1275, we take R500 = 1.3 Mpc (Urban et al. 2014).
Includes all emission within the 3σ contour. Uncertainties include a noise contribution and a 10% LoTSS DR2 calibration uncertainty (Shimwell et al. 2022) added in quadrature.
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