Table 2
Properties of the multiply-imaged galaxies behind A370.
| Imagesa | z | Δt | Δm1 | Δm2 | rCC × 102 | rIa × 103 | Detectable SN types | ||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (d) | (mag) | (yr−1) | Ia | IIP | IIL | IIn | Ib | Ic | faintb | ||||
| CC SNe | |||||||||||||
| 1.2 + 1.1 | 0.80 | 2350(70) | 1.78(0.05) | 2.80(0.07) | 0.06(0.03) | 0.04(0.02) | y | y | y | y | y | y | y |
| 1.2 + 1.3 | 0.80 | 2400(70) | ⋯ | 2.81(0.08) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| 2.1 + 2.2 | 0.73 | 143 (17) | 2.44(0.06) | 2.11(0.05) | 0.90(0.05) | 0.54(0.04) | y | y | y | y | y | y | y |
| 2.1 + 2.3 | 0.73 | 89(17) | ⋯ | 2.75(0.07) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| 2.1 + 2.4 | 0.73 | 92(17) | ⋯ | 4.11(0.10) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| 2.1 + 2.5 | 0.73 | 61(17) | ⋯ | 4.23(0.10) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| 3.3 + 3.1 | 1.95 | 660(60) | 2.40(0.07) | 3.59(0.19) | 0.31(0.13) | 0.18(0.07) | y | y | y | y | y | y | y |
| 3.3 + 3.2 | 1.95 | 910(100) | ⋯ | 3.69(0.18) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| 4.3 + 4.1 | 1.27 | 800(90) | 1.45(0.03) | 1.62(0.05) | 0.64(0.19) | 0.36(0.11) | y | y | y | y | y | y | y |
| 4.3 + 4.2 | 1.27 | 7080(70) | ⋯ | 1.74(0.05) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| 5.4 + 5.1 | 1.28 | 94(4) | 4.21(0.13) | 2.99(0.08) | 0.12(0.02) | 0.07(0.01) | y | y | y | y | y | y | y |
| 5.4 + 5.2 | 1.28 | 104(8) | ⋯ | 4.09(0.09) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| 5.4 + 5.3 | 1.28 | 135(7) | ⋯ | 4.27(0.12) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| 6.3 + 6.1 | 1.06 | 8320(110) | 1.41(0.03) | 1.68(0.04) | 3.16(0.16) | 2.06(0.20) | y | y | y | y | y | y | y |
| 6.3 + 6.2 | 1.06 | 6720(100) | ⋯ | 1.71(0.04) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| *7.4 + 7.1 | 2.75 | 36520(300) | 1.29(0.04) | 2.79(0.17) | 4.70(1.5) | 2.7(0.8) | y | y | y | y | y | y | y |
| *7.4 + 7.2 | 2.75 | 36560(300) | ⋯ | 2.80(0.16) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| *7.4 + 7.3 | 2.75 | 34650(300) | ⋯ | 1.14(0.04) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| *7.4 + *7.5 | 2.75 | 31040(300) | ⋯ | 1.57(0.04) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| 9.3 + 9.1 | 1.52 | 10830(170) | 1.52(0.03) | 1.48(0.03) | 0.11(0.03) | 0.06(0.01) | y | y | y | y | y | y | y |
| 9.3 + 9.2 | 1.52 | 15500(160) | ⋯ | 1.61(0.03) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| *14.5 + 14.1 | 3.13 | 32930(170) | 0.89(0.03) | 2.37(0.06) | 0.33(0.11) | 0.19(0.06) | y | y | y | y | |||
| *14.5 + 14.2 | 3.13 | 33010(190) | ⋯ | 0.88(0.07) | ⋯ | ⋯ | y | y | y | y | |||
| *14.5 + 14.3 | 3.13 | 30320(180) | ⋯ | 1.87(0.04) | ⋯ | ⋯ | y | y | y | y | |||
| *14.5 + *14.4 | 3.13 | 25800(170) | ⋯ | 1.96(0.06) | ⋯ | ⋯ | y | y | y | y | |||
| *15.5 + 15.1 | 3.71 | 23090(150) | 1.06(0.02) | 0.97(0.02) | 0.23(0.04) | 0.13(0.02) | y | y | y | ||||
| *15.5 + 15.2 | 3.71 | 18990(130) | ⋯ | 1.34(0.04) | ⋯ | ⋯ | y | y | y | ||||
| *15.5 + 15.3 | 3.71 | 22950(150) | ⋯ | 1.97(0.06) | ⋯ | ⋯ | y | y | y | ||||
| *15.5 + *15.4 | 3.71 | 4980(250) | ⋯ | 1.61(0.04) | ⋯ | ⋯ | y | y | y | ||||
| *16.3 + 16.1 | 3.77 | 13160(200) | 1.50(0.03) | 2.63(0.07) | 0.07(0.04) | 0.04(0.02) | y | y | y | ||||
| *21.3 + 21.1 | 1.26 | 12230(130) | 1.27(0.03) | 3.73(0.09) | 0.24(0.13) | 0.14(0.08) | y | y | y | y | y | y | y |
| *21.3 + 21.2 | 1.26 | 12300(130) | ⋯ | 3.89(0.10) | ⋯ | ⋯ | y | y | y | y | y | y | y |
| *22.3 + 22.1 | 3.13 | 26940(210) | 0.91(0.03) | 2.25(0.06) | 0.15(0.08) | 0.08(0.05) | y | y | y | y | |||
| *22.3 + *22.2 | 3.13 | 2260(140) | ⋯ | 2.19(0.06) | ⋯ | ⋯ | y | y | y | y | |||
Notes. Time delays (Δt) of the multiply-imaged galaxies as predicted from the lensing model in L17 are listed in Col. 3. The time delays are measured relative to the first image in Col. 1. The reference image in each case is that with the shortest path length between the galaxy and us. The time delays are with respect to the reference image. The magnifications of the images in Col. 1 are given in magnitudes in Cols. 4 and 5, and are computed using the lensing model in L17. Estimates of the core-collapse and SN Ia rates are given with 1σ errors in Cols. 6 and 7, respectively. Given that the SFR of the galaxy depends on the luminosity of the galaxy, it is dependent of the predicted magnification, thus the lensing model. In Cols. 8–14, the detectability of a lensed SN for the different SN types assuming a 27.5 mag in F150W, e.g. in a survey using 1 h exposure of the JWST/NIRCam instrument. In order to be observable, the luminosity of both images must lie above the observation threshold. (a)Images labeled with an asterisk (*) do not have spectroscopic redshifts. (b)Population of intrinsically faint CC SNe (MB > −15) which could be contributing importantly in the CC SN rates. See e.g. Strolger et al. (2015) for a discussion.
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