Table 3.
M87* large-scale quantities measured by ALMA and horizon-scale quantities measured by the EHT over the years in the 226–230 GHz band.
| Year | FALMA | RMALMA | Stokes ℐ PA (η) | ⟨|m|⟩ | ∠β2 |
|---|---|---|---|---|---|
| month, day | (Jy) | (105 rad m−2) | (deg) | (%) | (deg) |
| 2017 | |||||
| April 5 | 1.27 ± 0.13 | 1.2 ± 0.3 | [150, 200] | [5.7, 10.7] | [ − 163, −127] |
| April 11 | 1.30 ± 0.13 | −0.3 ± 0.2 | [150, 183] | ||
| 2018† | |||||
| April 21 | 1.05 ± 0.11 | −4.3 ± 0.3 | [209, 222] | [2.0, 3.6] | [ − 156, −99] |
| 2021 | |||||
| April 13 | 1.31 ± 0.13 | −3.7 ± 0.4 | [192, 208] | [2.8, 3.9] | [155, 165] |
| April 18 | 1.41 ± 0.14 | −1.6 ± 0.3 | [200, 208] | [3.0, 4.7] | [156, 168] |
Notes. From ALMA we quote the flux density (F) and rotation measure (RM). These ALMA measurements were obtained using a calibration procedure similar to that described in Goddi et al. (2019), but with additional refinements. These include Tsys-based opacity corrections for the amplitude scale and residual X − Y delay corrections for polarization calibration (see Carlos et al., in prep., for details). As a result, the derived FALMA and RMALMA values for the 2017 and 2018 datasets differ slightly from those reported in Goddi et al. (2021), although they remain consistent within 1σ uncertainties. †In 2018, the source underwent a very high-energy γ-ray flare between April 18 and 24 (M87 MWL2018).
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