Table 1.
Distance estimates for NGC 6397.
| Authors | Method | Observations | Distance |
|---|---|---|---|
| (kpc) | |||
| Harris (2010) | CMD | Various | 2.3 |
| Reid & Gizis (1998) | CMD | HST | 2.67 ± 0.25 |
| Gratton et al. (2003) | CMD | VLT | 2.53 ± 0.05 |
| Hansen et al. (2007) | CMD | HST | 2.55 ± 0.11 |
| Dotter et al. (2010) | CMD | HST | 3.0 |
| Heyl et al. (2012) | Kinematics | HST | 2.0 ± 0.2 |
| Watkins et al. (2015b) | Kinematics | HST | 2.39 |
| Brown et al. (2018) | Parallax | HST | 2.39 ± 0.07 |
| Gaia Collaboration (2018a) | Parallax | Gaia | 2.64 ± 0.005 |
| Baumgardt et al. (2019) | Kinematics | N-body | 2.44 ± 0.04 |
| Shao & Li (2019) | Parallax | Gaia | 2.62 ± 0.02 |
| Valcin et al. (2020) | CMD | HST | 2.67 |
| This work | Kinematics | HST & MUSE | 2.35 ± 0.10 |
Notes. The columns are: (1) authors; (2) method; (3) observations; (4) distance in kpc. Distances based on kinematics seek dynamical models that match the observed LOS and PM dispersion profiles, where Watkins et al. (2015b) used Jeans modeling, while Baumgardt et al. (2019) used N-body simulations. The distance of Baumgardt et al. (2019) is a weighted mean with the value given by Harris (1996), while that of Valcin et al. (2020) used the value of Dotter et al. (2010) as a prior.
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