No abstract

No abstract

It has recently come to our attention that there are axis scale errors in three of the figures presented in Dull et al. (1997, hereafter D97). This paper presented Fokker-Planck models for the collapsed-core globular cluster M15 that include a dense, centrally concentrated population of neutron stars and massive white dwarfs. These models do not include a central black hole. Figure 12 of D97, which presents the predicted mass-tolight profile, is of particular interest, since it was used by Gerssen et al. We appreciate the thoughtful cooperation of Roeland van der Marel in resolving this issue. Using our corrected version of Figure 12 (see below), Gerssen et al. (2003) now find that the velocity dispersion profile that they infer from the D97 mass-to-light ratio profile is entirely consistent with the velocity dispersion profile presented in Figure 6 of D97. Gerssen et al. (2003) further find that there is no statistically significant difference between the fit to the van der Marel et al. (2002) velocity measurements provided by the D97 intermediate-phase model and that provided by their model, which supplements this D97 model with a 1:7 þ2:7 À1:7 Â 10 3 M black hole. Thus, the choice between models with and without black holes will require additional model predictions and observational tests.We present corrected versions of Figures 9, 10, and 12 of D97. We take responsibility for the errors in the original versions of these figures and regret any confusion that these may have caused. We also present an expanded version of Figure 6, which extends the radial scale to both smaller and larger values, in order to show the full run of the velocity dispersion profile. The profile of the intermediate-phase model of D97 is in good agreement with the HST-STIS velocity dispersion profile presented by Gerssen et al. (2002). In particular, the central value of $14 km s À1 , predicted by this model, nicely coincides with their findings.We note that three independent studies have now demonstrated that there is a dense, central concentration of dark mass in M15, by use of three alternative methods: Fokker-Planck simulations (D97), GRAPE-6 simulations (Baumgardt et al. 2003), and Jeans equation modeling (Gerssen et al. , 2003. The dark mass is proposed to consist of neutron stars and massive white dwarfs, in the former two studies, versus a central black hole in the latter. Irrespective of these different interpretations of the nature of the dark mass, its presence now appears to be well established on dynamical grounds.

No abstract

The bright and understudied classical Be star HD 6226 has exhibited multiple outbursts in the last several years during which the star grew a viscous decretion disk. We analyse 659 optical spectra of the system collected from 2017-2020, along with a UV spectrum from the Hubble Space Telescope and high cadence photometry from both TESS and the KELT survey. We find that the star has a spectral type of B2.5IIIe, with a rotation rate of 74 per cent of critical. The star is nearly pole-on with an inclination of 13${_{.}^{\circ}}$4. We confirm the spectroscopic pulsational properties previously reported, and report on three photometric oscillations from KELT photometry. The outbursting behaviour is studied with equivalent width measurements of Hα and Hβ, and the variations in both of these can be quantitatively explained with two frequencies through a Fourier analysis. One of the frequencies for the emission outbursts is equal to the difference between two photometric oscillations, linking these pulsation modes to the mass ejection mechanism for some outbursts. During the TESS observation time period of 2019 October 7 to 2019 November 2, the star was building a disk. With a large dataset of Hα and Hβ spectroscopy, we are able to determine the timescales of dissipation in both of these lines, similar to past work on Be stars that has been done with optical photometry. HD 6226 is an ideal target with which to study the Be disk-evolution given its apparent periodic nature, allowing for targeted observations with other facilities in the future.