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Figure showing three spectra with measurement uncertainties and best-fit. Each has an arrow showing where the Mg b spectral feature should be located. — apjaa9064f2_hr
Normalized object spectra (black lines) and the 68% confidence intervals on the observed spectrum fluxes (gray shaded areas) shown for A2261 knots 1, 2, and 3 from top to bottom, respectively. The best fits obtained for each knot are shown as red lines. The arrow indicates the rest-frame wavelength of the Mgb spectral feature.

Fig 14 from Rupke et al. (2017). Shows a positive correlation between log outflow mass and log black hole mass. — rupke_etal_2017_fig_14
Fig 14 from Rupke et al. (2017). Shows a positive correlation between log outflow mass and log black hole mass.

Turkey Trot 2017 — Turkey Trot 2017
Turkey Trot 2017

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Fig 14 from Rupke et al. (2017). Shows a positive correlation between log outflow mass and log black hole mass. — rupke_etal_2017_fig_14
Fig 14 from Rupke et al. (2017). Shows a positive correlation between log outflow mass and log black hole mass.

Picture of a crowded field of stars some red, some blue of varying brightness — Galaxy Bulge Stars
HST image of Milky Way Bulge

Figure showing three spectra with measurement uncertainties and best-fit. Each has an arrow showing where the Mg b spectral feature should be located. — apjaa9064f2_hr
Normalized object spectra (black lines) and the 68% confidence intervals on the observed spectrum fluxes (gray shaded areas) shown for A2261 knots 1, 2, and 3 from top to bottom, respectively. The best fits obtained for each knot are shown as red lines. The arrow indicates the rest-frame wavelength of the Mgb spectral feature.

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Fig 14 from Rupke et al. (2017). Shows a positive correlation between log outflow mass and log black hole mass.

Picture of a crowded field of stars some red, some blue of varying brightness — Galaxy Bulge Stars
HST image of Milky Way Bulge

Figure showing three spectra with measurement uncertainties and best-fit. Each has an arrow showing where the Mg b spectral feature should be located. — apjaa9064f2_hr
Normalized object spectra (black lines) and the 68% confidence intervals on the observed spectrum fluxes (gray shaded areas) shown for A2261 knots 1, 2, and 3 from top to bottom, respectively. The best fits obtained for each knot are shown as red lines. The arrow indicates the rest-frame wavelength of the Mgb spectral feature.