tokens: for their stellar halos from the Galaxy Halos, Outer disks, Substructure, Thick disks and Star clusters (GHOSTS) survey ( http://vo.aip.de/ghosts/survey.html ; Radburn-Smith et al. 2011 ; Monachesi et al. 2016a ). RGB star counts allowed GHOSTS to reach V -band (Vega) surface brightness sensitivities of ∼33 mag arcsec −2 , revealing roughly power-law stellar halos between minor axis distances of 10 kpc to >50 kpc. These profiles were integrated within the observed range of radii and extrapolated to total stellar halo mass as discussed above. The RGB color is sensitive to stellar halo metallicity (Monachesi et al. 2016a ), and we adopt a derived [Fe/H] value at 30 kpc along the minor axis following the observational calibration of [Fe/H] as a function of RGB colors for globular clusters (Streich et al. 2014 ) assuming . We add stellar halo masses and metallicities at 30 kpc along the minor axis for the MW (Sesar et al. 2011 ; Xue et al. 2015 ; Bland-Hawthorn Gerhard 2016 ), M31 (Gilbert et al. 2014 ; Ibata et al. 2014 ), and NGC 3115 (Peacock et al. 2015 ). Peacock et al. ( 2015 ) estimated a mass in low-metallicity stars in NGC 3115 of , which they adopted as an estimate of the stellar halo mass. As there is a considerable population of high-metallicity stars at large radii in NGC 3115, which could be argued to legitimately belong to its stellar halo, we choose to adopt as a lower limit to its halo mass. No published estimate of stellar halo mass exists for Cen A; we adopt the metallicity along the minor axis at 30 kpc from Rejkuba et al. ( 2014 ). Stellar halo masses (for UGC 180, NGC 1084, NGC 2903, and NGC 4220) or upper limits (for NGC 3351, NGC 3368, NGC 4258, and M101; galaxies that were either presented as upper limits or detections with 1 σ error bars overlapping with zero) are adopted from Trujillo Fliri ( 2016 ; UGC 180) and Merritt et al. ( 2016 ). The stellar halo masses from Merritt et al. ( 2016 ) are extrapolated to total stellar mass as described above and as tabulated by Harmsen et al. ( 2017 ). As these halo masses were constrained using integrated light, these galaxies have no stellar halo metallicity estimates. Total stellar masses were adopted from the source papers, adjusted to a universally applicable Chabrier ( 2003 ) stellar IMF. Bulge-to-total ratios were derived from near-IR ( K -band or longer) photometry from a variety of sources (described in Table 1 ; for Cen A we assume and UGC 180's B / T was roughly estimated to be ). Typical differences between independent estimates for the same galaxies are , comparable to the quoted uncertainties. BH masses and uncertainties (or limits) were adopted primarily from Kormendy Ho ( 2013 ), where again the source papers are tabulated in Table 1 . Table 1 Galaxy Properties Note. Stellar masses are assumed to have an uncertainty of 0.15 dex. a Galaxies with dominant classical bulges. References. (1) Licquia Newman ( 2015 ), (2) Bland-Hawthorn Gerhard ( 2016 ), (3) Sesar
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