Notes. Fits to emission lines in this paper. F₀ is the integrated flux (sum of all components for multiplet lines), and the second value is corrected for reddening assuming E(B − V) = 0.02 (see Sect. 2). σ_r is the velocity dispersion along the line of sight, and v_r is the mean radial velocity of the line relative to M87. For convenience we also convert dereddened fluxes into luminosities assuming a distance of 16.7 Mpc. The top panel shows our fits to observed FUV lines. For Lyα, both values of F₀ are corrected for Galactic absorption as well as discussed in Sect. 3.4. The second panel shows new fits we have made for C IV and He II, which are observed in the same sightline but based on COS G140L data as discussed in Anderson & Sunyaev (2016) since they fall outside the COS G130M bandpass (Sect. 3.6.2). These two lines have artificially broadened measured velocity dispersions due to the extended emission covering multiple pixels of the low-resolution G140L spectrograph (Sect. 8.1), so we mark these dispersions with asterisks. In the third panel we list estimates for selected lines in other portions of the electromagnetic spectrum. We obtain Hα from HST-WFPC2 data (see Sect. 6.2) and [C II] λ158 μm from Herschel-PACS data (rescaling the latter to the HST-COS aperture, see Sects. 2.1 and 3.2). He II λ304 is not observed, but we estimate its strength in Sect. 6.3.2 and note that it may be up to six times larger if the effects of photoionization are included as well. The three lines in this panel have additional systematic uncertainties which are discussed in the text but not included in the measurement errors quoted in this table. Finally, the lower panel shows various continuum luminosities within our aperture for comparison. The X-ray luminosity is evaluated in the 0.5–7.0 keV band (Sect. 6.4) and the FUV luminosity from 1160 Å to 1450 Å (Sect. 3.1). We note that Lyα and He II λ304 are more luminous than these continua. The V-band luminosity in our aperture is calculated from the stellar surface brightness profile measured by Kormendy et al. (2009), and kinematics for the stars are included on this line as well, as measured by Gebhardt & Thomas (2009) using absorption lines.