SIMBAD references

We present new Hubble Space Telescope - Cosmic Origins Spectrograph (HST-COS) G130M spectroscopy which we have obtained for a sightline toward a filament projected 1.9 kpc from the nucleus of M87, near the edge of the inner radio lobe to the east of the nucleus. The combination of the sensitivity of COS and the proximity of M87 allows us to study the structure of this filament in unparalleled detail. We propose that the filament is composed of many cold clumps, each surrounded by an FUV-emitting boundary layer, with the filament having a radius r_c∼10pc and the clumps filling the cylinder with a low volume filling factor. The observed velocity dispersion in emission lines from the filament results from the random motions of these clumps within the filament. We have measured fluxes and kinematics for emission lines of Lyα, CIIλ1335, and NVλ1238, finding v_r=147±2km/s, 138±18km/s, and 148_–16⁺¹⁴km/s^–1 relative to M87, and line broadenings σ_r=171±2km/s, 189_–11⁺¹²km/s, and 128_–17⁺²³km/s respectively. We associate these three lines, as well as archival measurements of Hα, CIVλ1549, and HeIIλ1640, with a multitemperature boundary layer around clumps which are moving with supersonic random motions in the filament. This boundary layer is a significant coolant of the hot gas. We show that the [CII]λ158µm flux observed by Herschel-PACS from this region implies the existence of a massive cold (T∼10³K) component in the filament which contains significantly more mass (M∼8000M_☉ within our r~=100pc sightline) than the FUV-emitting boundary layer. It has about the same bulk velocity and velocity dispersion as the boundary layer. We also detect [FeXXI] λ1354 in emission at 4-5σ. This line is emitted from 1keV (T~=10⁷K) plasma, and we use it to measure the bulk radial velocity v_r=-92_–22⁺³⁴km/s and velocity dispersion σ_r=69_–27⁺⁷⁹km/s of the plasma at this temperature. In contrast to the intermediate-temperature FUV lines, [FeXXI] is blueshifted relative to M87 and matches the bulk velocity of a nearby filament to the south. We hypothesize that this line arises from the approaching face of the radio bubble expanding through this sightline, while the filament lies on the receding side of the bubble. A byproduct of our observations is the detection of absorption from interstellar gas in our Galaxy, observed in CIIλ1335 and Lyα.