A Novel Measurement of Turbulence and Bulk Flows in the Hot Halo of M87

0 Assigned ID: 635 ----- Attempting Submission 1 (Fri Apr 08 17:51:33 GMT 2016) ----- HST Phase I Proposal 635 (proposal.apt) successfully submitted. Receipt: # 635-1 ----- Attempting Submission 2 (Fri Apr 08 22:47:46 GMT 2016) ----- HST Phase I Proposal 635 (proposal.apt) successfully submitted. Receipt: # 635-2 COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. This phase II program is based on the phase II programs for proposals 12271 and 13439, both of which observed the same target (a UV-emitting filament in M87) with COS FUV spectroscopy. Also, we note that the nucleus of M87 is flagged in the BOT based on GALEX NUV photometry. However, numerous high-resolution observations of the nucleus with HST (including with COS) have shown that the nuclear flux is well within safety limits, even during rare flaring events. 490083445 ----- Attempting Submission 1 (Fri Jul 08 15:17:07 GMT 2016) ----- ----- Attempting Submission 2 (Thu Oct 20 11:42:21 GMT 2016) ----- We have discussed the expected effect of extended emission on the spectral resolution in our phase I proposal. A Novel Measurement of Turbulence and Bulk Flows in the Hot Halo of M87 Decades of observational and theoretical effort have focused on understanding the velocity structure of the hot gaseous halos (T > 10^7 K) suffusing galaxy clusters, groups, and massive ellipticals. The turbulence and bulk flows in these media transport energy, mass, and metals from the nucleus into the diffuse halo, and they provide important non-thermal pressure support which is crucial to understand for accurate hydrostatic mass modeling. The Hitomi X-ray mission was intended to measure these motions in massive clusters, but it was only able to observe one system, and its calorimeter does not have sufficient resolution for lower-mass systems like the Virgo Cluster. As an alternative, we have identified a forbidden ground-state transition in highly ionized Iron -- [Fe XXI] at 1354.08 A -- which traces plasma in a narrow range around 10^7 K (1 keV). With the sensitivity and spectral resolution of COS, this line can be used to measure the velocity structure of the hot halo gas directly. In a recent paper, we examined archival COS G140L spectra of an FUV-bright filament system projected 1.9 kpc from the center of M87 and found tentative (2-5 sigma) evidence of [Fe XXI] emission. This region also has deep X-ray observations which confirm the presence of 1 keV plasma, and the expected [Fe XXI] signal from the X-ray observations is consistent with our FUV measurement. Here we propose follow-up observations using the G130M grating in order to confirm this detection and to measure the velocity structure of the line with 50 km/s precision. Observing this unique line will allow us to measure directly the turbulence and bulk flows in the hot ambient medium of M87. We will use the same observing procedure as the COS observations in proposals 12271 and 13439, namely taking an NUV ACQ/IMAGE of the nucleus of M87 (called M87-FILAMENT-OFFSET here and in those proposals) and then using that image to point towards the filament (which is about 20" away from the nucleus and called M87-FILAMENT). It is important to make sure to use the nucleus of M87 for target acquisition and not the knots in the jet which are located ~0.85 arcsec to the NW. Intergalactic Medium and Cosmology 12 false true false false false false SUPPORTED EXT-MEDIUM CORONAL GAS FILAMENT HOT GAS ICM YES J2000 J2000 GALAXY NUCLEUS RADIO GALAXY NO this is the nucleus of M87 J2000 COS/FUV Spectroscopic No No G130M 1291 1476959930578 /private/var/folders/tl/xws3kqdx3rn8ynz2h75vj9jm0000gn/T/OPVisit8762118003107950595.xml The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 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