0 Assigned ID: 489 ----- Attempting Submission 1 (Fri Apr 10 14:30:24 GMT 2015) ----- HST Phase I Proposal 489 (HST_prop_C23_3C326_Guillard.apt) successfully submitted. Receipt: # 489-1 ----- Attempting Submission 2 (Fri Apr 10 16:17:17 GMT 2015) ----- ----- Attempting Submission 3 (Sat Apr 25 13:36:10 GMT 2015) ----- COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See the proposal instructions for more details. 0 ----- Attempting Submission 1 (Tue Jul 07 15:00:31 GMT 2015) ----- Those warning about COS calibration for extended sources are only important for when we will begin processing our data. Now that we have moved to lifetime position 3 (LP3), the COS team has deployed a new extraction technique called “TWO-ZONE”, which is optimized for point sources. This extraction technique will underestimate the flux of an extended target, so the warning is set to alert observers. Once we will get our data, we will re-calibrate it using the old “BOXCAR” method and use that instead, or at least see the difference between the old and new extractions. The 3C326N radio-galaxy is one of the best examples of negative AGN feedback: with 2e9 Msun of molecular gas, its star formation rate is below 0.07 Msun/year, 20 times lower than what the Kennicutt law predicts. Why there is so much of molecular gas and why it is not forming stars? Powerful mid-IR H2 emission and very broad optical and far-IR lines suggest that strong turbulence may heat the H2 gas and prevent it from being gravitationnally bound at all scales. The turbulence driven at large scales by the radio jet would cascade down to smaller scales where it is dissipated. It must be powerful enough to drive high-speed shocks (100-400 km/s) in the hot (1e7 K) plasma that will compress it and allows it to cool down to temperatures where the gas becomes molecular. This cooling is expected to occur through UV line emission, and especially through CIV and OVI lines. To test this prediction, we propose to observe those lines in the 3C326N radio-galaxy. This will allow us to: (1) determine whether UV line emission is a significant cooling process of the hot gas, compute the mass cooling rate of the hot gas (is it high enough to form the H2 disk?), and (2) test our model of the multiphase turbulent gas energized by a radio-jet which would account for both H2 masses and energetics (can turbulence be sustained by shocks pressurizing the disk?). These observations will greatly enhance our understanding of why 3C~326N, and massive early-type galaxies in general, have large masses of molecular gas but yet weak star formation. The physics explored in this proposal applies to a wide range of environments, including cluster cooling flows and hot gas cooling in haloes of galaxies. We request observations of the 3C326N radio-galaxy at moderate resolution using the G130M and G160M settings for all positions. This ensures, even if the emission is extended, a minimum resolution of 1400, which is enough to avoid line blending issues that we may encounter with the low-resolution grating. In order to achieve continuous spectral coverage and minimize fixed pattern noise, observations in each grating will be made at two (three) central wavelengths for G140L (G130M and G160M). The O{\sc vi} and C{\sc iv} lines are redshifted at 1138A and 1703A, so we will use central wavelengths settings at 1222 and 1096A for G130M and 1589 and 1600A for G160M. Note that the Lya line falls in the 1222A G130M setting. We will optimize S/N using the on-orbit line spread function and correcting for fixed pattern noise. We will also dither instrumental and gain-sag features. AGN/QUASARS 12 false false false false SUPPORTED GALAXY RADIO GALAXY YES This object was generated by the targetselector and retrieved from the NED database. J2000 J2000 COS/FUV Spectroscopic No No G130M 1096 COS/FUV Spectroscopic No No G130M 1222 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1600 1436260183816 /Users/guillard/proposals/hst/cos/2015_04_Cycle23/OP-cache/3C326N_COS_Phase2-v01.xml The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 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