0 Assigned ID: 1205 ----- Attempting Submission 1 (Thu Oct 01 20:45:05 GMT 2015) ----- HST Phase I Proposal 1205 (PG1411_midcycle.apt.2015_10_01_15_22.aptbackup.2015_10_01_15_35.aptbackup) successfully submitted. Receipt: # 1205-1 ----- Attempting Submission 2 (Fri Oct 02 13:28:22 GMT 2015) ----- Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. Sensitive exposures should have an ETC run number provided. These observations exactly repeat successful observations we obtained for the same target in Cycle 21. For this reason we did not perform any new ETC calculations. we did not -296874767 ----- Attempting Submission 1 (Thu Dec 03 16:25:16 GMT 2015) ----- This program exactly repeats successful observations of the same target that we obtained in Cycle 21. For this reason, there is no need to confirm the target or do a BOT check as that was all done last time with no issues. Quasar outflows are fundamental components of quasar environments and they might play an important role in feedback to host galaxy evolution. We obtained HST COS spectra of a known outflow "mini-BAL" quasar, PG1411+442 (redshift = 0.089), in February 2015 that revealed the remarkable emergence of a unique new transient absorber that produces MANY weak blended ripple distortions in the rest-frame UV. Our initial skepticism about the reality of these ripples and failed attempts to identify them led to missing the normal Cycle 23 deadline for followup observations. However, subsequent visible spectroscopy with Gemini GMOS (July 2015) confirmed the outflow nature of the ripples by clearly showing many more similar rare/unique absorption features such as the HI Balmer lines, Na I, and highly excited-state lines of FeII and HeI. These lines have velocity shifts v ~ 1900 km/s and widths of only FWHM ~ 170 km/s. Altogether, these lines and the UV ripples identify a small outflow structure (covering only ~20% of the quasar continuum source) that is mostly neutral/low-ionization gas with an enormous column density of N_H > 10^23 cm^-2. This unique extreme transient absorber represents a new phenomenon in quasar research that might offer important clues to the general nature of quasar outflows and their interactions with the host galaxies. We request 3 orbits with COS/FUV to monitor the evolution of the remarkable transient outflow in PG1411+442. These observations are urgent because there might be rapid evolution and short-term constraints on the absorber variability are important to understand its location, energetics and physical nature. We will use 3 orbits with COS FUV to observe PG1411+442 in a way that duplicates our successful Cycle 21 observations of this source in February 2015. This includes 1 orbit with G130M-1096 to cover rest-frame wavelengths 1000-1236A, 1 orbit with G130M- 1309 to cover 1153-1449A, and 1 orbit with G160M-1589 to cover 1398-1761A. We note that our Cycle 21 program used 2 orbits with G130M-1096 for a total of 4 orbits to measure broad lines in the BAL-like outflow in an observed wavelength range 940-1060A with very low sensitivity. The ripples are not detectable at those wavelengths even with 2 orbits because of low signal-to-noise. Thus we request only 1 orbit with G130M-1096 because it is more economical and sufficient to measure the ripples and BAL-like features both at wavelengths 1000-1236A. We performed extensive ETC calculations using these setting for our original Cycle 21 proposal. Here we note simply that the feasibility of the observations now proposed is demonstrated by the high-quality spectra we already obtained in February 2015. AGN/QUASARS 12 false true false false SUPPORTED GALAXY QUASAR NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 COS/FUV Spectroscopic No No G130M 1096 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G160M 1589 1449158797241 /Users/hamann/Google_Drive/proposals/hst15/OP-cache/APT_phase2-v01.xml The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. 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