0 Assigned ID: 515 ----- Attempting Submission 1 (Fri Apr 11 15:02:16 GMT 2014) ----- HST Phase I Proposal 515 (wierdobj.apt) successfully submitted. There is a warning about a nearby dwarf galaxy in Galex for the NUV being too bright. This is a dwarf galaxy, not a star so the emission is diffuse.. 1622749189 ----- Attempting Submission 1 (Fri Jul 11 13:40:35 GMT 2014) ----- ----- Attempting Submission 2 (Fri Jul 11 19:50:00 GMT 2014) ----- We have discovered a BH recoil candidate offset by 800 pc from a nearby dwarf galaxy. The object, SDSS1133, shows offset broad lines and strong variability. While originally classified as a supernova because of its non-detection in 2005, we detect it in recent and past observations over 63 years. Using high-resolution adaptive optics observations, we constrain the source emission region to be <12 pc. Overall these properties are consistent with theoretical predictions for a runaway BH ejected from its host by gravitational-wave recoil following a merger. We propose a small, 4 orbit HST observation using the COS spectrograph in the FUV, to test for broad C IV emission and other high ionization emission lines which would decisively favor the recoiling BH interpretation. The unique UV spectroscopic capability of HST is critical to decide whether this is a recoiling black hole or an unprecedented 50 year outbursting LBV star (e.g. Eta Carina) followed by a unique long duration SN IIn with rebrightening. Either discovery would be extremely exciting. Finally, SDSS1133 has recently undergone a 1.3 mag rebrightening in PanSTARRS imaging suggesting that the coming year is a critical time to observe the source at maximum. Our main focus is to study the broad line C IV 1550 emission along with other nearby UV spectral lines (Lyman alpha, N V 1240, and SiIV+OIV complex near 1400) by measuring their width and flux. The medium-resolution COS FUV modes results in a discovery space (throughput times wavelength coverage) best suited for observations of faint FUV point sources, it is therefore the preferred instrument for this study. The astrometry is based on the centroid of the point source from SDSS and PS1 observations in the optical. We expect at most a 0.3'' uncertainty given fits to many images. Lower spatial resolution images in the FUV and NUV with SWIFT show a point source consistent with the optical image. High resolution images in the NIR AO and NIR narrow band (tracing Paschen Beta which also traces NUV emission from SF) suggest a point source at 0.1'' offset by 6'' from the galaxy nucleus. We will use a NUV ACQ/Image exposure first, which we also use for science purposes to confirm it is a point source in the NUV as well as NIR. For exposure time planning we use NUV+FUV observations from SWIFT and FUV from galex as well as the broad hbeta emission for line emission. While the NUV show significant contamination from the galaxy, at HST resolutions similar to the NIR AO, the point source is much brighter than the surrounding background and even the nucleus of the galaxy 6'' away so centroiding is not an issue. For the ACQ/Image, we use a S/N of 40 and a conservative estimate that our NUV emission is overestimated by a mag because of contamination from the galaxy. Obtaining a full spectrum of an object requires several set-ups and exposures (5 setups for G130M in one orbit and 4 setups for G160M in another orbit), but covers a large spectra range 1140-1800 to observe the interested lines. The separate exposures will be coadded using the routines provided on the COS Tools Web site. AGN/QUASARS Default false true false false false SUPPORTED UNIDENTIFIED ACCRETION DISK BLR NUCLEUS SDSSJ113323.97+550415.8 VV2006CJ113324.0+550416 J2000 J2000 COS/NUV Imaging No No MIRRORB COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1300 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G130M 1318 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1600 COS/FUV Spectroscopic No No G160M 1611 COS/FUV Spectroscopic No No G160M 1623 1405107833101 /private/var/folders/zf/_qv5k6q575l0jv5tgstkflj80000gn/T/OPVisit8481624492889535864.xml The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 13843 :visit-id "01" :proposal-version -1 :trans-version "20140605" :date "11-Jul-2014 21:43:52.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 922432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13843 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13843 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3132 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3470 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13843 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3247 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3470 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13843 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3246 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3470 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13843 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3247 :al-overhead-at-end 0 :internal-dur-at-end 376 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3470 :pcs-gap 0 ) true 4 0