0 Assigned ID: 1071 ----- Attempting Submission 1 (Fri Apr 07 23:03:19 GMT 2017) ----- HST Phase I Proposal 1071 (hst_asassn14li_cycle25.apt) failed submission. ----- Attempting Submission 2 (Fri Apr 07 23:06:38 GMT 2017) ----- HST Phase I Proposal 1071 (hst_asassn14li_cycle25.apt) failed submission. ----- Attempting Submission 3 (Fri Apr 07 23:09:32 GMT 2017) ----- ----- Attempting Submission 4 (Fri Apr 07 23:12:36 GMT 2017) ----- HST Phase I Proposal 1071 (hst_asassn14li_cycle25.apt) failed submission. ----- Attempting Submission 5 (Fri Apr 07 23:13:03 GMT 2017) ----- ----- Attempting Submission 6 (Fri Apr 07 23:55:27 GMT 2017) ----- HST Phase I Proposal 1071 (hst_asassn14li_cycle25.apt) successfully submitted. Receipt: # 1071-6 ----- Attempting Submission 7 (Fri Apr 07 23:58:20 GMT 2017) ----- This program is essentially an extension of programs 14272 and 14812 and uses similar configurations to observe a fading UV transient in a galactic nucleus. The new epoch is longer than the most recent epoch from the previous cycle, and has been broken up for flexibility in scheduling. All visits should be within 6 days, however. Acquisition time has been modestly increased from last cycle, and we have a preference for minimal separation between this block of STIS visits and the associated XMM-Newton joint time. 1567676311 ----- Attempting Submission 1 (Thu Jul 20 20:13:39 GMT 2017) ----- Continued Long-Term Ultraviolet Spectroscopy of a Tidal Disruption Event at only 90 Mpc We propose continued long-term multi-epoch ultraviolet spectroscopy of ASASSN-14li, a stellar tidal disruption event (TDE) at ~90 Mpc. Such a bright, nearby stellar TDEs provides an exceptional opportunity to study broad emission lines which describe the abundances and accretion flow of the stellar debris in one of the most important physical regimes for understanding basic TDE behavior. We also request brief XMM observations to constrain the high-energy spectral evolution on similar timescales. These observations will build upon surprising new results, and will provide an important foundation for follow-up of more ambiguous TDE candidates subsequently identified by LSST and WFIRST at higher redshifts. We are observing the UV-bright tidal disruption event (TDE) on extended baselines to study the spectroscopic evolution of this transient and how it relates to its accretion history. Complementary joint XMM-Newton observations have been granted to constrain the bolometric luminosity and relate high-energy emission to the UV. We will discuss XMM-Newton scheduling with the XMM-Newton team given the visibility windows available. <2 weeks separation is preferred, and the closer the better. Current predictions for XMM-Newton visibility look favorable for this strategy in June and July of 2018. This program is essentially an extension of programs 14272 and 14812, so the instrumental requirements are similar. The TDE is fainter, so we have requested (and been granted) an additional orbit per grating per epoch, but only one epoch per year is necessary since the TDE is evolving slowly. For the purposes of this program, LEDA-43234, PGC-043234 and ASASSN-14LI are effectively the same target. We kept the name "LEDA-43234" to agree with the Phase I proposal data in APT, but changing it to "ASASSN-14LI" would be more consistent with previous programs. As before, we are taking spectroscopy in FUV (STIS-MAMA/G140L) and NUV (STIS-MAMA/G230L). TIME-TAG mode should still be practical. All visits are grouped within 6 days to measure broadly representative properties within that time. We have broken observations into 4 groups of 2 orbits each to allow more flexible scheduling than 2 groups of 4 orbits would allow. Under this configuration, the optimal monitoring strategy is to keep each FUV visit tightly grouped with a NUV visit (<2 days) to allow full-spectrum variability comparisons with timescales of ~days if the signal-to-noise ratio warrants it. We have increased the acquisition times modestly per visit, but we expect most of the acquisition photons to come from the host galaxy at this point and not the transient. Since the transient is at the nucleus, identification of the nuclear peak is fine for acquisition and has been effective in the previous cycle. Massive Black Holes And Their Host Galaxies 6 false true false false false 40 true SUPPORTED GALAXY ACCRETION DISK BLR NUCLEUS UNDESIGNATED NO Phase I coordinates in Cycle 25 were taken using SIMBAD. Phase II coordinates are adjusted to match those of Cycle 24 observations. PGC-043234 ASASSN-14LI J2000 J2000 Currently AB mag ~16.4 at 1500 AA. Host GALEX baseline is (21.7, 19.0) for (FUV, NUV). STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 STIS/NUV-MAMA Spectroscopic No No G230L 2376 /data/CXC/PROPOSALS/OP-cache/hst_c25_asassn14li_phase2_v3-v01.xml Timing link suitability includes constraints ([Group (01 02) Within 2.0 days] [Group (01 02 03 04) Within 6.0 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. Joint XMM observations have been awarded to complement the HST STIS observations. Although the transient is currently evolving slowly over years, coordination with XMM is preferred if possible, to minimize discrepencies due to short-timescale variability. A gap of <2 weeks between XMM and HST would be representative, but ideally the shorter the better. 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CASM was run in Phase II mode. Joint XMM observations have been awarded to complement the HST STIS observations. Although the transient is currently evolving slowly over years, coordination with XMM is preferred if possible, to minimize discrepencies due to short-timescale variability. A gap of <2 weeks between XMM and HST would be representative, but ideally the shorter the better. 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CASM was run in Phase II mode. Joint XMM observations have been awarded to complement the HST STIS observations. Although the transient is currently evolving slowly over years, coordination with XMM is preferred if possible, to minimize discrepencies due to short-timescale variability. A gap of <2 weeks between XMM and HST would be representative, but ideally the shorter the better. (Tic-Visit :proposal-id 15351 :visit-id "03" :proposal-version -1 :trans-version "20170613" :date "20-Jul-2017 14:58:28.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 452704 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15351 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15351 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2883 :al-overhead-at-end 0 :internal-dur-at-end 178 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3216 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15351 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2994 :al-overhead-at-end 0 :internal-dur-at-end 582 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3216 :pcs-gap 0 ) true 2 0 /data/CXC/PROPOSALS/OP-cache/hst_c25_asassn14li_phase2_v3-v04.xml Timing link suitability includes constraints ([Group (01 02 03 04) Within 6.0 days] [Group (03 04) Within 2.0 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. Joint XMM observations have been awarded to complement the HST STIS observations. Although the transient is currently evolving slowly over years, coordination with XMM is preferred if possible, to minimize discrepencies due to short-timescale variability. A gap of <2 weeks between XMM and HST would be representative, but ideally the shorter the better. (Tic-Visit :proposal-id 15351 :visit-id "04" :proposal-version -1 :trans-version "20170613" :date "20-Jul-2017 14:58:30.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 313536 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15351 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15351 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2883 :al-overhead-at-end 0 :internal-dur-at-end 178 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3216 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15351 :visit-id "04" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2994 :al-overhead-at-end 0 :internal-dur-at-end 582 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3216 :pcs-gap 0 ) true 2 0