This combines the last visit for V1369 Cen of GO 13828 (cycle 22) with the one visit of GO 14338. This has been extensively discussed with STScI staff. The visit should take place in Feb.-Mar. 2016, contemporaraneous observations are planned with UVES/ESO. -320380945 ----- Attempting Submission 1 (Fri Jul 31 01:57:09 GMT 2015) ----- I have run the target confirmation charts tool but it is blocking the system and does not seem to be read by the APT. The same for the visit planner. Please advise. The major obstacle to understanding the classical nova phenomenon is the lack of systematic observations, primarily spectroscopic, through the various stages of the ejecta and white dwarf evolution. Progress is only possible if long term, coordinated multi-wavelength spectroscopic data at high spectral resolution and high signal to noise are available. Our objective is to use HST/STIS spectra, along with coordinated space- and ground-based observations, to fully characterize three bright recent Galactic classical novae within a panchromatic framework. This proposed data set will be a benchmark sample for any future modeling efforts. All three, V959 Mon (ONe type), V339 Del (CO-type), and V1369 Cen (CO-type), were detected in gamma-rays by Fermi/LAT and well observed in the first months after outburst. We propose to use these data to address fundamental unsolved problems, such as: the origin of the large-scale bipolar structure, the origin and time development of the fragmentation detected in the ejecta, the uniformity of the abundances among the emission knots, and the determination of filling factors and masses for the ejecta. All are essential for understanding the thermonuclear explosion on the white dwarf and its related hydrodynamic events. Multiple UV visits are required to observe the changes as the ejecta expand and the central source evolves. One E140M and two E230M (c: 1978 A and 2707 A) exposures will provide the continuous UV coverage (1123 A to 3111 A) we require for the spectral sequence. The E140M provides access to resonance transitions of many ionization stages, e.g., C II - C IV, N IV-V, O III], and Ne IV]-V], along with the He II 1640 A and other excited state lines. The E230M short wavelength will provide C II, N III] and C III] emission, and the E230M long will provide Mg II, O III, and the Fe II lines. For V1369 Cen we request four (4) separate one-orbit HST/STIS visits during cycles 22 and 23 to capture the same epochs obtained with V339 Del. Two exposures will be obtained in the current cycle 21 ending just before the start of the next cycle. We expect that during cycle 22 the brightness will still be sufficient in the UV, without risk to the detectors, to obtain a medium resolution sequence within a single orbit based on our experience with V339 Del. At the moment the source is still increasing in X-rays so we do not yet know when the SSS phase will either start or end. Thus, we request the longest possible period for the sequence. We expect this source to be observable with STIS for at least two years (to the end of Cycle 23), permitting an extraordinary view of the later stages with only modest observing times. For V959 Mon, since the nova is now at a steady stage, we request a single epoch/visit with all three settings of the echelle gratings, each lasting two orbits (i.e. a total of 6 orbits). Since HST operation imposes a limit of 5 orbits per visit, the V959 Mon observation can be split into 2 or 3 relatively closely timed visits increasing to 7 the number of requested orbits (due to the extra acquisition). The exposure time is based on scaling from the T Pyx sequence after Day 600 scaled to the higher UV reddening (E(B-V) ~0.8 compared to E(B- V) ~0.5 for T Pyx). Only one sequence is requested, this will suffice to provide a baseline similar to that obtained in T Pyx after outburst. The previous STIS sequence, taken on Day 151, provides a sufficient comparison and baseline, especially for the interstellar spectrum. For V339 Del, request two (2) additional visits. The period of invisibility of the source should occur in the first half of cycle 22 so we request one immediately after the first appearance (Feb-Mar 2015) and one near the end of the cycle. We expect that at the rate of decline of the nova each sequence will require two orbits for a total of four (4) orbits. HOT STARS 12 false true false false SUPPORTED STAR CLASSICAL NOVA The positions are from the observatioons of Nova-Cen-2013 (V1369 Cen) during Cycle 22 GO 13828. Those listed in SIMBAD and used previously as the default are not precise enough. V1369-CEN J2000 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No E230M 1978 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No E230M 1978 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/NUV-MAMA Spectroscopic No No E230M 1978 STIS/NUV-MAMA Spectroscopic No No E230M 2707 1438307212438 The scheduling data was generated by CASM 23.2. CASM was run in Phase II mode. /Users/shore/Downloads/OP-cache/V1369Cen-Visit06-cycle23-v06.xml (Tic-Visit :proposal-id 14338 :visit-id "06" :proposal-version -1 :trans-version "20150609" :date "31-Jul-2015 03:46:50.0" :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 278832 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14338 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14338 :visit-id "06" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3123 :al-overhead-at-end 194 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3456 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14338 :visit-id "06" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3234 :al-overhead-at-end 0 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3456 :pcs-gap 0 ) true 2 0 the input spectrum in the ETC is the stis/FUV/E140M spectrum of nova Del 2013 when at 11 mag. Cen 2013 and Del 2013 are two very alike noave in type (CO-WD) and spectral evolution. Cen is supposed to be at the same mag in Dec 2014. Our first obs is in Feb 2015, when it will be even fainter. the input spectrum in the ETC is the stis/NUV/E230M/1978 spectrum of nova Del 2013 when at 11 mag. Cen 2013 and Del 2013 are two very alike noave in type (CO-WD) and spectral evolution. Cen is supposed to be at the same mag in Dec 2014. Our first obs is in Feb 2015, when it will be even fainter. the input spectrum in the ETC is the stis/NUV/E230M/2070 spectrum of nova Del 2013 when at 11 mag. Cen 2013 and Del 2013 are two very alike noave in type (CO-WD) and spectral evolution. Cen is supposed to be at the same mag in Dec 2014. Our first obs is in Feb 2015, when it will be even fainter.