Initial submission CY33 Sun Feb 23 08:58:45 CST 202587831547Assigned ID: 6059
----- Attempting Submission 1 (Sun Feb 23 14:58:55 GMT 2025) -----
HST Phase I Proposal 6059 successfully submitted.
Receipt: # 6059-1Disruptive is a required field.
Ultra Disruptive: 0 is too small. It must be >= 1.
This target is not used in this proposal.Initial submission of Phase II program from review by StSci contact scientist to check for optimization and proper application of 1G approach to science execution and orbit utilization [cew Fri Jul 25 14:35:51 CDT 2025].
Resubmission of version 2 Wed Jul 30 12:40:40 CDT 2025. Revises the Phase II after CS M. Mingozzi review and critiques (email of 2025 Jul 29). This version (1) removes orient requirements to minimize observing constraints to
improve scheduability; (2) changes from ACCUM mode to TIME-TAG mode for the STIS/MAMA observations where the BUFFER_TIME values used is 4/5 * STIS ETC Buffer Time; and (3) changes
quiding requirements from 1G to None Selected. We also have re-run all the STIS spectroscopic ETC simulations after Orbital Planner optimization and include these updated ETC workbook numbers
as required.
Added target that should be first tigger, but having trouble getting APT to update. Hopefuly Blair will fix properly ... cew Tue May 26 13:15:46 CDT 2026
Updated ETC calculations notebooks .... Need to place on Old NOVA2-Epoch1 and activate NOVA2-Epoch3 (three orbits) to achive the SNR ratio given the target brightness, sent not to Matlide Mingozzi email note about this Wed May 27 08:58:51 CDT 2026
Updated the STIS TA ETC V34.1.1 computations to 2348076, which assume AOV and V=8.25 (current AAVSO mag) Vega mag, F25ND3 E(B-V) =0.332 mag, NASA IPAC Galactic DUST and Reddeding website in direction of target for SN=40 Fri May 29 13:44:54 CDT 2026
Update after Zoom Discussion with A. Armstrong, attempting to achieve (04), (05), (06) visits on DOY 155-156, DOY 202-210, and DOY 212-217 respectively to achieve desired science goals Fri May 29 14:11:54 CDT 2026-1781711716----- Attempting Submission 1 (Fri Jul 25 19:37:45 GMT 2025) -----
HST Phase II Proposal 18064 successfully submitted.
Receipt: # 18064-1
----- Attempting Submission 2 (Wed Jul 30 17:50:22 GMT 2025) -----
----- Attempting Submission 3 (Tue May 26 18:18:30 GMT 2026) -----
----- Attempting Submission 4 (Wed May 27 13:59:25 GMT 2026) -----
----- Attempting Submission 6 (Fri May 29 19:12:34 GMT 2026) -----Generic ToO so precise coordinates unknown. Orbital Planner runs with no errors reported.
Cannot seem to get the fixed target ToO into the NOVA2 eopch 1,2,3 series of observations and hence acnnot ru n orbit planner / visit plannerAre Novae Galactic Lithium Factories ?The astrophysical origin of lithium in the Galaxy represents one of the major open questions in modern astrophysics. While lithium is destroyed by stellar evolution, many astrophysical processes and sources actively produce lithium. However, galactic chemical evolution studies suggest that none of these latter sources except novae appears sufficiently efficient to synthesize the total amount of Li. Detection of the 7Be II 313.0 nm resonance doublet transition in novae has finally confirmed theoretical predictions that 7Be is produced during the thermonuclear runaway on the surface of an accreting white dwarf that drives nova explosions. 7Be decays into 7Li with a half-life of 53.2 days, but when 7Be abundances are measured relative to calcium (current technique) the derived abundance of 7Li is 4 to 5 dex higher than the meteoritic value. The Ca result hints novae could be the major factories of 7Li. We propose a synoptic ToO study using the HST UV STIS echelle to set stringent constraints on in situ 7Li production using 7Be and Mg II as novel proxies. The objective is to derive an independent and accurate estimate of the nova 7Be (=7Li) yields, its evolution as it decays, and the dependence of lithium yield on nova type (classical novae or recurrent) using Mg II 280.0 nm as a reference element. The goal is to determine whether novae are the Galactic lithium factories. Two novae targets are proposed to enable comparision of 7Li yields in different nova types which will constrain the tension between theoretical models and observations.HST/STIS echelle spectra will be analyzed to quantify the amount of 7Be produced in CNeby using the Mg II 280.0 nm doublet transitions as a proxy. Simultaneous observations of both the Mg II 280.0 nm and the 7Be II 313.0 nm lines at high spectral resolution require HST/STIS. The use of HST/STIS in echelle mode is crucial to identify and analyze the resonance lines of Be II and Mg II and disentangle their narrow absorption troughs from possible Fe, Cr, Ti and V contaminants. HST observations will be conducted with the E230H grating, an a 0.2 x 0.2 arcsec slit (novae are point-sources), and tilt centered on 276.2 nm and 301.2 nm, reaching a resolving power of approximetly 2.5 km/s at 280.0 nm. This resolution is well-suited to unambiguously resolve narrow non-saturated absorption features necessary to identify possible multiple components.
The science goal will be achieved by observing two bright (Vpeak approximately 7) novae at three distinct epochs sampling over the time of the 7Be half-life (53 days). The ToO trigger observations will be executed within ~21-30 days after the nova discovery (non-disruptive ToO; 21 day from submission of trigger request to scheduling and execution) when the nova brightness is around V >=7.5 mag. These STIS wavelengths are chosen to provide direct information on Mg II 280.0 nm, and 7Be II 313.0 nm lines, respectively. All three epochs will use the same instrumental setup and will be planned as a non-disruptive ToO, with an observing cadence of approximately 10-20 days between consecutive visits. The exact execution plan of HST/STIS observations depends on the nova evolution (which will be followed by ancillary facilities both grround- and space-based).
The ToO trigger will be reserved for for classical novae (CNe) or recurrent novae (RNe), with Vmax >=7 mag, and with low extinction, E(B-V) ~ 0.5 mag (corresponding to NH = 3 x 10^21 cm-2) as deteremined from extinction and N(H) maps and ancillary observations.
Use of the NASA Gehrels Swift Observatory will provide UVOT monitoring to estimate the UV brightness and ensure the safety of the MAMA detectors. To calculate exposure times, we assume a Bruzual synthetic spectrum of a V aproximately 7.5, 8.5, and 9.5 mag A0-type star selected from the templates in the STIS ETC, available on the HST website, which best resembles the spectrum during the late-bright phases of a nova. The exposure times are chosen to obtain S/N per spectral resolution element of >=12, enough to disentangle narrow features from the bright continuum and to measure their equivalent widths for the abundance estimates. This implies initial (epoch#1) exposure times of ~600 s (optimized to account for full utilization of a given orbit) and ~1100s (optimized to account for full utilization of a given orbit)for the 276.2 and 301.2 tilts, respectively. Likely the nova brightness will fade by approximately 1-2 magnitudes over the epochs of the synoptic observations, hence the requisite increase of one to two orbits per visit. HST/STIS data will be reduced using the calstis pipeline, available in the AstroConda python environment through the stistool packages if high level data products are not directly available from the MAST.
The final exposure times have been adjusted acoring to the Orbit Planner in the APT v2025.3.04 software during Phase II. TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation buffer time.
The average number of observed novae in the whole sky is approximately 3 novae per year brighter than Vmax <= 9.0. The requested time is conservatively benchmarked to be 2 CNe/RNe in HST proposal Cycle 33. The selection of the targets and epochs of observations will be based on their brightness in order to not exceed the bright-object limit values (Vmag approximately 6 mag for the E230H echelle observations). The safety of the STIS MAMA detectors is of paramount importance and to ensure their safety we will use the appropriate STIS archival spectrum, scaled to the latest Swift UVOT and AAVSO photometry, to confirm that the source does not exceed the MAMA bright source limits. Finally, the observational strategy uses the STIS MAMA detectors, the observations must be taken in non-SAA impacted orbits and have a bright source check of the field done prior to release for scheduling.
One of the most important requirements for the success of our proposal consists in measuring equivalent widths from Mg II and 7Be II absorption features that are not affected by saturation, and this condition is generally obtained from approximetaly 40-50 days after the nova outburst. However, this constraint is dependent on the speed class of the nova. Accompanying, complementary ground-based spectroscopic programs and Swift ToO requests will be activated to determine the spectral evolution of the nova, its speed class and to control that its brightness does not exceed the bright-object limit along the entire wavelength range. Once a suitable target has been identified, we will construct and trigger the final HST observing plan according to our early results from our complementary observations. The initial visit (#1) is a non-disruptive ToO, followed by two additional observations (#2 nominally 10-20 days after #1; and #3 nominally 10-20 days after #2) for three epochs total. We will work with the HST planners to implement a cadence to maximize science return. In total, this ToO is comprised of two non-distruptive triggers. The multi-epoch observations of the same selected target(s) triggered in this ToO program are required as CNe/RNe are temporally (i.e., variable) evolving objects. The exact execution plan of HST/STIS observations depends on the nova evolution.
If not triggered during the cycle, a request to the TTRB for carry-over consideration will be sent (using the N+1 cycle policy). The proposed ToO trigger could take advantage of the Flexible Thursday scheduling opportunities only in Cycle 33as outlined in the proposal narrative.
We will update the astrometric coordinates of the generic targets for the specific targeted novae when they become available.The PI and Co-Is have an abundance of experience using several ground-based (ESO/VLT, GTC, TNG, NOT, Calar Alto, SOAR, MMT, LBT, IRTF, MDM and SALT) and space-based UV telescopes (JWST, HST, IUE, Swift) with proposals dedicated to the observations of novae in outburst with high-resolution spectrographs. CoI Izzo led efforts resulting in the first identification of lithium in the ejecta of a nova (V1369 Cen, Izzo et al. 2015), has recently led a work with the first detection of 7Be II in the Small Magellanic Cloud (Izzo et al. 2022), and has been co-I of a previous HST proposal dedicated to the observations of two bright novae in outburst (GO 13828) and of gamma-ray bursts/kilonovae (GO 15708, 15979, 15980). CoI Sumner Starrfield, Regents' Professor at the Arizona State University, has published over 260 refereed publications on novae and variable stars. He was the PI of successful IUE, Chandra, and HST nova proposals. PI Charles "Chick" Woodward (team lead) is an experienced UVOIR observer using a variety of ground- and spaced-based facilities (including HST, Swift, and JWST), with over 190 refereed publications. He will lead the HST observational planning and reduction efforts. Paolo Molaro is the PI of an ongoing ToO program dedicated to study the evolution of 7Be II in nova outbursts with the high resolution spectrograph UVES. PierLuigi Selvelli has an in-depth knowledge, certified by the publication of >20 papers, of the analysis of novae in the UV range in particular with the IUE satellite. Massimo Della Valle has a great deal of experience in observing at ESO telescopes and in analysing astrophysical transients, including novae. Co-I Dr. Eamonn J. Harvey UK Astronomy Technology Centre UK, is employed developing the HARMONI and METIS instruments for the ELT, and has great experience in modelling nova ejecta using emission line profiles and ratios. Co-I Peter Hauschildt is the main developer of the special relativistic NLTE model atmosphere code PHOENIX and has successfully constructed models and synthetic spectra for novae in their fireball and optically thick wind phases. Co-I Kim Page is a core member of the Swift-XRT team, with experience in both X-ray and UV/optical data analysis.Stellar Physics and Stellar Types6falsetruefalsefalsefalsefalsefalseSUPPORTEDSTARCLASSICAL NOVANOVA-LIKEFirst Nova Trigger ATEL# 17813 reports a spectra of ASASSN-26no obtained on the SOAR 4.1m on 2026 May 24 (UT 00:43) showed a " flat continuum (suggesting only modest reddening) with strong emission lines of H (Hbeta FWHM about 1400 km/s), He I, and Fe II. Most of the emission lines show strong P Cygni profiles extending to about -1000 km/s from rest. The spectrum and light curve evolution are consistent with a slow classical nova." Photometery (ASASSN site) indicates that the nova is currently V= 9 mag. This meets the trigger criteria outlined in the technical section of the original ToO proposal. We have triggered our VLT ToO program for additionalt spectroscopic follow-up. This is the first (EPOCH1) trigger (visit) NON-DISRUPTUVE activations and replace Genergic Target NOVA2. Note that the GAIA position puts the target 7.9 arcseconds away ....The coordinates entered were the pointing coordinates used by the investigators reporting in the discovery cricular ATEL 17813 (confirmed via email corresponance). Discovey date 2026-May-11. Revised cew: Tue May 26 13:12:08 CDT 2026NVMUSCA2026J2000g-band 9.59STARCLASSICAL NOVARECURRENT NOVAThe ToO trigger will be reserved for a bright novae or recurrent novae, with Vmax >=7 mag, and with low extinction, E(B-V) ~ 0.5 mag (corresponding to NH = 3 x 10^21 cm-2) as determined from extinction and N(H) maps and ancillary observations.Next bright nova 18.5, 9.5STIS/NUV-MAMASpectroscopicNoNoE230H2762STIS/NUV-MAMASpectroscopicNoNoE230H3012STIS/NUV-MAMASpectroscopicNoNoE230H2762STIS/NUV-MAMASpectroscopicNoNoE230H3012STIS/NUV-MAMASpectroscopicNoNoE230H2762STIS/NUV-MAMASpectroscopicNoNoE230H3012STIS/NUV-MAMASpectroscopicNoNoE230H2762STIS/NUV-MAMASpectroscopicNoNoE230H3012STIS/NUV-MAMASpectroscopicNoNoE230H2762STIS/NUV-MAMASpectroscopicNoNoE230H3012STIS/NUV-MAMASpectroscopicNoNoE230H2762STIS/NUV-MAMASpectroscopicNoNoE230H3012/System/Volumes/Data/solaris/user1/armstrong/hst/working/OP-cache/18064-v04.xmlThe scheduling data was generated by CASM 34.1.CASM was run in Phase II mode.FIRST spectroscopic epoch of NOVA2 target. The ToO trigger will be reserved for a bright novae or recurrent novae, with Vmax >=7 mag, and with low extinction, E(B-V) ~ 0.5 mag (corresponding to NH = 3 x 10^21 cm-2) as determined from extinction and N(H) maps and ancillary observations. The Epoch 1 observations will be executed within ~21-30 days after the nova discovery (non-disruptive ToO tigger) when the nova brightness is around V ~7 to 7.5 mag. Both grating settings (c2762 and c3012) must be observed during a single visit to achieve the proposal science goals, as the source is temporally variable.(Tic-Visit
:proposal-id 18064
:visit-id "04"
:proposal-version -1
:trans-version "20260319"
:date "01-Jun-2026 13:36:46.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
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(Tic-Obset
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)true10The ToO trigger will be reserved (ON-HOLD) for a bright novae or recurrent novae, with Vmax >=7 mag, and with low extinction, E(B-V) ~ 0.5 mag (corresponding to NH = 3 x 10^21 cm-2) as determined from extinction and N(H) maps and ancillary observations.
Updated the STIS TA ETC V34.1.1 computations to 2346649, which assume AOV and V=10 Vega magnitude, F25ND3 E(B-V) =0.332 mag from NASA IPAC Galactic DUST and Reddeding website in direction of target for SN=40 Wed May 27 08:25:44 CDT 2026
Updated the STIS TA ETC V34.1.1 computations to 2348076, which assume AOV and V=8.25 (current AAVSO mag) Vega mag, F25ND3 E(B-V) =0.332 mag, NASA IPAC Galactic DUST and Reddeding website in direction of target for SN=40 Fri May 29 13:44:54 CDT 2026Original 2022811 | OB for target with V = 7.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 2800AA (near MgII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time.
Update Wed May 27 08:34:35 CDT 2026:
OB for target with V = 9.5 mag, STIS ETC v33.2 2022856 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 2800AA (near MgII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time.Original 2022805 : OB for target with V = 7.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 3130AA (near 7BeII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time.
Update Wed May 27 08:34:35 CDT 2026
OB for target with V = 9.5 mag, STIS ETC v33.2 2022857| AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 3130AA (near 7BeII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time./System/Volumes/Data/solaris/user1/armstrong/hst/working/OP-cache/18064-v05.xmlTiming link suitability includes constraints ([06 After 05 by 10.0 to 20.0 days])The scheduling data was generated by CASM 34.1.CASM was run in Phase II mode.SECOND spectroscopic epoch of NOVA2 target. The observations of Visit 2 should occur within ~10-20 days after Visit 1 (Epoch1 the ToO trigger visit). We will work with assigned StScI contact scientist to optimimize follow-on cadence as the HST/STIS observations depends on the nova evolution (as described in the proposal). Both grating settings (c2762 and c3012) must be observed during a single visit to achieve the proposal science goals, as the source is temporally variable.(Tic-Visit
:proposal-id 18064
:visit-id "05"
:proposal-version -1
:trans-version "20260319"
:date "01-Jun-2026 13:36:47.0"
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)false20Epoch 2 Visit to NOVA 2 (ON-HOLD) for cadence assessment and science optimization after initial ToO trigger visit (Epoch 1).
Updated the STIS TA ETC V34.1.1 computations to 2346649, which assume AOV and V=10 Vega magnitude, F25ND3 E(B-V) =0.332 mag from NASA IPAC Galactic DUST and Reddeding website in direction of target for SN=40 Wed May 27 08:25:44 CDT 2026
Updated the STIS TA ETC V34.1.1 computations to 2348076, which assume AOV and V=8.25 (current AAVSO mag) Vega mag, F25ND3 E(B-V) =0.332 mag, NASA IPAC Galactic DUST and Reddeding website in direction of target for SN=40 Fri May 29 13:44:54 CDT 2026Original 2022833: OB for target with V = 8.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 2800AA (near MgII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations.
Update Wed May 27 08:34:35 CDT 2026:
OB for target with V = 9.5 mag, STIS ETC v33.2 2022856 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 2800AA (near MgII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time.Original 2022835 | OB for target with V = 8.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 3130AA (near 7BeII line position). Split between orbits. TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations.
Update Wed May 27 08:34:35 CDT 2026
OB for target with V = 9.5 mag, STIS ETC v33.2 2022857 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 3130AA (near 7BeII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time./System/Volumes/Data/solaris/user1/armstrong/hst/working/OP-cache/18064-v06.xmlTiming link suitability includes constraints ([06 After 05 by 10.0 to 20.0 days])The scheduling data was generated by CASM 34.1.CASM was run in Phase II mode.THIRD spectroscopic epoch of NOVA2 target. The observations of Visit 3 should occur within ~10-20 days after Visit2. We will work with assigned StScI contact scientist to optimimize follow-on cadence as the HST/STIS observations depends on the nova evolution (as described in the proposal). Both grating settings (c2762 and c3012) must be observed during a single visit to achieve the proposal science goals, as the source is temporally variable.(Tic-Visit
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:visit-id "06"
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:date "01-Jun-2026 13:36:48.0"
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:saa-model "24"
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:data-volume 835392
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)false30Generic Target is a ToO. The Epoch 3 observations are designed to follow Epoch 2 visit by ~10-20 days (when nova brightness has declined to V~9.5 mag).Epoch 3 Visit to NOVA 2 (ON-HOLD) for cadence assessment and science optimization after initial ToO trigger visit (Epoch 1).
Updated the STIS TA ETC V34.1.1 computations to 2346649, which assume AOV and V=10 Vega magnitude, F25ND3 E(B-V) =0.332 mag from NASA IPAC Galactic DUST and Reddeding website in direction of target for SN=40 Wed May 27 08:25:44 CDT 2026
Updated the STIS TA ETC V34.1.1 computations to 2348076, which assume AOV and V=8.25 (current AAVSO mag) Vega mag, F25ND3 E(B-V) =0.332 mag, NASA IPAC Galactic DUST and Reddeding website in direction of target for SN=40 Fri May 29 13:44:54 CDT 2026Original 2022856 OB for target with V = 9.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 2800AA (near MgII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations.
Update Wed May 27 08:34:35 CDT 2026
OB for target with V = 9.5 mag, STIS ETC v33.2 2022856 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 2800AA (near MgII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time.Original : OB for target with V = 9.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=9 @ 3130AA (near 7BeII line position). Split between orbits. TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. Two exposures (one orbit each) are required to reach the minimum SNR requirements outlined in the proposal for this epoch when the source has faded on brightness.
Update Wed May 27 08:34:35 CDT 2026
OB for target with V = 9.5 mag, STIS ETC v33.2 2022857 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 3130AA (near 7BeII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time.OB 2022857 for target with V = 9.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=9 @ 3130AA (near 7BeII line position). Split between orbits. TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. Two exposures (one orbit each) are required to reach the minimum SNR requirements outlined in the proposal for this epoch when the source has faded on brightness.
Update Wed May 27 08:34:35 CDT 2026
OB for target with V = 9.5 mag, STIS ETC v33.2 2022857 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 3130AA (near 7BeII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time./System/Volumes/Data/solaris/user1/armstrong/hst/working/OP-cache/18064-v07.xmlThe scheduling data was generated by CASM 34.1.CASM was run in Phase II mode.FIRST spectroscopic epoch of NOVA1
target. The ToO trigger will be reserved for a bright novae or recurrent novae, with Vmax >=7 mag, and with low extinction, E(B-V) ~ 0.5 mag (corresponding to NH = 3 x 10^21 cm-2) as determined from extinction and N(H) maps and ancillary observations. The Epoch 1 observations will be executed within ~21-30 days after the nova discovery (non-disruptive ToO tigger) when the nova brightness is around V ~7 to 7.5 mag. Both grating settings (c2762 and c3012) must be observed during a single visit to achieve the proposal science goals, as the source is temporally variable.(Tic-Visit
:proposal-id 18064
:visit-id "07"
:proposal-version -1
:trans-version "20260319"
:date "01-Jun-2026 13:36:48.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 591840
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 18064
:visit-id "07"
:obset-id "07"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18064
:visit-id "07"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2597.0
:al-overhead-at-end 0
:internal-dur-at-end 440.0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2979
:pcs-gap 0
)true10Generic Target is a ToO. The ToO trigger will request the first target visit (Epoch 1) to occur ~21-30 observations days after the nova discovery when the nova brightness is around V ~ 7.5 mag.The ToO trigger will be reserved (ON-HOLD) for a bright novae or recurrent novae, with Vmax >=7 mag, and with low extinction, E(B-V) ~ 0.5 mag (corresponding to NH = 3 x 10^21 cm-2) as determined from extinction and N(H) maps and ancillary observations.OB for target with V = 7.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 2800AA (near MgII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time.OB for target with V = 7.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 3130AA (near 7BeII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. BUFFER-TIME is 4/5 of STIS ETC returned simulation time./System/Volumes/Data/solaris/user1/armstrong/hst/working/OP-cache/18064-v08.xmlThe scheduling data was generated by CASM 34.1.CASM was run in Phase II mode.SECOND spectroscopic epoch of NOVA1 target. The observations of Visit 2 should occur within ~10-20 days after Visit 1 (Epoch1 the ToO trigger visit). We will work with assigned StScI contact scientist to optimimize follow-on cadence as the HST/STIS observations depends on the nova evolution (as described in the proposal). Both grating settings (c2762 and c3012) must be observed during a single visit to achieve the proposal science goals, as the source is temporally variable.(Tic-Visit
:proposal-id 18064
:visit-id "08"
:proposal-version -1
:trans-version "20260319"
:date "01-Jun-2026 13:36:49.0"
: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 887600
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 18064
:visit-id "08"
:obset-id "08"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18064
:visit-id "08"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2592.0
:al-overhead-at-end 0
:internal-dur-at-end 2303.0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2979
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 18064
:visit-id "08"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2592
:al-overhead-at-end 0
:internal-dur-at-end 578
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2979
:pcs-gap 0
)true20Generic Target is a ToO. The Epoch 2 observations are designed to follow Epoch 1 visit by ~10-20 days (when nova brightness has declined to V~8.5 mag).Epoch 2 Visit to NOVA 2 (ON-HOLD) for cadence assessment and science optimization after initial ToO trigger visit (Epoch 1).OB for target with V = 8.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 2800AA (near MgII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations.OB for target with V = 8.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 3130AA (near 7BeII line position). Split between orbits. TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations./System/Volumes/Data/solaris/user1/armstrong/hst/working/OP-cache/18064-v09.xmlThe scheduling data was generated by CASM 34.1.CASM was run in Phase II mode.THIRD spectroscopic epoch of NOVA1 target. The observations of Visit 3 should occur within ~10-20 days after Visit2. We will work with assigned StScI contact scientist to optimimize follow-on cadence as the HST/STIS observations depends on the nova evolution (as described in the proposal). Both grating settings (c2762 and c3012) must be observed during a single visit to achieve the proposal science goals, as the source is temporally variable.(Tic-Visit
:proposal-id 18064
:visit-id "09"
:proposal-version -1
:trans-version "20260319"
:date "01-Jun-2026 13:36:50.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 3
:saa-model "24"
:si-bright-earth-limb-angle 20.0
:data-volume 835392
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 18064
:visit-id "09"
:obset-id "09"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18064
:visit-id "09"
:orbit-number 1
:pcs-time 380
:si-vis-utilization 2592.0
:al-overhead-at-end 0
:internal-dur-at-end 2303.0
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2979
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 18064
:visit-id "09"
:orbit-number 2
:pcs-time 380
:si-vis-utilization 2592
:al-overhead-at-end 0
:internal-dur-at-end 316
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2979
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 18064
:visit-id "09"
:orbit-number 3
:pcs-time 380
:si-vis-utilization 2592
:al-overhead-at-end 0
:internal-dur-at-end 578
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 2979
:pcs-gap 0
)true30Generic Target is a ToO. The Epoch 3 observations are designed to follow Epoch 2 visit by ~10-20 days (when nova brightness has declined to V~9.5 mag).Epoch 3 Visit to NOVA 2 (ON-HOLD) for cadence assessment and science optimization after initial ToO trigger visit (Epoch 1).OB for target with V = 9.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=12 @ 2800AA (near MgII line position). TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations.OB for target with V = 9.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=9 @ 3130AA (near 7BeII line position). Split between orbits. TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. Two exposures (one orbit each) are required to reach the minimum SNR requirements outlined in the proposal for this epoch when the source has faded on brightness.OB for target with V = 9.5 mag, STIS ETC v33.2 | AOV Bruzual spectral type, E(B-V) = 0.3, SNR >=9 @ 3130AA (near 7BeII line position). Split between orbits. TIME-TAG mode for the MAMA detectors is used, as it offers several advantages and increases the legacy value of the observations. Two exposures (one orbit each) are required to reach the minimum SNR requirements outlined in the proposal for this epoch when the source has faded on brightness.