Digging deep into massive star variability: Do massive stars vary due to internal gravity waves or stellar winds?

0 Assigned ID: 1014 ----- Attempting Submission 1 (Sat Mar 07 00:31:02 GMT 2020) ----- HST Phase I Proposal 1014 successfully submitted. Receipt: # 1014-1 ----- Attempting Submission 2 (Sat Mar 07 00:57:28 GMT 2020) ----- Unschedulable Visit STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME Unschedulable Visit STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME Unschedulable Visit STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME Unschedulable Visit STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME Unschedulable Visit STIS TIME-TAG EXPOSURE GENERATES HEAVY DATA VOLUME After consultation with Daniel, I have updated the Peak Ups to be imaging instead of in dispersed light. To do this, I changed each "Peak up" and "Re-Peak Up" action to be in the MIRROR spectral element and removed the wavelength. I also updated the exposure time to 0.3 s and the ETC run used to determine this signal to noise. We have updated the Proposal Description to mirror these changes. changed visit 01 to non-CVZ, 83m visibility. tweaked to 89m visibility added accum alternates as on hold, visits 11-18 -1690770964 ----- Attempting Submission 1 (Tue Jun 30 19:12:45 GMT 2020) ----- HST Phase II Proposal 16304 successfully submitted. Receipt: # 16304-1 ----- Attempting Submission 2 (Wed Jul 01 17:29:37 GMT 2020) ----- HST Phase II Proposal 16304 successfully submitted. Receipt: # 16304-2 ----- Attempting Submission 3 (Thu Jul 02 13:09:43 GMT 2020) ----- ----- Attempting Submission 4 (Mon Nov 30 14:00:47 GMT 2020) ----- ----- Attempting Submission 5 (Tue Dec 15 13:23:34 GMT 2020) ----- HST Phase II Proposal 16304 successfully submitted. Receipt: # 16304-5 ----- Attempting Submission 6 (Tue Dec 15 13:46:12 GMT 2020) ----- ----- Attempting Submission 8 (Thu Dec 24 19:47:07 GMT 2020) ----- The errors correspond to scheudling and time-tag mode issues that have been cross-referenced with the PC. Digging deep into massive star variability: Do massive stars vary due to internal gravity waves or stellar winds? Recent high-precision and high-cadence space-based missions have used asteroseismology to dig deep to the cores of low-mass stars and determine their internal properties. Much of the metals produced throughout the history of the Universe are forged deep in the cores of massive stars, but astonishingly little is known about the core properties of the most massive stars. Recent TESS observations found stochastic variations of blue supergiants that could be the long-sought signal of internal gravity waves near the convective cores of massive stars. These oscillations may revolutionize our understanding of the cores of the most massive stars, but winds from the same stars vary with similar periods and patterns as these stochastic oscillations. Here, we propose a 26 orbit HST/STIS E140M time-series of the stellar winds from one blue LMC supergiant, SK-67 166, which is observed to have stochastic oscillations on 0.5 day periods and has a rotation rate of 4 days. This proposed time-series will be concurrent with future TESS observations, have the same cadence as TESS, and have a total baseline of 10 days to determine whether the TESS oscillations correspond to changes in the stellar winds or result from internal gravity waves. If the stochastic oscillations are confirmed to be due to internal gravity waves, high-cadence observations and asteroseismology models can determine the interior properties of the most massive stars. If the TESS oscillations are in phase with the stellar wind variations, TESS can determine crucial properties of the elusive stellar winds. Either outcome will dramatically impact our view of the massive stars that drive galactic and chemical evolution. The goal of this proposal is to get a time series analysis of the FUV spectrum of the LMC O 4Ia star, HD269698. We will measure how the FUV spectral features vary with time and correlate it with concurrent TESS variability observations. Previous TESS observations show that the luminosity of this star varies on a nearly half-day period. We will use these new HST observations to determine how the stellar photosphere varies on multiple half-day periods. Thus, the main aspect of this proposal is to obtain simultaneous observations of the star with HST/STIS and TESS with the same cadence as the upcoming concurrent TESS over multiple periods of the star. TESS observes HD269698 on both 2- and 30-minute cadences. The HST/STIS Time-Tag observations will allow both cadences to be tested for stellar oscillations. We break up the observations into two segments: (1) observations that aim to densely sample the full temporal period of the star (2) longer more sparsely sampled baseline observations will constrain subsequent low frequency patterns in the photosphere. The densely sampled configuration will have 15 orbits in 3 visits, one of which is a CVZ orbit, which are 5 orbits each and 1 visit with 3 orbits. These will be as closely sampled as possible (while avoiding the SAA) to sample two full oscillatory periods. The sparsely sampled observations will consist of four visits of 2-orbits each, each sampled between 0-2 days after the densely sampled observations. The timing is very important to this project. It cannot occur when TESS is not observing this object. TESS will continuously observe the object every 2 and 30 minutes from November 19th, 2020 to December 17th 2020. The 2-minute cadence of TESS is a crucial reason why the TIME-TAG observations are required. Further, the TIME-TAG observations are required to exactly match the TESS and HST observations in time. The first segment of densely packed observations requires nearly contiguous observations of the star and will require a Continuous Viewing Zone orbit. To optimize continuous temporal coverage, we have exposures that are as close to the 40-minute maximum of wavelength calibration and fit within each orbit. This will enable the STIS observations to be as closely aligned in time with the TESS observations as possible. We require wavelength calibrations between each of these exposures to ensure proper relative wavelength calibrations. There will be one 3-orbit visit immediately after the 5 orbit visits to complete the required full oscillatory period of the star. This visit must be as close in time to the CVZ orbits as possible to sample the full oscillatory period. We will obtain the wavelength calibration while the object is not observable. The sparsely sampled configuration will consist of 4 visits each of 2-orbits. These sparsely sampled orbits will have 1 exposure on the first orbit and 1 8-minute exposure to finish the first orbit, and 2 exposures on the second orbit. This will enable the STIS observations to be as closely aligned in time with the TESS observations. We will use the STIS E140M grating with the 0.2x0.2 slit. We will use the time-tag mode and perform a wavelength calibration after each long observation to ensure proper relative wavelength calibration which is crucial to compare the temporal variations of the stellar features. We calculated the required exposure times from previous IUE and FOS observations of this star which observe a flux of 2e-12 erg/s/cm/A at 1370A. This will deliver a signal-to-noise of 36 at 1370A in each 40-minute exposure. Using the TIME-TAG observations, we will break these 40-minute exposures up to sample the TESS observations. Even for a 2 minute observation, which matches the shortest TESS cadence, the ETC predicts a signal-to-noise ratio at 1370 of 8. The STIS ETC gives the expected buffer time of 163, thus we take the total buffer time of 4/5ths this to be 130. Since we are using the 0.2x0.2 slit, we will require precise pointing. Thus, on the first orbit of each visit we will first perform an Acq followed by an Acq/PEAK in imaging mode (undispersed light) with the 0.06x0.2 apeture. To determine the exposure times on the observations we use the STIS ETC with the observed V-band magnitude of 12.22, the observed E(B-V) = 0.10, and a Castelli-Kurucz O5V 41000 model with the same observed stellar temperature as the proposed star. During the long orbis, we will perform another Acq/PEAK to recenter the star within the slit. This occurs in the middle of the third orbit. This will ensure that the object always remains centered. Our team has extensive history dealing with TESS high-cadence observations and FUV observations, including that of massive stars. PI Chisholm is an expert at FUV spectral observations and stellar wind characterization (Chisholm et al. 2019). Co-I Leitherer has extensive history with FUV spectral observations of massive stars (e.g. Leitherer et al. 1995). Co-I Tayar is an expert on TESS observations and has the required expertise for the TESS light curve and time-series observations (e.g. Tayar et al. 2015). Co-I Bard has modeled the stellar atmospheres of massive stars and included the impacts of magnetic fields. Stellar Physics and Stellar Types 6 false false true false false false 1 true SUPPORTED EXT-STAR SUPERGIANT O NO The star HD-269698 is a O 4Ia star within the LMC. The coordinates and proper motions are drawn from TESS version 20190415 measurements accessed through the MAST archive. The E(B-V) = 0.98 from TESS using Schlegel. SK-67-166 TIC-425083410 J2000 J2000 Continuum flux of 2E-12 erg/s/cm^2/AA at 1370 from previous IUE and FOS spectra. The TESS Magnitude (Tmag) is 11.1492 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/FUV-MAMA Spectroscopic No No E140M 1425 1608838128394 /private/var/folders/dv/kllm6qvx1m3bq_0v7lp6wwtc000702/T/OPVisit17604117365484544536.xml The scheduling data was generated by CASM 28.2. 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1608838164125 85 /private/var/folders/dv/kllm6qvx1m3bq_0v7lp6wwtc000702/T/OPVisit16385269799935640036.xml (Tic-Visit :proposal-id 16304 :visit-id "14" :proposal-version -1 :trans-version "20200619" :date "24-Dec-2020 14:29:23.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1566384 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16304 :visit-id "14" :obset-id "14" :pcs-mode "FGS" ) (Tic-Orbit :cvz T :proposal-id 16304 :visit-id "14" :orbit-number 1 :pcs-time 393 :si-vis-utilization 27662 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 0 :low-sky "N" :pcs-visibility 0 :pcs-gap 0 ) true 5 0 This set of visits uses accum exposures instead and is on hold in case the data volume of visits 1-8 cannot be accomodated. 1608838352787 /private/var/folders/dv/kllm6qvx1m3bq_0v7lp6wwtc000702/T/OPVisit6142485042667275577.xml (Tic-Visit :proposal-id 16304 :visit-id "15" :proposal-version -1 :trans-version "20200619" :date "24-Dec-2020 14:32:32.0" :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 644240 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16304 :visit-id "15" :obset-id "15" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16304 :visit-id "15" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2991 :al-overhead-at-end 81 :internal-dur-at-end 132 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3486 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16304 :visit-id "15" :orbit-number 2 :pcs-time 392 :si-vis-utilization 3094 :al-overhead-at-end 81 :internal-dur-at-end 132 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3486 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16304 :visit-id "15" :orbit-number 3 :pcs-time 392 :si-vis-utilization 3094 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3486 :pcs-gap 0 ) true 3 0 This set of visits uses accum exposures instead and is on hold in case the data volume of visits 1-8 cannot be accomodated. 1608838169833 /private/var/folders/dv/kllm6qvx1m3bq_0v7lp6wwtc000702/T/OPVisit13466905257271951403.xml (Tic-Visit :proposal-id 16304 :visit-id "16" :proposal-version -1 :trans-version "20200619" :date "24-Dec-2020 14:29:29.0" :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 400672 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16304 :visit-id "16" :obset-id "16" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16304 :visit-id "16" :orbit-number 1 :pcs-time 393 :si-vis-utilization 3093 :al-overhead-at-end 81 :internal-dur-at-end 132 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3486 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16304 :visit-id "16" :orbit-number 2 :pcs-time 392 :si-vis-utilization 3094 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3486 :pcs-gap 0 ) true 2 0 This set of visits uses accum exposures instead and is on hold in case the data volume of visits 1-8 cannot be accomodated. 1608838172002 /private/var/folders/dv/kllm6qvx1m3bq_0v7lp6wwtc000702/T/OPVisit15101932300888768431.xml (Tic-Visit :proposal-id 16304 :visit-id "17" :proposal-version -1 :trans-version "20200619" :date "24-Dec-2020 14:29:31.0" :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 400672 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16304 :visit-id "17" :obset-id "17" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16304 :visit-id "17" :orbit-number 1 :pcs-time 393 :si-vis-utilization 3093 :al-overhead-at-end 81 :internal-dur-at-end 132 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3486 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16304 :visit-id "17" :orbit-number 2 :pcs-time 392 :si-vis-utilization 3094 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3486 :pcs-gap 0 ) true 2 0 This set of visits uses accum exposures instead and is on hold in case the data volume of visits 1-8 cannot be accomodated. 1608838173489 56.5 /private/var/folders/dv/kllm6qvx1m3bq_0v7lp6wwtc000702/T/OPVisit5339518412746641728.xml (Tic-Visit :proposal-id 16304 :visit-id "18" :proposal-version -1 :trans-version "20200619" :date "24-Dec-2020 14:29:33.0" :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 314208 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16304 :visit-id "18" :obset-id "18" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 16304 :visit-id "18" :obset-id "B8" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16304 :visit-id "18" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2997 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3390.0 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16304 :visit-id "18" :orbit-number 2 :pcs-time 393 :si-vis-utilization 2997 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3390.0 :pcs-gap 0 ) true 2 0 This set of visits uses accum exposures instead and is on hold in case the data volume of visits 1-8 cannot be accomodated.