0 Assigned ID: 1803 ----- Attempting Submission 1 (Fri Mar 01 21:40:20 GMT 2013) ----- For some reason, despite updating the database and confirming the country and state [Germany] for Co-I Stancliffe is correct, the APT does not recognise the Institute for Astronomy in Bonn as being in Germany - and that Co-I Stancliffe qualifies as an ESA member The number of orbits used exceeds the number allocated David Goilimowski inserted visits A1 and A2, each containing one internal orbit of 13 ACS subarray bias frames obtained in WFC1-1K mode. These visits are linked to visit 02, which utilizes fully supported WFC1-1K subarrays. The two internal orbits should be charged to the Cycle 21 ACS Calibration Program. Contact David Golimowski (x4808) for more information. -40038131 ----- Attempting Submission 1 (Thu Jun 06 09:28:20 GMT 2013) ----- ----- Attempting Submission 2 (Sun Jul 13 16:58:26 GMT 2014) ----- ----- Attempting Submission 3 (Mon Jul 14 18:18:35 GMT 2014) ----- Orbit allocation exceeded because 2 internal calibration orbits have been inserted by STScI. These 2 orbits should be charged to the Cycle 21 ACS Calibration Program. Stellar Forensics V: A post-explosion view of the progenitor of SN 2011dh Recent studies have used high spatial resolution HST observations of supernova (SN) sites to directly identify the progenitors of core-collapse SNe on pre-explosion images. These studies have set constraints about the nature of massive stars and their evolution just prior to their explosion as SNe. Now, at late-times when the SNe have faded sufficiently, it is possible to return to the sites of these core-collapse supernovae to search for clues about the nature of their progenitors. We request time to conduct deep, late-time, high-resolution imaging with WFC3 UVIS and ACS WFC of the site of the Type IIb supernova 2011dh. The nature of the observed yellow supergiant progenitor conflicts with the predictions of stellar evolution models and our understanding of the optical and radio light curves of the subsequent supernova. We aim to: 1) Confirm our original identification, made in pre-explosion images, by confirming that the yellow supergiant is now missing; 2) Apply image subtraction techniques for the pre-explosion images with this late-time imaging to determine accurate photometry of the progenitor to constrain its temperature and luminosity; 3) conduct a deep search for the hypothesised hot binary companion; and 4) use the stellar population in the immediate vicinity of the SN to determine the reddening and extinction that affected the progenitor. HST provides the unique combination of high-resolution UV/optical imaging at very faint magnitudes that will facilitate this study. We require deep 5 colour imaging of the site of the Type IIb SN 2011dh at late-times. A progenitor object was identified in deep pre-explosion WFPC2 and ACS imaging; we wish to see if the object that was identified in the pre-explosion WFPC2 F336W and ACS F435W, F555W and F814W images has disappeared. In addition, we wish to ascertain the presence of a possible binary companion (either hot or cool) that may have been blended with the pre-explosion source, such that we also request an observation with the F225W filter (to probe a hot companion). This late-time imaging consists of a series of deep observations at the site of SN 2011dh, using WFC3 UVIS and the 1kx1k subarray and ACS and the 1kx1k subarry (to reduce readout times, since only a small area around the SN is actually required). The WFC3 UVIS observations are to be conducted in the F225W and F336W filters, while the ACS/WFC observations will use the F435W, F555W and F814W filters. We use these filter combinations to accurately match the corresponding pre-explosion HST observations. A standard 4-point box dither pattern is employed to aid the rejection of cosmic rays and hotpixels, as well as improve the sampling of the PSF. The observations are designed to go down to levels of m_F225W~25.5, m_F336W~26., m_F435W~27, m_F555W~27, m_F814W~27 (to a S/N of 3) to probe the nature of the faint background. Given the duration of the four individual exposures that make up the dither pattern, any nearby bright sources should not saturate (which we have confirmed with our previous photometry of the position of this SN and the BOT). The F225W and F336W observations use a larger box dither pattern to overcome the effects of local droplets in the UVIS field. The pattern A4 (from ISR WFC3-2010-09, Dahlen et al.) has been adopted, and I have calculated the values of the point spacing, line spacing, pattern orientation and angles between sides using their prescription - the resulting positions for the fovs for the individual pointings in this dither pattern (checked using Aladin) seem consistent with what I would expect for this pattern, but a check of my calculations would be useful. The F225W, F336W and F438W observations have been updated to include a postflash - which has been set to 12e- per pixel, in accordance with Anderson et al. 2012, for the WFC3 observation and 40e- following Smith et al. 2013. Post-flash is not required for the F555W and F814W observations. The 2 orbits per instrument have been broken into separate visits; however it will be useful to have them conducted at approximately similar times. This will enable us to evaluate any residual SN flux at UV and optical wavelength, using colour terms to derive the likely SN parameters and, hence, calculate the relative contamination at different wavelengths. In order to enable this science we require the SN to be as faint as possible, and loosely constrain the time window for the two visits to be in the second half of Cycle 21 (and loosely constrain Visit 2 to be conducted within 28 days of Visit 1). ------ Calibration Justification ------- A series of 26 ACS bias frames in the WFC1-1K subarray mode have been inserted directly into this program for the purpose of calibration of the ACS subarray images in visit 02. This subarray mode is fully supported, so the two internal orbits required to obtain these 26 frames should be charged to the Cycle 21 ACS Calibration Program. Contact David Golimowski (x4808) for more information. --------- Additional Comments ---------- We note that there are previous observations of the site of SN 2011dh in the HST archive. These observations were either taken before the SN exploded (i.e. with the progenitor still present) or post-explosion (i.e. with the SN still bright). We aim to make the authoritative study of this progenitor system by probing the disappearance of the putative YSG progenitor and probe any hot/cool companion star remaining at the SN position (with minimal contribution from SN). HOT STARS Default false true false false false SUPPORTED EXT-STAR SUPERGIANT O SUPERNOVA SUPERNOVA TYPE II This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F225W ACS/WFC Imaging No No F435W ACS/WFC Imaging No No F555W ACS/WFC Imaging No No F814W POS-TARG DITHER 0.265 LINE 0.187 false false 69.05 4 20.67 ACS-WFC-DITHER-BOX 2 false POS-TARG DITHER DITHER 2 4.26 WFC3-UVIS-DITHER-LINE false false 0.145 2 47.616 POS-TARG LINE 46.84 3 true /private/var/folders/2w/3zgcdz2n75d5pwpctrwqmvl000048_/T/OPVisit4260860821051330365.xml Timing link suitability includes constraints ([02 After 01 by at most 28.0 days]) The scheduling data was generated by CASM 22.2. 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CASM was run in Phase II mode. 2 orbits to acquire ACS/WFC F435W, F555W and F814W imaging of the site of SN 2011dh (Tic-Visit :proposal-id 13433 :visit-id "02" :proposal-version -1 :trans-version "20140605" :date "14-Jul-2014 14:16:35.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "27" :si-bright-earth-limb-angle 20.0 :data-volume 213328 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13433 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13433 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3024 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3358 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13433 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3133 :al-overhead-at-end 0 :internal-dur-at-end 270 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3358 :pcs-gap 0 ) true 2 0 /private/var/folders/2w/3zgcdz2n75d5pwpctrwqmvl000048_/T/OPVisit534160363060525782.xml Timing link suitability includes constraints ([Sequence (A1 A2) within 1.0 days]) The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. This orbit is charged to the Cycle 21 ACS Subarray Bias Calibration Program. (Tic-Visit :proposal-id 13433 :visit-id "A1" :proposal-version -1 :trans-version "20140605" :date "14-Jul-2014 14:16:36.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "27" :si-bright-earth-limb-angle 0.0 :data-volume 231104 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13433 :visit-id "A1" :obset-id "A1" :pcs-mode "GYRO" ) (Tic-Orbit :proposal-id 13433 :visit-id "A1" :orbit-number 1 :pcs-time 0 :si-vis-utilization 0 :al-overhead-at-end 0 :internal-dur-at-end 1781 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) true 1 0 /private/var/folders/2w/3zgcdz2n75d5pwpctrwqmvl000048_/T/OPVisit1917940261372854401.xml Timing link suitability includes constraints ([Group (02 A2) Within 14.0 days] [Sequence (A1 A2) within 1.0 days]) The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. This orbit is charged to the Cycle 21 ACS Subarray Bias Calibration Program. (Tic-Visit :proposal-id 13433 :visit-id "A2" :proposal-version -1 :trans-version "20140605" :date "14-Jul-2014 14:16:37.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "27" :si-bright-earth-limb-angle 0.0 :data-volume 231104 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13433 :visit-id "A2" :obset-id "A2" :pcs-mode "GYRO" ) (Tic-Orbit :proposal-id 13433 :visit-id "A2" :orbit-number 1 :pcs-time 0 :si-vis-utilization 0 :al-overhead-at-end 0 :internal-dur-at-end 1781 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3222 :pcs-gap 0 ) true 1 0