0Assigned ID: 3124
----- Attempting Submission 1 (Fri Mar 25 03:42:47 GMT 2022) -----
HST Phase I Proposal 3124 successfully submitted.
Receipt: # 3124-1
----- Attempting Submission 2 (Fri Mar 25 23:45:53 GMT 2022) -----Dear Alison:
OK...I have made the three visits (19,20,21) with
ORIENT values of 271 degrees.
This put the replacement observations in late May.
Let me know if this will work...or not.
-Rob Fesen2010294314----- Attempting Submission 1 (Mon Jul 04 23:41:13 GMT 2022) -----
HST Phase II Proposal 17210 successfully submitted.
Receipt: # 17210-1
----- Attempting Submission 2 (Wed Jul 06 17:55:39 GMT 2022) -----
----- Attempting Submission 3 (Mon Aug 29 21:38:49 GMT 2022) -----
HST Phase II Proposal 17210 successfully submitted.
Receipt: # 17210-3
----- Attempting Submission 4 (Wed Aug 31 04:13:18 GMT 2022) -----
----- Attempting Submission 5 (Thu Sep 01 14:40:48 GMT 2022) -----
HST Phase II Proposal 17210 successfully submitted.
Receipt: # 17210-5
----- Attempting Submission 6 (Thu Sep 01 17:26:38 GMT 2022) -----
----- Attempting Submission 7 (Mon Feb 20 18:24:21 GMT 2023) -----
HST Phase II Proposal 17210 failed submission.
----- Attempting Submission 8 (Mon Feb 20 18:25:56 GMT 2023) -----
----- Attempting Submission 9 (Mon Feb 20 20:49:21 GMT 2023) -----The targets have not changed.A Multi-Bandpass ACS Survey of Cassiopeia A: Keeping Up with its Rapidly Evolving StructureThe supernova remnant Cassiopeia A (Cas A) provides the clearest look at the properties and explosion dynamics of a core-collapse supernova (CCSN). With an explosion date around 1670, Cas A is the youngest Galactic core-collapse SNR known and, at an estimated distance of 3.4 kpc, it is also among the closest and brightest. However, Cas A exhibits significant changes in its emission structure on timescales as short as 1-2 years, and large-scale changes in one or two decades, meaning that upcoming multi-wavelength investigations require nearly contemporaneous, high-resolution optical observations.
This proposal describes a multi-bandpass ACS imaging program with the goals of: 1) a high-resolution optical survey that can discriminate O-Ne rich ejecta from S-Ar-Ca rich ejecta, thereby assisting new multi-wavelength studies of Cas A's ejecta and its dust content, including JWST approved Cycle 1 Near and Mid-IR observations, deep new 50 to 100 ksec Chandra high spatial resolution X-ray observations, and high spectral resolution X-ray data from the upcoming XRISM mission, 2) resolve the remnant's newly emerging and freshly reverse shocked O-Ne rich and S-Ar-Ca rich ejecta along the southern limb and north-central region, 3) add new constraints on reverse shock velocity estimates across multiple regions, and 4) measure the proper motions of the remnant's highest-velocity (8000 to 14,500 km/s) outer ejecta providing improved age and explosion center estimates plus deceleration measurements probing the density and arrangement of the local circumstellar medium as well as ejecta knot lifetimes.The goal is to obtain a set of ACS/WFC images nearly identical to those obtained in March and December 2004. These will yield excellent discrimination between O-Ne rich from S-Ar-Ca rich ejecta through the use of the ACS F450W and F775W filters sensitive to O-Ne rich SN ejecta via oxygen line emissions of [O III] 4959,5007 and [O II] 7319,7330. Likewise, detection of S-Ca rich ejecta through the use of ACS filters F625W and F850LP sensitive to sulfur-rich ejecta through [S II] 6716,6731 [S III] 9069,9531 and [S II] 10350 lines.
There are six (6) target regions be imaged with virtually the same ORIENT angle of around 90 degrees to fully cover Cas A wide E-W dimension. To do this, we have constructed an observing program of eight (8) visits. Each of the first six visits target one remnant region in three ACS filters (F625W, F775W, and F850LP) using roughly 2 x 590 sec exposures plus 2 x 590 sec exposures dithered by a two point the ACS-WFC-DITHER-LINE, plus a smaller, secondary two point ACS-WFC-DITHER-LINE to help with hot pixels and cosmic rays. Thus 1 orbit is needed for each filter. A single visit will comprise three orbits for three filters for each region The 7th and 8th visits each target three of the six remnant regions using just the F475W filter, with expoures again of roughly 2 x 590 sec dithered by the two ACS-WFC-DITHER-LINE dithers.
Thus, we will have ~ 4 x 590 sec exposures for each of the four filters (F450W, F625W, F775W, and F850LP) for six target regions in Cas A. Note: We have revised the coordinates of the six targets, increasing the RA and Dec by 10-20 arcseconds to permit detections of high-speed ejecta knots (mu = 0.55"/yr) located north and east of the remnant's main shell and first detected in 2004 ACS/WFC images.
We have also revised the six target coordinates to avoid having bright stars just off the ACS/WFC and away from potential "Dragon Breath"
light scatterings from bright stars located just off the FOV.
All eight visits can be done in the 14 day window between 28 Nov 2022 and 12 Dec 2022. We have included a timing request for this time frame to match JWST Cycle 1 observations of Cas A, as noted in our Phase I submission. First set of JWST data are MIRI images have now been obtained between Jul 28, 2022 - Aug 8, 2022. The remaining observations are NIRCam images and are scheduled for Nov 4-14, 2022.
Thus having the HST data taken in late Nov/early Dec 2022 is ideal.Prof. Robert Fesen (PI) is an expert on supernova remnants and Cas A in particular, having authored nearly two dozen refereed papers on it. He has been the PI on several Hubble programs on Cas A.
Prof. Dan Milisavljevic is an expert in multiwavelength observations and interpretations of supernovae and supernova remnants. He has published on the 3D kinematic and chemical properties of Cas A (Milisavljevic & Fesen 2013, 2015), including its high-velocity jet-like outflows (Fesen & Milisavljevic 2016).
Dr. Dan Patnaude is an expert in correlations between X-ray and optical emission in young supernova remnants. He is also an expert in shock dynamics and applying machine learning techniques to X-ray observations of supernova remnants.
Prof. Roger Chevalier is an expert on Cas A who has undertaken theoretical and observational studies of the emission and dynamics of Cas A begining in the 1970s.
Dr. John Raymond has performed both theoretical studies and data analysis related to both shocked and unshocked ejecta in Cas A, as well as the clumpy circumstellar material seen around the remnant.
Dr. Tea Temim is an expert in the evolution of supernova remnants and pulsar wind nebulae, with particular interest in dust production and processing in supernovae.
Dr. Kathryn Weil is an expert in supernova-supernova remnant connections. She has studied the circumstellar environment around Cassiopeia A (Weil+ 2020) and connected late-time spectroscopy of supernovae with ejecta-CSM interaction and dust.
Dr. William Blair is an expert in the UV and optical emissions from both Galactic and extragalactic SNRs. He is also very familiar with HST's data and its analysis.
Dr. Pat Slane is an expert on the X-ray emissions from SNRs, especially young SNRs like Cas A.
Prof. Bon-Chul Koo is an expert in supernova remnants. He has performed near infrared studies of both shocked and unshocked supernova ejecta material as well as the dense circumstellar knots in Cas A (Koo+ 2018, 2020).Stellar Physics and Stellar TypesStellar Populations and the Interstellar Medium6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDISMEJECTAEMISSION LINE NEBULASNRJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRJ2000J2000ACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF775WACS/WFCImagingNoNoF850LPACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF775WACS/WFCImagingNoNoF850LPACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF775WACS/WFCImagingNoNoF850LPACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF775WACS/WFCImagingNoNoF850LPACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF775WACS/WFCImagingNoNoF850LPACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF850LPPOS-TARGDITHERDITHER23.034ACS-WFC-DITHER-LINEfalsefalse0.364285.29POS-TARGACS-WFC-DITHER-LINE47.231trueThe scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.(Tic-Visit
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)true30The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.166960253000087.80000000000001(Tic-Visit
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)true30