Please let me know if this submission is OK.
Thank You.-2060871898Assigned ID: 6229
----- Attempting Submission 1 (Wed Apr 09 14:24:39 GMT 2025) -----
HST Phase I Proposal 6229 successfully submitted.
Receipt: # 6229-1
----- Attempting Submission 2 (Wed Apr 09 19:32:35 GMT 2025) -----
HST Phase I Proposal 6229 successfully submitted.
Receipt: # 6229-2
----- Attempting Submission 3 (Thu Apr 10 02:43:06 GMT 2025) -----Hi Alison:
Here's my revised submitted Phase II submission for GO 18127
which includes changes to the pattern used and ORIENT settings
to allow the data to be taken only in August 2026.
Thanks for all your help.
-Rob Fesen-243207974----- Attempting Submission 1 (Mon Jul 28 22:33:27 GMT 2025) -----
HST Phase II Proposal 18127 successfully submitted.
Receipt: # 18127-1
----- Attempting Submission 2 (Tue Aug 05 03:16:26 GMT 2025) -----
HST Phase II Proposal 18127 successfully submitted.
Receipt: # 18127-2
----- Attempting Submission 3 (Thu Aug 07 18:11:10 GMT 2025) -----
----- Attempting Submission 4 (Tue Oct 21 23:30:04 GMT 2025) -----Imaging the Exceptional Nebulosity of the Suspected Iax Supernova Remnant of 1181 ADA recently discovered Galactic nebula appears to be the likely remnant of the historic Galactic guest star of 1181 AD which was a subluminous supernova (SN) outburst. The remnant's striking and unique filamentary morphology, relatively low 1200 km/s expansion velocity, the extraordinary properties of its central star, plus its unusual elemental make-up matches predicted properties of the poorly understood Iax subclass of H-poor thermonuclear supernovae. As one of only five Milky Way supernova reported in the past millennium, we propose WFC3/IR images sensitive to its sulfur and iron emission lines to reveal its subarcsecond structure, compare these line emissions to the dust distribution seen in the mid-infrared, and understand the luminosity history of the central star's 16,000 km/s wind. These data will provide crucial insights into the nature of Iax supernovae.The goal is to obtain near infrared [S II], [S III], and [Fe II] emission line images of Pa 30 using the WFC3/IR camera that are deeper and of higher resolution than ground-based [S II] images. WFC3/IR offers good filament detections due to its large pixels, less extinction than in the optical (Pa 30: E(B-V ) ~ 0.90 mag), and high throughputs. WFC3/IR also allows the imaging of Pa 30's [Fe II] 12,570 - 12,946 Ang emission which is expected to be strong based on spectra of ejecta of other young SNRs (e.g., Cas A, Crab, and Kepler]).
Images are to be taken in these two filters centered at four regions using four orbits for each region, thus requring 4 x 4 orbits = 16 orbits done in 12 visits, keeping within the requirment of visits being less than or equal to 3 orbits.
Both the F098M and F127M image data would be taken in standard MULTACCUM mode with aperture IR-FIX and SAMPSEQ= SPARS50 or SPARS100and NSAMP=13 requiring two orbits (46.1 minutes each) to execute for each of the four target region of the Pa 30 nebula. The primary dither patten would be a four point WFC3-IR-DITHER-BOX-MIN. This dither patten will recover more than 95% of the detector's bad pixels.
Pa 30's filaments are relatively faint with the brighter ones having a measured [S II] 6716,6731 flux of 2.5 x 10^(-17) erg cm^2 s^-1. Ground-based spectra suggests the [S III] 9531 Ang line is similar in strength to the [S II] 6716 Ang line. Adopting this and the sum of [S II] 10,290-10,373 lines equal to the strength of [S III] 9531, the WFC3 ETC yield a S/N of 14 for a 45 minute exposure. This should insure a good detection in two orbits on Pa 30's fainter filaments for each filter even given Pa 30's unknown sub-arcsecond structure.
To cover the entire remnant without the "Death Star" defect, we requested and was approved for ORIENT settings to enable a complete mosaic. We have chosen the specific ORIENT of 45, 135, or 225 degrees.Prof. Robert Fesen (PI) is an expert in supernova remnants. He has studied several young Galactic SNRs with HST (Fesen 2001, Fesen+ 2006, Fesen+ 2011, Fesen & Milisavljevic 2016), and discovered the young type Ia SNR (S And: SN 1885) in M31. He has also done extensive work on the Cassiopeia A SNR (SN ~1670) using
HST data and was the lead author on the paper that first revealed the striking morphology of the Pa 30 nebula (Fesen et al. 2023, ApJL).
Prof. Dan Milisavljevic (Co-I) is an expert in multiwavelength observations and interpretations of supernovae and supernova remnants. He has published on the 3D kinematic and chemical properties of Cassiopeia A (Milisavljevic & Fesen 2013, 2015), and the Crab Nebula (Martin, Milisavljevic, Drissen 2021). He also investigates exotic supernovae, including Ca-rich transients (Milisavljevic et al. 2017; Dong, Milisavljevic et al. 2022). He is PI of a JWST Cycle 1 proposal on Cassiopeia A and PI on JWST Cycle 4 on the Kepler SNR.
Dr. Tea Temim (Co-I) is an expert in the evolution of supernova remnants and pulsar wind nebulae, with particular interest in dust production and processing in supernovae. She led numerous studies focused on infrared imaging and spectroscopy of supernova remnants and will help with the data analysis, modeling, and interpretation of data.
Dr. Dan Patnaude (Co-I) 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.
Dr. Dillon Dong (Co-I) is an expert on analysis of radio emission from faint extragalactic sources and have used the VLA Sky Survey (VLASS) to detect and understand emission from young pulsar wind nebulae and other transient sources and has studied the SN 1181's radio emission.Stellar Populations and the Interstellar MediumStellar Physics and Stellar Types6falsefalsefalsefalsefalsefalsefalseSUPPORTEDISMEJECTAEMISSION LINE NEBULASNRYESJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRYESJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRYESJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRYESJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRYESJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRYESJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRYESJ2000J2000ISMEJECTAEMISSION LINE NEBULASNRYESJ2000J2000WFC3/IRImagingNoNoF098MWFC3/IRImagingNoNoF127MWFC3/IRImagingNoNoF098MWFC3/IRImagingNoNoF127MWFC3/IRImagingNoNoF098MWFC3/IRImagingNoNoF127MWFC3/IRImagingNoNoF098MWFC3/IRImagingNoNoF127MPOS-TARGDITHERDITHER423.02WFC3-IR-DITHER-BOX-MIN35.212false74.653true0.36589.2870.57240.713POS-TARGWFC3-IR-DITHER-BOX-UVIS18.5282falseHst Same orient constraint links visits (01 02 03 04 05 06 07 08 09 10 11 12)The scheduling data was generated by CASM 33.1.CASM was run in Phase II mode.(Tic-Visit
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