Imaging the Crab Nebula-Like Supernova Remnant 3C 58

Removed ORIENT from visit 01 as per discussion with PC (but still wish the first target in visit to be done in ORIENT 129-130), and changed the off-band filter used from F665N to F645N (as per OK from PC) to assure no line emission is detected in offband images ----- Attempting Submission 2 (Mon Jul 06 18:09:21 GMT 2009) ----- ----- Attempting Submission 3 (Mon Sep 21 21:20:51 GMT 2009) ----- Imaging the Crab Nebula-Like Supernova Remnant 3C 58 The Galactic supernova remnant 3C 58 shares several important properties with the Crab Nebula. It possesses a young, rapidly spinning pulsar and an associated compact optical/IR synchrotron wind nebula. This makes 3C 58, along with the Crab and PSR B0540-69 in the LMC, only the third such PWN detected in the optical and IR. Also like the Crab, 3C58 has been associated with a historically reported `guest star', in this case, the apparent SN of 1181 CE. Its optical nebulosity contains an unusually large fraction of shocked circumstellar material, with the remnant's high-velocity, N-rich ejecta knots exhibiting a strong bi-polar expansion asymmetry. Despite having a relatively extensive optical nebula, it is the only young and nearby Galactic SNR that has not yet been imaged by HST. However, some recent deep, high-resolution Gemini images show a surprising amount of fine-scale filament detail, revealing some peculiar optical emission morphologies. Here we propose a WFC3 imaging survey of 3C 58 in order to investigate: 1) the optical luminosity and emission efficiency of the remnant's young, 65.7 ms pulsar PSR J0205+6449 thereby providing a rare testing of pulsar emission models, 2) the effect of the remnant's expanding synchrotron nebula on the formation of Rayleigh-Taylor instabilities in its optical filaments like that observed so far only in the Crab through HST imaging, and 3) the fine-scale structure of 3C 58's slow moving circumstellar and high-velocity SN ejecta and the morphological and distribution differences between them.

This project is to use WFP3 to image the galactic supernova remnant 3C58. The object is broken up into 7 target fields. For all 7 pointings, the filters F657N and F665N will be used to obatin on/off Halpha images. For the remnant's central region, two other filter images will be taken in addition to the F657N and F665N ones. These are SDSS r and i filters (F625W and F775W). ISM AND CIRCUMSTELLAR MATTER 12 false 0.0 0.0 false false false false false false SUPPORTED ISM SNR J2000 02 06 1.4220 +64 48 13.10 J2000 ISM SNR J2000 02 06 1.3970 +64 45 45.70 J2000 ISM SNR J2000 02 05 38.1810 +64 48 50.00 J2000 ISM SNR J2000 02 05 38.8800 +64 47 6.60 J2000 ISM SNR J2000 02 05 39.2330 +64 43 35.90 J2000 ISM SNR J2000 02 05 15.3720 +64 48 30.00 J2000 ISM SNR J2000 02 05 16.2000 +64 45 57.71 J2000 WFC3/UVIS Imaging No No F657N WFC3/UVIS Imaging No No F665N WFC3/UVIS Imaging No No F657N WFC3/UVIS Imaging No No F665N WFC3/UVIS Imaging No No F657N WFC3/UVIS Imaging No No F665N WFC3/UVIS Imaging No No F657N WFC3/UVIS Imaging No No F665N WFC3/UVIS Imaging No No F625W WFC3/UVIS Imaging No No F775W WFC3/UVIS Imaging No No F850LP WFC3/UVIS Imaging No No F657N WFC3/UVIS Imaging No No F665N WFC3/UVIS Imaging No No F657N WFC3/UVIS Imaging No No F665N WFC3/UVIS Imaging No No F657N WFC3/UVIS Imaging No No F665N POS-TARG DITHER 1.5 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE 1

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