Kinematics of Young SNRs P. Frank Winkler, Middlebury College Conference on SNe, YITP, Kyoto 30 October 2013 Collaborators: Knox Long Steve Reynolds Rob Petre William Blair Brian Williams Satoru Katsuda Dan Milisavljevic Undergraduate Students: Adele Plunkett Karl Twelker Claudine Reith Guarav Gupta Jillian Garber

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Kinematics of Young SNRs P. Frank Winkler, Middlebury College Conference on SNe, YITP, Kyoto 30 October 2013 Collaborators: Knox Long Steve Reynolds Rob Petre William Blair Brian Williams Satoru Katsuda Dan Milisavljevic Undergraduate Students: Adele Plunkett Karl Twelker Claudine Reith Guarav Gupta Jillian Garber

Kinematics of Young SNRs  G : Core-collapse SNR, ~ 3000 years old; “Cas A’s older cousin”  Similarities to other young C-C SNRs  SN 1006: Type Ia SN, 1007 years old F. Winkler Kyoto, “Young” = < few thousand years Composition and/or kinematics hold traces of the explosion

O-rich SNR G (MSH 11-54)  Optical knots: pure ejecta: O, Ne, no H, almost no S  X-ray emission enriched by heavy elements, except along central belt (Park 2002, 2004, 2007 — see Poster 60)  Active pulsar and associated PWN (Hughes 2001, Camillo 2002)  Distance ~6 kpc (Gaensler & Wallace 2003); Diameter ~8' => 15 pc PSR Park (2007) F. Winkler Kyoto, [O III] 5007

Kinematics I: Proper Motions  Proper motions from 7 epochs: F. Winkler Kyoto,  Continuum-subtracted [O III] image shows expansion center and proper motions of 67 filaments projected forward 1000 years (Winkler et al. 2009)  Trajectories are ballistic: proper motion well correlated with distance from center

Kinematics I: Proper Motions  Above: 2’ x 2’ section of unsubtracted [O III] image shows PSR J  Backwards extrapolation gives expansion center and age ~3000 years  PSR transverse velocity = 440 km/s to SE (at 6 kpc) F. Winkler Kyoto,

 Longslit and multi-fiber spectra from 1.5m and 4m telescopes at CTIO  Doppler velocities for 93 spectroscopically distinct knots  –1500 km/ s < V r < km/s  Gives a high-resolution 3-D picture of O-rich ejecta in G292  Results qualitatively similar to F-P spectra of Ghavamian 2005, extending to outer knots, and with higher resolution CTIO image credit: T. Abbott and NOAO/AURA/NSFF. Winkler Kyoto, Kinematics II: Doppler Mapping V r < – 300km/s V r > km/s |V r | < 300 km/s

 Fastest knots are distributed along broad, bipolar jets, roughly N-S  Brightest knots are along "eastern spur” CTIO image credit: T. Abbott and NOAO/AURA/NSFF. Winkler Kyoto, Kinematics II: Doppler Mapping V r = – 1500km/s V r = km/s V r ≈ 0 km/s

CTIO image credit: T. Abbott and NOAO/AURA/NSFF. Winkler Kyoto, Kinematics II: Doppler Mapping  Fastest knots are distributed along broad, bipolar jets, roughly N-S  Brightest knots are along "eastern spur” PSR

Blue = keV (Park 07) Red = 24  m (dust, Ghavamian 2012) Green = [O III]  [O III]  keV (Park 2007)  24 μm (Ghavamian 2012) Multiwavelength Relationship  Dense circumstellar belt gives brightest X-rays, IR from dust  Encounter with belt on East drives reverse shock into ejecta to give bright spur

3 more C-C SNRs with bipolar jets/cones  Cas A (Age ~ 340 yr) (Milisavljevic & Fesen 2013)  3C58 = SN 1181? (Fesen+ 2008)  1E0102.2–7219 (SMC, age ~2000 yr) (Vogt & Dopita 2010) And one that's different:  Puppis A (age ~ 4000 yr) (Winkler+ 1988; J. Garber thesis) NS recoil measured: at 700 km/s (Becker+ 2012) CTIO image credit: T. Abbott and NOAO/AURA/NSFF. Winkler Kyoto, Other Core-Collapse SNR Examples Chandra HRI

SN 1006 SN Ia remnant Synchrotron limbs Shocked ISM (primarily) Shocked Ejecta

Chandra ACIS 2012 (PFW+ ApJ, submitted) SN 1006 SN Ia remnant

Chandra ACIS 2003 (Cassam-Chenai 2008) SN 1006 SN Ia remnant

Deep Hα image  Faint emission surrounding shell  Intriguing interior features

Ejecta Bullets + Balmer Bowshocks Ejecta reaching outer boundary of shell (neutral H) Green = X-ray Red = Hα

Large Scale Ejecta Inhomogeneities: X-ray equivalent-width maps  Si concentrated in SE  O, Mg in SE and central region  Ne is mainly interstellar Previously seen from Suzaku by Uchida+ (2013), with lower resolution UV absorption spectra toward a few UV “light bulbs” also show front-back asymmetries in cold ejecta (e.g. Hamilton+ 2007; Winkler & Long 2005)

Summary  Optically emitting ejecta in G292 is loosely organized along bi-polar cones; spectra show O, Ne almost exclusively—almost no S or other O-burning products  Broad bipolar outflows (jets?) are a common—but not universal—feature of core-collapse SNe  SN 1006: ejecta show clear asymmeties on large scale (NW- SE, front-back)  SN 1006 ejecta also show small-scale clumpiness (scales ~ pc); some have reached the shell edge and show Balmer bowshocks from encountering neutral H. Origin: instabilities in explosion? Or subsequently via R-T instabilities? F. Winkler Kyoto,

EXTRA SLIDES F. Winkler Kyoto,

2010

Kinematics I: Proper Motions  For all knots, distance traveled from the common expansion center is well correlated with proper motion—signature of ballistic trajectories.  Assuming un-decelerated expansion, radial velocity is proportional to distance from center along the line of sight. F. WinklerKyoto,

(a) (b) (c) (d) (e) [O III] (b) 29 km/s (a) km/s (c) 1211 km/s (d) 482 km/s 1109 km/s (e) -341 km/s 27 km/s 986 km/s FWHM ≈ 360 km/s F. WinklerKyoto,

For Cas A, most ejecta knots lie near a spherical shell, plus jets of much faster material (Reed et al. 1995) Three-Dimensional Structure Do similar patterns persist in G292 (~ 10 x older)? Systemic velocity ~ km/s Fesen et al F. Winkler Kyoto,

Outer Fast-Moving Knots (mostly) lie near a spherical shell? (GHW 05) More distant (faster) knots lie far outside posited shell to the South Systemic radial velocity is small (~ +100 km/s, GHW05) Three-Dimensional Structure F. Winkler Kyoto,