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Kinematics of Young Supernova Remnants: Observations and Analysis

Explore the kinematics of young supernova remnants through detailed observations and analysis of key features such as proper motions, Doppler mapping, and multiwavelength relationships. Collaborators and undergraduate students contributed to this research presented at the Middlebury College Conference on Supernovae in Kyoto, 2013.

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Kinematics of Young Supernova Remnants: Observations and Analysis

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  1. 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 P. Frank Winkler, Middlebury College Conference on SNe, YITP, Kyoto 30 October 2013

  2. Tuesday, October 29, 2013 Last Update:11:04 PM ET Betelgeuse Explodes as Supernova Gravitational Waves Detected Worldwide First Exploding Star in Milky Way for 400 Years Spectacular Star in Orion Visible in Pre-dawn Skies NOT!

  3. 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 P. Frank Winkler, Middlebury College Conference on SNe, YITP, Kyoto 30 October 2013

  4. Kinematics of Young SNRs “Young” = < few thousand years Composition and/or kinematics hold traces of the explosion • G292.0+1.8: 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 Kyoto, 2013

  5. PSR Park (2007) O-rich SNR G292.0+1.8 (MSH 11-54) [O III] 5007 • 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 Kyoto, 2013

  6. Kinematics I: Proper Motions • Proper motions from 7 epochs: 1986 - 2008 • 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 Kyoto, 2013

  7. Kinematics I: Proper Motions • Above: 2’ x 2’ section of unsubtracted [O III] image shows PSR J1124-5916 • Backwards extrapolation gives expansion center and age ~3000 years • PSR transverse velocity = 440 km/s to SE (at 6 kpc) Kyoto, 2013

  8. Kinematics II: Doppler Mapping • Longslit and multi-fiber spectra from 1.5m and 4m telescopes at CTIO • Doppler velocities for 93 spectroscopically distinct knots • –1500 km/s < Vr< +1800 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 Vr < –300km/s |Vr | < 300 km/s Vr > + 300 km/s Kyoto, 2013 CTIO image credit: T. Abbott and NOAO/AURA/NSF

  9. Kinematics II: Doppler Mapping • Fastest knots are distributed along broad, bipolar jets, roughly N-S • Brightest knots are along "eastern spur” Vr = –1500km/s Vr ≈ 0 km/s Vr = + 1800 km/s Kyoto, 2013 CTIO image credit: T. Abbott and NOAO/AURA/NSF

  10. Kinematics II: Doppler Mapping • Fastest knots are distributed along broad, bipolar jets, roughly N-S • Brightest knots are along "eastern spur” PSR Kyoto, 2013 CTIO image credit: T. Abbott and NOAO/AURA/NSF

  11. MultiwavelengthRelationship • [O III] • 0.5 - 7 keV (Park 2007) • 24 μm (Ghavamian 2012) • Dense circumstellar belt gives brightest X-rays, IR from dust • Encounter with belt on East drives reverse shock into ejecta to give bright spur Blue = 0.5-7 keV (Park 07) Green = [O III] Red = 24 μm (dust, Ghavamian 2012)

  12. Other Core-Collapse SNR Examples 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) Chandra HRI Kyoto, 2013 CTIO image credit: T. Abbott and NOAO/AURA/NSF

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

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

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

  16. Deep Hα image • Faint emission surrounding shell • Intriguing interior features

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

  18. Large Scale EjectaInhomogeneities: 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)

  19. 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 ~ 0.1-0.3 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? Kyoto, 2013

  20. EXTRA SLIDES Kyoto, 2013

  21. 2010

  22. 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. Kyoto, 2013

  23. [O III]  4959  5007 (a) -1267 km/s (b) 29 km/s (c) 1211 km/s (d) 482 km/s 1109 km/s (e) -341 km/s 27 km/s 986 km/s (d) (e) (a) (c) FWHM ≈ 360 km/s (b) Kyoto, 2013

  24. Fesen et al. 2006 Three-Dimensional Structure • For Cas A, most ejecta knots lie near a spherical shell, plus jets of much faster material (Reed et al. 1995) • Systemic velocity ~ + 770 km/s • Do similar patterns persist in G292 (~ 10 x older)? Kyoto, 2013

  25. Three-Dimensional Structure • Outer Fast-Moving Knots (mostly) lie near a spherical shell? (GHW 05) • Systemic radial velocity is small (~ +100 km/s, GHW05) • More distant (faster) knots lie far outside posited shell to the South Kyoto, 2013

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