Kinematics of Young SNRs

Kinematics of Young SNRsP. Frank Winkler, Middlebury College

Conference on SNe, YITP, Kyoto

30 October 2013

Collaborators:Knox LongSteve ReynoldsRob PetreWilliam BlairBrian WilliamsSatoru KatsudaDan

Milisavljevic

Undergraduate Students:Adele PlunkettKarl TwelkerClaudine ReithGuarav GuptaJillian Garber

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!

Kinematics of Young SNRsP. Frank Winkler, Middlebury College

Conference on SNe, YITP, Kyoto

30 October 2013

Collaborators:Knox LongSteve ReynoldsRob PetreWilliam BlairBrian WilliamsSatoru KatsudaDan

Milisavljevic

Undergraduate Students:Adele PlunkettKarl TwelkerClaudine ReithGuarav GuptaJillian Garber

Kinematics of Young SNRs

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

F. Winkler Kyoto, 2013 4

“Young” = < few thousand yearsComposition and/or kinematics hold traces of the explosion

O-rich SNR G292.0+1.8 (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)


[O III] 5007

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


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)


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

CTIO image credit: T. Abbott and NOAO/AURA/NSF F. Winkler Kyoto, 2013 8

Kinematics II: Doppler Mapping

Vr < – 300km/s

Vr > + 300 km/s|Vr | < 300 km/s

Fastest knots are distributed along broad, bipolar jets, roughly N-S

Brightest knots are along "eastern spur”



Vr = – 1500km/s

Vr = + 1800 km/s Vr ≈ 0 km/s



Fastest knots are distributed along broad, bipolar jets, roughly N-S

Brightest knots are along "eastern spur”

PSR

Blue = 0.5-7 keV (Park 07)

Red = 24 μm (dust, Ghavamian 2012)

Green = [O III]

[O III] 0.5 - 7 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)


Other Core-Collapse SNR Examples

Chandra HRI

SN 1006SN Ia remnant

Synchrotron limbs

Shocked ISM (primarily)

Shocked Ejecta

Chandra ACIS 2012(PFW+ ApJ, submitted)


Chandra ACIS 2003(Cassam-Chenai 2008)


Deep Hα imageFaint emission surrounding shellIntriguing interior features

Ejecta Bullets + Balmer Bowshocks

Ejecta reaching outer boundary of shell (neutral H)

Green = X-rayRed = 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 ~ 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?


EXTRA SLIDES


2010


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.


(a)

(b)

(c)

(d)(e)

[O III] 4959 5007

(b) 29 km/s

(a) -1267 km/s

(c) 1211 km/s

(d) 482 km/s 1109 km/s

(e) -341 km/s 27 km/s986 km/s

FWHM ≈ 360 km/s


• 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 ~ + 770 km/s

Fesen et al. 2006


• 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


Documents

Kinematics of Young SNRs