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Gamma-Rays from SupernovaeGamma-Rays from Supernovae

Roland DiehlMPE Garching

• Gamma-Ray Line Astronomy and Supernovae• Specific Objects

• Thermonuclear Supernovae (56Co; SN1991T, SN1998bu)•Core-Collapse Supernovae (44Ti; Cas A; 26Al and 60Fe)

•Prospects

withThe COMPTEL Team: Hans Bloemen, Robert Georgii, Wim Hermsen, Jürgen Knödlseder, Giselher Lichti, Dan Morris,

Uwe Oberlack, Stefan Plüschke, Jim Ryan, Andrew Strong, Volker Schönfelder, et al.and Karsten Kretschmer, Nikos Prantzos, Dieter Hartmann, Mark Leising, Frank Timmes, Georges Meynet, the SPI Team,

et al.

Roland Diehl The Physics of Supernovae, Garching (D) 29-31 July 2002

Supernova Gamma-Ray Astronomy:Supernova Gamma-Ray Astronomy:Lines of InterestLines of Interest

Radioactive IsotopesDecay Time > Source Dilution TimeYields > Instrumental Sensitivities

Isotope MeanLifetime

Decay Chain γγγγ -Ray Energy(keV)

Source

7Be 77 d 7Be →→→→ 7Li* 478 Novae56Ni 111 d 56Ni →→→→ 56Co* →→→→ 56Fe*+e+ 158, 812; 847,

1238Supernovae

57Ni 390 d 57Co→→→→ 57Fe* 122 Supernovae22Na 3.8 y 22Na →→→→ 22Ne* + e+ 1275 Novae44Ti 89 y 44Ti→→→→ 44Sc*→→→→ 44Ca*+e+ 78, 68; 1157 Supernovae26Al 1.04 106y 26Al →→→→ 26Mg* + e+ 1809 Stars, Novae

Supernovae60Fe 2.0 106y 60Fe →→→→ 60Co* →→→→ 60Ni* 59, 1173, 1332 Supernovae,

Stars

e+ … . 105y e++e- →→→→ Ps →→→→ γγγγγγγγ.. 511, <511 Supernovae,Novae, …


Gamma-Ray Astronomy: InstrumentsGamma-Ray Astronomy: Instruments

Photon Counters and Telescopes

Coded Mask TelescopesCoded Mask Telescopes(Shadowing Mask & Detector Array)(Shadowing Mask & Detector Array)(e.g. SIGMA, INTEGRAL)Spatial Resolution Defined by Mask & Detector Elements Sizes

Compton TelescopesCompton Telescopes(Coincidence-Setup ofPosition-Sensitive Detectors)(e.g. CGRO-COMPTEL, LXeGRiT, MEGA, ACS)Spatial Resolution Defined by Detectors’ Spatial Resolution

Achieved Sensitivity: ~10-5 ph cm-2 s-1, Angular Resolution ≥ deg

Simple Detector (& Collimator)Simple Detector (& Collimator)(e.g. HEAO-C, SMM, CGRO-OSSE)Spatial Resolution (=Aperture) Defined Through Shield

Focussing TelescopesFocussing Telescopes(Laue Lens & Detector Array)(Laue Lens & Detector Array)(CLAIRE, MAX)Spatial Resolution Defined by Lens Diffraction & Distance


SN1987A: First Supernova Gamma-RaysSN1987A: First Supernova Gamma-Rays

SN1987A 56Co DecayGamma-Rays DetectedEarlier Than Expected;First Proof of Supernova56Ni Synthesis(SMM; Matz et al. 1988)

SN1987A 57Co DecayGamma-Ray DetectionUsed to Infer CoIsotopic Ratio (~1.5 xsolar)(OSSE; Kurfess et al. 1992;Clayton et al. 1992)

SN1987A 56Co Line at847 keV Used for LineShape Analysis(GRIS; Teegarden et al. 1988)


5656Ni Decay Gamma-RaysNi Decay Gamma-Rays

56Ni →→→→ 8.8d→→→→ 56Co* →→→→ 111d→→→→ 56Fe*+e+

158, 812; 847, 1238 keV γγγγ-Rays

Early Envelope γγγγ-Transparency(e.g. SNIa within ~30-100d)Direct Measurement of SN „Driver“

56Ni

56Fe

e--capture (98%)

γγγγ 750 keV (50%)

ττττ =8.8 d

56Co

γγγγ 847 keV (100%)

ττττ = 111.3 d

γγγγ 812 keV (86%)

0+

1+

2+

4+

2+

0+

4+

γγγγ 1238 keV (68%)

e- - capture (81%) γγγγ 158 keV (100%)

3+

0+ γγγγ 270+480 keV (36%)

3,4+ ββββ+ - decay(19%,E~0.6MeV) γγγγ’s 3.2,2.8,2.0,1.04,

1.4,1.8 MeV (2-16%)


SN1991TSN1991T

SN1991T:SN1991T:in NGC4527 on 10 Apr 1991Distance 9..11..13..17 MpcPeculiar SNIaearly: no Si absorption, Fe emission instead;overluminous; late: ~standard SNIa; overluminous

COMPTEL Measurement:COMPTEL Measurement:Observations at Days 66-79, 176-1903-5σσσσ Significance of Line Detection:11.7 (±3.2 ±2.7) 10-5 ph cm-2 s-1 (all combined)9(±3) 10-5 ph cm-2 s-1 (847 keV day 70)6(±2) 10-5 ph cm-2 s-1 (1238 keV day 70)

Inferred 56Ni Mass: ~ 1.65 Mo (0.7...2.6 Mo)(cmp 1.14 Mo from Bolometric Lightcurve, Contardo et al. 2000)

Large Uncertainties of Gamma-Ray Flux MeasurementInadequate Spectral Resolution

Morris et al., 1995, 1997, 2002


SN1998buSN1998bu

Szuntzeff et al., AJ 117 (1999)

Whipple Obs; Jha et al., ApJS 125 (1999)

• SN on May 1..2, 1998• Discovery on May 9.9, Ia Identification on May 14• Host Galaxy M96 / NGC 3368 in Leo I (RA 10 46.8 Dec 11 50; l=234.5, b=57.0)

• ~Closest SNIa: D~8...12 Mpc (D98bu~0.7 D91T)(Ceph.8.2 by Tanvir et al. 1995(!); Tully-F.~8.1; HST-Ceph.11.6±0.8; PN 9.6±0.6)

• “Standard” Type-Ia Lightcurve & Spectra <VBmax>=11.89 -> Mv=-19.42

• Unusual Reddening (Host Galaxy Dust?) ; Extinction AV~0.94 ±0.2 mag


SN1998bu:SN1998bu: COMPTEL Limits on COMPTEL Limits on 5656Ni Decay LinesNi Decay Lines

14 Weeks of CGRO Observations(May 19 - Sep 22 1998)

No Gamma-Ray Line Signal847 keV Line

Ispectral<4.1 10-5 ph cm-2 s-1

Iimaging<3.3 10-5 ph cm-2 s-1

1238 keV LineIspectral<2.3 10-5 ph cm-2 s-1

Iimaging<3.2 10-5 ph cm-2 s-1

(for 11.3 Mpc; 2σσσσ Limits)

I56Co Lines < 3.3 10-5 ph cm-2 s-1

M56Ni-visible< 0.35 Mo (ττττ=0 idealized)(bolometric lightcurve -> 0.77 Mo, Leibundgut 2000)

“Fast” / Large-Mixing Models(He Cap, W7DT) Unlikely

Georgii et al., 2002


56Ni Mass versus γγγγ-Ray Flux

SN1998bu:SN1998bu: COMPTEL Limits on COMPTEL Limits on 5656Ni Decay LinesNi Decay Lines

I56Co Lines < 3.3 10-5 ph cm-2 s-1

M56Ni-visible< 0.35 Mo (ττττ=0 idealized)(bolometric lightcurve -> 0.77 Mo, Leibundgut 2000)

“Fast” / Large-Mixing Models(He Cap, W7DT) Unlikely

Georgii et al., 2002


Supernova Supernova 5656Ni Gamma-RaysNi Gamma-Rays

Early Envelope γγγγ-Transparency (e.g. SNIa within ~30-100d)Gamma-Ray Transport Comparatively StraightforwardLine Ratio Diagnostics -> Envelope Structure; MixingLine Shape Diagnostics -> Velocities of Inner SN Ejecta

Instrumental Range: ~15 Mpc (Ia; ~Virgo Cluster) ~ Galaxy & LMC/SMC (Ib/c,II)

-> Rare OpportunitiesTimely Observations are Critical

No Real Help on SN Physics Yet,Let‘s Hope for INTEGRAL et al.


44Ti

44Ca

ττττ =89y, EC

44Sc

ττττ = 5.4 h, ββββ+

Core-Collapse Supernovae: Core-Collapse Supernovae: 4444Ti from Cas ATi from Cas A

44Ti Decay: ττττ~89y -> Young SNR

44Ti Decay Gamma-ray Fluxes from Cas A

0

1

2

3

4

5

COMPTEL 1999 OSSE 1996 RXTE 1997 SAX 2000

I * 1

0-5 p

h cm

-2 s

-1

Difficult γγγγ-Ray Region (78, 68, 1157 keV) -> Uncertain Iγγγγ->44Ti Ejected Mass ~0.8-2.5 10-4 Mo

Iyudin et al., 1994; The et al.1996; Rothchild et al. 1998; Vinket al. 2000


4444Ti from Cas A / cc-SNae: The IssueTi from Cas A / cc-SNae: The Issue

Consistency ofCas A cc-SN Model:

44Ti Yield in Models: ~2-4 10-5 Mo44Ti Estimate for SN1987A: ~5-20 10-5 Mo44Ti Estimate from γγγγ-Rays for Cas A: ~8-25 10-5 Mo44Ti Ejection Should Be Correlated to

High-Entropy Material -> a-Rich Freeze-OutLarge Explosion EnergyLarge Mass of Ejected 56Ni (Bright Supernova)

Timmes et al., 1996


XMM-NewtonXMM-Newton

ISOISO

Cas A: A Well-Studied Young Nearby SNRCas A: A Well-Studied Young Nearby SNR

~330 year-old SNR at ~3.4 kpcMassive Progenitor (10-25 Mo)Filaments, Fast Ejecta (knots),Fe-rich Clumps, No Onion-Shell-Like Elemental Morphology, Jet:Asymmetric ExplosionUnseen SN -> CSM DustCentral Object (NS/BH?)44Ti (and 56Ni) Ejection

ChandraChandra

HSTHST

=> (?)Non-Typical Core Collapse SN,AsymmetriesThe SN with Proven 44Ti Ejection


Search for Search for 4444Ti from Galactic cc-SupernovaeTi from Galactic cc-Supernovae

No 44Ti Sourcesin Inner Galaxy

Parent Distribution of Sources ~ 26AlMonte-Carlo Study-> 44Ti SNR Number Low

Small-Number Statistics?Observational Bias?Metallicity Anticorrelation?

The et al., 2000


4444Ti Emission from cc-SNae: Open IssuesTi Emission from cc-SNae: Open Issues

Consistency of Cas A cc-SN Model:44Ti from Models/SN1987A/γγγγ-Rays: ~2-25 10-5 Mo44Ti Ejection Should Be Correlated to

High-Entropy Material -> a-Rich Freeze-OutLarge Explosion EnergyLarge Mass of Ejected 56Ni (Bright Supernova)

No 44Ti Sources in Inner GalaxyParent Distribution of Sources ~ 26AlMonte-Carlo Study -> 44Ti SNR Number Low

Small-Number Statistics? Observational Bias?Metallicity Anticorrelation?

Can 44Ti Sources Reveal...Inner SN Velocity Profiles? Ionization-Inhibited Decay (EC)? (44Ti Line Shape!)Asymmetric Core Collapses?

The et al., 2000


The Sky at 1809 keV: The Sky at 1809 keV: 2626AlAl

Complete CGRO Mission(Plüschke et al. 2001)

Inner-Galaxy RidgeInner-Galaxy Ridge VelaVelaCygnusCygnus OrionOrionEridanusEridanus

Sco-Cen?Sco-Cen?

Auriga/Auriga/αα Per? Per?

CarinaCarina


2626Al Map & Possible Source TracersAl Map & Possible Source Tracers

Massive Stars are theMassive Stars are thePlausible SourcesPlausible SourcesMap Irregularity and Scale Height,Bright Spiral-Arm TangentsCorrelated with Star-Forming GasCorrelated with Warm DustCorrelated with Diffuse Ionized Gas

26Al Ejection by WR Starsor by cc-SNae?

CO map ofmolecular gas

IR map at240 µµµµm, dust

Radio map at53 GHz,free electrons

Hαααα Emissionfrom IonizedGas

RD with Knödlseder, Prantzos, Oberlack, Plüschke, Bloemen, et al. (1996...2002)


Modeling Modeling 2626Al from Star ClustersAl from Star Clusters

Stellar Content(OB Association Richness, IMF)

Stellar EvolutionLifetimeWR Phase

26Al Yields per Staryields

1.809 MeV “Light Curve” for aMassive-Star Cluster

->-> Plüschke et al., 2001; Cerviño et al. 2002

WR Stars cc-SNae

plusother Observables

UV / Ionization (-> free-free Emission)

Kinetic Energy / X Brightness

Plüschke Ph D Thesis, 2001


Interesting Nearby Sources infront of Vela Molecular Ridge

Vela SNR (d~250 pc)RXJ0852 (200pc<d<1500pc)γγγγ2Velorum (WR11) (d~258/400pc)

Extended Diffuse 26Al Emission

2626Al from Nearby Supernovae:Al from Nearby Supernovae: The Vela Region The Vela RegionModel Emissivity Along Galactic Plane

0.00

2.00

4.00

6.00

8.00

10.00

-180-150-120-90-60-300306090120150180

Galactic Longitude

Mod

el A

mpl

itude

IR240/10

IR240/4

free-free/10free-free/4

rod 05/2000COMPTEL 1.8 MeV C1-9

None of These Close SNR ClearlySeen in 26Al


2626Al from Supernovae: Help from Al from Supernovae: Help from 6060Fe?Fe?

SN Debris in Solar System?60Fe Detected in SeefloorSediment=> Nearby SN ~ 3-5 My ago26Al in Sediment, too?

Production in SNae (and Stars)through n Capture on 56,58Fe(s-Process; 13C/22Ne(αααα,n))

26Al/60Fe Flux Ratio Limits

0.00

0.10

0.20

0.30

0.40

0.50

0.60

COMP'99 COMPTEL GRIS SMM OSSE

I(60

Fe)/

I(26

Al)

R Diehl 1/99

01/1999: new bgd model; 0.3 syst error, 2sig stat error

Predicted from Theory

Decay Time 2 Myr + SN Yields ->Iγγγγ60Fe~0.16 Iγγγγ26Al for 26Al from SN only

60Fe from 26Al Sources? ~Little.


Gamma-Ray Lines from Supernovae: SummaryGamma-Ray Lines from Supernovae: Summary

Specific Supernova Nucleosynthesis56Ni

44Ti

Accumulated Nucleosynthesis in ISM26Al e+

44Ti Decay Gamma-ray Fluxes from Cas A

0

1

2

3

4

5

COMPTEL 1999 OSSE 1996 RXTE 1997 SAX 2000

I * 1

0-5 p

h cm

-2 s

-1

511

keV

Lin

ie


Questions:Origin of 26Al, e+, 60Fe Distinguish Massive Stars/SNaeCore Collapse SNae: Inner Explosion, AsymmetriesThermonuclear SNae: Deflagration/Detonation Transition

Gamma-Ray Lines from Cosmic Nuclei: ProspectsGamma-Ray Lines from Cosmic Nuclei: Prospects

Opportunities:Gamma-Ray Line Shapes -> INTEGRAL

Launch Oct2002,1.5 Msec on Cas A, SN87A

Surveys at Improved Sensitivity -> MEGA, ACTDeep SN Measurements -> Laue Tel.


γγγγγγγγ-Ray Line Conference / Workshop Opportunities-Ray Line Conference / Workshop Opportunities

...

May 26-31, 2003: Kloster Seeon, Germany

Astronomy with Radioactivities IVFeb 16-20, 2004: München, Germany

5th INTEGRAL Workshop

...

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