[sup 44]Ti gamma-ray line emission from Cas A and RXJ0852-4622/GROJ0852-4642

Schönfelder, V.; Bloemen, H.; Collmar, W.; Diehl, R.; Hermsen, W.; Knödlseder, J.; Lichti, G.; Plüschke, S.; Ryan, J.; Strong, A. W.; Winkler, C.

doi:10.1063/1.1303173

Cited by 19 publications

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“…As a result, assuming that the continuum is a simple power-law spectrum gives a line flux for each line of (1.9 ± 0.4) × 10 −5 ph cm −2 s −1 (68% confidence range), whereas the gradual steepening of synchrotron and specific non-thermal bremsstrahlung models results in a line flux of (3.2 ± 0.3) × 10 −5 ph cm −2 s −1 (Vink et al, 2001;Vink and Laming, 2003). Within the errors both values are consistent with the latest COMPTEL results (Schönfelder et al, 2000). We can average the COMP-TEL and BeppoSAX results to obtain a 44 Ti line flux of (2.6 ± 0.4 ± 0.5) × 10 −5 ph cm −2 s −1 per line, where the first error is the 1σ statistical error and the second error is the systematic error, due to uncertainty in the continuum modeling.…”

Section: Ti Detections By Comptel and Bepposaxsupporting

confidence: 86%

“…Together this suggests a remnant with an age of more than 1000 yr, which is hard to reconcile with the observed 1157 keV line flux of (3.8 ± 0.7) × 10 −5 ph cm −2 s −1 (Aschenbach et al, 1999;Slane et al, 2001). Also the detection itself, although formally at the 5σ level is less secure than the detection of 44 Ti in Cas A (Schönfelder et al, 2000). Nevertheless, Vela Jr is an interesting object and an important INTEGRAL target (von Kienlin et al, 2004).…”

Section: Potential Other Sources Of 44 Ti γ-Ray Emissionmentioning

confidence: 81%

“…A preliminary analysis shows that narrow line 44 Ti emission (∆E = 4 keV,∆v = 1000 km s −1 ) can almost be excluded at the 2-3σ level, as the 3σ upper limit for emission is 3.1 × 10 −5 ph cm −2 s −1 the flux level found by COMP-TEL (Schönfelder et al, 2000). and the 2σ upper limit is 1.7×10 −5 ph cm −2 s −1 .…”

Section: Cas Amentioning

confidence: 92%

“…, the 1157 keV line flux should have been below the COMPTEL detection limit. Surprisingly, COMPTEL detected the 1157 keV line emission, with the latest, most reliable flux estimate based on COMP-TEL observations being (3.4 ± 0.9) × 10 −5 ph cm −2 s −1 (Schönfelder et al, 2000).…”

Section: Ti Detections By Comptel and Bepposaxmentioning

confidence: 99%

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Gamma-ray observations of explosive nucleosynthesis products

Vink

2005

Advances in Space Research

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In this review I discuss the various γ-ray emission lines that can be expected and, in some cases have been observed, from radioactive explosive nucleosynthesis products. The most important γ-ray lines result from the decay chains of 56 Ni, 57 Ni, and 44 Ti. 56 Ni is the prime explosive nucleosynthesis product of Type Ia supernovae, and its decay determines to a large extent the Type Ia light curves.56 Ni is also a product of core-collapse supernovae, and in fact, γ-ray line emission from its daughter product, 56 Co, has been detected from SN1987A by several instruments. The early occurrence of this emission was surprising and indicates that some fraction of 56 Ni, which is synthesized in the innermost supernova layers, must have mixed with the outermost supernova ejecta.Special attention is given to the γ-ray line emission of the decay chain of 44 Ti ( 44 Ti→ 44 Sc→ 44 Ca), which is accompanied by line emission at 68 keV, 78 keV, and 1157 keV. As the decay time of 44 Ti is ∼ 86 yr, one expects this line emission from young supernova remnants. Although the 44 Ti yield (typically 10 −5 − 10 −4 M⊙) is not very high, its production is very sensitive to the energetics and asymmetries of the supernova explosion, and to the mass cut, which defines the mass of the stellar remnant. This makes 44 Ti an ideal tool to study the inner layers of the supernova explosion. This is of particular interest in light of observational evidence for asymmetric supernova explosions.The γ-ray line emission from 44 Ti has so far only been detected from the supernova remnant Cas A. I discuss these detections, which were made by COMPTEL (the 1157 keV line) and BeppoSAX (the 68 keV and 78 keV lines), which, combined, give a flux of (2.6 ± 0.4 ± 0.5) × 10 −5 ph cm −2 s −1 per line, suggesting a 44 Ti yield of (1.5 ± 1.0) × 10 −4 M⊙. Moreover, I present some preliminary results of Cas A observations by INTEGRAL, which so far has yielded a 3σ detection of the 68 keV line with the ISGRI instrument with a flux that is consistent with the BeppoSAX detections. Future observations by INTEGRAL-ISGRI will be able to constrain the continuum flux above 90 keV, as the uncertainty about the continuum shape, is the main source of systematic error for the 68 keV and 78 keV line flux measurements. Moreover, with the INTEGRAL-SPI instrument it will be possible to measure or constrain the line broadening of the 1157 keV line. A preliminary analysis of the available data indicates that narrow line emission (i.e. ∆v < 1000 km s −1 ) can be almost excluded at the 2σ level, for an assumed line flux of 1.9 × 10 −5 ph cm −2 s −1 .

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Section: Ti Detections By Comptel and Bepposaxsupporting

confidence: 86%

Section: Potential Other Sources Of 44 Ti γ-Ray Emissionmentioning

confidence: 81%

Section: Cas Amentioning

confidence: 92%

Section: Ti Detections By Comptel and Bepposaxmentioning

confidence: 99%

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Gamma-ray observations of explosive nucleosynthesis products

Vink

2005

Advances in Space Research

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“…Current estimates of the Galactic core collapse SNe rate is 1.9±1.1 per century [18], implying ∼8 young supernova remnants (SNR) should be visible in their 44 Ti emission. COMPTEL discovered only one source in the 44 Sc decay line at 1.157 MeV (Cas A) and saw some controversial evidence for a second SNR in Vela [19], [20]. INTEGRAL's instruments have reaffirmed the Cas A detection [21], but no additional 44 Ti sources have been detected to date.…”

Section: B) Core-collapse Snementioning

confidence: 99%

Overview of the Nuclear Compton Telescope

Perez-Becker¹

2009

Proceedings of 7th INTEGRAL Workshop — PoS(Integral08)

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The Nuclear Compton Telescope (NCT) is a balloon-borne soft gamma-ray (0.2-10 MeV) telescope designed to study astrophysical sources of nuclear line emission and polarization. It consists of twelve high spectral resolution 3D Germanium strip detectors that track gamma-ray Compton scatter interactions with a resolution better than 2 mm 3 . Tracking technologies together with NCT's ultra-compact design provide dramatic improvements in Compton efficiency and sensitivity, achieving a similar effective area to COMPTEL with less than 1% of the detector volume. NCT will be breaking new ground in the measurement of polarized gamma-ray emission from astrophysical sources, while simultaneously providing a testing platform for novel event analysis, background reduction, and imaging techniques. Thus NCT is also serving as technology demonstration testbed for modern Compton telescopes, such as the Advanced Compton Telescope, or a focal plane detector of a gamma-ray focusing telescope. The instrument is currently being prepared for a 36-hour flight from New Mexico in Spring of 2009, followed by a long duration flight from Australia. On these science flights, NCT will map the Galactic positron annihilation, 26 Al, and 60 Fe emission, and perform a discovery study of polarization from all classes of gammaray sources. We present an overview of the NCT instrument, the planned flight program, and preliminary results of calibration and performance tests. 7th INTEGRAL Workshop

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Nucleosynthesis

Diehl¹

2001

The Universe in Gamma Rays

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[sup 44]Ti gamma-ray line emission from Cas A and RXJ0852-4622/GROJ0852-4642

Cited by 19 publications

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Gamma-ray observations of explosive nucleosynthesis products

Gamma-ray observations of explosive nucleosynthesis products

Overview of the Nuclear Compton Telescope

Nucleosynthesis

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