INTEGRAL/SPI ground calibration

Attié, D.; Cordier, B.; Gros, M.; Laurent, Philippe; Schanne, S.; Tauzin, G.; Ballmoos, P. von; Bouchet, L.; Jean, P.; Knödlseder, Jürgen; Mandrou, P.; Paul, P.; Roques, J. P.; Skinner, G.; Védrenne, G.; Georgii, R.; Kienlin, A. von; Lichti, G.; Schönfelder, V.; Strong, A. W.; Wunderer, C.; Shrader, C. R.; Sturner, Steven J.; Teegarden, B. J.; Weidenspointner, G.; Kiener, J.; Porquet, M. G.; Tatischeff, V.; Crespin, S.; Joly, Simon; André, Y.; Sánchez, F.; Leleux, Pierre

doi:10.1051/0004-6361:20031302

Cited by 69 publications

(78 citation statements)

References 6 publications

(8 reference statements)

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“…Imaging analysis makes use of the detailed response of the SPI instrument as is obtained from Monte Carlo simulations (Sturner et al 2003), including the properties of the coded mask, the Ge camera, and all other material possibly interacting with incident gamma-rays. Calibrations before INTEGRAL's launch (Attié et al 2003) and on Cyg-X1 and the Crab in the first part of the mission have verified the validity of this response Sturner et al 2003). Adopting an intensity distribution on the sky, one may thus predict the measured event distribution from 26 Al for the observed exposure pattern.…”

Section: Observations Data and Analysismentioning

confidence: 76%

SPI measurements of Galactic $\mathsf{^{26}}$Al

Diehl

Knödlseder

Lichti

et al. 2003

A&A

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Abstract. The precision measurement of the 1809 keV gamma-ray line from Galactic 26 Al is one of the goals of the SPI spectrometer on INTEGRAL with its Ge detector camera. We aim for determination of the detailed shape of this gamma-ray line, and its variation for different source regions along the plane of the Galaxy. Data from the first part of the core program observations of the first mission year have been inspected. A clear detection of the 26 Al line at 5-7 σ significance demonstrates that SPI will deepen 26 Al studies. The line intensity is consistent with expectations from previous experiments, and the line appears narrower than the 5.4 keV FWHM reported by GRIS, more consistent with RHESSI's recent value. Only preliminary statements can be made at this time, however, due to the multi-component background underlying the signal at 40 times higher intensity than the signal from Galactic 26 Al.

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Section: Observations Data and Analysismentioning

confidence: 76%

SPI measurements of Galactic $\mathsf{^{26}}$Al

Diehl

Knödlseder

Lichti

et al. 2003

A&A

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“…A detailed description of the instruments and the calibration can be found in Vedrenne et al (2003) and Attié et al (2003). The main differences to the standard response function are the strongly reduced full-energy peak efficiencies due to absorption and a continuum component from forward Compton scattered photons in the passive and active material of the satellite.…”

Section: Discussionmentioning

confidence: 99%

“…The results for the full-energy peak effective detector areas and the transmission probabilities are listed in Table 1. The transmission factors have been obtained assuming that the intrinsic efficiency of the detector array in this configuration equals the intrinsic efficiency of the Ge camera determined in the ground calibration campaign at Bruyères-le-châtel (Attié et al 2003). Uncertainties of the effective area are estimated to be smaller than 10%.…”

Section: Discussionmentioning

confidence: 99%

Properties of the energetic particle distributions during the October 28, 2003 solar flare from INTEGRAL/SPI observations

Kiener¹,

Gros

Tatischeff³

et al. 2005

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Analysis of spectra obtained with the gamma-ray spectrometer SPI onboard INTEGRAL of the GOES X17-class flare on October 28, 2003 is presented. In the energy range 600 keV-8 MeV three prominent narrow lines at 2.223, 4.4 and 6.1 MeV, resulting from nuclear interactions of accelerated ions within the solar atmosphere could be observed. Time profiles of the three lines and the underlying continuum indicate distinct phases with several emission peaks and varying continuum-to-line ratio for several minutes before a smoother decay phase sets in. Due to the high-resolution Ge detectors of SPI and the exceptional intensity of the flare, detailed studies of the 4.4 and 6.1 MeV line shapes was possible for the first time. Comparison with calculated line shapes using a thick target interaction model and several energetic particle angular distributions indicates that the nuclear interactions were induced by downward-directed particle beams with alpha-to-proton ratios of the order of 0.1. There are also indications that the 4.4 MeV to 6.1 MeV line fluence ratio changed between the beginning and the decay phase of the flare, possibly due to a temporal evolution of the energetic particle alpha-to-proton ratio.

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“…The high-energy 44 Ti decay line has a FWHM of (8.94 ± 1.42) keV and is thus broadened with respect to the instrumental resolution at 1.157 MeV of 2.4 keV (Attié et al 2003). This FWHM can be converted to an estimate of the expansion velocity of the 44 Ti ejecta of (2200 ± 400) km s −1 .…”

Section: Ti Gamma-ray Line Measurementsmentioning

confidence: 99%

Revisiting INTEGRAL/SPI observations of⁴⁴Ti from Cassiopeia A

Siegert

Diehl

Krause

et al. 2015

A&A

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Context. The 340-yr old supernova remnant Cassiopeia A, located at 3.4 kpc distance, is the best-studied young core-collapse supernova remnant. Nucleosynthesis yields in radioactive isotopes have been studied with different methods, in particular for production and ejection of 44 Ti and 56 Ni, which originate in the innermost regions of the supernova. 44 Ti was first discovered in this remnant, but is not seen consistently in other core-collapse sources. Aims. We aim to measure radioactive 44 Ti ejected in Cassiopeia A and to place constraints on velocities of these ejecta by determining X-and γ-ray line-shape parameters of the emission lines. Methods. We analyzed the observations made with the SPI spectrometer on INTEGRAL together with an improved instrumental background method, to achieve a high spectroscopic resolution that enables interpretation for a velocity constraint on 44 Ti ejecta from the 1.157 MeV γ-ray line of the 44 Sc decay. Results. We observe both the hard X-ray line at 78 keV and the γ-ray line at 1157 keV from the 44 Ti decay chain at a combined significance of 3.8σ. Measured fluxes are (2.1 ± 0.4) × 10 −5 ph cm −2 s −1 and (3.5 ± 1.2) × 10 −5 ph cm −2 s −1 , which corresponds to (1.5 ± 0.4) × 10 −4 and (2.4 ± 0.9) × 10 −4 M of 44 Ti, respectively. The measured Doppler broadening of the lines implies expansion velocities of 4300 and 2200 km s −1 , respectively. By combining our results with previous studies, we determine a more precise estimate of ejected 44 Ti of (1.37 ± 0.19) × 10 −4 M . Conclusions. The measurements of the two lines are consistent with previous studies. The flux in the line originating from excited 44 Ca is significantly higher than the flux determined in the lines from 44 Sc. Cosmic-ray acceleration within the supernova remnant may be responsible for an additional contribution to this line from nuclear de-excitation following energetic particle collisions in the remnant and swept-up material.

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INTEGRAL/SPI ground calibration

Cited by 69 publications

References 6 publications

SPI measurements of Galactic $\mathsf{^{26}}$Al

SPI measurements of Galactic $\mathsf{^{26}}$Al

Properties of the energetic particle distributions during the October 28, 2003 solar flare from INTEGRAL/SPI observations

Revisiting INTEGRAL/SPI observations of⁴⁴Ti from Cassiopeia A

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INTEGRAL/SPI ground calibration

Cited by 69 publications

References 6 publications

SPI measurements of Galactic $\mathsf{^{26}}$Al

SPI measurements of Galactic $\mathsf{^{26}}$Al

Properties of the energetic particle distributions during the October 28, 2003 solar flare from INTEGRAL/SPI observations

Revisiting INTEGRAL/SPI observations of44Ti from Cassiopeia A

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Revisiting INTEGRAL/SPI observations of⁴⁴Ti from Cassiopeia A