The spectrometer/telescope for imaging X-rays on board the ESA Solar Orbiter spacecraft

Krucker, S.; Benz, A. O.; Hurford, G. J.; Arnold, N. G.; Orleański, P.; Gröbelbauer, H.-P.; Casadei, D.; Kobler, S.; Iseli, L.; Wiehl, H. J.; Csillaghy, A.; Etesi, L.; Hochmuth, N.; Battaglia, Marina; Bednarzik, Martin; Resanovič, R.; Grimm, O.; Viertel, G.; Commichau, V.; Howard, Andrew W.; Meuris, A.; Limousin, O.; Brun, S.; Vilmer, Nicole; Skup, Konrad; Graczyk, Rafał; Stolarski, M.; Michalska, Małgorzata; Nowosielski, W.; Cichocki, Andrzej; Mosdorf, M.; Seweryn, K.; Białek, Agnieszka; Sylwester, J.; Kowaliński, Mirosław; Mrozek, Tomasz; Pоdgórski, P.; Mann, G.; Önel, H.; Auraß, H.; Bauer, Svend‐Marian; Bittner, Wilbert; Dionies, Frank; Paschke, J.; Plüschke, D.; Popow, Emil; Rendtel, J.; Warmuth, A.; Woche, M.; Wolter, Dieter; Beek, H. F. van; Fárník, F.; Lin, R. P.

doi:10.1016/j.nima.2013.05.050

Cited by 18 publications

(7 citation statements)

References 4 publications

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“…While developed for analysis of RHESSI data, the algorithm is not restricted to RHESSI visibilities. Early tests indicate that VIS CS is a competitive image reconstruction algorithm for the upcoming STIX instrument (Krucker et al 2013), which uses a similar imaging principle but with a different uv-coverage. We encourage the use of of VIS CS whenever fast, reliable reconstruction of a large number of images is needed and for less experienced users of RHESSI data.…”

Section: Discussionmentioning

confidence: 99%

A Compressed Sensing-based Image Reconstruction Algorithm for Solar Flare X-Ray Observations

Felix

Bolzern

Battaglia

2017

ApJ

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One way of imaging X-ray emission from solar flares is to measure Fourier components of the spatial X-ray source distribution. We present a new Compressed Sensing-based algorithm named VIS CS, which reconstructs the spatial distribution from such Fourier components. We demonstrate the application of the algorithm on synthetic and observed solar flare X-ray data from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI ) satellite and compare its performance with existing algorithms. VIS CS produces competitive results with accurate photometry and morphology, without requiring any algorithm-and X-ray source-specific parameter tuning. Its robustness and performance make this algorithm ideally suited for generation of quicklook images or large image cubes without user intervention, such as for imaging spectroscopy analysis.Back projection -The back projection algorithm performs an inverse Fourier transform where all non-measured Fourier components are assumed to be zero. The resulting reconstructions show heavy ringing artefacts

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Section: Discussionmentioning

confidence: 99%

A Compressed Sensing-based Image Reconstruction Algorithm for Solar Flare X-Ray Observations

Felix

Bolzern

Battaglia

2017

ApJ

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“…To obtain a sufficient number of Fourier components for image reconstruction 32 grid pairs and detectors are used. A more comprehensive overview of the instrument is found in [3], details about the electronics in [4], and about the Caliste-SO hybrids in [5].…”

Section: Stix Instrument Designmentioning

confidence: 99%

Performance and qualification of CdTe pixel detectors for the Spectrometer/Telescope for Imaging X-rays

et al. 2015

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The Spectrometer/Telescope for Imaging X-rays (STIX) is a remote sensing instrument on-board the ESA Solar Orbiter spacecraft. STIX is designated to the study of energetic phenomena in solar flares. A Fourier-imaging technique using tungsten grid collimators in front of CdTe pixel detectors is employed, covering the 4 to 150 keV energy range with a full-width-half maximum resolution around 1 keV at low energies.Acrorad CdTe detectors of 1 mm thickness with a planar aluminum Schottky contact are used as basis for a subsequent patterning process into eight large pixels, four small pixels, and a guard ring. The patterning is done by means of microfabrication technologies. The area of the patterned sensor is 10×10 mm 2 .Test equipment has been developed for selecting the detectors with best performance prior to integration with the read-out system, and for qualification purposes. The set-up allows pixel-based dark current measurements at low temperatures. Pixel dark currents below 60 pA are needed to avoid excess noise in the read-out ASIC. The best pixels show dark currents below 10 pA at 300 V bias and −20°C. Spectroscopic measurements with 133 Ba sources confirm the good performance.This paper briefly explains the mission context of the CdTe detectors and then gives details of the production and testing procedures. Typical results are shown, with emphasis on performance degradation studies from displacement damage by proton irradiation. This is expected to be the dominant degradation mechanism for this application.

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“…The Spectrometer Telescope for Imaging X-rays (STIX; Krucker et al 2013), is an instrument to be flown on board the ESA/NASA Solar Orbiter mission (Müller et al 2013) within the ESA Cosmic Vision programme. Solar Orbiter will be launched in October 2018 and it will start its science programme after a three year cruise phase.…”

Section: Introductionmentioning

confidence: 99%

Measuring X-ray anisotropy in solar flares. Prospective stereoscopic capabilities of STIX and MiSolFA

Casadei

Jeffrey

Kontar

2017

A&A

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Context. During a solar flare, a large percentage of the magnetic energy released goes into the kinetic energy of non-thermal particles, with X-ray observations providing a direct connection to keV flare-accelerated electrons. However, the electron angular distribution, a prime diagnostic tool of the acceleration mechanism and transport, is poorly known. Aims. During the next solar maximum, two upcoming space-borne X-ray missions, STIX on board Solar Orbiter and MiSolFA, will perform stereoscopic X-ray observations of solar flares at two different locations: STIX at 0.28 AU (at perihelion) and up to inclinations of ∼25• , and MiSolFA in a low-Earth orbit. The combined observations from these cross-calibrated detectors will allow us to infer the electron anisotropy of individual flares confidently for the first time. Methods. We simulated both instrumental and physical effects for STIX and MiSolFA including thermal shielding, background and X-ray Compton backscattering (albedo effect) in the solar photosphere. We predict the expected number of observable flares available for stereoscopic measurements during the next solar maximum. We also discuss the range of useful spacecraft observation angles for the challenging case of close-to-isotropic flare anisotropy.Results. The simulated results show that STIX and MiSolFA will be capable of detecting low levels of flare anisotropy, for M1-class or stronger flares, even with a relatively small spacecraft angular separation of 20-30• . Both instruments will directly measure the flare X-ray anisotropy of about 40 M-and X-class solar flares during the next solar maximum. Conclusions. Near-future stereoscopic observations with Solar Orbiter/STIX and MiSolFA will help distinguishing between competing flare-acceleration mechanisms, and provide essential constraints regarding collisional and non-collisional transport processes occurring in the flaring atmosphere for individual solar flares.

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The spectrometer/telescope for imaging X-rays on board the ESA Solar Orbiter spacecraft

Cited by 18 publications

References 4 publications

A Compressed Sensing-based Image Reconstruction Algorithm for Solar Flare X-Ray Observations

A Compressed Sensing-based Image Reconstruction Algorithm for Solar Flare X-Ray Observations

Performance and qualification of CdTe pixel detectors for the Spectrometer/Telescope for Imaging X-rays

Measuring X-ray anisotropy in solar flares. Prospective stereoscopic capabilities of STIX and MiSolFA

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