A fast onboard star-extraction algorithm optimized for the SVOM Visible Telescope

Wang, T.; Qiu, Y. L.; Cai, Hongbo; Deng, J. S.

doi:10.1007/s11433-010-0010-8

Cited by 10 publications

(3 citation statements)

References 5 publications

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“…At high energies, the ECLAIRs (Takahashi et al 2014) telescope (>4 keV) and the Gamma-Ray Monitor (Dong et al 2010) (>30 keV) will trigger on gamma-ray sources. These sources will then be followed up by the Microchannel X-ray Telescope (MXT) (Caraveo et al 2015) and the Visible Telescope (VT) (Wang et al 2010). The MXT is designed to observe X-ray sources from 0.2 to 10 keV.…”

Section: Introductionmentioning

confidence: 99%

Analysis Methods to Localize and Characterize X-Ray Sources with the Microchannel X-Ray Telescope on Board the SVOM Satellite

Hussein

Robinet

Boutelier

et al. 2023

ApJ

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The Space-based multiband astronomical Variableonboard computing resources. This Object Monitor (SVOM) is a Sino–French space mission targeting high-energy transient astrophysical objects such as gamma-ray bursts. The soft X-ray part of the spectrum is covered by the Microchannel X-ray Telescope (MXT), which is a narrow field telescope designed to localize X-ray sources precisely. This paper presents the methods implemented on board to characterize and localize X-ray sources with the MXT. A specific localization method was developed to accommodate the optical system of the MXT, which is based on “Lobster Eye” grazing incidence micropore optics. For the first time, the algorithm takes advantage of cross-correlation techniques to achieve a localization accuracy down to 2′ with fewer than 200 photons, which guarantees rapid follow-up for most of the gamma-ray bursts that SVOM will observe. In this paper, we also study the limitations of the algorithm and characterize its performance.

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Section: Introductionmentioning

confidence: 99%

Analysis Methods to Localize and Characterize X-Ray Sources with the Microchannel X-Ray Telescope on Board the SVOM Satellite

Hussein

Robinet

Boutelier

et al. 2023

ApJ

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“…Space multi-band variable object monitor (SVOM) [1,2] is a proposed Chinese-French astronomical satellite, dedicated to the detection, localization, and measurement of gammaray bursts (GRBs), while visible telescope (VT) [3,4] is a visible and near-infrared instrument onboard the SVOM. There are two simultaneous channels in VT, which are the 400-650 nm, named the Blue Channel, and 650-1000 nm, named the Red Channel [5,6].…”

Section: Introductionmentioning

confidence: 99%

Accurate Determination of Conversion Gains of SVOM VT CCDs Based on a Signal-Dependent Charge-Sharing Mechanism

Pan

Fan

et al. 2021

Electronics

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The signal-variance method and the photon transfer curve method are the most valuable tools for calculating the conversion gains of charge-coupled device (CCD) detectors. This paper describes the phenomena that arise in the conversion gain measurements of space multi-band variable object monitor (SVOM) visible telescope (VT) CCDs, where the results of the signal-variance method increase with the image gray level, and the results of the photon transfer curve method appear with nonlinearity, which is caused by the signal-dependent charge sharing mechanism of back-illuminated CCDs. A numerical simulation model based on random variables was adopted to analyze the influence of the mechanism on the gain determination. The model simulates all the signals and noise in the flat field image, including the photon signal and photon-shot noise, readout noise, fixed pattern noise, and the signal-dependent charge-sharing signal, and it demonstrated agreement with the experimental data. Then, we proposed a quadratic polynomial curve-fitting formula for the photon transfer curve, and we quantitatively analyzed the relationship between the fitting coefficients and the gain, the signal-dependent charge sharing coefficient, and the full well capacity using the control variable method. Finally, the formula was used to accurately determine the conversion gains of SVOM VT CCDs.

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“…a platform consisting of a multi-wavelength payload coupled to rapid autonomous slewing capability [34 -see Mercier et al -paper 9144-73 this conference]. The science payload will consist of 2 wide-field cameras: the GRB trigger coded-mask camera ECLAIRs [35] and the Gamma-Ray Monitor [36] (see this conference) as well as two narrow-field instruments, the Micro X-ray channel plate Telescope (MXT - [37]; see also Götz et al paper 9144-74 this conference) working in the 0.3-10 keV band and the Visible Telescope (VT - [38,39] French and European astrophysics institutes. The IRAP is Principal Investigator of ECLAIRs, while the CEA is PI of the MXT.…”

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confidence: 99%

The x-/gamma-ray camera ECLAIRs for the gamma-ray burst mission SVOM

Godet

Nasser²,

Atteia³

et al. 2014

SPIE Proceedings

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We present ECLAIRs, the Gamma-ray burst (GRB) trigger camera to fly on-board the Chinese-French mission SVOM. ECLAIRs is a wide-field (∼ 2 sr) coded mask camera with a mask transparency of 40% and a 1024 cm 2 detection plane coupled to a data processing unit, so-called UGTS, which is in charge of locating GRBs in near real time thanks to image and rate triggers. We present the instrument science requirements and how the design of ECLAIRs has been optimized to increase its sensitivity to high-redshift GRBs and low-luminosity GRBs in the local Universe, by having a low-energy threshold of 4 keV. The total spectral coverage ranges from 4 to 150 keV. ECLAIRs is expected to detect ∼ 200 GRBs of all types during the nominal 3 year mission lifetime.To reach a 4 keV low-energy threshold, the ECLAIRs detection plane is paved with 6400 4 × 4 mm 2 and 1 mm-thick Schottky CdTe detectors. The detectors are grouped by 32, in 8x4 matrices read by a low-noise ASIC, forming elementary modules called XRDPIX. In this paper, we also present our current efforts to investigate the performance of these modules with their front-end electronics when illuminated by charged particles and/or photons using radioactive sources. All measurements are made in different instrument configurations in vacuum and with a nominal in-flight detector temperature of −20 • C. This work will enable us to choose the in-flight configuration that will make the best compromise between the science performance and the in-flight operability of ECLAIRs. We will show some highlights of this work.

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A fast onboard star-extraction algorithm optimized for the SVOM Visible Telescope

Cited by 10 publications

References 5 publications

Analysis Methods to Localize and Characterize X-Ray Sources with the Microchannel X-Ray Telescope on Board the SVOM Satellite

Analysis Methods to Localize and Characterize X-Ray Sources with the Microchannel X-Ray Telescope on Board the SVOM Satellite

Accurate Determination of Conversion Gains of SVOM VT CCDs Based on a Signal-Dependent Charge-Sharing Mechanism

The x-/gamma-ray camera ECLAIRs for the gamma-ray burst mission SVOM

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