Development of the X-ray CCD camera for the MAXI mission

Katayama, Haruyoshi; Tomida, H.; Matsuoka, M.; Tsunemi, H.; Miyata, Emi; Kamiyama, Daisuke; Nemes, Norbert

doi:10.1016/j.nima.2005.01.075

Cited by 5 publications

(2 citation statements)

References 8 publications

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“…The use of a back-illuminated (BI) chip for the focal plane CMOS-APS is essential not only for the reason of energy range (down to ~0.5 keV), but also for conservation of signal charges in split events (Sakao et al 2011) and to minimize contamination from signal charges partially-absorbed in the gate insulation layer in the lower-energy end of energy spectra (Katayama et al 2005). We have been working with e2v, U.K., for the possible development of BI CMOS-APS devices, with several X-ray evaluation on commercially-available BI devices from e2v currently ongoing, including that with an 55 Fe isotope (Figure 4 left) and with a soft X-ray beam line in collaboration with Tokyo Metropolitan University (TMU; Figure 4 right).…”

Section: X-ray Evaluation Activities On Cmos-aps Devicesmentioning

confidence: 99%

The soft x-ray photon-counting spectroscopic imager for the sun

Sakao

Narukage

Shimojo

et al. 2013

Solar Physics and Space Weather Instrumentation V

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We present science and development activities of the soft X-ray photon-counting spectroscopic imager for the solar corona that we conceive as a possible scientific payload for the Japanese Solar-C mission. The imager employs a grazing-incidence sector mirror of Wolter-I type with which images of the corona are to be taken in a wide temperature range (1 MK to beyond 10 MK) with the highest-ever angular resolution (0.5"/pixel for a focal length of 4 m) as an Xray telescope for the Sun. Moreover, by employing a back-thinned CMOS image sensor as the focal-plane device, we attempmt to implement photon-counting capability with which imaging-spectroscopy of the X-ray corona will be performed for the first time, in the energy range from ~0.5 keV up to 10 keV. The imaging-spectroscopic observations will provide totally-new information on mechanism(s) for magnetic reconnection, generation of supra-thermal electrons in the reconnecting magnetic structure during flares, and for the generation of hot coronal plasmas (heated beyond a few MK) which may be responsible for the formation of the hot cores of solar active regions.

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Section: X-ray Evaluation Activities On Cmos-aps Devicesmentioning

confidence: 99%

The soft x-ray photon-counting spectroscopic imager for the sun

Sakao

Narukage

Shimojo

et al. 2013

Solar Physics and Space Weather Instrumentation V

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“…The CCDs used in MAXI/SSC are fabricated by Hamamatsu Photonics (Tsunemi et al) 1 The CCD wafer is front-illuminated and CCD (Katayama et al) 2 and operated in full frame transfer mode. The number of pixel in each CCD is 1024×1024, and the pixel size is 24μm×24μm, this gives the area of about 25mm×25mm.…”

Section: Overview Of Maxi/sscmentioning

confidence: 99%

Solid state slit camera (SSC) onboard MAXI

Kimura

Tsunemi

Tomida

et al. 2010

Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray

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The MAXI Mission on the ISS: Science and Instruments for Monitoring All-Sky X-Ray Images

Matsuoka¹,

Kawasaki²,

Ueno³

et al. 2009

Publications of the Astronomical Society of Japan

726

342

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The Monitor of All-sky X-ray Image (MAXI) mission is the first astronomical payload to be installed on the Japanese Experiment Module — Exposed Facility (JEM-EF or Kibo-EF) on the International Space Station. It has two types of X-ray slit cameras with wide FOVs and two kinds of X-ray detectors consisting of gas proportional counters covering the energy range of 2 to 30 keV and X-ray CCDs covering the energy range of 0.5 to 12 keV. MAXI will be more powerful than any previous X-ray All Sky Monitor payloads, being able to monitor hundreds of Active Galactic Nuclei. A realistic simulation under optimal observation conditions suggests that MAXI will provide all-sky images of X-ray sources of $\sim $20 mCrab ($\sim $7 $\times$ 10$^{-10} $erg cm$^{-2} $s$^{-1}$ in the energy band of 2–30 keV) from observations during one ISS orbit (90 min), $\sim $4.5 mCrab for one day, and $\sim $2 mCrab for one week. The final detectability of MAXI could be $\sim $0.2 mCrab for two years, which is comparable to the source confusion limit of the MAXI field of view (FOV). The MAXI objectives are: (1) to alert the community to X-ray novae and transient X-ray sources, (2) to monitor long-term variabilities of X-ray sources, (3) to stimulate multi-wavelength observations of variable objects, (4) to create unbiased X-ray source cataloges, and (5) to observe diffuse cosmic X-ray emissions, especially with better energy resolution for soft X-rays down to 0.5 keV.

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Development of the X-ray CCD camera for the MAXI mission

Cited by 5 publications

References 8 publications

The soft x-ray photon-counting spectroscopic imager for the sun

The soft x-ray photon-counting spectroscopic imager for the sun

Solid state slit camera (SSC) onboard MAXI

The MAXI Mission on the ISS: Science and Instruments for Monitoring All-Sky X-Ray Images

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