ATHENA WFI optical blocking filters development status toward the end of the instrument phase-A

Ugo Lo Cicero, Marco Barbera, Luisa Sciortino, Fabio D'Anca, Ugo Lo Cicero, Adam Pilch, Graziella Branduardi Raymont, Giancarlo Parodi, Szymon Polak, Marco Barbera, Miroslaw Rataj, Salvatore Varisco, Emanuele Perinati, Norbert Meidinger, Alfonso Collura, Salvatore Sciortino, Gregor Rauw, Marco Barbera, Roberto Candia, Teresa Mineo

Risultato della ricerca: Other

3 Citazioni (Scopus)

Abstract

The Wide Field Imager (WFI) is one of the two instruments of the ATHENA astrophysics space mission approved by ESA as the second large mission in the Cosmic Vision 2015-2025 Science Programme. The WFI, based on a large array of depleted field effect transistors (DEPFET), will provide imaging in the 0.2-15 keV band over a 40'x40' field of view, simultaneously with spectrally and time resolved photon counting. The WFI detector is also sensitive to UV/Vis photons, with an electron-hole pair production efficiency in the UV/VIS larger than that for X-ray photons. Optically generated photo-electrons may degrade the spectral resolution as well as change the energy scale by introducing a signal offset. For this reason, the use of X-ray transparent optical blocking filters (OBFs) are needed to allow the observation of X-ray sources that present a UV/Vis bright counterpart. The OBFs design is challenging since one of the two required filters is quite large (∼ 160 mm × 160 mm), very thin (< 200 nm), and shall survive the mechanical load during the launch. In this paper, we review the main results of modeling and characterization tests of OBF partially representative samples, performed during the phase A study, to identify the suitable materials, optimize the design, prove that the filters can be launched in atmospheric pressure, and thus demonstrate that the chosen technology can reach the proper technical readiness before mission adoption.
Lingua originaleEnglish
Pagine55-
Numero di pagine13
Stato di pubblicazionePublished - 2018

Fingerprint

Wide-field
Imager
Image sensors
Photons
Filter
filters
X rays
Astrophysics
Photon
Electrons
Spectral resolution
Electron
Field effect transistors
photons
Space Missions
Atmospheric pressure
Field-effect Transistor
Photon Counting
Filter Design
Spectral Resolution

All Science Journal Classification (ASJC) codes

  • Condensed Matter Physics
  • Computer Science Applications
  • Applied Mathematics
  • Electrical and Electronic Engineering
  • Electronic, Optical and Magnetic Materials

Cita questo

ATHENA WFI optical blocking filters development status toward the end of the instrument phase-A. / Lo Cicero, Ugo; Barbera, Marco; Sciortino, Luisa; D'Anca, Fabio; Lo Cicero, Ugo; Pilch, Adam; Branduardi Raymont, Graziella; Parodi, Giancarlo; Polak, Szymon; Barbera, Marco; Rataj, Miroslaw; Varisco, Salvatore; Perinati, Emanuele; Meidinger, Norbert; Collura, Alfonso; Sciortino, Salvatore; Rauw, Gregor; Barbera, Marco; Candia, Roberto; Mineo, Teresa.

2018. 55-.

Risultato della ricerca: Other

Lo Cicero, U, Barbera, M, Sciortino, L, D'Anca, F, Lo Cicero, U, Pilch, A, Branduardi Raymont, G, Parodi, G, Polak, S, Barbera, M, Rataj, M, Varisco, S, Perinati, E, Meidinger, N, Collura, A, Sciortino, S, Rauw, G, Barbera, M, Candia, R & Mineo, T 2018, 'ATHENA WFI optical blocking filters development status toward the end of the instrument phase-A', pagg. 55-.
Lo Cicero, Ugo ; Barbera, Marco ; Sciortino, Luisa ; D'Anca, Fabio ; Lo Cicero, Ugo ; Pilch, Adam ; Branduardi Raymont, Graziella ; Parodi, Giancarlo ; Polak, Szymon ; Barbera, Marco ; Rataj, Miroslaw ; Varisco, Salvatore ; Perinati, Emanuele ; Meidinger, Norbert ; Collura, Alfonso ; Sciortino, Salvatore ; Rauw, Gregor ; Barbera, Marco ; Candia, Roberto ; Mineo, Teresa. / ATHENA WFI optical blocking filters development status toward the end of the instrument phase-A. 13 pag.
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abstract = "The Wide Field Imager (WFI) is one of the two instruments of the ATHENA astrophysics space mission approved by ESA as the second large mission in the Cosmic Vision 2015-2025 Science Programme. The WFI, based on a large array of depleted field effect transistors (DEPFET), will provide imaging in the 0.2-15 keV band over a 40'x40' field of view, simultaneously with spectrally and time resolved photon counting. The WFI detector is also sensitive to UV/Vis photons, with an electron-hole pair production efficiency in the UV/VIS larger than that for X-ray photons. Optically generated photo-electrons may degrade the spectral resolution as well as change the energy scale by introducing a signal offset. For this reason, the use of X-ray transparent optical blocking filters (OBFs) are needed to allow the observation of X-ray sources that present a UV/Vis bright counterpart. The OBFs design is challenging since one of the two required filters is quite large (∼ 160 mm × 160 mm), very thin (< 200 nm), and shall survive the mechanical load during the launch. In this paper, we review the main results of modeling and characterization tests of OBF partially representative samples, performed during the phase A study, to identify the suitable materials, optimize the design, prove that the filters can be launched in atmospheric pressure, and thus demonstrate that the chosen technology can reach the proper technical readiness before mission adoption.",
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T1 - ATHENA WFI optical blocking filters development status toward the end of the instrument phase-A

AU - Lo Cicero, Ugo

AU - Barbera, Marco

AU - Sciortino, Luisa

AU - D'Anca, Fabio

AU - Lo Cicero, Ugo

AU - Pilch, Adam

AU - Branduardi Raymont, Graziella

AU - Parodi, Giancarlo

AU - Polak, Szymon

AU - Barbera, Marco

AU - Rataj, Miroslaw

AU - Varisco, Salvatore

AU - Perinati, Emanuele

AU - Meidinger, Norbert

AU - Collura, Alfonso

AU - Sciortino, Salvatore

AU - Rauw, Gregor

AU - Barbera, Marco

AU - Candia, Roberto

AU - Mineo, Teresa

PY - 2018

Y1 - 2018

N2 - The Wide Field Imager (WFI) is one of the two instruments of the ATHENA astrophysics space mission approved by ESA as the second large mission in the Cosmic Vision 2015-2025 Science Programme. The WFI, based on a large array of depleted field effect transistors (DEPFET), will provide imaging in the 0.2-15 keV band over a 40'x40' field of view, simultaneously with spectrally and time resolved photon counting. The WFI detector is also sensitive to UV/Vis photons, with an electron-hole pair production efficiency in the UV/VIS larger than that for X-ray photons. Optically generated photo-electrons may degrade the spectral resolution as well as change the energy scale by introducing a signal offset. For this reason, the use of X-ray transparent optical blocking filters (OBFs) are needed to allow the observation of X-ray sources that present a UV/Vis bright counterpart. The OBFs design is challenging since one of the two required filters is quite large (∼ 160 mm × 160 mm), very thin (< 200 nm), and shall survive the mechanical load during the launch. In this paper, we review the main results of modeling and characterization tests of OBF partially representative samples, performed during the phase A study, to identify the suitable materials, optimize the design, prove that the filters can be launched in atmospheric pressure, and thus demonstrate that the chosen technology can reach the proper technical readiness before mission adoption.

AB - The Wide Field Imager (WFI) is one of the two instruments of the ATHENA astrophysics space mission approved by ESA as the second large mission in the Cosmic Vision 2015-2025 Science Programme. The WFI, based on a large array of depleted field effect transistors (DEPFET), will provide imaging in the 0.2-15 keV band over a 40'x40' field of view, simultaneously with spectrally and time resolved photon counting. The WFI detector is also sensitive to UV/Vis photons, with an electron-hole pair production efficiency in the UV/VIS larger than that for X-ray photons. Optically generated photo-electrons may degrade the spectral resolution as well as change the energy scale by introducing a signal offset. For this reason, the use of X-ray transparent optical blocking filters (OBFs) are needed to allow the observation of X-ray sources that present a UV/Vis bright counterpart. The OBFs design is challenging since one of the two required filters is quite large (∼ 160 mm × 160 mm), very thin (< 200 nm), and shall survive the mechanical load during the launch. In this paper, we review the main results of modeling and characterization tests of OBF partially representative samples, performed during the phase A study, to identify the suitable materials, optimize the design, prove that the filters can be launched in atmospheric pressure, and thus demonstrate that the chosen technology can reach the proper technical readiness before mission adoption.

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