7 results on '"Colasanti, L."'
Search Results
2. EURECA: European-Japanese Microcalorimeter Array
- Author
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Rohlfs, R., de, Korte P., Anquita, J., Bakker, F., Barcons, X., Bastia, P., Beyer, J., Boersma, D., Briones, F., Bruijn, M., Bussons, J., Camon, A., Carrera, F., Ceballos, M., Colasanti, L., Drung, D., Fabrega, L., Ferrari, L., Gatti, F., Gonzalez-Arrabal, R., Gottardi, L., Hajdas, W., Helisto, P., den, Herder J. W., Hoevers, H., Ishisaki, Y., Kiviranta, M., van, der Kuur J., Macculi, C., Mchedlishvili, A., Mitsuda, Kazuhisa, Monna, B., Mossel, R., Ohashi, T., Pantali, S., Parra, M., Piro, L., Sese, J., Takei, Yoh, Torrioli, G., van, Weers H., Yamasaki, Noriko, and Netherlands Organization for Scientific Research
- Subjects
Cryostat ,Physics ,business.industry ,Transition edge sensors ,Pixel array ,Frequency domain multiplexing ,X-ray microcalorimeters ,Condensed Matter Physics ,Atomic and Molecular Physics, and Optics ,Synchrotron ,law.invention ,Optics ,Beamline ,law ,Frequency-domain-multiplexing ,General Materials Science ,Detector array ,business - Abstract
The EURECA project aims to demonstrate technological readiness of a micro-calorimeter array for application in future X-ray astronomy missions, like Constellation-X, EDGE, and XEUS. The prototype instrument consists of a 5 × 5 pixel array of TES-based micro-calorimeters read out by two SQUID-amplifier channels using frequency-domain-multiplexing (FDM) with digital base-band feedback. The detector array is cooled by a cryogen-free cryostat consisting of a pulse tube cooler and a two stage ADR. Initial tests of the system at the PTB beam line of the BESSY synchrotron showed stable performance and an X-ray energy resolution of 1.5 eV at 250 eV for read-out of one TES-pixel only. Next step is deployment of FDM to read-out the full array. Full performance demonstration is expected end 2008., This work was financially supported by the Dutch Organization for Scientific Research (NWO).
- Published
- 2008
3. The Cryogenic Anticoincidence Detector for ATHENA-XMS
- Author
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Michele Biasotti, S. Lotti, Lorenzo Natalucci, Flavio Gatti, L. Piro, D. Bagliani, Teresa Mineo, Claudio Macculi, L. Colasanti, Marco Barbera, Guido Torrioli, G. La Rosa, Emanuele Perinati, Macculi, C, Colasanti, L, Lotti, S, Natalucci, L, Piro, L, Bagliani, D, Biasotti, M, Gatti, F, Torrioli, G, Barbera, M, Rosa, G, Mineo, T, and Perinati, E
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Physics ,Spectrometer ,Physics::Instrumentation and Detectors ,business.industry ,Detector ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrophysics ,Condensed Matter Physics ,Atomic and Molecular Physics, and Optics ,Space exploration ,Spectral line ,Low temperature detectors · Astronomy and astrophysics · Superconductivity · Silicon · TES ,Settore FIS/05 - Astronomia E Astrofisica ,Cardinal point ,Optics ,Orbit (dynamics) ,General Materials Science ,Spectral resolution ,business ,Energy (signal processing) - Abstract
The TES cryogenic detectors, due to their high spectral resolution and imaging capability in the soft X-ray domain, are the reference devices for the next proposed space missions whose aims are to characterize the spectra of faint or diffuse sources. ATHENA is the re-scoped IXO mission, and one of its focal plane instrument is the X-ray Microcalorimeter Spectrometer (XMS) working in the energy range 0.3-10 keV. XMS will be able to achieve the proposed scientific goals if a background lower than 0.02 cts/cm2/s/keV is guaranteed. The studies performed by GEANT4 simulations depict a scenario where it is mandatory to use an active Anti-Coincidence (AC) to reduce the expected background in the L2 orbit down to the required level. This is possible using a cryogenic AC detector able to provide a rejection efficiency of about 99%. We are developing for this purpose a TES-based detector made by Silicon absorbers (total assembled area about 1 cm2 and 300 ?m thick) and sensed by a Ir:Au TES. All the work done for IXO is applicable to ATHENA, with more margins due to the smaller area required for the detector. Here we present the results obtained from different samples, as a step towards the final detector design.
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- 2012
4. The Cryogenic AntiCoincidence Detector Project for ATHENA+: An Overview Up to the Present Status
- Author
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Emanuele Perinati, Simone Lotti, Lorenzo Natalucci, Luigi Piro, Michele Biasotti, Guido Torrioli, Teresa Mineo, L. Colasanti, Marco Barbera, D. Bagliani, Claudio Macculi, Flavio Gatti, Macculi, C., Piro, L., Colasanti, L., Lotti, S., Natalucci, L., Bagliani, D., Biasotti, M., Gatti, F., Torrioli, G., Barbera, M., Mineo, T., and Perinati, E
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Physics ,Silicon ,business.industry ,Anticoincidence detector ,Detector ,Order (ring theory) ,Space ,TES, Silicon, Iridium, Anticoincidence detector, Space ,Iridium ,Condensed Matter Physics ,Atomic and Molecular Physics, and Optics ,Galaxy ,Optics ,Cardinal point ,TES ,Materials Science (all) ,Settore FIS/05 - Astronomia E Astrofisica ,Atomic and Molecular Physics ,Orbit (dynamics) ,General Materials Science ,Sensitivity (control systems) ,and Optics ,business ,Energy (signal processing) - Abstract
ATHENA+ is a space mission proposal for the next ESA L2-L3 slot. One of the focal plane instruments is the X-ray integral field unit (X-IFU) working in the energy range 0.3–10 keV. It is a multi-array based on TES detectors aimed at characterizing faint or diffuse sources (e.g. WHIM or galaxy outskirt). The X-IFU will be able to achieve the required sensitivity if a low background is guaranteed. The studies performed by GEANT4 simulations depict a scenario where the use of an active anticoincidence (AC) is mandatory to reduce the background expected in L2 orbit down to the goal level of 0.005 cts cm $$^{-2}$$ s $$^{-1}$$ keV $$^{-1}$$ . This is possible using a cryogenic anticoincidence (CryoAC) detector placed within a proper optimized environment surrounding the X-IFU. We propose a 2 $$\times $$ 2 array of microcalorimeter detectors made by silicon absorber (each of about 1 cm $$^{2}$$ and 300 $$\upmu $$ m thick) and sensed by an Ir TES. In order to better understand the involved physics and optimize the performance, we have produced several samples featured by different absorber areas, TES size, and QPs Al collectors. Here we will discuss, as a review, the obtained results and the related impact to the final detector design.
- Published
- 2014
5. The Cryogenic AntiCoincidence detector for ATHENA: the progress towards the final pixel design
- Author
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Michele Biasotti, Teresa Mineo, G. Pizzigoni, D. Bagliani, Donatella Cea, Luigi Piro, Lorenzo Natalucci, Marco Barbera, Simone Lotti, D. Corsini, Emanuele Perinati, L. Colasanti, Guido Torrioli, Flavio Gatti, Claudio Macculi, Macculi, C., Piro, L., Cea, D., Colasanti, L., Lotti, S., Natalucci, L., Gatti, F., Bagliani, D., Biasotti, M., Corsini, D., Pizzigoni, G., Torrioli, G., Barbera, M., Mineo, T., and Perinati, E.
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Simulations ,Silicon ,Warm–hot intergalactic medium ,Field of view ,Orbital mechanics ,Optics ,Field spectroscopy ,Galactic astronomy ,X-rays ,Electronic ,Angular resolution ,Optical and Magnetic Materials ,Electrical and Electronic Engineering ,Anticoincidence ,Image resolution ,Spectroscopy ,Physics ,Spatial resolution ,Equipment and services ,Spectrometer ,Spectrometers ,business.industry ,Sensors ,Applied Mathematics ,Detector ,Computer Science Applications1707 Computer Vision and Pattern Recognition ,Condensed Matter Physics ,ATHENA ,Cryogenic detectors ,TES ,Electronic, Optical and Magnetic Materials ,Transition edge sensor ,business - Abstract
“The Hot and Energetic Universe” is the scientific theme approved by the ESA SPC for a Large mission to be flown in the next ESA slot (2028th) timeframe. ATHENA is a space mission proposal tailored on this scientific theme. It will be the first X-ray mission able to perform the so-called “Integral field spectroscopy”, by coupling a high-resolution spectrometer, the X-ray Integral Field Unit (X-IFU), to a high performance optics so providing detailed images of its field of view (5’ in diameter) with an angular resolution of 5” and fine energy-spectra (2.5eV@E
- Published
- 2014
6. The cryogenic anticoincidence detector for ATHENA-XMS: preliminary results from the new prototype
- Author
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Michele Biasotti, Guido Torrioli, D. Bagliani, L. Colasanti, Marco Barbera, L. Piro, Claudio Macculi, Simone Chiarucci, Lorenzo Natalucci, Flavio Gatti, Teresa Mineo, Simone Lotti, Emanuele Perinati, Macculi, C., Piro, L., Colasanti, L., Lotti, S., Natalucci, L., Bagliani, D., Biasotti, M., Gatti, F., Torrioli, G., Chiarucci, S., Barbera, M., Mineo, T., and Perinati, E.
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Anticoincidence detector ,Low temperature Detector ,Anticoincidence detectors ,Astrophysics ,Orbital mechanics ,law.invention ,Optics ,law ,Electronic ,Optical and Magnetic Materials ,Electrical and Electronic Engineering ,High Energy Astrophysics ,Low temperature Detectors ,TES ,Electronic, Optical and Magnetic Materials ,Condensed Matter Physics ,Computer Science Applications1707 Computer Vision and Pattern Recognition ,Applied Mathematics ,Physics ,Spectrometer ,business.industry ,Electronic, Optical and Magnetic Material ,Bolometer ,Detector ,Applied Mathematic ,Cardinal point ,Millimeter ,Satellite ,Transition edge sensor ,High Energy Astrophysic ,business - Abstract
ATHENA has been the re-scoped IXO mission, and one of the foreseen focal plane instrument was the X-ray Microcalorimeter Spectrometer (XMS) working in the energy range 0.3-10 keV, which was a kilo-pixel array based on TES (Transition Edge Sensor) detectors. The need of an anticoincidence (AC) detector is legitimated by the results performed with GEANT4 simulations about the impact of the non x-ray background onto XMS at L2 orbit (REQ. < 0.02 cts/cm2/s/keV). Our consortium has both developed and tested several samples, with increasing area, in order to match the large area of the XMS (64 mm2). Here we show the preliminary results from the last prototype. The results achieved in this work offer a solution to reduce the particle background not only for the presently study mission, but also for any satellite/balloon borne instrument that foresees a TES-based microcalorimeters/bolometers focal plane (from millimeter to x-ray domain). © 2012 SPIE.
- Published
- 2012
7. The TES-based cryogenic anticoincidence detector for IXO: First results from large area prototypes
- Author
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A. Bonati, Luigi Piro, Guido Torrioli, Flavio Gatti, Emanuele Perinati, Lorenzo Natalucci, Claudio Macculi, Giovanni La Rosa, Simone Lotti, Teresa Mineo, Francesco Brunetto, Marco Barbera, P. Bastia, D. Bagliani, L. Colasanti, L. Ferrari, Macculi, C., Colasanti, L., Lotti, S., Natalucci, L., Piro, L., Bagliani, D., Brunetto, F., Ferrari, L., Gatti, F., Torrioli, G., Bastia, P., Bonati, A., Barbera, M., La Rosa, G., Mineo, T., and Perinati, E.
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Cryogenic Detectors ,IXO ,SQUID ,TES ,X-ray ,Electronic, Optical and Magnetic Materials ,Condensed Matter Physics ,Computer Science Applications1707 Computer Vision and Pattern Recognition ,Applied Mathematics ,Electrical and Electronic Engineering ,Space exploration ,Signal-to-noise ratio ,Optics ,Settore FIS/05 - Astronomia E Astrofisica ,Observatory ,Electronic ,Optical and Magnetic Materials ,Physics ,Spectrometer ,Pixel ,business.industry ,Detector ,Pulse duration ,Cardinal point ,business ,TES, Cryogenic Detectors, X-ray, SQUID, IXO - Abstract
The technique which combines high resolution spectroscopy with imaging capability is a powerful tool to extract fundamental information in X-ray Astrophysics and Cosmology. TES (Transition Edge Sensors)-based microcalorimeters match at best the requirements for doing fine spectroscopy and imaging of both bright (high count rate) and faint (poor signal-to-noise ratio) sources. For this reason they are considered among the most promising detectors for the next high energy space missions and are being developed for use on the focal plane of the IXO (International X-ray Observatory) mission. In order to achieve the required signal-to-noise ratio for faint or diffuse sources it is necessary to reduce the particle-induced background by almost two orders of magnitude. This reduction can only be achieved by adopting an active anticoincidence technique. In this paper, we will present a novel anticoincidence detector based on a TES sensor developed for the IXO mission. The pulse duration and the large area of the IXO TESarray (XMS X-ray Microcalorimeter Spectrometer) require a proper design of the anticoincidence detector. It has to cover the full XMS area, yet delivering a fast response. We have therefore chosen to develop it in a four-pixel design. Experimental results from the large-area pixel prototypes will be discussed, also including design considerations.
- Published
- 2010
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