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43 results on '"Gburek, S"'

1. XIPE: The X-ray imaging polarimetry explorer

Author

Soffitta, P, Bellazzini, R, Bozzo, E, Burwitz, V, Castro-Tirado, AJ, Costa, E, Courvoisier, T, Feng, H, Gburek, S, Goosmann, R, Karas, V, Matt, G, Muleri, F, Nandra, K, Pearce, M, Poutanen, J, Reglero, V, Sabau Maria, D, Santangelo, A, Tagliaferri, G, Tenzer, C, Vink, J, Weisskopf, MC, Zane, S, Agudo, I, Antonelli, A, Attina, P, Baldini, L, Bykov, A, Carpentiero, R, Cavazzuti, E, Churazov, E, Del Monte, E, De Martino, D, Donnarumma, I, Doroshenko, V, Evangelista, Y, Ferreira, I, Gallo, E, Grosso, N, Kaaret, P, Kuulkers, E, Laranaga, J, Latronico, L, Lumb, DH, Macian, J, Malzac, J, Marin, F, Massaro, E, Minuti, M, Mundell, C, Ness, JU, Oosterbroek, T, Paltani, S, Pareschi, G, Perna, R, Petrucci, PO, Pinazo, HB, Pinchera, M, Rodriguez, JP, Roncadelli, M, Santovincenzo, A, Sazonov, S, Sgro, C, Spiga, D, Svoboda, J, Theobald, C, Theodorou, T, Turolla, R, Wilhelmi De Ona, E, Winter, B, Akbar, AM, Allan, H, Aloisio, R, Altamirano, D, Amati, L, Amato, E, Angelakis, E, Arezu, J, Atteia, JL, Axelsson, M, Bachetti, M, Ballo, L, Balman, S, Bandiera, R, Barcons, X, Basso, S, Baykal, A, Becker, W, Behar, E, Beheshtipour, B, Belmont, R, Berger, E, Bernardini, F, Bianchi, S, Bisnovatyi-Kogan, G, Blasi, P, Blay, P, Bodaghee, A, and Boer, M

Subjects
X-ray Astronomy, Polarimetry, X-ray optics, Gas Pixel Detector
Abstract

XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to X-ray Astronomy. At the time of writing XIPE is in a competitive phase A as fourth medium size mission of ESA (M4). It promises to reopen the polarimetry window in high energy Astrophysics after more than 4 decades thanks to a detector that efficiently exploits the photoelectric effect and to X-ray optics with large effective area. XIPE uniqueness is time-spectrally-spatially-resolved X-ray polarimetry as a breakthrough in high energy astrophysics and fundamental physics. Indeed the payload consists of three Gas Pixel Detectors at the focus of three X-ray optics with a total effective area larger than one XMM mirror but with a low weight. The payload is compatible with the fairing of the Vega launcher. XIPE is designed as an observatory for X-ray astronomers with 75 % of the time dedicated to a Guest Observer competitive program and it is organized as a consortium across Europe with main contributions from Italy, Germany, Spain, United Kingdom, Poland, Sweden.

Published
2016

2. EUV and HXR Signatures of Electron Acceleration During the Failed Eruption of a Filament

Author

Netzel, A., Mrozek, T., Kolomanski, S., and Gburek, S.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We search for EUV brightenings in TRACE 171 {\AA} images and HXR bursts observed during failed eruptions. We expect that if an eruption is confined due to interaction with overlying magnetic structures then we should observe effects connected with reconnection between magnetic structures and acceleration of particles. We utilized TRACE observations of three well observed failed eruptions. EUV images were compared to HXR spatial distribution reconstructed from Yohkoh/HXT and RHESSI data. The EUV light curves of a selected area were compared to height profiles of eruption, HXR emission and HXR photon spectral index of power-law fit to HXR data. We have found that EUV brightenings are closely related to the eruption velocity decrease, to HXR bursts and to episodes of hardening of HXR spectra. The EUV brightened areas are observed far from the flaring structure, in footpoints of large systems of loops observed 30-60 minutes after the maximum of a flare. These are not `post-flare' loops that are also observed but at significantly lower heights. The high lying systems of loops are observed at heights equal to height, at which eruption was observed to stop. We observed HXR source spatially correlated with EUV brightening only once. For other EUV brightened areas we estimated the expected brightness of HXR sources. We find that EUV brightenings are produced due to interaction between the erupting structure with overlying loops. The interaction is strong enough to heat the system of high loops. These loops cool down and are visible in EUV range about 30-60 minutes later. The estimated brightness of HXR sources associated with EUV brightenings shows that they are too weak to be detected with present instruments. However, next generation instruments will have enough dynamic range and sensitivity to enable such observations., Comment: A&A accepted

Published
2012
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3. X-raying hot plasma in solar active regions with the SphinX spectrometer

Author

Miceli, M., Reale, F., Gburek, S., Terzo, S., Barbera, M., Collura, A., Sylwester, J., Kowalinski, M., Podgorski, P., and Gryciuk, M.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The detection of very hot plasma in the quiescent corona is important for diagnosing heating mechanisms. The presence and the amount of such hot plasma is currently debated. The SphinX instrument on-board CORONAS-PHOTON mission is sensitive to X-ray emission well above 1 keV and provides the opportunity to detect the hot plasma component. We analyzed the X-ray spectra of the solar corona collected by the SphinX spectrometer in May 2009 (when two active regions were present). We modelled the spectrum extracted from the whole Sun over a time window of 17 days in the 1.34-7 keV energy band by adopting the latest release of the APED database. The SphinX broadband spectrum cannot be modelled by a single isothermal component of optically thin plasma and two components are necessary. In particular, the high statistics and the accurate calibration of the spectrometer allowed us to detect a very hot component at ~7 million K with an emission measure of ~2.7 x 10^44 cm^-3. The X-ray emission from the hot plasma dominates the solar X-ray spectrum above 4 keV. We checked that this hot component is invariably present both at high and low emission regimes, i.e. even excluding resolvable microflares. We also present and discuss a possible non-thermal origin (compatible with a weak contribution from thick-target bremsstrahlung) for this hard emission component. Our results support the nanoflare scenario and might confirm that a minor flaring activity is ever-present in the quiescent corona, as also inferred for the coronae of other stars., Comment: 6 pages, 5 figures. Accepted for publication in A&A

Published
2012
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4. Sphinx measurements of the 2009 solar minimum x-ray emission

Author

Sylwester, J., Kowalinski, M., Gburek, S., Siarkowski, M., Kuzin, S., Farnik, F., Reale, F., Phillips, K. J. H., Bakala, J., Gryciuk, M., Podgorski, P., and Sylwester, B.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The SphinX X-ray spectrophotometer on the CORONAS-PHOTON spacecraft measured soft X-ray emission in the 1-15 keV energy range during the deep solar minimum of 2009 with a sensitivity much greater than GOES. Several intervals are identified when the X-ray flux was exceptionally low, and the flux and solar X-ray luminosity are estimated. Spectral fits to the emission at these times give temperatures of 1.7-1.9 MK and emission measures between 4 x 10^47 cm^-3 and 1.1 x 10^48 cm^-3. Comparing SphinX emission with that from the Hinode X-ray Telescope, we deduce that most of the emission is from general coronal structures rather than confined features like bright points. For one of 27 intervals of exceptionally low activity identified in the SphinX data, the Sun's X-ray luminosity in an energy range roughly extrapolated to that of ROSAT (0.1-2.4 keV) was less than most nearby K and M dwarfs., Comment: Astrophysical Journal, in press. 14 pp, 3 figures

Published
2012
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7. Small Scale Events Seen in SXT Observations

Author

Gburek, S., Sylwester, J., Burton, W.B., editor, Kuijpers, J. M. E., editor, Van Den Heuvel, E. P. J., editor, Van Der Laan, H., editor, Appenzeller, I., editor, Bahcall, J. N., editor, Bertola, F., editor, Cassinelli, J. P., editor, Cesarsky, C. J., editor, Engvold, O., editor, McCray, R., editor, Murdin, P. G., editor, Pacini, F., editor, Radhakrishnan, V., editor, Sato, K., editor, Shu, F. H., editor, Somov, B. V., editor, Sunyaev, R. A., editor, Tanaka, Y., editor, Tremaine, S., editor, Weiss, N. O., editor, Hanslmeier, Arnold, editor, Veronig, Astrid, editor, and Messerotti, Mauro, editor

Published
2005
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19. XIPE: the x-ray imaging polarimetry explorer

Author

Soffitta, P., Bellazzini, R., Bozzo, E., Burwitz, V., Castro Tirado, A. J., Costa, E., Courvoisier, T., Feng, H., Gburek, S., Goosmann, R., Karas, V., Boettcher, M., Bogdanov, S., Bombaci, I., Bonino, R., Braga, J., Brandt, W., Brez, A., Bucciantini, N., Burderi, L., Caiazzo, I., Matt, G., Campana, R., Campana, S., Capitanio, F., Cappi, M., Cardillo, M., Casella, P., Catmabacak, O., Cenko, B., Cerda Duran, P., Cerruti, C., Muleri, F., Chaty, S., Chauvin, M., Chen, Y., Chenevez, J., Chernyakova, M., Cheung Teddy, C. C., Christodoulou, D., Connell, P., Corbet, R., Coti Zelati, F., Nandra, K., Covino, S., Cui, W., Cusumano, G., D'Ai, A., D'Ammando, F., Dadina, M., Dai, Z., De Rosa, A., De Ruvo, L., Degenaar, N., Pearce, M., Del Santo, M., Del Zanna, L., Dewangan, G., Di Cosimo, S., Di Lalla, N., Di Persio, G., Di Salvo, T., Dias, T., Done, C., Dovciak, M., Poutanen, J., Doyle, G., Ducci, L., Elsner, R., Enoto, T., Escada, J., Esposito, P., Eyles, C., Fabiani, S., Falanga, M., Falocco, S., Reglero, V., Fan, Y., Fender, R., Feroci, M., Ferrigno, C., Forman, W., Foschini, L., Fragile, C., Fuerst, F., Fujita, Y., Gasent Blesa, J. L., Sabau Maria, D., Gelfand, J., Gendre, B., Ghirlanda, G., Ghisellini, G., Giroletti, M., Goetz, D., Gogus, E., Gomez, J. L., Gonzalez, D., Gonzalez Riestra, R., Santangelo, A., Gotthelf, E., Gou, L., Grandi, P., Grinberg, V., Grise, F., Guidorzi, C., Gurlebeck, N., Guver, T., Haggard, D., Hardcastle, M., Tagliaferri, G., Hartmann, D., Haswell, C., Heger, A., Hernanz, M., Heyl, J., Ho, L., Hoormann, J., Horak, J., Huovelin, J., Huppenkothen, D., Tenzer, C., Iaria, R., Inam Sitki, C., Ingram, A., Israel, G., Izzo, L., Burgess, M., Jackson, M., Ji, L., Jiang, J., Vink, J., Johannsen, T., Jones, C., Jorstad, S., Kajava, J. J. E., Kalamkar, M., Kalemci, E., Kallman, T., Kamble, A., Kislat, F., Kiss, M., Weisskopf, M. C., Klochkov, D., Koerding, E., Kolehmainen, M., Koljonen, K., Komossa, S., Kong, A., Korpela, S., Kowalinski, M., Krawczynski, H., Kreykenbohm, I., Zane, S., Kuss, M., Lai, D., Lan, M., Larsson, J., Laycock, S., Lazzati, D., Leahy, D., Li, H., Li, J., L. X., Li, Agudo, I., Li, T., Li, Z., Linares, M., Lister, M., Liu, H., Lodato, G., Lohfink, A., Longo, F., Luna, G., Lutovinov, A., Antonelli, A., Mahmoodifar, S., Maia, J., Mainieri, V., Maitra, C., Maitra, D., Majczyna, A., Maldera, S., Malyshev, D., Manfreda, A., Manousakis, A., Attina, P., Manuel, R., Margutti, R., Marinucci, A., Markoff, S., Marscher, A., Marshall, H., Massaro, F., Mclaughlin, M., Medina Tanco, G., Mehdipour, M., Baldini, L., Middleton, M., Mignani, R., Mimica, P., Mineo, T., Mingo, B., Miniutti, G., Mirac, S. M., Morlino, G., Motlagh, A. V., Motta, S. E., Bykov, A., Mushtukov, A., Nagataki, S., Nardini, F., Nattila, J., Navarro, G. J., Negri, B., Negro, M., Nenonen, S., Neustroev, V., Nicastro, F., Carpentiero, R., Norton, A., Nucita, A., O'Brien, P., O'Dell, S., Odaka, H., Olmi, B., Omodei, N., Orienti, M., Orlandini, M., Osborne, J., Cavazzuti, E., Pacciani, L., Paliya, V. S., Papadakis, I., Papitto, A., Paragi, Z., Pascal, P., Paul, B., Pavan, L., Pellizzoni, A., Perinati, E., Churazov, E., Pesce Rollins, M., Piconcelli, E., Pili, A. G., Pilia, M., Pohl, M., Ponti, G., Porquet, D., Possenti, A., Postnov, K., Prandoni, I., Del Monte, E., Produit, N., Puehlhofer, G., Ramsey, B., Razzano, M., Rea, N., Reig, P., Reinsch, K., Reiprich, T., Reynolds, M., Risaliti, G., De Martino, D., Roberts, T., Rodriguez, J., Rossi, M. E., Rosswog, S., Rozanska, A., Rubini, A., Rudak, B., Russell, D., Ryde, F., Sabatini, S., Donnarumma, I., Sala, G., Salvati, M., Sasaki, M., Savolainen, T., Saxton, R., Scaringi, S., Schawinski, K., Schulz, N. S., Schwope, A., Severgnini, P., Doroshenko, V., Sharon, M., Shaw, A., Shearer, A., Shesheng, X., Shih, I. C., Silva, K., Silva, R., Silver, E., Smale, A., Spada, F., Evangelista, Y., Spandre, G., Stamerra, A., Stappers, B., Starrfield, S., Stawarz, L., Stergioulas, N., Stevens, A., Stiele, H., Suleimanov, V., Sunyaev, R., Ferreira, I., Slowikowska, A., Tamborra, F., Tavecchio, F., Taverna, Roberto, Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Tong, H., Torok, G., Gallo, E., Torres, D. F., Tortosa, A., Tramacere, A., Trimble, V., Trinchieri, G., Tsygankov, S., Tuerler, M., Turriziani, S., Ursini, F., Uttley, P., Grosso, N., Varniere, P., Vincent, F., Vurgun, E., Wang, C., Wang, Z., Watts, A., Wheeler, J. C., Wiersema, K., Wijnands, R., Wilms, J., Kaaret, P., Wolter, A., Wood, K., Wu, K., Wu, X., Xiangyu, W., Xie, F., Xu, R., Yan, S. P., Yang, J., Yu, W., Kuulkers, E., Yuan, F., Zajczyk, A., Zanetti, D., Zanin, R., Zanni, C., Zappacosta, L., Zdziarski, A. A., Zech, A., Zhang, H., Zhang, S., Laranaga, J., Zhang, W., Zoghbi, A., Latronico, L., Lumb, D. H., Macian, J., Malzac, J., Marin, F., Massaro, E., Minuti, M., Mundell, C., Ness, J. U., Oosterbroek, T., Paltani, S., Pareschi, G., Perna, R., Petrucci, P. O., Pinazo, H. B., Pinchera, M., Rodriguez, J. P., Roncadelli, M., Santovincenzo, A., Sazonov, S., Sgro, C., Spiga, D., Svoboda, J., Theobald, C., Theodorou, T., Turolla, Roberto, Wilhelmi De Ona, E., Winter, B., Akbar, A. M., Allan, H., Aloisio, R., Altamirano, D., Amati, L., Amato, E., Angelakis, E., Arezu, J., Atteia, J. L., Axelsson, M., Bachetti, M., Ballo, L., Balman, S., Bandiera, R., Barcons, X., Basso, S., Baykal, A., Becker, W., Behar, E., Beheshtipour, B., Belmont, R., Berger, E., Bernardini, F., Bianchi, S., Bisnovatyi Kogan, G., Blasi, P., Blay, P., Bodaghee, A., Boer, M., Gravitation and Astroparticle Physics Amsterdam, API (FNWI), den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Soffitta, P., Bellazzini, R., Bozzo, E., Burwitz, V., Castro-Tirado, A. J., Costa, E., Courvoisier, T., Feng, H., Gburek, S., Goosmann, R., Karas, V., Matt, G., Muleri, F., Nandra, K., Pearce, M., Poutanen, J., Reglero, V., Sabau Maria, D., Santangelo, A., Tagliaferri, G., Tenzer, C., Vink, J., Weisskopf, M. C., Zane, S., Agudo, I., Antonelli, A., Attina, P., Baldini, L., Bykov, A., Carpentiero, R., Cavazzuti, E., Churazov, E., Del Monte, E., De Martino, D., Donnarumma, I., Doroshenko, V., Evangelista, Y., Ferreira, I., Gallo, E., Grosso, N., Kaaret, P., Kuulkers, E., Laranaga, J., Latronico, L., Lumb, D. H., Macian, J., Malzac, J., Marin, F., Massaro, E., Minuti, M., Mundell, C., Ness, J. U., Oosterbroek, T., Paltani, S., Pareschi, G., Perna, R., Petrucci, P. -O., Pinazo, H. B., Pinchera, M., Rodriguez, J. P., Roncadelli, M., Santovincenzo, A., Sazonov, S., Sgro, C., Spiga, D., Svoboda, J., Theobald, C., Theodorou, T., Turolla, R., Wilhelmi De Ona, E., Winter, B., Akbar, A. M., Allan, H., Aloisio, R., Altamirano, D., Amati, L., Amato, E., Angelakis, E., Arezu, J., Atteia, J. -L., Axelsson, M., Bachetti, M., Ballo, L., Balman, S., Bandiera, R., Barcons, X., Basso, S., Baykal, A., Becker, W., Behar, E., Beheshtipour, B., Belmont, R., Berger, E., Bernardini, F., Bianchi, S., Bisnovatyi-Kogan, G., Blasi, P., Blay, P., Bodaghee, A., Boer, M., Boettcher, M., Bogdanov, S., Bombaci, I., Bonino, R., Braga, J., Brandt, W., Brez, A., Bucciantini, N., Burderi, L., Caiazzo, I., Campana, R., Campana, S., Capitanio, F., Cappi, M., Cardillo, M., Casella, P., Catmabacak, O., Cenko, B., Cerda-Duran, P., Cerruti, C., Chaty, S., Chauvin, M., Chen, Y., Chenevez, J., Chernyakova, M., Cheung Teddy, C. C., Christodoulou, D., Connell, P., Corbet, R., Coti Zelati, F., Covino, S., Cui, W., Cusumano, G., D'Ai, A., D'Ammando, F., Dadina, M., Dai, Z., De Rosa, A., De Ruvo, L., Degenaar, N., Del Santo, M., Del Zanna, L., Dewangan, G., Di Cosimo, S., Di Lalla, N., Di Persio, G., Di Salvo, T., Dias, T., Done, C., Dovciak, M., Doyle, G., Ducci, L., Elsner, R., Enoto, T., Escada, J., Esposito, P., Eyles, C., Fabiani, S., Falanga, M., Falocco, S., Fan, Y., Fender, R., Feroci, M., Ferrigno, C., Forman, W., Foschini, L., Fragile, C., Fuerst, F., Fujita, Y., Gasent-Blesa, J. L., Gelfand, J., Gendre, B., Ghirlanda, G., Ghisellini, G., Giroletti, M., Goetz, D., Gogus, E., Gomez, J. -L., Gonzalez, D., Gonzalez-Riestra, R., Gotthelf, E., Gou, L., Grandi, P., Grinberg, V., Grise, F., Guidorzi, C., Gurlebeck, N., Guver, T., Haggard, D., Hardcastle, M., Hartmann, D., Haswell, C., Heger, A., Hernanz, M., Heyl, J., Ho, L., Hoormann, J., Horak, J., Huovelin, J., Huppenkothen, D., Iaria, R., Inam Sitki, C., Ingram, A., Israel, G., Izzo, L., Burgess, M., Jackson, M., Ji, L., Jiang, J., Johannsen, T., Jones, C., Jorstad, S., Kajava, J. J. E., Kalamkar, M., Kalemci, E., Kallman, T., Kamble, A., Kislat, F., Kiss, M., Klochkov, D., Koerding, E., Kolehmainen, M., Koljonen, K., Komossa, S., Kong, A., Korpela, S., Kowalinski, M., Krawczynski, H., Kreykenbohm, I., Kuss, M., Lai, D., Lan, M., Larsson, J., Laycock, S., Lazzati, D., Leahy, D., Li, H., Li, J., Li, L. -X., Li, T., Li, Z., Linares, M., Lister, M., Liu, H., Lodato, G., Lohfink, A., Longo, F., Luna, G., Lutovinov, A., Mahmoodifar, S., Maia, J., Mainieri, V., Maitra, C., Maitra, D., Majczyna, A., Maldera, S., Malyshev, D., Manfreda, A., Manousakis, A., Manuel, R., Margutti, R., Marinucci, A., Markoff, S., Marscher, A., Marshall, H., Massaro, F., Mclaughlin, M., Medina-Tanco, G., Mehdipour, M., Middleton, M., Mignani, R., Mimica, P., Mineo, T., Mingo, B., Miniutti, G., Mirac, S. M., Morlino, G., Motlagh, A. V., Motta, S. E., Mushtukov, A., Nagataki, S., Nardini, F., Nattila, J., Navarro, G. J., Negri, B., Negro, M., Nenonen, S., Neustroev, V., Nicastro, F., Norton, A., Nucita, A., O'Brien, P., O'Dell, S., Odaka, H., Olmi, B., Omodei, N., Orienti, M., Orlandini, M., Osborne, J., Pacciani, L., Paliya, V. S., Papadakis, I., Papitto, A., Paragi, Z., Pascal, P., Paul, B., Pavan, L., Pellizzoni, A., Perinati, E., Pesce-Rollins, M., Piconcelli, E., Pili, A. G., Pilia, M., Pohl, M., Ponti, G., Porquet, D., Possenti, A., Postnov, K., Prandoni, I., Produit, N., Puehlhofer, G., Ramsey, B., Razzano, M., Rea, N., Reig, P., Reinsch, K., Reiprich, T., Reynolds, M., Risaliti, G., Roberts, T., Rodriguez, J., Rossi, M. E., Rosswog, S., Rozanska, A., Rubini, A., Rudak, B., Russell, D., Ryde, F., Sabatini, S., Sala, G., Salvati, M., Sasaki, M., Savolainen, T., Saxton, R., Scaringi, S., Schawinski, K., Schulz, N. S., Schwope, A., Severgnini, P., Sharon, M., Shaw, A., Shearer, A., Shesheng, X., Shih, I. -C., Silva, K., Silva, R., Silver, E., Smale, A., Spada, F., Spandre, G., Stamerra, A., Stappers, B., Starrfield, S., Stawarz, L., Stergioulas, N., Stevens, A., Stiele, H., Suleimanov, V., Sunyaev, R., Slowikowska, A., Tamborra, F., Tavecchio, F., Taverna, R., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Tong, H., Torok, G., Torres, D. F., Tortosa, A., Tramacere, A., Trimble, V., Trinchieri, G., Tsygankov, S., Tuerler, M., Turriziani, S., Ursini, F., Uttley, P., Varniere, P., Vincent, F., Vurgun, E., Wang, C., Wang, Z., Watts, A., Wheeler, J. C., Wiersema, K., Wijnands, R., Wilms, J., Wolter, A., Wood, K., Wu, K., Wu, X., Xiangyu, W., Xie, F., Xu, R., Yan, S. -P., Yang, J., Yu, W., Yuan, F., Zajczyk, A., Zanetti, D., Zanin, R., Zanni, C., Zappacosta, L., Zdziarski, A. A., Zech, A., Zhang, H., Zhang, S., Zhang, W., Zoghbi, A., Jan-Willem A. den Herder, Tadayuki Takahashi, Marshall Bautz, Castro-Tirado, A., Weisskopf, M., Lumb, D., Ness, J., Petrucci, P., Pinazo, H., Akbar, A., Atteia, J., Cheung Teddy, C., Gasent-Blesa, J., Gomez, J., Kajava, J., Li, L., Mirac, S., Motlagh, A., Motta, S., Navarro, G., Paliya, V., Pili, A., Rossi, M., Schulz, N., Shih, I., Torres, D., Wheeler, J., Yan, S., and Zdziarski, A.

Subjects
X-ray Astronomy, High-energy astronomy, Polarimetry, X-ray optics, X-ray telescope, Condensed Matter Physic, 01 natural sciences, Observatory, 0103 physical sciences, Electronic, Optical and Magnetic Materials, Spectral resolution, Electrical and Electronic Engineering, 010303 astronomy & astrophysics, Gas Pixel Detector, Physics, X-ray astronomy, ta115, 010308 nuclear & particles physics, Electronic, Optical and Magnetic Material, Applied Mathematics, Vega, Astronomy, Computer Science Applications1707 Computer Vision and Pattern Recognition, Condensed Matter Physics, Computer Science Applications, Applied Mathematic, Electronic, Optical and Magnetic Materials, Computer Vision and Pattern Recognition, X-ray optic
Abstract

XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to X-ray Astronomy. At the time of writing XIPE is in a competitive phase A as fourth medium size mission of ESA (M4). It promises to reopen the polarimetry window in high energy Astrophysics after more than 4 decades thanks to a detector that efficiently exploits the photoelectric effect and to X-ray optics with large effective area. XIPE uniqueness is time-spectrally-spatially- resolved X-ray polarimetry as a breakthrough in high energy astrophysics and fundamental physics. Indeed the payload consists of three Gas Pixel Detectors at the focus of three X-ray optics with a total effective area larger than one XMM mirror but with a low weight. The payload is compatible with the fairing of the Vega launcher. XIPE is designed as an observatory for X-ray astronomers with 75 % of the time dedicated to a Guest Observer competitive program and it is organized as a consortium across Europe with main contributions from Italy, Germany, Spain, United Kingdom, Poland, Sweden.

Published
2016

20. Exploring impulsive solar magnetic energy release and particle acceleration with focused hard X-ray imaging spectroscopy

Author

Christe, Steven, Krucker, S., Glesener, L., Shih, A., Saint-Hilaire, P., Caspi, A., Allred, J., Battaglia, M., Chen, B., Drake, J., Dennis, B., Gary, D., Gburek, S., Goetz, K., Grefenstette, B., Gubarev, M., Hannah, I., Holman, G., Hudson, H., Inglis, A., Ireland, J., Ishikawa, S., Kilmchuk, J., Kontar, E., Kowalski, A., Longcope, D., Massone, A., Musset, S., Piana, M., Ramsey, B., Ryan, D., Schwartz, R., Stęślick, M., Turin, P., Warmuth, A., Wilson-Hodge, C., White, S., Veronig, A., Vilmer, N., and Woods, T.

Subjects
Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics
Abstract

How impulsive magnetic energy release leads to solar eruptions and how those eruptions are energized and evolve are vital unsolved problems in Heliophysics. The standard model for solar eruptions summarizes our current understanding of these events. Magnetic energy in the corona is released through drastic restructuring of the magnetic field via reconnection. Electrons and ions are then accelerated by poorly understood processes. Theories include contracting loops, merging magnetic islands, stochastic acceleration, and turbulence at shocks, among others. Although this basic model is well established, the fundamental physics is poorly understood. HXR observations using grazing-incidence focusing optics can now probe all of the key regions of the standard model. These include two above-the-looptop (ALT) sources which bookend the reconnection region and are likely the sites of particle acceleration and direct heating. The science achievable by a direct HXR imaging instrument can be summarized by the following science questions and objectives which are some of the most outstanding issues in solar physics (1) How are particles accelerated at the Sun? (1a) Where are electrons accelerated and on what time scales? (1b) What fraction of electrons is accelerated out of the ambient medium? (2) How does magnetic energy release on the Sun lead to flares and eruptions? A Focusing Optics X-ray Solar Imager (FOXSI) instrument, which can be built now using proven technology and at modest cost, would enable revolutionary advancements in our understanding of impulsive magnetic energy release and particle acceleration, a process which is known to occur at the Sun but also throughout the Universe.

Published
2017

21. XIPE

Author

Soffitta, P., Bellazzini, R., Bozzo, E., Burwitz, V., Castro-Tirado, A. J., Costa, E., Courvoisier, T., Feng, H., Gburek, S., Goosmann, R., Karas, V., Matt, G., Muleri, F., Nandra, K., Pearce, M., Poutanen, J., Reglero, V., Sabau Maria, D., Santangelo, A., Tagliaferri, G., Tenzer, C., Vink, J., Weisskopf, M. C., Zane, S., Agudo, I., Antonelli, A., Attina, P., Baldini, L., Bykov, A., Carpentiero, R., Cavazzuti, E., Churazov, E., Del Monte, E., De Martino, D., Donnarumma, I., Doroshenko, V., Evangelista, Y., Ferreira, I., Gallo, E., Grosso, N., Kaaret, P., Kuulkers, E., Laranaga, J., Latronico, L., Lumb, D. H., Macian, J., Malzac, J., Marin, F., Massaro, E., Minuti, M., Mundell, C., Ness, J. U., Oosterbroek, T., Paltani, S., Pareschi, G., Perna, R., Petrucci, P. O., Pinazo, H. B., Pinchera, M., Rodriguez, J. P., Roncadelli, M., Santovincenzo, A., Sazonov, S., Sgro, C., Spiga, D., Svoboda, J., Theobald, C., Theodorou, T., Turolla, R., Wilhelmi De Ona, E., Winter, B., Akbar, A. M., Allan, H., Aloisio, R., Altamirano, D., Amati, L., Amato, E., Angelakis, E., Arezu, J., Atteia, J. L., Axelsson, M., Bachetti, M., Ballo, L., Balman, S., Bandiera, R., Barcons, X., Basso, S., Baykal, A., Becker, W., Behar, E., Beheshtipour, B., Belmont, R., Berger, E., Bernardini, F., Bianchi, S., Bisnovatyi-Kogan, G., Blasi, P., Blay, P., Bodaghee, A., Boer, M., Boettcher, M., Bogdanov, S., Bombaci, I., Bonino, R., Braga, J., Brandt, W., Brez, A., Bucciantini, N., Burderi, L., Caiazzo, I., Campana, R., Campana, S., Capitanio, F., Cappi, M., Cardillo, M., Casella, P., Catmabacak, O., Cenko, B., Cerda-Duran, P., Cerruti, C., Chaty, S., Chauvin, M., Chen, Y., Chenevez, J., Chernyakova, M., Cheung Teddy, C. C., Christodoulou, D., Connell, P., Corbet, R., Coti Zelati, F., Covino, S., Cui, W., Cusumano, G., D'Ai, A., D'Ammando, F., Dadina, M., Dai, Z., De Rosa, A., De Ruvo, L., Degenaar, N., Del Santo, M., Del Zanna, L., Dewangan, G., Di Cosimo, S., Di Lalla, N., Di Persio, G., Di Salvo, T., Dias, T., Done, C., Dovciak, M., Doyle, G., Ducci, L., Elsner, R., Enoto, T., Escada, J., Esposito, P., Eyles, C., Fabiani, S., Falanga, M., Falocco, S., Fan, Y., Fender, R., Feroci, M., Ferrigno, C., Forman, W., Foschini, L., Fragile, C., Fuerst, F., Fujita, Y., Gasent-Blesa, J. L., Gelfand, J., Gendre, B., Ghirlanda, G., Ghisellini, G., Giroletti, M., Goetz, D., Gogus, E., Gomez, J. L., Gonzalez, D., Gonzalez-Riestra, R., Gotthelf, E., Gou, L., Grandi, P., Grinberg, V., Grise, F., Guidorzi, C., Gurlebeck, N., Guver, T., Haggard, D., Hardcastle, M., Hartmann, D., Haswell, C., Heger, A., Hernanz, M., Heyl, J., Ho, L., Hoormann, J., Horak, J., Huovelin, J., Huppenkothen, D., Iaria, R., Inam Sitki, C., Ingram, A., Israel, G., Izzo, L., Burgess, M., Jackson, M., Ji, L., Jiang, J., Johannsen, T., Jones, C., Jorstad, S., Kajava, J. J E, Kalamkar, M., Kalemci, E., Kallman, T., Kamble, A., Kislat, F., Kiss, M., Klochkov, D., Koerding, E., Kolehmainen, M., Koljonen, K., Komossa, S., Kong, A., Korpela, S., Kowalinski, M., Krawczynski, H., Kreykenbohm, I., Kuss, M., Lai, D., Lan, M., Larsson, J., Laycock, S., Lazzati, D., Leahy, D., Li, H., Li, J., Li, L. X., Li, T., Li, Z., Linares, M., Lister, M., Liu, H., Lodato, G., Lohfink, A., Longo, F., Luna, G., Lutovinov, A., Mahmoodifar, S., Maia, J., Mainieri, V., Maitra, C., Maitra, D., Majczyna, A., Maldera, S., Malyshev, D., Manfreda, A., Manousakis, A., Manuel, R., Margutti, R., Marinucci, A., Markoff, S., Marscher, A., Marshall, H., Massaro, F., McLaughlin, M., Medina-Tanco, G., Mehdipour, M., Middleton, M., Mignani, R., Mimica, P., Mineo, T., Mingo, B., Miniutti, G., Mirac, S. M., Morlino, G., Motlagh, A. V., Motta, S. E., Mushtukov, A., Nagataki, S., Nardini, F., Nattila, J., Navarro, G. J., Negri, B., Negro, M., Nenonen, S., Neustroev, V., Nicastro, F., Norton, A., Nucita, A., O'Brien, P., O'Dell, S., Odaka, H., Olmi, B., Omodei, N., Orienti, M., Orlandini, M., Osborne, J., Pacciani, L., Paliya, V. S., Papadakis, I., Papitto, A., Paragi, Z., Pascal, P., Paul, B., Pavan, L., Pellizzoni, A., Perinati, E., Pesce-Rollins, M., Piconcelli, E., Pili, A. G., Pilia, M., Pohl, Martin, Ponti, G., Porquet, D., Possenti, A., Postnov, K., Prandoni, I., Produit, N., Puehlhofer, G., Ramsey, B., Razzano, M., Rea, N., Reig, P., Reinsch, K., Reiprich, T., Reynolds, M., Risaliti, G., Roberts, T., Rodriguez, J., Rossi, M. E., Rosswog, S., Rozanska, A., Rubini, A., Rudak, B., Russell, D., Ryde, F., Sabatini, S., Sala, G., Salvati, M., Sasaki, M., Savolainen, T., Saxton, R., Scaringi, S., Schawinski, K., Schulz, N. S., Schwope, A., Severgnini, P., Sharon, M., Shaw, A., Shearer, A., Shesheng, X., Shih, I. C., Silva, K., Silva, R., Silver, E., Smale, A., Spada, F., Spandre, G., Stamerra, A., Stappers, B., Starrfield, S., Stawarz, L., Stergioulas, N., Stevens, A., Stiele, H., Suleimanov, V., Sunyaev, R., Slowikowska, A., Tamborra, F., Tavecchio, F., Taverna, R., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Tong, H., Torok, G., Torres, D. F., Tortosa, A., Tramacere, A., Trimble, V., Trinchieri, G., Tsygankov, S., Tuerler, M., Turriziani, S., Ursini, F., Uttley, P., Varniere, P., Vincent, F., Vurgun, E., Wang, C., Wang, Z., Watts, A., Wheeler, J. C., Wiersema, K., Wijnands, R., Wilms, J., Wolter, A., Wood, K., Wu, K., Wu, X., Xiangyu, W., Xie, F., Xu, R., Yan, S. P., Yang, J., Yu, W., Yuan, F., Zajczyk, A., Zanetti, D., Zanin, R., Zanni, C., Zappacosta, L., Zdziarski, A. A., Zech, A., Zhang, H., Zhang, S., Zhang, W., Zoghbi, A., den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Istituto di Astrofisica e Planetologia Spaziali, University of Pisa, University of Geneva, Max Planck Institute for Extraterrestrial Physics, CSIC, Tsinghua University, Polish Academy of Sciences, Université de Strasbourg, Czech Academy of Sciences, Roma Tre University, KTH Royal Institute of Technology, University of Turku, Universidad de Valencia, Instituto Nacional de Tecnica Aeroespacial, University of Tübingen, INAF—Osservatorio Astronomico di Brera, University of Amsterdam, National Aeronautics and Space Administration, University College London, ASI Science Data Center, Ioffe Institute, Agenzia Spaziale Italiana, Max-Planck-Institut für Astrophysik, INAF Osservatorio Astronomico di Capodimonte, European Space Research and Technology Centre, University of Michigan, Ann Arbor, Michigan State University, INFN, Sezione di Torino, IRAP, Università La Sapienza, INFN Pisa, University of Bath, European Space Astronomy Centre, Stony Brook University, Université Grenoble Alpes, Istituto Nazionale di Fisica Nucleare (INFN), Russian Academy of Sciences, University of Padova, Autonomous University of Barcelona, Effat University, Danmarks Tekniske Universitet, Osservatorio Astrofisico Di Arcetri, Florence, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, Max Planck Institute for Radio Astronomy, Buein Zahra Technical University, Osservatorio Astronomico Cagliari, Middle East Technical University, Universidad de Cantabria, Osservatorio Astronomicodi Roma, Technion-Israel Institute of Technology, Washington University St. Louis, Harvard University, New York University Abu Dhabi, Space Research Institute of the Russian Academy of Sciences, Georgia College, Centre National de la Recherche Scientifique (CNRS), North West University, Columbia University, Sapienza University of Rome, Instituto Nacional de Pesquisas Espaciais, Pennsylvania State University, University of Cagliari, University of British Columbia, INAF/IASF Bologna, INAF, Osservatorio Astronomico di Roma, Sabanci University, Université Paris Diderot, Nanjing University, Dublin City University, Naval Research Laboratory, University of Massachusetts Lowell, University of Maryland, Baltimore, Purdue University, INAF-IASF Palermo, University of Palermo, Inter-University Centre for Astronomy and Astrophysics India, Durham University, Armagh Observatory, NASA Goddard Space Flight Center, Universidade de Coimbra, INAF/IASF Milano, International Space Science Institute, University of Naples Federico II, CAS - Purple Mountain Observatory, University of Oxford, College of Charleston, California Institute of Technology, Osaka University, University of the Virgin Islands, European Space Agency - ESA, Chinese Academy of Sciences, Massachusetts Institute of Technology, University of Bremen, Istanbul University, McGill University, University of Hertfordshire, Clemson University, Open University Milton Keynes, Monash University, University of Helsinki, Cardiff University, CAS - Institute of High Energy Physics, Fudan University, Perimeter Institute for Theoretical Physics, Boston University, Radboud University Nijmegen, National Tsing Hua University, Friedrich-Alexander University Erlangen-Nürnberg, Cornell University, Oregon State University, University of Calgary, Kavli Institute for Astronomy and Astrophysics, XiangTan University, Guangxi University, University of Milano, University of Cambridge, Università Degli Studi di Trieste, Universidad de Buenos Aires, European Southern Observatory, Wheaton College, National Centre for Nuclear Research, Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences, New York University, West Virginia University, Universidad Nacional Autónoma de México, SRON Netherlands Institute for Space Research, University of Leicester, Gran Sasso Science Institute, RIKEN, Keele University, Oxford Instruments Analytical Oy, University of Salento, JAXA Institute of Space and Astronautical Science, University of Florence, Kavli Institute for Particle Astrophysics and Cosmology, University of Crete, Joint Institute for VLBI in Europe, Université Paul Sabatier, Raman Research Institute, Lomonosov Moscow State University, Foundation for Research and Technology - Hellas, University of Göttingen, Argelander-Institut für Astronomie, Leiden University, Stockholm University, Polytechnic University of Catalonia, Metsähovi Radio Observatory, Swiss Federal Institute of Technology Zurich, Leibniz Institut für Astrophysik Potsdam, University of Alberta, University of Southampton, National University of Ireland, Galway, Paris Observatory, INAF—Osservatorio Astrofisico di Torino, University of Manchester, Arizona State University, Jagiellonian University in Kraków, Aristotle University of Thessaloniki, University of Zielona Gora, Istituto Universitario di Studi Superiori di Pavia, University of Maryland, College Park, University of California Berkeley, Silesian University in Opava, University of California Irvine, Università di Roma Tor Vergata, Institut national de physique nucléaire et de physique des particules, Université Pierre and Marie Curie, Tongji University, University of Texas at Austin, Peking University, CAS - Shanghai Astronomical Observatory, Technische Universität Darmstadt, Los Alamos National Laboratory, Aalto-yliopisto, and Aalto University

Subjects
X-ray Astronomy, X-ray optics, Polarimetry, Gas Pixel Detector
Abstract

XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to X-ray Astronomy. At the time of writing XIPE is in a competitive phase A as fourth medium size mission of ESA (M4). It promises to reopen the polarimetry window in high energy Astrophysics after more than 4 decades thanks to a detector that efficiently exploits the photoelectric effect and to X-ray optics with large effective area. XIPE uniqueness is time-spectrally-spatially-resolved X-ray polarimetry as a breakthrough in high energy astrophysics and fundamental physics. Indeed the payload consists of three Gas Pixel Detectors at the focus of three X-ray optics with a total effective area larger than one XMM mirror but with a low weight. The payload is compatible with the fairing of the Vega launcher. XIPE is designed as an observatory for X-ray astronomers with 75 % of the time dedicated to a Guest Observer competitive program and it is organized as a consortium across Europe with main contributions from Italy, Germany, Spain, United Kingdom, Poland, Sweden.

Published
2016

22. The on-board calibration system of the X-ray Imaging Polarimetry Explorer (XIPE)

Author

Zane, S., Winter, B., Theobald, C., Theodorou, T., Pinchera, M., Muleri, F., Spada, F., Sgro, C., Zanetti, D., Feng, H., del Monte, E., Rubini, A., Soffitta, P., Bellazzini, R., Bozzo, E., Burwitz, V., Castro Tirado, A.J., Costa, E., Gburek, S., Goosmann, R., Karas, V., Matt, G., Nandra, K., Pearce, M., Poutanen, J., Reglero, V., Sabau, M.D., Santangelo, A., Tagliaferri, G., Tenzer, C., Vink, J., Weisskopf, M., den Herder, J.-W.A., Takahashi, T., Bautz, M., and Gravitation and Astroparticle Physics Amsterdam

Subjects
Physics, ta115, business.industry, Calibration (statistics), Detector, Polarimetry, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, Astrophysics::Instrumentation and Methods for Astrophysics, Field of view, 02 engineering and technology, Orbital mechanics, 021001 nanoscience & nanotechnology, 01 natural sciences, 010309 optics, Optics, Filter (video), 0103 physical sciences, Modulation (music), Orbit (dynamics), 0210 nano-technology, business, Remote sensing
Abstract

The calibration system for XIPE is aimed at providing a way to check and correct possible variations of performance of the Gas Pixel Detector during the three years of operation in orbit (plus two years of possible extended operation), while facilitating the observation of the celestial sources. This will be performed by using a filter wheel with a large heritage having a set of positions for the calibration and the observation systems. In particular, it will allow for correcting possible gain variation, for measuring the modulation factor using a polarized source, for removing non interesting bright sources in the field of view and for observing very bright celestial sources. The on-board calibration system is composed of three filter wheels, one for each detector and it is expected to operate for a small number of times during the year. Moreover, since it operates once at a time, within the observation mode, it allows for simultaneous calibration and acquisition from celestial sources on different detectors. In this paper we present the scope and the requirements of the on-board calibration system, its design, and a description of its possible use in space.

Published
2016
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23. XIPE: the X-ray imaging polarimetry explorer

Author

Soffitta, P., Barcons, X., Bellazzini, R., Braga, J., Costa, E., Fraser, G., Gburek, S., Huovelin, J., Matt, G., Pearce, M., Poutanen, J., Reglero, V., Santangelo, A., Sunyaev, R., Tagliaferri, G., Weisskopf, M., Aloisio, R., Amato, E., Attiná, P., Axelsson, M., Baldini, L., Basso, S., Bianchi, S., Blasi, P., Bregeon, J., Brez, A., Bucciantini, N., Burderi, L., Burwitz, V., Casella, P., Churazov, E., Civitani, M., Covino, S., Curado da Silva, R., Cusumano, G., Dadina, M., D'Amico, F., Rosa, A., Cosimo, S., Persio, G., Salvo, T., Dovciak, M., Elsner, R., Eyles, C., Fabian, A., Fabiani, S., Feng, H., Giarrusso, S., Goosmann, R., Grandi, P., Grosso, N., Israel, G., Jackson, M., Kaaret, P., Karas, V., Kuss, M., Lai, D., Rosa, G., Larsson, J., Larsson, S., Latronico, L., Maggio, A., Maia, J., Marin, F., Massai, M., Mineo, T., Minuti, M., Moretti, E., Muleri, F., O'Dell, S., Pareschi, G., Peres, G., Pesce, M., Petrucci, P., Pinchera, M., Porquet, D., Ramsey, B., Rea, N., Reale, F., Rodrigo, J., Rózanska, A., Rubini, A., Rudawy, P., Ryde, F., Salvati, M., de Santiago, V., Sazonov, S., Sgró, C., Silver, E., Spandre, G., Spiga, D., Stella, L., Tamagawa, T., Tamborra, F., Tavecchio, F., Dias, T., Adelsberg, M., Wu, K., Zane, S., DI SALVO, T., Soffitta, P, Barcons, X, Bellazzini, R, Braga, J, Costa, E, Fraser, Gw, Gburek, S, Huovelin, J, Matt, Giorgio, Pearce, M, Poutanen, J, Reglero, V, Santangelo, A, Sunyaev, Ra, Tagliaferri, G, Weisskopf, M, Aloisio, R, Amato, E, Attina, P, Axelsson, M, Baldini, L, Basso, S, Bianchi, Stefano, Blasi, P, Bregeon, J, Brez, A, Bucciantini, N, Burderi, L, Burwitz, V, Casella, P, Churazov, E, Civitani, M, Covino, S, da Silva, Rmc, Cusumano, G, Dadina, M, D'Amico, F, De Rosa, A, Di Cosimo, S, Di Persio, G, Di Salvo, T, Dovciak, M, Elsner, R, Eyles, Cj, Fabian, Ac, Fabiani, S, Feng, H, Giarrusso, S, Goosmann, Rw, Grandi, P, Grosso, N, Israel, G, Jackson, M, Kaaret, P, Karas, V, Kuss, M, Lai, D, La Rosa, G, Larsson, J, Larsson, S, Latronico, L, Maggio, A, Maia, J, Marin, F, Massai, Mm, Mineo, T, Minuti, M, Moretti, E, Muleri, F, O'Dell, Sl, Pareschi, G, Peres, G, Pesce, M, Petrucci, Po, Pinchera, M, Porquet, D, Ramsey, B, Rea, N, Reale, F, Rodrigo, Jm, Rozanska, A, Rubini, A, Rudawy, P, Ryde, F, Salvati, M, de Santiago, Va, Sazonov, S, Sgro, C, Silver, E, Spandre, G, Spiga, D, Stella, L, Tamagawa, T, Tamborra, F, Tavecchio, F, Dias, Tt, van Adelsberg, M, Wu, K, Zane, S., INAF-IASF/Rome, Istituto Nazionale di Astrofisica (INAF), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Istituto Nazionale di Fisica Nucleare, Fraser, G, Matt, G, Sunyaev, R, Attiná, P, Bianchi, S, Curado da Silva, R, Rosa, A, Cosimo, S, Persio, G, Salvo, T, Eyles, C, Fabian, A, Goosmann, R, Rosa, G, Massai, M, O'Dell, S, Petrucci, P, Rodrigo, J, Rózanska, A, de Santiago, V, Sgró, C, Dias, T, Adelsberg, M, Zane, S, DI SALVO, T, PERES, G, and REALE, F

Subjects
Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, FOS: Physical sciences, Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, X-ray, Settore FIS/05 - Astronomia E Astrofisica, law, 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astronomy, X-ray, Polarimetry, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar flare, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], White dwarf, Astronomy and Astrophysics, Torus, Magnetic reconnection, Polarization (waves), Neutron star, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Flare
Abstract

arXiv:1309.6995v1.-- et al., X-ray polarimetry, sometimes alone, and sometimes coupled to spectral and temporal variability measurements and to imaging, allows a wealth of physical phenomena in astrophysics to be studied. X-ray polarimetry investigates the acceleration process, for example, including those typical of magnetic reconnection in solar flares, but also emission in the strong magnetic fields of neutron stars and white dwarfs. It detects scattering in asymmetric structures such as accretion disks and columns, and in the so-called molecular torus and ionization cones. In addition, it allows fundamental physics in regimes of gravity and of magnetic field intensity not accessible to experiments on the Earth to be probed. Finally, models that describe fundamental interactions (e.g. quantum gravity and the extension of the Standard Model) can be tested. We describe in this paper the X-ray Imaging Polarimetry Explorer (XIPE), proposed in June 2012 to the first ESA call for a small mission with a launch in 2017. The proposal was, unfortunately, not selected. To be compliant with this schedule, we designed the payload mostly with existing items. The XIPE proposal takes advantage of the completed phase A of POLARIX for an ASI small mission program that was cancelled, but is different in many aspects: the detectors, the presence of a solar flare polarimeter and photometer and the use of a light platform derived by a mass production for a cluster of satellites. XIPE is composed of two out of the three existing JET-X telescopes with two Gas Pixel Detectors (GPD) filled with a He-DME mixture at their focus. Two additional GPDs filled with a 3-bar Ar-DME mixture always face the Sun to detect polarization from solar flares. The Minimum Detectable Polarization of a 1 mCrab source reaches 14 % in the 2-10 keV band in 105 s for pointed observations, and 0.6 % for an X10 class solar flare in the 15-35 keV energy band. The imaging capability is 24 arcsec Half Energy Width (HEW) in a Field of View of 14.7 arcmin × 14.7 arcmin. The spectral resolution is 20 % at 6 keV and the time resolution is 8 μs. The imaging capabilities of the JET-X optics and of the GPD have been demonstrated by a recent calibration campaign at PANTER X-ray test facility of the Max-Planck-Institut für extraterrestrische Physik (MPE, Germany). XIPE takes advantage of a low-earth equatorial orbit with Malindi as down-link station and of a Mission Operation Center (MOC) at INPE (Brazil). The data policy is organized with a Core Program that comprises three months of Science Verification Phase and 25 % of net observing time in the following 2 years. A competitive Guest Observer program covers the remaining 75 % of the net observing time. © 2013 Springer Science+Business Media Dordrecht., This work is partially funded by ASI, INAF and INFN.

Published
2013
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27. SphinX MEASUREMENTS OF THE 2009 SOLAR MINIMUM X-RAY EMISSION

Author

Sylwester, J., primary, Kowalinski, M., additional, Gburek, S., additional, Siarkowski, M., additional, Kuzin, S., additional, Farnik, F., additional, Reale, F., additional, Phillips, K. J. H., additional, Bakała, J., additional, Gryciuk, M., additional, Podgorski, P., additional, and Sylwester, B., additional

Published
2012
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28. Calibration of the SphinX experiment at the XACT facility in Palermo

Author

Collura, A., primary, Barbera, M., additional, Varisco, S., additional, Calderone, G., additional, Reale, F., additional, Gburek, S., additional, Kowalinski, M., additional, Sylwester, J., additional, Siarkowski, M., additional, Bakala, J., additional, Podgorski, P., additional, Trzebinski, W., additional, Plocieniak, S., additional, and Kordylewski, Z., additional

Published
2008
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36. XIPE: the x-ray imaging polarimetry explorer

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Soffitta, P., Bellazzini, R., Bozzo, E., Burwitz, V., Castro-Tirado, A., Costa, E., Courvoisier, T., Feng, H., Gburek, S., Goosmann, R., Karas, V., Matt, G., Muleri, F., Nandra, K., Pearce, M., Poutanen, J., Reglero, V., Sabau Maria, D., Santangelo, A., Tagliaferri, G., Tenzer, C., Vink, J., Weisskopf, M. C., Zane, S., Agudo, I., Antonelli, A., Attina, P., Baldini, L., Bykov, A., Carpentiero, R., Cavazzuti, E., Churazov, E., Del Monte, E., De Martino, D., Donnarumma, I., Doroshenko, V., Evangelista, Y., Ferreira, I., Gallo, E., Grosso, N., Kaaret, P., Kuulkers, E., Laranaga, J., Latronico, L., Lumb, D. H., Macian, J., Malzac, J., Marin, F., Massaro, E., Minuti, M., Mundell, C., Ness, J. U., Oosterbroek, T., Paltani, S., Pareschi, G., Perna, R., Petrucci, P.-O., Pinazo, H. B., Pinchera, M., Rodriguez, J. P., Roncadelli, M., Santovincenzo, A., Sazonov, S., Sgro, C., Spiga, D., Svoboda, J., Theobald, C., Theodorou, T., Turolla, R., Wilhelmi de Ona, E., Winter, B., Akbar, A. M., Allan, H., Aloisio, R., Altamirano, D., Amati, L., Amato, E., Angelakis, E., Arezu, J., Atteia, J.-L., Axelsson, M., Bachetti, M., Ballo, L., Balman, S., Bandiera, R., Barcons, X., Basso, S., Baykal, A., Becker, W., Behar, E., Beheshtipour, B., Belmont, R., Berger, E., Bernardini, F., Bianchi, S., Bisnovatyi-Kogan, G., Blasi, P., Blay, P., Bodaghee, A., Boer, M., Boettcher, M., Bogdanov, S., Bombaci, I., Bonino, R., Braga, J., Brandt, W., Brez, A., Bucciantini, N., Burderi, L., Caiazzo, I., and Campana, R.

Published
2016
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37. ADAHELI+: Exploring the fast, dynamic Sun in the X-ray, optical, and near-infrared

Author

BERRILLI, FRANCESCO, SOFFITTA, PAOLO, VELLI, MARCO, Sabatini, Paolo, Bigazzi, Alberto, Bellazzini, Ronaldo, Bellot Rubio, Luis Ramon, Brez, Alessandro, CARBONE, VINCENZO, CAUZZI, Gianna, CAVALLINI, Fabio, CONSOLINI, Giuseppe, Curti, Fabio, DEL MORO, DARIO, DI GIORGIO, Anna Maria, ERMOLLI, Ilaria, FABIANI, Sergio, Faurobert, Marianne, Feller, Alex, Galsgaard, Klaus, Gburek, Szymon, Giannattasio, Fabio, GIOVANNELLI, LUCA, Hirzberger, Johann, Jefferies, Stuart M., Madjarska, Maria S., Manni, Fabio, Mazzoni, Alessandro, MULERI, FABIO, Penza, Valentina, Peres, Giovanni, PIAZZESI, ROBERTO, Pieralli, Francesca, PIETROPAOLO, ERMANNO, Martinez Pillet, Valentin, Pinchera, Michele, Reale, Fabio, ROMANO, Paolo, Romoli, Andrea, ROMOLI, MARCO, RUBINI, ALDA, Rudawy, Pawel, Sandri, Paolo, Scardigli, Stefano, Spandre, Gloria, Solanki, Sami K., STANGALINI, MARCO, Vecchio, Antonio, Zuccarello, Francesca, Berrilli, F., Soffitta, P., Velli, M., Sabatini, P., Bigazzi, A., Bellazzini, R., Bellot Rubio, L., Brez, A., Carbone, V., Cauzzi, G., Cavallini, F., Consolini, G., Curti, F., Del Moro, D., Di Giorgio, A., Ermolli, I., Fabiani, S., Faurobert, M., Feller, A., Galsgaard, K., Gburek, S., Giannattasio, F., Giovannelli, L., Hirzberger, J., Jefferies, S., Madjarska, M., Manni, F., Mazzoni, A., Muleri, F., Penza, V., Peres, G., Piazzesi, R., Pieralli, F., Pietropaolo, E., Pillet, V., Pinchera, M., Reale, F., Romano, P., Romoli, A., Romoli, M., Rubini, A., Rudawy, P., Sandri, P., Scardigli, S., Spandre, G., Solanki, S., Stangalini, M., Vecchio, A., Zuccarello, F., ITA, USA, DEU, ESP, KOR, DNK, and POL

Subjects
Mechanical Engineering, Sun, Astronomy and Astrophysics, Fabry-Pérot, infrared spectroscopy, polarimetry, satellites, X-rays, Control and Systems Engineering, Electronic, Optical and Magnetic Materials, Instrumentation, Space and Planetary Science, Fabry-Pérot, Settore FIS/05 - Astronomia E Astrofisica, Electronic, Optical and Magnetic Materials, Settore FIS/06 - Fisica per il Sistema Terra e Il Mezzo Circumterrestre
Abstract

Advanced Astronomy for Heliophysics Plus (ADAHELI+) is a project concept for a small solar and space weather mission with a budget compatible with an European Space Agency (ESA) S-class mission, including launch, and a fast development cycle. ADAHELI+ was submitted to the European Space Agency by a European-wide consortium of solar physics research institutes in response to the "Call for a small mission opportunity for a launch in 2017," of March 9, 2012. The ADAHELI+ project builds on the heritage of the former ADAHELI mission, which had successfully completed its phase-A study under the Italian Space Agency 2007 Small Mission Programme, thus proving the soundness and feasibility of its innovative low-budget design. ADAHELI+ is a solar space mission with two main instruments: ISODY+: an imager, based on Fabry-Perot interferometers, whose design is optimized to the acquisition of highest cadence, long-duration, multiline spectropolarimetric images in the visible/near-infrared region of the solar spectrum. XSPO: an x-ray polarimeter for solar flares in x-rays with energies in the 15 to 35 keV range. ADAHELI+ is capable of performing observations that cannot be addressed by other currently planned solar space missions, due to their limited telemetry, or by ground-based facilities, due to the problematic effect of the terrestrial atmosphere. (C) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

Published
2015

38. SphinX: The Solar Photometer in X-Rays

Author

František Fárník, Z. Kordylewski, Sergey Kuzin, Szymon Gburek, W. Trzebiński, Fabio Reale, Marek Siarkowski, S. Płocieniak, Kenneth J. H. Phillips, Jaroslaw Bakala, Piotr Podgorski, Yurij D. Kotov, Janusz Sylwester, A. A. Pertsov, Barbara Sylwester, Miroslaw Kowalinski, Gburek, S, Sylwester, J, Kowalinski, M, Bakala, J, Kordylewski, Z, Podgorski, P, Plocieniak, S, Siarkowski, M, Sylwester, B, Trzebinski, W, Kuzin, S V, Pertsov, A A, Kotov, Y D, Farnik, F, Reale, F, and Phillips, K J H

Subjects
Physics, Sphinx, 010504 meteorology & atmospheric sciences, Astronomy, Astronomy and Astrophysics, Photometer, 01 natural sciences, law.invention, Telescope, Settore FIS/05 - Astronomia E Astrofisica, Space and Planetary Science, law, 0103 physical sciences, Satellite, Instrument design, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Solar corona, Solar instrumentation, X-rays
Abstract

Solar Photometer in X-rays (SphinX) was a spectrophotometer developed to observe the Sun in soft X-rays. The instrument observed in the energy range ≈ 1 – 15 keV with resolution ≈ 0.4 keV. SphinX was flown on the Russian CORONAS–PHOTON satellite placed inside the TESIS EUV and X telescope assembly. The spacecraft launch took place on 30 January 2009 at 13:30 UT at the Plesetsk Cosmodrome in Russia. The SphinX experiment mission began a couple of weeks later on 20 February 2009 when the first telemetry dumps were received. The mission ended nine months later on 29 November 2009 when data transmission was terminated. SphinX provided an excellent set of observations during very low solar activity. This was indeed the period in which solar activity dropped to the lowest level observed in X-rays ever. The SphinX instrument design, construction, and operation principle are described. Information on SphinX data repositories, dissemination methods, format, and calibration is given together with general recommendations for data users. Scientific research areas in which SphinX data find application are reviewed.

Published
2013

39. Sphinx measurements of the 2009 solar minimum x-ray emission

Author

Sergey Kuzin, Kjh Phillips, Jaroslaw Bakala, Barbara Sylwester, Miroslaw Kowalinski, Janusz Sylwester, M. Gryciuk, Fabio Reale, Piotr Podgorski, Szymon Gburek, František Fárník, Marek Siarkowski, Sylwester, J, Kowalinski, M, Gburek, S, Siarkowski, M, Kuzin, S, Farnik, F, Reale, F, Phillips, K J H, Bakala, J, Gryciuk, M, Podgorski, P, and Sylwester, B

Subjects
Solar minimum, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Luminosity, Telescope, Settore FIS/05 - Astronomia E Astrofisica, law, 0103 physical sciences, ROSAT, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, Range (particle radiation), Spacecraft, 010308 nuclear & particles physics, business.industry, X-ray, Astronomy and Astrophysics, activity, Sun: corona, Sun: X-rays, gamma rays [Sun], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Sun: activity, Sun: corona, Sun: X-rays, gamma rays, business
Abstract

The SphinX X-ray spectrophotometer on the CORONAS-PHOTON spacecraft measured soft X-ray emission in the 1-15 keV energy range during the deep solar minimum of 2009 with a sensitivity much greater than GOES. Several intervals are identified when the X-ray flux was exceptionally low, and the flux and solar X-ray luminosity are estimated. Spectral fits to the emission at these times give temperatures of 1.7-1.9 MK and emission measures between 4 x 10^47 cm^-3 and 1.1 x 10^48 cm^-3. Comparing SphinX emission with that from the Hinode X-ray Telescope, we deduce that most of the emission is from general coronal structures rather than confined features like bright points. For one of 27 intervals of exceptionally low activity identified in the SphinX data, the Sun's X-ray luminosity in an energy range roughly extrapolated to that of ROSAT (0.1-2.4 keV) was less than most nearby K and M dwarfs., Astrophysical Journal, in press. 14 pp, 3 figures

Published
2012

40. Calibration of the SphinX experiment at the XACT facility in Palermo

Author

Fabio Reale, W. Trzebiński, Szymon Gburek, Janusz Sylwester, S. Płocieniak, G. Calderone, Marek Siarkowski, Piotr Podgorski, Jaroslaw Bakala, Z. Kordylewski, Marco Barbera, Alfonso Collura, Miroslaw Kowalinski, Salvatore Varisco, Collura, A., Barbera, M., Varisco, S., Calderone, G., Reale, F., Gburek, S., Kowalinski, M., Sylwester, J., Siarkowski, M., Bakala, J., Podgorski, P., Trzebinski, W., Plocieniak, S., and Kordylewski, Z.

Subjects
X-ray, Physics, Settore FIS/05 - Astronomia E Astrofisica, Sphinx, Optics, Observatory, Calibration (statistics), business.industry, solar corona, Detector, Astronomy, business
Abstract

Three of the four detectors of the SphinX experiment to be flown on the Russian mission Coronas-Photon have been measured at the XACT Facility of the Palermo Observatory at several wavelengths in the soft X-ray band. We describe the instrumental set-up and report some measurements. The analysis work to obtain the final calibration is still in progress.

Published
2008
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41. A Segmental 2D Readout Board Manufactured in Printed Circuit Board Technology for Gas Electron Multiplier Detectors.

Author

Babij M, Bielówka P, Gburek S, and Malecha K

Abstract

The Gas Electron Multiplier (GEM) was introduced by Fabio Sauli in 1997. This technology is broadly used in current and planned High-Energy Physics (HEP) experiments. One of the key components of these detectors is a readout board, which collects charges amplified by GEM foils and transfers them to readout electronics. The commonly used Cartesian XY readout boards are manufactured from the same type of polyamide film used to produce the GEM foils. The manufacturing process utilizes a deep polyimide etching, similar to the Micro Chemical Vias (MCV) etching process, which is protected by patent. The material prepared in this way is glued onto a rigid substrate and mounted in a detector. The production process was developed at CERN, and the technology has been commercialized to a small extent. Consequently, only a few research centers have the ability to make dedicated readout strips readouts. GEM detectors are characterized by a segmented structure that allows the separation of an electron-multiplying structure from a readout. This feature enables the implementation of a new type of charge reading system without the need to interfere with the GEM foil system. A new approach is proposed to simplify production and reduce the costs of GEM detector readout boards. It is based on the concept of segmental readout structures that are manufactured in standard Printed Circuit Board (PCB) technology. The interconnectors and mountings are located on the back of the bottom, so it is possible to place the readout electronics behind the readout plate. The boards are designed in such a way that they can be panelized into a readout with a more extensive active area. The margin between PCBs is minimalized to approximately 200 µm, which is less than 1% of the 70 × 70 mm 2 board area, so the active area is as big as possible. Therefore, this solution gives us the ability to further increase the size of a readout by adding additional segments, which reduces the cost of scaling up the detector size. A few research groups have suggested similar solutions that utilize PCB technology, but currently, only detectors with 1D zigzag readouts have been validated and used. The measurement results of other 2D (XY) redouts using PCB technology have not been presented. The measurements shown and discussed in this paper validated the proposed technology. X-ray radiographs were obtained, validating the ability to use this technology to manufacture readout boards for GEM detectors. In opposition to state-of-the-art readouts, the proposed solution can be manufactured by any PCB manufacturer without using MCV-patented technology. This gives the users flexibility in designing and ordering low-cost custom readouts.

Published
2023
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43. Chromosomal anomalies in stage D1 prostate adenocarcinoma primary tumors and lymph node metastases detected by fluorescence in situ hybridization.

Author

Gburek BM, Kollmorgen TA, Qian J, D'Souza-Gburek SM, Lieber MM, and Jenkins RB

Subjects
Adenocarcinoma pathology, Adenocarcinoma secondary, Humans, Lymphatic Metastasis, Male, Neoplasm Staging, Ploidies, Prostatic Neoplasms pathology, Adenocarcinoma genetics, Chromosome Aberrations, Chromosome Disorders, In Situ Hybridization, Fluorescence, Prostatic Neoplasms genetics
Abstract

Purpose: We determined if characteristic chromosomal anomalies exist within the primary tumors and lymph node metastases in patients with stage D1 prostate cancer, and compared the patterns of chromosomal alterations between primary tumors and nodal metastases., Materials and Methods: Fluorescence in situ hybridization analysis using peri-centromeric probes for chromosomes 6, 7, 8, 17, X and Y was performed on 5 mu. sections from paraffin embedded tissue blocks obtained from 23 consecutive patients who underwent radical prostatectomy and bilateral pelvic lymphadenectomy in 1990 for stage D1 prostate cancer., Results: The dominant focus of primary tumor was compared to matched nodal metastases in 12 cases. Five of 12 primary tumor foci (41.7%) had similar chromosomal gains and the same fluorescence in situ hybridization ploidy result as the corresponding nodal metastases. Chromosomes 7 and X (73.2% of cases) were most frequently gained in the primary tumors, and chromosomes X and Y (81.2% of cases) were most frequently gained in the metastases. No primary tumor or metastasis demonstrated chromosomal loss. Three of 19 primary tumors (15.7%) were diploid, while 16 of 19 (84.3%) were nondiploid. Chromosomal aneusomy was inversely correlated with increasing Gleason summary score., Conclusions: These data indicate that the dominant primary tumor foci may not give rise to nodal metastases, gains of chromosomes 7, X and Y may be associated with metastatic behavior, and patients with stage D1 disease have a greater rate of aneuploidy than those with lower stage cancer.

Published
1997

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