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1. Nanostructured 3C-SiC on Si by a network of (111) platelets: a fully textured film generated by intrinsic growth anisotropy

Author

G. M. Vanacore, D. Chrastina, E. Scalise, L. Barbisan, A. Ballabio, M. Mauceri, F. La Via, G. Capitani, D. Crippa, A. Marzegalli, R. Bergamaschini, L. Miglio, Vanacore, G, Chrastina, D, Scalise, E, Barbisan, L, Ballabio, A, Mauceri, M, La Via, F, Capitani, G, Crippa, D, Marzegalli, A, Bergamaschini, R, and Miglio, L

Subjects
General Physics and Astronomy, Chemical vapor deposition, Defects, nanosheet, Physical and Theoretical Chemistry, 3C-SiC
Abstract

In this paper, we address the unique nature of fully textured, high surface-to-volume 3C-SiC films, as produced by intrinsic growth anisotropy, in turn generated by the high velocity of the stacking fault growth front in two-dimensional (111) platelets. Structural interpretation of high resolution scanning electron microscopy and transmission electron microscopy data is carried out for samples grown in a hot-wall low-pressure chemical vapour deposition reactor with trichlorosilane and ethylene precursors, under suitable deposition conditions. By correlating the morphology and the X-ray diffraction analysis we also point out that twinning along (111) planes is very frequent in such materials, which changes the free-platelet configuration.

Published
2022

2. The Instrument of the Imaging X-ray Polarimetry Explorer

Author

Leonardo Lucchesi, S. Nenonen, Alessandro Brez, Simonetta Puccetti, Luca Latronico, Hans Andersson, Mattia Barbanera, Ciro Caporale, Leonardo Orsini, Luca Baldini, Michele Pinchera, Alessandro Profeti, Federico Mosti, Alessandro Di Marco, M. Perri, M. Ceccanti, Ettore Del Monte, Ajay Ratheesh, Claudia Cardelli, Elisa D'Alba, Antonino Tobia, Paolo Lorenzi, Niccolò Di Lalla, Maura Pilia, Elio Mangraviti, Rita Carpentiero, E. Scalise, Barbara Negri, Daniele Brienza, Matteo Bachetti, Alfredo Morbidini, Carlo Magazzu, Toru Tamagawa, Alessio Trois, Carmelo Sgrò, Fei Xie, Pasqualino Loffredo, Giuseppe Di Persio, Melissa Pesce-Rollins, Sergio Di Cosimo, S. Castellano, John Rankin, Massimo Minuti, Primo Attinà, Riccardo Ferrazzoli, Marco Castronuovo, Marco Marengo, Francesco Santoli, Luca Cavalli, Saverio Citraro, Takao Kitaguchi, Fabrizio Amici, Paolo Mereu, Toshio Nakano, I. Donnarumma, Y. Evangelista, Paolo Soffitta, Mauro Centrone, Alberto Manfreda, Asami Hayato, Fabio D'Amico, E. Cavazzuti, Ronaldo Bellazzini, Gloria Spandre, Enrico Costa, Stefano Ciprini, Raffaele Piazzolla, Giorgio Matt, Fabio La Monaca, Alda Rubini, Marcello Tardiola, Alessio Nuti, Marco Vimercati, Sergio Fabiani, Fabio Borotto, S. Maldera, Andrea Sciortino, Carlo Lefevre, Fabio Muleri, Paolo Sarra, Hikmat Nasimi, Soffitta, P., Baldini, L., Bellazzini, R., Costa, E., Latronico, L., Muleri, F., Del Monte, E., Fabiani, S., Minuti, M., Pinchera, M., Sgro', C., Spandre, G., Trois, A., Amici, F., Andersson, H., Attina', P., Bachetti, M., Barbanera, M., Borotto, F., Brez, A., Brienza, D., Caporale, C., Cardelli, C., Carpentiero, R., Castellano, S., Castronuovo, M., Cavalli, L., Cavazzuti, E., Ceccanti, M., Centrone, M., Ciprini, S., Citraro, S., D'Amico, F., D'Alba, E., Di Cosimo, S., Di Lalla, N., Di Marco, A., Di Persio, G., Donnarumma, I., Evangelista, Y., Ferrazzoli, R., Hayato, A., Kitaguchi, T., La Monaca, F., Lefevre, C., Loffredo, P., Lorenzi, P., Lucchesi, L., Magazzu, C., Maldera, S., Manfreda, A., Mangraviti, E., Marengo, M., Matt, G., Mereu, P., Morbidini, A., Mosti, F., Nakano, T., Nasimi, H., Negri, B., Nenonen, S., Nuti, A., Orsini, L., Perri, M., Pesce-Rollins, M., Piazzolla, R., Pilia, M., Profeti, A., Puccetti, S., Rankin, J., Ratheesh, A., Rubini, A., Santoli, F., Sarra, P., Scalise, E., Sciortino, A., Tamagawa, T., Tardiola, M., Tobia, A., Vimercati, M., and Xie, F.

Subjects
Physics, X-ray astronomy, business.industry, Astrophysics::High Energy Astrophysical Phenomena, X-ray, Polarimetry, X-ray detector, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Optics, Space and Planetary Science, X-ray, Polarimetry — Instrumentation, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

While X-ray Spectroscopy, Timing and Imaging have improved verymuch since 1962, when the first astronomical non-solar source was discovered, especially with the launch of Newton/X-ray Multi-Mirror Mission, Rossi/X-ray Timing Explorer and Chandra/Advanced X-ray Astrophysics Facility, the progress of X-ray polarimetry has been meager. This is in part due to the lack of sensitive polarization detectors, in part due to the fate of approved missions and in part because the celestial X-ray sources appeared less polarized than expected. Only one positive measurement has been available until now. Indeed the eight Orbiting Solar Observatory measured the polarization of the Crab nebula in the 70s. The advent of techniques of microelectronics allowed for designing a detector based on the photoelectric effect in gas in an energy range where the optics are efficient in focusing X-rays. Herewe describe the Instrument, which is the major contribution of the Italian collaboration to the SmallExplorer mission called IXPE, the Imaging X-ray Polarimetry Explorer, which will be flown in late 2021. The instrument, is composed of three Detector Units, based on this technique, and a Detector Service Unit. Three Mirror Modules provided by Marshall Space Flight Center focus X-rays onto the detectors. In the following we will show the technological choices, their scientific motivation and the results from the calibration of the Instrument. IXPE will perform imaging, timing and energy resolved polarimetry in the 2-8 keV energy band opening this window of X-ray astronomy to tens of celestial sources of almost all classes., 25 pages, 12 figures, 5 tables (accepted for publication in Astronomical Journal)

Published
2021

3. IXPE DU-FM ions-UV filters characterization

Author

Francesco Santoli, Sergio Fabiani, Riccardo Ferrazzoli, Y. Evangelista, Pasqualino Loffredo, John Rankin, Fabio La Monaca, Fabrizio Amici, Alessandro Di Marco, Fabio Muleri, Raffaele Piazzolla, Sergio Di Cosimo, Paolo Soffitta, Ben Zeiger, Alessio Trois, Carlo Lefevre, Ajay Ratheesh, Primo Attina, Alfredo Morbidini, E. Scalise, Alda Rubini, Fei Xie, Enrico Costa, Daniele Brienza, Giuseppe Di Persio, Antonino Tobia, ITA, and USA

Subjects
Physics, X-Ray polarimetry, business.industry, Detector, X-ray, Polarimetry, Polarimeter, Collimator, law.invention, Optics, Filter (video), law, GPD, Calibration, X-Ray, IXPE, Monochromatic color, business, IXPE, X-Ray, X-Ray polarimetry, ions-UV filter, GPD, ions-UV filter
Abstract

IXPE (Imaging X-ray Polarimetry Explorer) is a NASA SMEX in a partnership with ASI. The focal plane Detector Units (DUs) and the Detector Service Unit (DSU) were developed by the Italian research Institutes INAF-IAPS and INFN and were manufactured by OHB-I. IXPE will investigate X-ray polarimetry in the 2-8 keV energy band. The payload comprises three identical telescopes, each composed of a mirror and a detector unit with an X-ray polarimeter based on the Gas Pixel Detector (GPD). A stray-light collimator (SLC) is mounted on the top of the DU to shield the GPD from background X-rays not coming from the optics. At the bottom of the SLC, an ions-UV filter is mounted to reduce the thermal load and to prevent ions and UV from entering the DU. The ions-UV filters consist mainly of 1 um LUXFilm (based on polyimide). During on-ground calibration activities of the IXPE DUs, X-ray transparency of DU-FM ions-UV filters was measured with monochromatic X-ray at 2.7 keV and 6.4 keV at INAF-IAPS.

Published
2021

4. Design, construction, and test of the Gas Pixel Detectors for the IXPE mission

Author

Carlo Magazzu, E. Del Monte, Paolo Sarra, Alessandro Brez, Alessandra Marrocchesi, Elisa D'Alba, A. Rubini, Rita Carpentiero, Takao Kitaguchi, Luca Cavalli, Guido Magazzu, John Rankin, Alfredo Morbidini, S. Nenonen, E. Cavazzuti, Fabio Borotto, C. Oppedisano, Marco Marengo, Gloria Spandre, Federico Mosti, Francesco Zanetti, Primo Attina, Sergio Fabiani, E. Scalise, Barbara Negri, Michele Pinchera, Francesco Santoli, Simonetta Puccetti, Ciro Caporale, F. La Monaca, Saverio Citraro, R. Bonino, Fabrizio Amici, Fei Xie, F. Muleri, Paolo Lorenzi, Luca Latronico, Leonardo Orsini, Marcello Tardiola, Antonino Tobia, Matteo Bachetti, Mauro Centrone, Allyn F. Tennant, Alessandro Profeti, Claudia Cardelli, Alberto Manfreda, S. Di Cosimo, P. Soffitta, Daniele Brienza, Raffaele Piazzolla, Wayne H. Baumgartner, S. Maldera, Andrea Sciortino, M. Perri, Carlo Lefevre, Ajay Ratheesh, Steve O'Dell, N. Di Lalla, Luca Baldini, Maura Pilia, Elio Mangraviti, Marco Castronuovo, Alessio Trois, Fabio D'Amico, Alessio Nuti, Paolo Mereu, A. Di Marco, K. Uchiyama, Leonardo Lucchesi, D. Zanetti, Giorgio Matt, Enrico Costa, Martin C. Weisskopf, Y. Zhou, Toshio Nakano, Marco Vimercati, S. Pieraccini, Ronaldo Bellazzini, R. Ferrazzoli, T. Meilahti, Toru Tamagawa, Pasqualino Loffredo, Massimo Minuti, G. Di Persio, Melissa Pesce-Rollins, Carmelo Sgrò, S. Castellano, Hikmat Nasimi, Hans Andersson, Brian D. Ramsey, I. Donnarumma, Y. Evangelista, M. Ceccanti, M. Barbanera, Baldini, L., Barbanera, M., Bellazzini, R., Bonino, R., Borotto, F., Brez, A., Caporale, C., Cardelli, C., Castellano, S., Ceccanti, M., Citraro, S., Di Lalla, N., Latronico, L., Lucchesi, L., Magazzu, C., Magazzu, G., Maldera, S., Manfreda, A., Marengo, M., Marrocchesi, A., Mereu, P., Minuti, M., Mosti, F., Nasimi, H., Nuti, A., Oppedisano, C., Orsini, L., Pesce-Rollins, M., Pinchera, M., Profeti, A., Sgro, C., Spandre, G., Tardiola, M., Zanetti, D., Amici, F., Andersson, H., Attina, P., Bachetti, M., Baumgartner, W., Brienza, D., Carpentiero, R., Castronuovo, M., Cavalli, L., Cavazzuti, E., Centrone, M., Costa, E., D'Alba, E., D'Amico, F., Del Monte, E., Di Cosimo, S., Di Marco, A., Di Persio, G., Donnarumma, I., Evangelista, Y., Fabiani, S., Ferrazzoli, R., Kitaguchi, T., La Monaca, F., Lefevre, C., Loffredo, P., Lorenzi, P., Mangraviti, E., Matt, G., Meilahti, T., Morbidini, A., Muleri, F., Nakano, T., Negri, B., Nenonen, S., O'Dell, S. L., Perri, M., Piazzolla, R., Pieraccini, S., Pilia, M., Puccetti, S., Ramsey, B. D., Rankin, J., Ratheesh, A., Rubini, A., Santoli, F., Sarra, P., Scalise, E., Sciortino, A., Soffitta, P., Tamagawa, T., Tennant, A. F., Tobia, A., Trois, A., Uchiyama, K., Vimercati, M., Weisskopf, M. C., Xie, F., Zanetti, F., and Zhou, Y.

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics - Instrumentation and Detectors, Pixel, Emphasis (telecommunications), Detector, Gas detectors, X-ray polarimetry, Polarimetry, FOS: Physical sciences, Astronomy and Astrophysics, Instrumentation and Detectors (physics.ins-det), Dead time, X-ray polarimetry Gas detectors, Noise (electronics), Cardinal point, Application-specific integrated circuit, Gas detector, Electronic engineering, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Due to be launched in late 2021, the Imaging X-Ray Polarimetry Explorer (IXPE) is a NASA Small Explorer mission designed to perform polarization measurements in the 2-8 keV band, complemented with imaging, spectroscopy and timing capabilities. At the heart of the focal plane is a set of three polarization-sensitive Gas Pixel Detectors (GPD), each based on a custom ASIC acting as a charge-collecting anode. In this paper we shall review the design, manufacturing, and test of the IXPE focal-plane detectors, with particular emphasis on the connection between the science drivers, the performance metrics and the operational aspects. We shall present a thorough characterization of the GPDs in terms of effective noise, trigger efficiency, dead time, uniformity of response, and spectral and polarimetric performance. In addition, we shall discuss in detail a number of instrumental effects that are relevant for high-level science analysis -- particularly as far as the response to unpolarized radiation and the stability in time are concerned., Comment: To be published in Astroparticle Physics

Published
2021

5. The IXPE Instrument Calibration Equipment

Author

Maura Pilia, Pasqualino Loffredo, Alessio Trois, Paolo Soffitta, Ettore Del Monte, Y. Evangelista, Carlo Lefevre, Alessandro Di Marco, Sergio Di Cosimo, Alfredo Morbidini, Matteo Bachetti, Sergio Fabiani, Enrico Costa, Alda Rubini, Primo Attina, E. Scalise, Antonino Tobia, Fabrizio Amici, Francesco Santoli, M. Perri, Fei Xie, Fabio Muleri, Mauro Centrone, Giuseppe Di Persio, Simonetta Puccetti, Ajay Ratheesh, R. Ferrazzoli, John Rankin, Daniele Brienza, Raffaele Piazzolla, and Fabio La Monaca

Subjects
Physics, Physics - Instrumentation and Detectors, Payload, Detector, Polarimetry, Astrophysics::Instrumentation and Methods for Astrophysics, X-rays Polarimetry Calibration Space missions, FOS: Physical sciences, Astronomy and Astrophysics, Instrumentation and Detectors (physics.ins-det), Polarization (waves), Space exploration, Cardinal point, Calibration, Sensitivity (control systems), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Remote sensing
Abstract

The Imaging X-ray Polarimetry Explorer is a mission dedicated to the measurement of X-ray polarization from tens of astrophysical sources belonging to different classes. Expected to be launched at the end of 2021, the payload comprises three mirrors and three focal plane imaging polarimeters, the latter being designed and built in Italy. While calibration is always an essential phase in the development of high-energy space missions, for IXPE it has been particularly extensive both to calibrate the response to polarization, which is peculiar to IXPE, and to achieve a statistical uncertainty below the expected sensitivity. In this paper we present the calibration equipment that was designed and built at INAF-IAPS in Rome, Italy, for the calibration of the polarization-sensitive focal plane detectors on-board IXPE. Equipment includes calibration sources, both polarized and unpolarized, stages to align and move the beam, test detectors and their mechanical assembly. While all these equipments were designed to fit the specific needs of the IXPE Instrument calibration, their versatility could also be used in the future for other projects., Comment: 17 pages, 25 figures

Published
2021
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7. Study of the γ-ray source 1AGL J2022+4032 in the Cygnus region

Author

F. Longo, Elsa Beatriz Giacani, G. Piano, Arnaud Ferrari, A. Zambra, F. D'Ammando, C. Pittori, M. Feroci, M. Fiorini, P. Picozza, M. Rapisarda, G. De Paris, Gloria Mabel Dubner, A. Pellizzoni, E. Costa, E. Del Monte, G. Pucella, V. Vittorini, F. Perotti, A. Trois, M. Trifoglio, A. Morselli, M. Tavani, E. Vallazza, F. Gianotti, P. A. Caraveo, A. Argan, M. Pilia, A. Giuliani, Francesco Lucarelli, P. Soffitta, Andrea Bulgarelli, F. Lazzarotto, F. Fuschino, S. Vercellone, P. Lipari, P. Santolamazza, A. Rappoldi, E. Scalise, E. Striani, M. Giusti, L. Pacciani, P. W. Cattaneo, A. W. Chen, L. A. Antonelli, M. Galli, F. Verrecchia, M. Prest, S. Sabatini, P. Giommi, E. Moretti, Claudio Labanti, L. Salotti, D. Zanello, G. Di Cocco, Sandro Mereghetti, I. Donnarumma, Y. Evangelista, S. Colafrancesco, Martino Marisaldi, G. Barbiellini, A. W., Chen, G., Piano, M., Tavani, A., Troi, G., Dubner, E., Giacani, A., Argan, G., Barbiellini, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, E., Costa, F., D'Ammando, Paris, G., Monte, E., Cocco, G., I., Donnarumma, Y., Evangelista, M., Feroci, A., Ferrari, M., Fiorini, F., Fuschino, M., Galli, F., Gianotti, A., Giuliani, M., Giusti, C., Labanti, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, S., Mereghetti, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, P., Picozza, M., Pilia, M., Prest, G., Pucella, M., Rapisarda, A., Rappoldi, S., Sabatini, E., Scalise, P., Soffitta, E., Striani, M., Trifoglio, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, D., Zanello, C., Pittori, P., Giommi, F., Verrecchia, F., Lucarelli, P., Santolamazza, S., Colafrancesco, L. A., Antonelli, L., Salotti, Chen AW, Piano G, Tavani M, Trois A, Dubner G, Giacani E, Argan A, Barbiellini G, Bulgarelli A, Caraveo P, Cattaneo PW, Costa E, DAmmando F, De Paris G, Del Monte E, Di Cocco G, Donnarumma I, Evangelista Y, Feroci M, Ferrari A, Fiorini M, Fuschino F, Galli M, Gianotti F, Giuliani A, Giusti M, Labanti C, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mereghetti S, Moretti E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Picozza P, Pilia M, Prest M, Pucella G, Rapisarda M, Rappoldi A, Sabatini S, Scalise E, Soffitta P, Striani E, Trifoglio M, Vallazza E, Vercellone S, Vittorini V, Zambra A, Zanello D, Pittori C, Giommi P, Verrecchia F, Lucarelli F, Santolamazza P, Colafrancesco S, Antonelli LA, and Salotti L

Subjects
pulsars: individual: 1FGL J2021.5+4026, Astrophysics::High Energy Astrophysical Phenomena, Ciencias Físicas, pulsars: individual: 1AGL J2022+4032, gamma rays: stars, pulsars: individual: LAT PSR J2021+4026, pulsars: individual: 3EG J2020+4017, individual: LAT PSR J2021+4026 [pulsars], Flux, FOS: Physical sciences, Astrophysics, star [gamma rays], law.invention, Telescope, purl.org/becyt/ford/1 [https], Pulsar, law, Blazar, Supernova remnant, individual: 1FGL J2021.5+4026 [pulsars], Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gamma ray, Astronomy and Astrophysics, individual: 3EG J2020+4017 [pulsars], purl.org/becyt/ford/1.3 [https], Light curve, stars [gamma rays], Astronomía, gamma ray, Space and Planetary Science, AGILE satellite, galactic source, supernova remnant Gamma Cygni, individual: 1AGL J2022+4032 [pulsars], pulsars: individual: 1AGL J2022+4032 / gamma rays: stars / pulsars: individual: 1FGL J2021.5+4026 / pulsars: individual: LAT PSR J2021+4026 / pulsars: individual: 3EG J2020+4017, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Fermi Gamma-ray Space Telescope
Abstract

Identification of gamma-ray-emitting Galactic sources is a long-standing problem in astrophysics. One such source, 1AGL J2022+4032, coincident with the interior of the radio shell of the supernova remnant Gamma Cygni (SNR G78.2+2.1) in the Cygnus Region, has recently been identified by Fermi as a gamma-ray pulsar, LAT PSR J2021+4026. We present long-term observations of 1AGL J2022+4032 with the AGILE gamma-ray telescope, measuring its flux and light curve. We compare the light curve of 1AGL J2022+4032 with that of 1AGL J2021+3652 (PSR J2021+3651), showing that the flux variability of 1AGL J2022+4032 appears to be greater than the level predicted from statistical and systematic effects and producing detailed simulations to estimate the probability of the apparent observed variability. We evaluate the possibility that the gamma-ray emission may be due to the superposition of two or more point sources, some of which may be variable, considering a number of possible counterparts. We consider the possibility of a nearby X-ray quiet microquasar contributing to the flux of 1AGL J2022+4032 to be more likely than the hypotheses of a background blazar or intrinsic gamma-ray variabilty of LAT PSR J2021+4026., 7 pages, 7 figures, accepted for publication in Astronomy & Astrophysics

Published
2010

8. Direct Evidence for Hadronic Cosmic-Ray Acceleration in the Supernova Renmant IC 443

Author

C. Pittori, Marco Feroci, F. Fuschino, Luigi Pacciani, Paolo Soffitta, G. De Paris, A. Giuliani, E. Scalise, Filippo D'Ammando, V. Cocco, M. Mastropietro, E. Del Monte, V. Vittorini, Arnaud Ferrari, Paolo Lipari, M. Trifoglio, Y. Evangelista, S. Vercellone, F. Perotti, Francesco Lazzarotto, P. Santolamazza, A. Zambra, A. Pellizzoni, G. Di Cocco, E. Striani, I. Lapshov, Fulvio Gianotti, I. Donnarumma, Martino Marisaldi, L. Salotti, Elena Moretti, Alda Rubini, P. W. Cattaneo, A. Rappoldi, A. W. Chen, P. Picozza, P. Giommi, Massimo Rapisarda, G. Pucella, F. Longo, D. Zanello, A. Argan, Andrea Bulgarelli, T. Contessi, Enrico Costa, Claudio Labanti, L. A. Antonelli, G. Piano, P. A. Caraveo, M. Galli, F. Verrecchia, Sandro Mereghetti, A. Morselli, S. Colafrancesco, M. Prest, Alessio Trois, M. Pilia, Marco Tavani, S. Sabatini, Ennio Morelli, G. Barbiellini, E. Vallazza, M., Tavani, A., Giuliani, A. W., Chen, A., Argan, G., Barbiellini, A., Bulgarelli, P., Caraveo, P. W., Cattaneo, V., Cocco, T., Contessi, F., D'Ammando, E., Costa, G. D., Pari, E. D., Monte, G. D., Cocco, I., Donnarumma, Y., Evangelista, A., Ferrari, M., Feroci, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, M., Mastropietro, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, G., Pucella, M., Prest, M., Rapisarda, A., Rappoldi, E., Scalise, A., Rubini, S., Sabatini, E., Striani, P., Soffitta, M., Trifoglio, A., Troi, E., Vallazza, S., Vercellone, V., Vittorini, A., Zambra, D., Zanello, C., Pittori, F., Verrecchia, P., Santolamazza, P., Giommi, S., Colafrancesco, L. A., Antonelli, L., Salotti, Tavani M, Giuliani A, Chen AW, Argan A, Barbiellini G, Bulgarelli A, Caraveo P, Cattaneo PW, Cocco V, Contessi T, DAmmando F, Costa E, De Paris G, Del Monte E, Di Cocco G, Donnarumma I, Evangelista Y, Ferrari A, Feroci M, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mastropietro M, Mereghetti S, Morelli E, Moretti E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Pucella G, Prest M, Rapisarda M, Rappoldi A, Scalise E, Rubini A, Sabatini S, Striani E, Soffitta P, Trifoglio M, Trois A, Vallazza E, Vercellone S, Vittorini V, Zambra A, Zanello D, Pittori C, Verrecchia F, Santolamazza P, Giommi P, Colafrancesco S, Antonelli LA, and Salotti L

Subjects
Agile, Photon, Supernova Remnants, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Cosmic ray, Electron, Astrophysics, High Energy Gamma-ray Astronomy, gamma ray production, supernova, Supernova remnant, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Molecular cloud, AGILE satellite, Gamma ray, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Supernova, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, cosmic rays – gamma rays: general – ISM: supernova remnants – supernovae: general – supernovae: individual (IC 443)
Abstract

The Supernova Remnant (SNR) IC 443 is an intermediate-age remnant well known for its radio, optical, X-ray and gamma-ray energy emissions. In this Letter we study the gamma-ray emission above 100 MeV from IC 443 as obtained by the AGILE satellite. A distinct pattern of diffuse emission in the energy range 100 MeV-3 GeV is detected across the SNR with its prominent maximum (source "A") localized in the Northeastern shell with a flux F = (47 \pm 10) 10^{-8} photons cm^{-2} s^{-1} above 100 MeV. This location is the site of the strongest shock interaction between the SNR blast wave and the dense circumstellar medium. Source "A" is not coincident with the TeV source located 0.4 degree away and associated with a dense molecular cloud complex in the SNR central region. From our observations, and from the lack of detectable diffuse TeV emission from its Northeastern rim, we demonstrate that electrons cannot be the main emitters of gamma-rays in the range 0.1-10 GeV at the site of the strongest SNR shock. The intensity, spectral characteristics, and location of the most prominent gamma-ray emission together with the absence of co-spatial detectable TeV emission are consistent only with a hadronic model of cosmic-ray acceleration in the SNR. A high-density molecular cloud (cloud "E") provides a remarkable "target" for nucleonic interactions of accelerated hadrons: our results show enhanced gamma-ray production near the molecular cloud/shocked shell interaction site. IC 443 provides the first unambiguous evidence of cosmic-ray acceleration by SNRs., Comment: 5 pages, 2 figures; accepted by ApJLetters on Jan 21, 2010

Published
2010
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9. The Extraordinary Gamma-Ray Flare Of The Blazar 3c 454.3

Author

E. Striani, S. Vercellone, M. Tavani, V. Vittorini, F. D’Ammando, I. Donnarumma, L. Pacciani, G. Pucella, A. Bulgarelli, M. Trifoglio, F. Gianotti, P. Giommi, A. Argan, G. Barbiellini, P. Caraveo, P. W. Cattaneo, A. W. Chen, E. Costa, G. De Paris, E. Del Monte, G. Di Cocco, Y. Evangelista, M. Feroci, A. Ferrari, M. Fiorini, F. Fuschino, M. Galli, A. Giuliani, M. Giusti, C. Labanti, F. Lazzarotto, P. Lipari, F. Longo, M. Marisaldi, S. Mereghetti, E. Morelli, E. Moretti, A. Morselli, A. Pellizzoni, F. Perotti, G. Piano, P. Picozza, M. Pilia, M. Prest, M. Rapisarda, A. Rappoldi, S. Sabatini, E. Scalise, P. Soffitta, A. Trois, E. Vallazza, A. Zambra, D. Zanello, C. Pittori, F. Verrecchia, P. Santolamazza, F. Lucarelli, S. Colafrancesco, L. A. Antonelli, L. Salotti, E., Striani, S., Vercellone, M., Tavani, V., Vittorini, F., D'Ammando, I., Donnarumma, L., Pacciani, G., Pucella, A., Bulgarelli, M., Trifoglio, F., Gianotti, P., Giommi, A., Argan, G., Barbiellini, P., Caraveo, P. W., Cattaneo, A. W., Chen, E., Costa, G. D., Pari, E. D., Monte, G. D., Cocco, Y., Evangelista, M., Feroci, A., Ferrari, M., Fiorini, F., Fuschino, M., Galli, A., Giuliani, M., Giusti, C., Labanti, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, M., Prest, M., Rapisarda, A., Rappoldi, S., Sabatini, E., Scalise, P., Soffitta, A., Troi, E., Vallazza, A., Zambra, D., Zanello, C., Pittori, F., Verrecchia, P., Santolamazza, F., Lucarelli, S., Colafrancesco, L. A., Antonelli, L., Salotti, Striani E, Vercellone S, Tavani M, Vittorini V, DAmmando F, Donnarumma I, Pacciani L, Pucella G, Bulgarelli A, Trifoglio M, Gianotti F, Giommi P, Argan A, Barbiellini G, Caraveo P, Cattaneo PW, Chen AW, Costa E, De Paris G, Del Monte E, Di Cocco G, Evangelista Y, Feroci M, Ferrari A, Fiorini M, Fuschino F, Galli M, Giuliani A, Giusti M, Labanti C, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mereghetti S, Morelli E, Moretti E, Morselli A, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Prest M, Rapisarda M, Rappoldi A, Sabatini S, Scalise E, Soffitta P, Trois A, Vallazza E, Zambra A, Zanello D, Pittori C, Verrecchia F, Santolamazza P, Lucarelli F, Colafrancesco S, Antonelli LA, and Salotti L

Subjects
Agile, Cosmology and Nongalactic Astrophysics (astro-ph.CO), blazar, gamma detection, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Astrophysics, Type (model theory), Vela, High Energy Gamma-ray Astronomy, AGILE satellite, Active Galactic Nuclei, law.invention, Pulsar, law, Blazar, Physics, gamma rays: galaxies – quasars: individual (3C 454.3), Gamma ray, Astronomy and Astrophysics, Quasar, Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics, Flare
Abstract

We present the gamma-ray data of the extraordinary flaring activity above 100 MeV from the flat spectrum radio quasar 3C 454.3 detected by AGILE during the month of December 2009. 3C 454.3, that has been among the most active blazars of the FSRQ type since 2007, was detected in the gamma-ray range with a progressively rising flux since November 10, 2009. The gamma-ray flux reached a value comparable with that of the Vela pulsar on December 2, 2009. Remarkably, between December 2 and 3, 2009 the source more than doubled its gamma-ray emission and became the brightest gamma-ray source in the sky with a peak flux of F_{\gamma,p} = (2000 \pm 400) x 10^-8 ph cm^-2 s^-1 for a 1-day integration above 100 MeV. The gamma-ray intensity decreased in the following days with the source flux remaining at large values near F \simeq (1000 \pm 200) x 10^-8 ph cm^-2 s^-1 for more than a week. This exceptional gamma-ray flare dissipated among the largest ever detected intrinsic radiated power in gamma-rays above 100 MeV (L_{\gamma, source, peak} \simeq 3 x 10^46 erg s^-1, for a relativistic Doppler factor of {\delta} \simeq 30). The total isotropic irradiated energy of the month-long episode in the range 100 MeV - 3 GeV is E_{\gamma,iso} \simeq 10^56 erg. We report the intensity and spectral evolution of the gamma-ray emission across the flaring episode. We briefly discuss the important theoretical implications of our detection., Comment: 17 pages, 3 figures, ApJ accepted

Published
2010

10. Episodic Transient Gamma-Ray Emission From The Microquasar Cygnus X-1

Author

E. Moretti, V. Vittorini, Claudio Labanti, A. Giuliani, M. Trifoglio, C. Pittori, Francesco Lazzarotto, Paolo Lipari, Martino Marisaldi, Attilio Ferrari, Guido Barbiellini, P. Santolamazza, A. Pellizzoni, F. Perotti, S. Vercellone, M. Galli, Piergiorgio Picozza, E. Striani, Y. Evangelista, M. Giusti, Francesco Longo, Alda Rubini, F. Verrecchia, Ennio Morelli, Paolo Giommi, G. De Paris, Massimiliano Fiorini, Marco Tavani, F. Fuschino, G. Di Cocco, A. Rappoldi, E. Vallazza, S. Sabatini, Sergio Colafrancesco, Fulvio Gianotti, A. Argan, Sandro Mereghetti, P. W. Cattaneo, Andrea Bulgarelli, A. Morselli, I. Donnarumma, Enrico Costa, Filippo D'Ammando, Marco Feroci, Luigi Pacciani, M. Prest, Paolo Soffitta, L. A. Antonelli, A. W. Chen, E. Del Monte, Massimo Rapisarda, G. Piano, P. A. Caraveo, Maura Pilia, D. Zanello, G. Pucella, Alessio Trois, E. Scalise, L. Salotti, A. Zambra, F. de Pasquale, Sabatini S, Tavani M, Striani E, Bulgarelli A, Vittorini V, Piano G, Del Monte E, Feroci M, de Pasquale F, Trifoglio M, Gianotti F, Argan A, Barbiellini G, Caraveo P, Cattaneo PW, Chen AW, DAmmando F, Costa E, De Paris G, Di Cocco G, Donnarumma I, Evangelista Y, Ferrari A, Fiorini M, Fuschino F, Galli M, Giuliani A, Giusti M, Labanti C, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mereghetti S, Morelli E, Moretti E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Picozza P, Pilia M, Pucella G, Prest M, Rapisarda M, Rappoldi A, Rubini A, Scalise E, Soffitta P, Trois A, Vallazza E, Vercellone S, Zambra A, Zanello D, Pittori C, Verrecchia F, Santolamazza P, Giommi P, Colafrancesco S, Antonelli LA, Salotti L, S., Sabatini, M., Tavani, E., Striani, A., Bulgarelli, V., Vittorini, G., Piano, E. D., Monte, M., Feroci, F. d., Pasquale, M., Trifoglio, F., Gianotti, A., Argan, G., Barbiellini, P., Caraveo, P. W., Cattaneo, A. W., Chen, F., D'Ammando, E., Costa, G. D., Pari, G. D., Cocco, I., Donnarumma, Y., Evangelista, A., Ferrari, M., Fiorini, F., Fuschino, M., Galli, A., Giuliani, M., Giusti, C., Labanti, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, P., Picozza, M., Pilia, G., Pucella, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, E., Scalise, P., Soffitta, A., Troi, E., Vallazza, S., Vercellone, A., Zambra, D., Zanello, C., Pittori, F., Verrecchia, P., Santolamazza, P., Giommi, S., Colafrancesco, L. A., Antonelli, and L., Salotti

Subjects
Agile, Black Holes, transient gamma-ray emission, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astrophysics, High Energy Gamma-ray Astronomy, X-rays: binaries, Cutoff, Cygnus X-1, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Range (particle radiation), Gamma ray, Astronomy and Astrophysics, gamma rays: general, stars: individual (Cygnus X-1), Galaxy, Black hole, Space and Planetary Science, AGILE satellite, Transient (oscillation), Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing)
Abstract

Cygnus X-1 is the archetypal black hole (BH) binary system in our Galaxy. We report the main results of an extensive search for transient gamma-ray emission from Cygnus X-1 carried out in the energy range 100 MeV - 3 GeV by the AGILE satellite, during the period 2007 July - 2009 October. The total exposure time is about 300 days, during which the source was in the "hard" X-ray spectral state. We divided the observing intervals in 2 or 4 week periods, and searched for transient and persistent emission. We report an episode of significant transient gamma-ray emission detected on 2009, October 16 in a position compatible with Cygnus X-1 optical position. This episode, occurred during a hard spectral state of Cygnus X-1, shows that a 1-2 day time variable emission above 100 MeV can be produced during hard spectral states, having important theoretical implications for current Comptonization models for Cygnus X-1 and other microquasars. Except for this one short timescale episode, no significant gamma-ray emission was detected by AGILE. By integrating all available data we obtain a 2$\sigma$ upper limit for the total integrated flux of $F_{\gamma,U.L.} = 3 \times 10^{-8} \rm ph cm^{-2} s^{-1}$ in the energy range 100 MeV - 3 GeV. We then clearly establish the existence of a spectral cutoff in the energy range 1-100 MeV that applies to the typical hard state outside the flaring period and that confirms the historically known spectral cutoff above 1 MeV., Comment: Accepted for publication by ApJ on the 9th of Feb 2010, 5 pages, 3 figures

Published
2010

11. Extreme particle acceleration in the microquasar Cygnus X-3

Author

Francesco Longo, Martino Marisaldi, C. Pittori, Paolo Lipari, Arnaud Ferrari, M. Prest, Sandro Mereghetti, P. W. Cattaneo, S. Sabatini, A. Pellizzoni, E. Striani, I. Lapshov, F. Perotti, S. Colafrancesco, Fulvio Gianotti, Francesco Lazzarotto, A. Giuliani, E. Rossi, Ennio Morelli, Karri I. I. Koljonen, Marco Tavani, E. Scalise, Y. Evangelista, Maura Pilia, Guy G. Pooley, M. Galli, F. Fuschino, Alessio Trois, I. Donnarumma, Massimo Rapisarda, F. Verrecchia, N. A. Nizhelskij, P. A. Caraveo, E. Del Monte, D. Zanello, L. Salotti, V. Cocco, M. Trifoglio, G. Pucella, A. Mauri, A. Rappoldi, E. Vallazza, G. De Paris, T. Contessi, G. Piano, A. W. Chen, P. Giommi, A. Argan, Andrea Bulgarelli, Enrico Costa, G. Di Persio, A. Morselli, Filippo D'Ammando, Paolo Soffitta, S. Vercellone, Michael L. McCollough, P. Picozza, P. Santolamazza, Alda Rubini, Sergei A. Trushkin, A. Zambra, M. Mastropietro, Guido Barbiellini, V. Vittorini, Marco Feroci, Luigi Pacciani, Angelo Antonelli, E. Mattaini, G. Di Cocco, Claudio Labanti, M., Tavani, A., Bulgarelli, G., Piano, S., Sabatini, E., Striani, Y., Evangelista, A., Troi, G., Pooley, S., Trushkin, N. A., Nizhelskij, M., Mccollough, K. I. I., Koljonen, G., Pucella, A., Giuliani, A. W., Chen, E., Costa, V., Vittorini, M., Trifoglio, F., Gianotti, A., Argan, G., Barbiellini, P., Caraveo, P. W., Cattaneo, V., Cocco, T., Contessi, F., D'Ammando, E. D., Monte, G. D., Pari, G. D., Cocco, G. D., Persio, I., Donnarumma, M., Feroci, A., Ferrari, F., Fuschino, M., Galli, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, E., Mattaini, M., Marisaldi, M., Mastropietro, A., Mauri, S., Mereghetti, E., Morelli, A., Morselli, L., Pacciani, A., Pellizzoni, F., Perotti, P., Picozza, M., Pilia, M., Prest, M., Rapisarda, A., Rappoldi, E., Rossi, A., Rubini, E., Scalise, P., Soffitta, E., Vallazza, S., Vercellone, A., Zambra, D., Zanello, C., Pittori, F., Verrecchia, P., Giommi, S., Colafrancesco, P., Santolamazza, A., Antonelli, L., Salotti, Tavani M, Bulgarelli A, Piano G, Sabatini S, Striani E, Evangelista Y, Trois A, Pooley G, Trushkin S, Nizhelskij NA, McCollough M, Koljonen KII, Pucella G, Giuliani A, Chen AW, Costa E, Vittorini V, Trifoglio M, Gianotti F, Argan A, Barbiellini G, Caraveo P, Cattaneo PW, Cocco V, Contessi T, DAmmando F, Del Monte E, De Paris G, Di Cocco G, Di Persio G, Donnarumma I, Feroci M, Ferrari A, Fuschino F, Galli M, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Mattaini E, Marisaldi M, Mastropietro M, Mauri A, Mereghetti S, Morelli E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Picozza P, Pilia M, Prest M, Rapisarda M, Rappoldi A, Rossi E, Rubini A, Scalise E, Soffitta P, Vallazza E, Vercellone S, Zambra A, Zanello D, Pittori C, Verrecchia F, Giommi P, Colafrancesco S, Santolamazza P, Antonelli A, and Salotti L

Subjects
Active galactic nucleus, Black Holes, Astrophysics::High Energy Astrophysical Phenomena, super massive black holes, X-ray binary, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, High Energy Gamma-ray Astronomy, Relativistic particle, AGILE, Astrophysical jet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Supermassive black hole, Cygnus, Multidisciplinary, particle acceleration, microquasar, Cygnus X-3, Astronomy, X-ray emission, Particle acceleration, Black hole, Neutron star, AGILE satellite
Abstract

Galactic microquasars are binaries with a neutron star or stellar-mass black hole accreting gas from a companion star. They can accelerate particles to relativistic energies and emit radio flares, but the mechanism of jet energization is not known. A survey of the Cygnus region between mid-2007 and mid-2009 has detected four major γ-ray flaring episodes with energies over 100 MeV, each lasting 1 or 2 days, emanating from the microquasar Cygnus X-3. There is a clear pattern of temporal correlation between the γ-ray flares and transitional spectral states of radio and X-ray emission. Particle acceleration occurred a few days before radio jet ejections for two of the flares, suggesting that jet formation involves the production of highly energetic particles. Super-massive black holes in active galaxies can accelerate particles to relativistic energies, producing jets with associated γ-ray emission. Galactic 'microquasars' also produce relativistic jets; however, apart from an isolated event detected in Cygnus X-1, there has hitherto been no systematic evidence for the acceleration of particles to gigaelectronvolt or higher energies in a microquasar. Here, a report of four γ-ray flares with energies above 100 MeV from the microquasar Cygnus X-3 illuminates this important problem. Super-massive black holes in active galaxies can accelerate particles to relativistic energies1, producing jets with associated γ-ray emission. Galactic ‘microquasars’, which are binary systems consisting of a neutron star or stellar-mass black hole accreting gas from a companion star, also produce relativistic jets, generally together with radio flares2. Apart from an isolated event detected3 in Cygnus X-1, there has hitherto been no systematic evidence for the acceleration of particles to gigaelectronvolt or higher energies in a microquasar, with the consequence that we are as yet unsure about the mechanism of jet energization. Here we report four γ-ray flares with energies above 100 MeV from the microquasar Cygnus X-3 (an exceptional X-ray binary4,5,6 that sporadically produces radio jets7,8,9). There is a clear pattern of temporal correlations between the γ-ray flares and transitional spectral states of the radio-frequency and X-ray emission. Particle acceleration occurred a few days before radio-jet ejections for two of the four flares, meaning that the process of jet formation implies the production of very energetic particles. In Cygnus X-3, particle energies during the flares can be thousands of times higher than during quiescent states.

Published
2009

12. First AGILE catalog of high-confidence gamma-ray sources

Author

Dario Gasparrini, I. Donnarumma, F. Mauri, E. Scalise, E. Mattaini, G. Di Cocco, E. Del Monte, E. Rossi, Geiland Porrovecchio, Fulvio Gianotti, F. Fornari, A. Morselli, G. De Paris, Marco Feroci, Luigi Pacciani, G. Di Persio, S. Cutini, A. W. Chen, Sandro Mereghetti, F. Boffelli, P. W. Cattaneo, S. Stellato, Francesco Longo, Massimo Rapisarda, R. Primavera, A. Antonelli, Filippo D'Ammando, M. Galli, Piergiorgio Picozza, F. Tamburelli, C. Pittori, L. Salotti, Paolo Soffitta, F. Verrecchia, A. Zambra, T. Froysland, B. Preger, P. Santolamazza, D. Zanello, V. Vittorini, G. Fanari, F. Fuschino, F. Perotti, Martino Marisaldi, A. Pellizzoni, Marcello Mastropietro, Francesco Lazzarotto, M. Trifoglio, A. Argan, Massimo Frutti, Andrea Bulgarelli, Maura Pilia, P. A. Caraveo, Enrico Costa, Alessio Trois, F. Liello, Claudio Labanti, Alda Rubini, E. Striani, Marco Tavani, S. Vercellone, S. Sabatini, Sergio Colafrancesco, I. Lapshov, Paolo Giommi, Ennio Morelli, M. Prest, Massimiliano Fiorini, P. Lipari, Attilio Ferrari, Guido Barbiellini, Elena Moretti, G. Pucella, A. Mauri, A. Rappoldi, E. Vallazza, Alessandro Traci, V. Cocco, A. Giuliani, Y. Evangelista, T. Contessi, G. Piano, C. Pontoni, C., Pittori, F., Verrecchia, A. W., Chen, A., Bulgarelli, A., Pellizzoni, A., Giuliani, S., Vercellone, Longo, Francesco, M., Tavani, P., Giommi, G., Barbiellini, M., Trifoglio, F., Gianotti, A., Argan, A., Antonelli, F., Boffelli, P., Caraveo, P. W., Cattaneo, V., Cocco, S., Colafrancesco, T., Contessi, E., Costa, S., Cutini, F., D'Ammando, E. D., Monte, G. D., Pari, G. D., Cocco, G. D., Persio, I., Donnarumma, Y., Evangelista, G., Fanari, M., Feroci, A., Ferrari, M., Fiorini, F., Fornari, F., Fuschino, T., Froysland, M., Frutti, M., Galli, D., Gasparrini, C., Labanti, I., Lapshov, F., Lazzarotto, F., Liello, P., Lipari, E., Mattaini, M., Marisaldi, M., Mastropietro, A., Mauri, F., Mauri, S., Mereghetti, E., Morelli, Moretti, Elena, A., Morselli, L., Pacciani, F., Perotti, G., Piano, P., Picozza, M., Pilia, C., Pontoni, G., Porrovecchio, B., Preger, M., Prest, R., Primavera, G., Pucella, M., Rapisarda, A., Rappoldi, E., Rossi, A., Rubini, S., Sabatini, P., Santolamazza, E., Scalise, P., Soffitta, S., Stellato, E., Striani, F., Tamburelli, A., Traci, A., Troi, E., Vallazza, V., Vittorini, A., Zambra, D., Zanello, L., Salotti, Pittori C, Verrecchia F, Chen AW, Bulgarelli A, Pellizzoni A, Giuliani A, Vercellone S, Longo F, Tavani M, Giommi P, Barbiellini G, Trifoglio M, Gianotti F, Argan A, Antonelli A, Boffelli F, Caraveo P, Cattaneo PW, Cocco V, Colafrancesco S, Contessi T, Costa E, Cutini S, DAmmando F, Del Monte E, De Paris G, Di Cocco G, Di Persio G, Donnarumma I, Evangelista Y, Fanari G, Feroci M, Ferrari A, Fiorini M, Fornari F, Fuschino F, Froysland T, Frutti M, Galli M, Gasparrini D, Labanti C, Lapshov I, Lazzarotto F, Liello F, Lipari P, Mattaini E, Marisaldi M, Mastropietro M, Mauri A, Mauri F, Mereghetti S, Morelli E, Moretti E, Morselli A, Pacciani L, Perotti F, Piano G, Picozza P, Pilia M, Pontoni C, Porrovecchio G, Preger B, Prest M, Primavera R, Pucella G, Rapisarda M, Rappoldi A, Rossi E, Rubini A, Sabatini S, Santolamazza P, Scalise E, Soffitta P, Stellato S, Striani E, Tamburelli F, Traci A, Trois A, Vallazza E, Vittorini V, Zambra A, Zanello D, and Salotti L

Subjects
Agile, catalog, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Field of view, Astrophysics, gamma-ray source, High Energy Gamma-ray Astronomy, Pulsar, X and gamma detection, Blazar, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Detector, Gamma ray, gamma rays: observations, catalogs, Astronomy and Astrophysics, Radius, AGILE satellite, Catalogs, Space and Planetary Science, Sky, Satellite, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the first catalog of high-confidence gamma-ray sources detected by the AGILE satellite during observations performed from July 9, 2007 to June 30, 2008. Catalogued sources are detected by merging all the available data over the entire time period. AGILE, launched in April 2007, is an ASI mission devoted to gamma-ray observations in the 30 MeV - 50 GeV energy range, with simultaneous X-ray imaging capability in the 18-60 keV band. This catalog is based on Gamma-Ray Imaging Detector (GRID) data for energies greater than 100 MeV. For the first AGILE catalog we adopted a conservative analysis, with a high-quality event filter optimized to select gamma-ray events within the central zone of the instrument Field of View (radius of 40 degrees). This is a significance-limited (4 sigma) catalog, and it is not a complete flux-limited sample due to the non-uniform first year AGILE sky coverage. The catalog includes 47 sources, 21 of which are associated with confirmed or candidate pulsars, 13 with Blazars (7 FSRQ, 4 BL Lacs, 2 unknown type), 2 with HMXRBs, 2 with SNRs, 1 with a colliding-wind binary system, 8 with unidentified sources., Revised version, 15 pages, 3 figures, 3 tables. To be published in Astronomy and Astrophysics. Text improved and clarified. Refined analysis of complex regions of the Galactic plane yields a new list of high-confidence sources including 47 sources (compared with the 40 sources appearing in the first version)

Published
2009

13. Multiwavelength Observations Of 3c 454.3. Ii. The Agile 2007 December Campaign

Author

I. Donnarumma, G. Pucella, V. Vittorini, F. D'Ammando, S. Vercellone, C. M. Raiteri, M. Villata, M. Perri, W. P. Chen, R. L. Smart, J. Kataoka, N. Kawai, Y. Mori, G. Tosti, D. Impiombato, T. Takahashi, R. Sato, M. Tavani, A. Bulgarelli, A. W. Chen, A. Giuliani, F. Longo, L. Pacciani, A. Argan, G. Barbiellini, F. Boffelli, P. Caraveo, P. W. Cattaneo, V. Cocco, T. Contessi, E. Costa, E. Del Monte, G. De Paris, G. Di Cocco, Y. Evangelista, M. Feroci, A. Ferrari, M. Fiorini, T. Froysland, M. Frutti, F. Fuschino, M. Galli, F. Gianotti, C. Labanti, I. Lapshov, F. Lazzarotto, P. Lipari, M. Marisaldi, M. Mastropietro, S. Mereghetti, E. Morelli, E. Moretti, A. Morselli, A. Pellizzoni, F. Perotti, G. Piano, P. Picozza, M. Pilia, G. Porrovecchio, M. Prest, M. Rapisarda, A. Rappoldi, A. Rubini, S. Sabatini, E. Scalise, P. Soffitta, E. Striani, M. Trifoglio, A. Trois, E. Vallazza, A. Zambra, D. Zanello, C. Pittori, P. Santolamazza, F. Verrecchia, P. Giommi, L. A. Antonelli, S. Colafrancesco, L. Salotti, Donnarumma I, Pucella G, Vittorini V, DAmmando F, Vercellone S, Raiteri CM, Villata M, Perri M, Chen WP, Smart RL, Kataoka J, Kawai N, Mori Y, Tosti G, Impiombato D, Takahashi T, Sato R, Tavani M, Bulgarelli A, Chen AW, Giuliani A, Longo F, Pacciani L, Argan A, Barbiellini G, Boffelli F, Caraveo P, Cattaneo PW, Cocco V, Contessi T, Costa E, Del Monte E, De Paris G, Di Cocco G, Evangelista Y, Feroci M, Ferrari A, Fiorini M, Froysland T, Frutti M, Fuschino F, Galli M, Gianotti F, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Marisaldi M, Mastropietro M, Mereghetti S, Morelli E, Moretti E, Morselli A, Pellizzoni A, Perotti F, Piano G, Picozza P, Pilia M, Porrovecchio G, Prest M, Rapisarda M, Rappoldi A, Rubini A, Sabatini S, Scalise E, Soffitta P, Striani E, Trifoglio M, Trois A, Vallazza E, Zambra A, Zanello D, Pittori C, Santolamazza P, Verrecchia F, Giommi P, Antonelli A, Colafrancesco S, Salotti L, I., Donnarumma, G., Pucella, V., Vittorini, F., D'Ammando, S., Vercellone, C. M., Raiteri, M., Villata, M., Perri, W. P., Chen, R. L., Smart, J., Kataoka, N., Kawai, Y., Mori, G., Tosti, D., Impiombato, T., Takahashi, R., Sato, M., Tavani, A., Bulgarelli, A. W., Chen, A., Giuliani, Longo, Francesco, L., Pacciani, A., Argan, G., Barbiellini, F., Boffelli, P., Caraveo, P. W., Cattaneo, V., Cocco, T., Contessi, E., Costa, E. D., Monte, G. D., Pari, G. D., Cocco, Y., Evangelista, M., Feroci, A., Ferrari, M., Fiorini, T., Froysland, M., Frutti, F., Fuschino, M., Galli, F., Gianotti, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, M., Marisaldi, M., Mastropietro, S., Mereghetti, E., Morelli, E., Moretti, A., Morselli, A., Pellizzoni, F., Perotti, G., Piano, P., Picozza, M., Pilia, G., Porrovecchio, M., Prest, M., Rapisarda, A., Rappoldi, A., Rubini, S., Sabatini, E., Scalise, P., Soffitta, E., Striani, M., Trifoglio, A., Troi, E., Vallazza, A., Zambra, D., Zanello, C., Pittori, P., Santolamazza, F., Verrecchia, P., Giommi, A., Antonelli, S., Colafrancesco, and L., Salotti

Subjects
Agile, Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, High Energy Gamma-ray Astronomy, AGILE satellite, Active Galactic Nuclei, blazar, law.invention, law, Target of opportunity, quasars: general, multiwavelength campaign, Blazar, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), We report on the second Astrorivelatore Gamma a Immagini Leggero (AGILE) multiwavelength campaign of the blazar 3C 454.3 during the first half of 2007 December. This campaign involved AGILE, Spitzer, Swift, Suzaku, the Whole Earth Blazar Telescope (WEBT) consortium, the Rapid Eye Mount (REM), and the Multicolor Imaging Telescopes for Survey and Monstrous Explosions (MITSuME) telescopes, offering a broadband coverage that allowed for a simultaneous sampling of the synchrotron and inverse Compton (IC) emissions. The two-week AGILE monitoring was accompanied by radio to optical monitoring by WEBT and REM, and by sparse observations in mid-infrared and soft/hard X-ray energy bands performed by means of Target of Opportunity observations by Spitzer, Swift, and Suzaku, respectively. The source was detected with an average flux of ~250 × 10^-8 photons cm^-2 s^-1 above 100 MeV, typical of its flaring states. The simultaneous optical and γ-ray monitoring allowed us to study the time lag associated with the variability in the two energy bands, resulting in a possible lsimone-day delay of the γ-ray emission with respect to the optical one. From the simultaneous optical and γ-ray fast flare detected on December 12, we can constrain the delay between the γ-ray and optical emissions within 12 hr. Moreover, we obtain three spectral energy distributions (SEDs) with simultaneous data for 2007 December 5, 13, and 15, characterized by the widest multifrequency coverage. We found that a model with an external Compton on seed photons by a standard disk and reprocessed by the broad-line regions does not describe in a satisfactory way the SEDs of 2007 December 5, 13, and 15. An additional contribution, possibly from the hot corona with T = 106 K surrounding the jet, is required to account simultaneously for the softness of the synchrotron and the hardness of the IC emissions during those epochs, Astronomy and Astrophysics, galaxies: jets, radiation mechanisms: non-thermal, Corona, Synchrotron, Space and Planetary Science, galaxies: individual: 3C 454.3, Astrophysics - High Energy Astrophysical Phenomena, gamma rays: observations, Astrophysics - Cosmology and Nongalactic Astrophysics, Flare
Abstract

著者人数：79名, Accepted: 2009-10-29, 資料番号: SA1000754000

Published
2009

14. Detection of Gamma-Ray Emission from the Vela Pulsar Wind Nebula with AGILE

Author

A. Pellizzoni, M. Galli, A. Giuliani, F. Verrecchia, Francesco Lazzarotto, E. Vallazza, C. Pittori, T. Contessi, N. D'Amico, G. Piano, G. De Paris, A. Argan, Sandro Mereghetti, E. Rossi, E. Scalise, A. Morselli, Arnaud Ferrari, E. Striani, P. Santolamazza, Andrea Bulgarelli, F. Fuschino, I. Lapshov, S. Colafrancesco, L. Salotti, I. Donnarumma, Y. Evangelista, Massimo Rapisarda, G. Di Cocco, A. Possenti, Enrico Costa, S. Sabatini, Alda Rubini, P. W. Cattaneo, G. Pucella, P. Picozza, Marco Tavani, G. Barbiellini, Elena Moretti, Martino Marisaldi, A. Rappoldi, D. Zanello, M. Prest, V. Cocco, M. Mastropietro, F. Perotti, M. Burgay, V. Vittorini, A. W. Chen, Claudio Labanti, A. Zambra, Paolo Lipari, P. Giommi, J. Palfreyman, Giovanni F. Bignami, P. A. Caraveo, M. Trifoglio, M. Fiorini, E. Del Monte, Aidan Hotan, F. Longo, Angelo Antonelli, Marco Feroci, Luigi Pacciani, Maura Pilia, Alessio Trois, Paolo Esposito, Fulvio Gianotti, G. Di Persio, Filippo D'Ammando, Paolo Soffitta, S. Vercellone, Pellizzoni A, Trois A, Tavani M, Pilia M, Giuliani A, Pucella G, Esposito P, Sabatini S, Piano G, Argan A, Barbiellini G, Bulgarelli A, Burgay M, Caraveo P, Cattaneo PW, Chen AW, Cocco V, Contessi T, Costa E, DAmmando F, Del Monte E, De Paris G, Di Cocco G, Di Persio G, Donnarumma I, Evangelista Y, Feroci M, Ferrari A, Fiorini M, Fuschino F, Galli M, Gianotti F, Hotan A, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mastropietro M, Mereghetti S, Moretti E, Morselli A, Pacciani L, Palfreyman J, Perotti F, Picozza P, Pittori C, Possenti A, Prest M, Rapisarda M, Rappoldi A, Rossi E, Rubini A, Santolamazza P, Scalise E, Soffitta P, Striani E, Trifoglio M, Vallazza E, Vercellone S, Verrecchia F, Vittorini V, Zambra A, Zanello D, Giommi P, Colafrancesco S, Antonelli A, Salotti L, D'Amico N, Bignami GF, A., Pellizzoni, A., Troi, M., Tavani, M., Pilia, A., Giuliani, G., Pucella, P., Esposito, S., Sabatini, G., Piano, A., Argan, G., Barbiellini, A., Bulgarelli, M., Burgay, P., Caraveo, P. W., Cattaneo, A. W., Chen, V., Cocco, T., Contessi, E., Costa, F., D'Ammando, E. D., Monte, G. D., Pari, G. D., Cocco, G. D., Persio, I., Donnarumma, Y., Evangelista, M., Feroci, A., Ferrari, M., Fiorini, F., Fuschino, M., Galli, F., Gianotti, A., Hotan, C., Labanti, I., Lapshov, F., Lazzarotto, P., Lipari, Longo, Francesco, M., Marisaldi, M., Mastropietro, S., Mereghetti, E., Moretti, A., Morselli, L., Pacciani, J., Palfreyman, F., Perotti, P., Picozza, C., Pittori, A., Possenti, M., Prest, M., Rapisarda, A., Rappoldi, E., Rossi, A., Rubini, P., Santolamazza, E., Scalise, P., Soffitta, E., Striani, M., Trifoglio, E., Vallazza, S., Vercellone, F., Verrecchia, V., Vittorini, A., Zambra, D., Zanello, P., Giommi, S., Colafrancesco, A., Antonelli, L., Salotti, N., D'Amico, and G. F., Bignami

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Vela, Pulsar wind nebula, High Energy Gamma-ray Astronomy, gamma detection, Relativistic particle, AGILE, Pulsar Wind Nebulae, Pulsar, Astrophysics::Solar and Stellar Astrophysics, AGILE satellite, education, Astrophysics::Galaxy Astrophysics, pulsar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Multidisciplinary, Vela Pulsar Wind Nebula, AGILE, gamma-rays, Gamma ray, Astronomy, Physics::Space Physics, Astrophysics - High Energy Astrophysical Phenomena, Phenomenology (particle physics), X-ray pulsar
Abstract

Pulsars are known to power winds of relativistic particles that can produce bright nebulae by interacting with the surrounding medium. These pulsar wind nebulae (PWNe) are observed in the radio, optical, x-rays and, in some cases, also at TeV energies, but the lack of information in the gamma-ray band prevents from drawing a comprehensive multiwavelength picture of their phenomenology and emission mechanisms. Using data from the AGILE satellite, we detected the Vela pulsar wind nebula in the energy range from 100 MeV to 3 GeV. This result constrains the particle population responsible for the GeV emission, probing multivavelength PWN models, and establishes a class of gamma-ray emitters that could account for a fraction of the unidentified Galactic gamma-ray sources., Comment: Accepted by Science; first published online on December 31, 2009 in Science Express. Science article and Supporting Online Material are available at http://www.sciencemag.org

Published
2009
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15. Masers in Massive Star-forming Regions Associated with the Brightest Steep-Spectrum [ITAL]IRAS[/ITAL] Point Sources

Author

Gordon C. MacLeod, John Galt, Michael J. Gaylard, Sharon Saedt, and E. Scalise

Subjects
Physics, Star formation, Reflection nebula, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Stellar classification, Spectral line, law.invention, Stars, Space and Planetary Science, law, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Maser, Astrophysics::Galaxy Astrophysics
Abstract

Twenty-four bright, steep-spectrum far-infrared IRAS point sources, which were originally discussed by Hughes & MacLeod, have been searched for hydroxyl, water, and methanol masers and for formaldehyde absorption features. Distances and spectral types for the stars exciting these masers were estimated using radio continuum, IRAS spectra, and maser velocity data. It is found that 21 of the 24 sources are regions of massive star formation containing stars earlier than type B2. We report the discovery of five new OH masers, one new 6.7 GHz CH3OH maser, and two new 12.2 GHz CH3OH masers toward these IRAS sources. By contrast, no 4.765 GHz excited-OH masers were found toward these sources. This sample contains only star-forming regions; there are no planetary or reflection nebulae or extragalactic sources present, as seen in samples with less extreme IRAS colors.

Published
1998
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16. Results of the Monitoring of a Very Strong Water Maser Event in W49N

Author

E. Scalise, G. M. Pacheco, A.M. Gómez Balboa, and Z. Abraham

Subjects
010504 meteorology & atmospheric sciences, 0103 physical sciences, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences
Abstract

Since the discovery of the 616-523 rotational transition of interstellar water in maser emission, several hundred sources have been discovered. Their profiles are very variable, presenting correlated variability (Gammon, 1976) or anticorrelated variability (Cesaroni, 1990). Several models have been proposed to explain this variability. Strong Galactic masers, such as W49 and W51 (Kylafis et al. 1991), and also an extremely strong outburst detected by Abraham et al. (1981) in Orion, could not be fully explained based on current models. We have monitored from October 1989 to July 1991 a very strong water vapour eruption in the +28 km s−1 feature, originated from W49N. Here we present the results and discuss the possible correlated variability of this feature with the one that appeared at +62 km s−1.

Published
1992
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17. G305.8 - 0.2: A Young Object with a Dust and Gas Envelope

Author

J.W.S. Vilas Boas, E. Scalise, G.G. Sanzovo, G. Mendes Pacheco, and A.M. Gómez Balboa

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The H2O maser source in G305.8 - 0.2 was first detected by Haynes et al. (1984). Inspection of the Southern Hemisphere radio surveys did not show any strong compact HII region or water maser placed nearby this source. The IRAS point source catalog (2.0) shows a strong source in the direction of the maser. We analysed the temporal variation and line profile of the H2O maser emission and discussed the nature of its associated IRAS source. These source characteristics seem compatible with the hypothesis that the maser is associated with a protostellar disk around an early-type star of spectral type 07 to 09 surrounded by a spherical shell of gas and dust.

Published
1992
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18. Mass Loss Rates of Three Comets

Author

P.D. Singh, W.F. Huebner, D.C. Boice, I. Konno, and E. Scalise

Abstract

Emission features of C2, C3, CN, and dust in Comets Thiele (1985m), Hartley-Good (1985l), and Giacobini-Zinner (1984e) have been analyzed and their mass loss rates of about 0.5, 1.1, and 0.8 Mg s−1 have been determined.

Published
1992
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19. G305.8 - 0.2 water vapor source - A young object

Author

J. W. S. Vilas Boas, C. G. Sanzovo, and E. Scalise

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics, Silicon monoxide, law.invention, chemistry.chemical_compound, chemistry, Space and Planetary Science, law, Astrophysics::Solar and Stellar Astrophysics, Protostar, OH/IR star, Maser, Stellar evolution, Astrophysics::Galaxy Astrophysics, Water vapor, Excitation
Abstract

Observations of water vapor and silicon monoxide masers were conducted in the direction of G305.8−0.2. No SiO maser emission above 7 Jy of flux density was detected. The short-time variability of the H 2 O maser together with the absence of compact radio continuum emission suggests that the excitation energy of the maser could originate from an O7-O9 protostar in its earlier evolutionary stages

Published
1991
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20. Radio Emission of NGC 5128 at = 1.35 cm

Author

P. Marques Dos Santos, Pierre Kaufmann, W. G. Fogarty, and E. Scalise

Subjects
Physics, Luminous infrared galaxy, Radiation flux, X-shaped radio galaxy, Space and Planetary Science, Wave propagation, Radio galaxy, Astronomy, Astronomy and Astrophysics, Quasar, Astrophysics, Spectral line, Radio astronomy
Published
1974
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22. Possible fast variability of the nucleus of Cen A at 13.5 mm

Author

P. Marques Dos Santos, J. C. Raffaelli, Pierre Kaufmann, and E. Scalise

Subjects
Physics, Multidisciplinary, Galactic astronomy, Radio galaxy, Astronomy, Scale (descriptive set theory), Astrophysics, Galactic nuclei, Wavelength, medicine.anatomical_structure, X-shaped radio galaxy, medicine, Nucleus, Radio astronomy
Abstract

INFORMATION about short time scale events in extragalactic objects can have very important implications for the theoretical interpretation of the physical mechanisms involved. Such data are only obtained by using time-consuming observing schedules and methods, and are not usually carried out at radio observatories. This kind of information is thus generally lacking. We report here a study of the nucleus of Cen A (NGC 5128) at a wavelength of 13.5mm. Possible fast variability was observed.

Published
1977
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23. Distribution of Circularly Polarized Emission across the Solar Disk at λ = 4.3 cm

Author

Pierre Kaufmann and E. Scalise

Abstract

(Solar Phys.). The emission of circularly polarized radiation of reversed senses from the respective solar hemispheres at λ = 4.3 cm is discussed, referring to consistent eclipse results obtained in November 1966 (Figure 1), March 1970, and January 1973 (Figure 2). Further qualitative information were obtained by performing a series of 18 daily solar maps (Figure 3) at the same wavelength, with moderate angular resolution (i.e., 12′). We were not able to resolve individual centers' polarities, but have confirmed that reversed senses of circular polarization occur, tending to be right-handed at southern areas of the solar disk, and left-handed at northern areas. These senses correspond to preceding polarities at the hemispheres for the 20th solar cycle, and a ‘neutral line’ divide the two polarized hemispheres, showing a contour that depends strongly on the presence of active centres and on their displacement with solar rotation. This suggest that the polarized features are strongly controlled, if not completely, by the presence of photospheric underlying magnetic areas.

Published
1974
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24. Observations with a 7 GHz polarimeter

Author

Oscar T. Matsuura, Pierre Kaufmann, E. Scalise, and P. Marques Dos Santos

Subjects
Physics, Multidisciplinary, Angular distribution, Astronomy, Polarimeter, Polarization (waves), Electronic equipment, Radio wave
Published
1970

25. The Imaging X-Ray Polarimetry Explorer (IXPE): technical overview II

Author

M. Negro, Roger W. Romani, Luca Baldini, Giorgio Matt, Colin Peterson, Fabio La Monaca, Christina Pentz, Paolo Soffitta, Alessandro Paggi, Brent Forsyth, Francesco Zanetti, Sergio Fabiani, Martin C. Weisskopf, D. Zachery Allen, James Masciarelli, Jeffery McCracken, Eli Gurnee, Toru Tamagawa, Michele Pinchera, Pasqualino Loffredo, Stephen D. Bongiorno, Brian T. Smith, Carmelo Sgrò, Noah Root, Steven D. Pavelitz, Scott C. Mitchell, Mattia Barbanera, Antonino Tobia, Richard Pacheco, Leonardo Lucchesi, Massimo Minuti, Stephen L. O'Dell, Javier Sánchez, Chet O. Speegle, Shelley Le Roy, Paolo Mereu, Bruce Weddendorf, Herman L. Marshall, Alessio Nuti, Ajay Ratheesh, Hikmat Nasimi, MacKenzie Ferrie, Anthony R. Kelley, C. Oppedisano, E. Cavazzuti, Fabio Borotto, Niccolò Di Lalla, Melissa Pesce-Rollins, Enrico Costa, Ronaldo Bellazzini, H. Kyle Bygott, Allyn F. Tennant, John Rankin, Raffaele Piazzola, Riccardo Ferrazzoli, Daniele Brienza, Cheryl Alexander, Primo Attina, Brian D. Ramsey, E. Scalise, Gloria Spandre, Shawn Breeding, I. Donnarumma, Y. Evangelista, Giuseppe Di Persio, Fei Xie, Kurtis L. Dietz, Alda Rubini, Federico Mosti, Simonetta Puccetti, Marcello Tardiola, Leonardo Orsini, Fabrizio Amici, Kiranmayee Kilaru, L. Guy, Andrea Sciortino, Jaganathan Ranganathan, Carlo Lefevre, Fabio Muleri, Raffaella Bonino, Alessio Trois, Darren Osborne, Victoria M. Kaspi, Michael McEachen, Shuichi Gunji, M. Perri, Ettore Del Monte, Ronald F. Elsner, Alfredo Morbidini, Marco Marengo, William Kalinowski, Alessandro Brez, Alessandra Marrocchesi, Francesco Santoli, Saverio Citraro, Michelle Foster, Mauro Centrone, Alberto Manfreda, Grant Hibbard, Amy L. Walden, Jeff Bladt, Luca Latronico, Jeffrey Wedmore, Claudia Cardelli, Alessandro Profeti, Ciro Caporale, M. Ceccanti, Francesco Massaro, Brad Porter, Jeffrey Kolodziejczak, Joseph Footdale, Guido Magazzu, Sandra R. Johnson, Eric Kelly, William D. Deininger, David Welch, W. H. Baumgartner, Ikuyuki Mitsuishi, Spencer Antoniak, Sarah Schindhelm, Stephanie Ruswick, ITA, USA, and JPN

Subjects
010302 applied physics, Physics, X-ray astronomy, Spacecraft, 010308 nuclear & particles physics, business.industry, gas pixel detectors, Astrophysics::High Energy Astrophysical Phenomena, Detector, grazing-incidence optics, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimetry, Polarization (waves), 01 natural sciences, IXPE, GPD, X-ray polarimetry, imaging, missions, polarimetry, Observatory, Attitude determination, 0103 physical sciences, Aerospace engineering, business
Abstract

SPIE grants to authors (and their employers) of papers, posters, and presentation recordings published in SPIE Proceedings or SPIE Journals on the SPIE Digital Library (hereinafter "publications") the right to post an author-prepared version or an official version (preferred version) of the publication on an internal or external server controlled exclusively by the author/employer or the entity funding the research, provided that (a) such posting is noncommercial in nature and the publication is made available to users without charge; (b) an appropriate copyright notice and citation appear with the publication; and (c) a link to SPIE's official online version of the publication is provided using the item's DOI. This authorization does not extend to third-party web sites not owned and maintained by the author/employer such as ResearchGate, Academia.edu, YouTube, etc. The Imaging X-ray Polarimetry Explorer (IXPE) will add polarization to the properties (time, energy, and position) observed in x-ray astronomy. A NASA Astrophysics Small Explorer (SMEX) in partnership with the Italian Space Agency (ASI), IXPE will measure the 2-8-keV polarization of a few dozen sources during the first 2 years following its 2021 launch. The IXPE Observatory includes three identical x-ray telescopes, each comprising a 4-m-focal-length (grazingincidence) mirror module assembly (MMA) and a polarization-sensitive (imaging) detector unit (DU), separated by a deployable optical bench. The Observatory's Spacecraft provides typical subsystems (mechanical, structural, thermal, power, electrical, telecommunications, etc.), an attitude determination and control subsystem for 3-axis stabilized pointing, and a command and data handling subsystem communicating with the science instrument and the Spacecraft subsystems.

26. Outcomes of the IXPE instrument calibration

Author

Hikmat Nasimi, John Rankin, Sergio Di Cosimo, Leonardo Lucchesi, Fabio La Monaca, Michele Pinchera, Francesco Santoli, Saverio Citraro, Mattia Barbanera, Alessio Nuti, Fei Xie, Antonino Tobia, Paolo Soffitta, Primo Attina, E. Scalise, Alberto Manfreda, Luca Baldini, Ettore Del Monte, Raffaele Piazzolla, Alda Rubini, Riccardo Ferrazzoli, Pasqualino Loffredo, Alessandro Di Marco, Alfredo Morbidini, Sergio Fabiani, Ajay Ratheesh, Carmelo Sgrò, Massimo Minuti, Y. Evangelista, S. Castellano, Enrico Costa, Carlo Lefevre, Fabio Muleri, Alessio Trois, Fabrizio Amici, Daniele Brienza, Giuseppe Di Persio, and Leonardo Orsini

Subjects
Physics, Physics::Instrumentation and Detectors, Linear polarization, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Measure (physics), Polarimetry, Polarimeter, Photoelectric effect, calibration, IXPE, X-ray polarimetry, calibration, Gas Pixel Detector, GPD, law.invention, Telescope, Optics, law, GPD, Calibration, X-ray polarimetry, IXPE, business, Gas Pixel Detector
Abstract

IXPE (Imaging X-ray Polarimetry Explorer) is the next Nasa Small Explorer mission foreseen for the lunch in 2021. It is a partnership with the Italian Space Agency (ASI). IXPE is devoted to X-ray polarimetry in the 2-8 keV energy band. The IXPE telescope comprises three grazing incidence mirror modules coupled to three detector units hosting each one a Gas Pixel Detector (GPD) polarimeter. The GPD exploits the photoelectric effect to measure the linear polarization of the X-ray emission from astrophysical sources. A wide and accurate on ground calibration was carried out on the IXPE detector units at INAF-IAPS in Italy. A dedicated facility was set-up to calibrate the detector units with polarized and unpolarised X-rays at different energies before Instrument integration.

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27. New H2O celestial sources associated with H II regions in the Southern Hemisphere

Author

Jacques Raymond Daniel Lépine, M. H. Paes De Barros, R. H. Gammon, P. Marques Dos Santos, E. Scalise, M. L. Meeks, J. M. Sobolewski, A. L. Ibanez, J. C. Carter, R. E. Schaal, S. H. Zisk, and Pierre Kaufmann

Subjects
Physics, Multidisciplinary, Meteorology, Amplifier, Astronomy, Galaxy, Spectral line, law.invention, Radio telescope, law, Emission spectrum, Maser, Southern Hemisphere, Water vapor
Abstract

WE report here the first results of a nearly complete, high-sensitivity, water vapour survey of galactic H II regions situated in the Southern Hemisphere.

Published
1976
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28. High-sensitivity survey of NH3 in the Southern Hemisphere

Author

J. W. S. Vilas Boas, Y. Bakor, E. Scalise, P. C. Myers, and R. E. Schaal

Subjects
Physics, media_common.quotation_subject, Analytical chemistry, Astronomy and Astrophysics, Atmospheric sciences, Spectral line, law.invention, Ammonia, chemistry.chemical_compound, chemistry, Space and Planetary Science, Sky, law, Emission spectrum, Maser, Absorption (electromagnetic radiation), Southern Hemisphere, Line (formation), media_common
Abstract

Microwave emission associated with the para form of ammonia, in the (1, 1) line, was searched for in the direction of 46 southern sky positions where strong H/sub 2/CO absorption or strong H/sub 2/O maser emission was observed previously. The results of those observations are presented with 17 new ammonia sources discovered.

Published
1981
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29. Observations of SiO maser sources at 43.122 GHz

Author

J. R. D. Lepine, E. Scalise, and A. M. Le Squeren

Subjects
Physics, R Aquarii, Astronomy, Astronomy and Astrophysics, Astrophysics, Spectral line, Astronomical spectroscopy, law.invention, Interstellar medium, Microwave emission, Space and Planetary Science, law, Emission spectrum, Maser, Radio astronomy
Published
1978
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30. The Itapetinga Contribution on North-South High Resolution VLBI Experiments

Author

E. Scalise, Y. Bakor, P. Kaufmann, C. B. Georges, R. E. Schaal, and Zulema Abraham

Subjects
Upgrade, Radio observatory, Observatory, Very-long-baseline interferometry, High resolution, Astronomy, Geodetic datum, Geology
Abstract

Since the very beginning of the Itapetinga 45-ft antenna operations in 1971, there were plans to use it as a southern hemisphere VLBI terminal for high north-south resolution. The first successful VLBI tests were performed on water vapor lines in cooperation with Haystack Observatory in 1978 in one of the last runs using the MkI system. This cooperation led to the construction of a MkII terminal for Itapetinga years later (1981–1983). Astrophysical VLBI runs have been carried out since 1984, with the cooperation of Caltech, producing maps of unique resolution on stronger quasars, especially on 3C273 whose evolution has been followed since then. Recently, Bonn joined the collaboration in astrophysical VLBI programs. Itapetinga also participated successfully in geodetic surveys, and in the Vega-Venus mission, in collaboration with JPL and French organizations CNES, Observatoire de Paris and IGN. Plans for continuation and expansion of the Itapetinga VLBI participation in international efforts depend strongly on support to maintain and upgrade instrumentation at the Brazilian Radio Observatory.

Published
1988
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31. H2O maser survey in the Magellanic Clouds

Author

Braz and E. Scalise

Subjects
Physics, Interstellar cloud, Astronomy, Astronomy and Astrophysics, Astrophysics, Planetary nebula, Astronomical spectroscopy, Galaxy, law.invention, Luminosity, Space and Planetary Science, law, Protostar, Maser, Stellar evolution
Abstract

An extensive search for water vapor maser emission towards the Large and Small Magellanic Clouds is reported. The 6/sub 16/--5/sub 23/ transition of water molecule was detected in two H II regions in LMC (including N 159, previously was detected) and in two H II regions in SMC. A total of 32 positions was searched in both Clouds. The strength of the sources detected is comparable with galactic masers with luminosities L< or approx. =10/sup -2/L/sub sun/.

Published
1982
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33. Observations of 3C 273 with high north-south resolution

Author

E. Scalise, H. E. Hardebeck, J. A. Biretta, Pierre Kaufmann, Zulema Abraham, R. E. Schaal, Maurice Cohen, P. M. Silva, and A. A. Perfetto

Subjects
Physics, Space and Planetary Science, Resolution (electron density), Compton scattering, Astronomy, Astronomy and Astrophysics, Quasar, Astrophysics
Published
1985
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34. A water vapour maser in the Large Magellanic Cloud

Author

M. A. Braz and E. Scalise

Subjects
Physics, Radio telescope, Solar System, Multidisciplinary, law, Satellite galaxy, Astronomy, Maser, Large Magellanic Cloud, Galaxy, law.invention, Luminosity, Radio astronomy
Abstract

Surveys of the Large Magellanic Cloud (LMC), the closest satellite galaxy to our Solar System, for water vapour sources of measurable intensity have so far yielded negative results. These searches, by Johnston et al.1 and Kaufmann et al.2, with detection limits of about 150 and 20 Jy (1 Jy = 10−26 Wm−2 Hz−1), respectively, suggest that any water vapour masers that exist in the LMC are much weaker than the sources recognized in our own Galaxy and in several more distant galaxies3–5. We now report the results of a survey using the 45-ft Itapetinga radio telescope which shows the presence of a water vapour maser in the N159 region of the LMC.

Published
1981
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36. Exploring age-related variations during talar growth

Author

Figus C, Stephens NB, Sorrentino R, Bortolini E, Scalise LM, Gabanini G, Romandini M, Lugli F, Arrighi S, Badino F, Marciani G, Oxilia G, Panetta D, Belcastro MG, Harcourt-Smith W, Ryan TM, Benazzi S., and Figus C, Stephens NB, Sorrentino R, Bortolini E, Scalise LM, Gabanini G, Romandini M, Lugli F, Arrighi S, Badino F, Marciani G, Oxilia G, Panetta D, Belcastro MG, Harcourt-Smith W, Ryan TM, Benazzi S.

Subjects
talus, ontogeny, geometric morphometrics, talar growth
Abstract

Age estimation is a fundamental aspect in juvenile osteological studies and, as such, there are many methods that rely on ontogenetic-related changes to bone morphology. The talus, being a small and compact bone, is generally well preserved in archaeological contexts, but little is known about its morphological trajectory during growth. To better nderstand this we apply a (semi)landmark-based approach to an ontogenetic sample of 26 modern human juvenile tali (known age/sex = 12; unknown age/sex = 14), grouped by 5 age categories ranging from 0 to 15 years. A template of 11 landmarks and 205 semilandmarks were applied to 26 microCT-based digital models of the juvenile tali. These were superimposed by Generalized Procrustes Analysis with the semilandmarks freely sliding against recursive updates of the Procrustes consensus. Finally, individuals of unknown age/sex were projected into the form-space determined from a Principal Component Analysis of the known sample. Our results show that most of the morphometric variation is explained by PC1 (⁓91%), which is highly correlated with size and accounts for ontogenetic allometry. Negative scores (i.e., youngest) are related to a small and globular morphology. The positive scores (i.e., oldest) account for an elongation of the talar body, which is mainly related to the development of the neck and growth of the lateral malleolar facet. Overall, our preliminary results suggest that age-related morphological variations of the talus may be used to determine the general age of juvenile skeletal remains, which could be valuable to many archaeological and forensic researchers.

Published
2019

37. Design and Test of a Calibration System for Avalanche Photodiodes Used in X-Ray Compton Polarimeters for Space.

Author

Alimenti A, Cologgi F, Fabiani S, Torokhtii K, Silva E, Del Monte E, Baffo I, Bonomo S, Brienza D, Campana R, Centrone M, De Iulis G, Costa E, Cucinella G, Curatolo A, De Angelis N, De Cesare G, Del Re A, Di Cosimo S, Di Filippo S, Di Marco A, Di Persio G, Donnarumma I, Fanelli P, Kumar A, Leonetti P, Locarini A, Loffredo P, Lombardi G, Minervini G, Modenini D, Muleri F, Natalucci S, Negri A, Perelli M, Rossi M, Rubini A, Scalise E, Soffitta P, Terracciano A, Tortora P, Zaccagnino E, and Zambardi A

Abstract

The development and calibration of a measurement system designed for assessing the performance of the avalanche photodiodes (APDs) used in the Compton scattering polarimeter of the CUSP project is discussed in this work. The designed system is able to characterize the APD gain GAPD and energy resolution across a wide range of temperatures T (from -20 °C to +60 °C) and bias voltages Vbias (from 260 V to 410 V). The primary goal was to experimentally determine the GAPD dependence on the T and Vbias in order to establish a strategy for stabilizing GAPD by compensating for T fluctuations, acting on Vbias. The results demonstrate the system capability to accurately characterize APD behavior and develop feedback mechanisms to ensure its stable operation. This work provides a robust framework for calibrating APDs for space environments. It is essential for the successful implementation of spaceborne polarimeters such as the Compton scattering polarimeter foreseen aboard the CUbeSat Solar Polarimeter (CUSP) mission under development to perform solar flare X-ray polarimetry.

Published
2024
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38. Omics Science and Social Aspects in Detecting Biomarkers for Diagnosis, Risk Prediction, and Outcomes of Carotid Stenosis.

Author

Costa D, Scalise E, Ielapi N, Bracale UM, Faga T, Michael A, Andreucci M, and Serra R

Subjects
Humans, Metabolomics methods, Carotid Stenosis diagnosis, Carotid Stenosis metabolism, Biomarkers metabolism, Genomics, Proteomics methods
Abstract

Carotid stenosis is characterized by the progressive narrowing of the carotid arteries due to the formation of atherosclerotic plaque, which can lead to stroke and death as major complications. Numerous biomarkers allow for its study and characterization, particularly those related to "omics" sciences. Through the most common research databases, we report representative studies about carotid stenosis biomarkers based on genomics, transcriptomics, proteomics, and metabolomics in a narrative review. To establish a priority among studies based on their internal validity, we used a quality assessment tool, the Scale for the Assessment of Narrative Review Articles (SANRA). Genes, transcriptomes, proteins, and metabolites can diagnose the disease, define plaque connotations, predict consequences after revascularization interventions, and associate carotid stenosis with other patient comorbidities. It also emerged that many aspects determining the patient's psychological and social sphere are implicated in carotid disease. In conclusion, when taking the multidisciplinary approach that combines human sciences with biological sciences, it is possible to comprehensively define a patient's health and thus improve their clinical management through precision medicine.

Published
2024
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39. Metalloproteinases as Biomarkers and Sociomarkers in Human Health and Disease.

Author

Costa D, Scalise E, Ielapi N, Bracale UM, Andreucci M, and Serra R

Subjects
Humans, Biomarkers, Proteolysis, Zinc, Matrix Metalloproteinases, Physicians
Abstract

Metalloproteinases (MPs) are zinc-dependent enzymes with proteolytic activity and a variety of functions in the pathophysiology of human diseases. The main objectives of this review are to analyze a specific family of MPs, the matrix metalloproteinases (MMPs), in the most common chronic and complex diseases that affect patients' social lives and to better understand the nature of the associations between MMPs and the psychosocial environment. In accordance with the PRISMA extension for a scoping review, an examination was carried out. A collection of 24 studies was analyzed, focusing on the molecular mechanisms of MMP and their connection to the manifestation of social aspects in human disease. The complexity of the relationship between MMP and social problems is presented via an interdisciplinary approach based on complexity paradigm as a new approach for conceptualizing knowledge in health research. Finally, two implications emerge from the study: first, the psychosocial states of individuals have a profound impact on their overall health and disease conditions, which implies the importance of adopting a holistic perspective on human well-being, encompassing both physical and psychosocial aspects. Second, the use of MPs as biomarkers may provide physicians with valuable tools for a better understanding of disease when used in conjunction with "sociomarkers" to develop mathematical predictive models.

Published
2024
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40. New Approaches and Understandings in the Growth of Cubic Silicon Carbide.

Author

La Via F, Zimbone M, Bongiorno C, La Magna A, Fisicaro G, Deretzis I, Scuderi V, Calabretta C, Giannazzo F, Zielinski M, Anzalone R, Mauceri M, Crippa D, Scalise E, Marzegalli A, Sarikov A, Miglio L, Jokubavicius V, Syväjärvi M, Yakimova R, Schuh P, Schöler M, Kollmuss M, and Wellmann P

Abstract

In this review paper, several new approaches about the 3C-SiC growth are been presented. In fact, despite the long research activity on 3C-SiC, no devices with good electrical characteristics have been obtained due to the high defect density and high level of stress. To overcome these problems, two different approaches have been used in the last years. From one side, several compliance substrates have been used to try to reduce both the defects and stress, while from another side, the first bulk growth has been performed to try to improve the quality of this material with respect to the heteroepitaxial one. From all these studies, a new understanding of the material defects has been obtained, as well as regarding all the interactions between defects and several growth parameters. This new knowledge will be the basis to solve the main issue of the 3C-SiC growth and reach the goal to obtain a material with low defects and low stress that would allow for realizing devices with extremely interesting characteristics.

Published
2021
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41. Exciton-driven change of phonon modes causes strong temperature dependent bandgap shift in nanoclusters.

Author

Muckel F, Lorenz S, Yang J, Nugraha TA, Scalise E, Hyeon T, Wippermann S, and Bacher G

Abstract

The fundamental bandgap E g of a semiconductor-often determined by means of optical spectroscopy-represents its characteristic fingerprint and changes distinctively with temperature. Here, we demonstrate that in magic sized II-VI clusters containing only 26 atoms, a pronounced weakening of the bonds occurs upon optical excitation, which results in a strong exciton-driven shift of the phonon spectrum. As a consequence, a drastic increase of dE g /dT (up to a factor of 2) with respect to bulk material or nanocrystals of typical size is found. We are able to describe our experimental data with excellent quantitative agreement from first principles deriving the bandgap shift with temperature as the vibrational entropy contribution to the free energy difference between the ground and optically excited states. Our work demonstrates how in small nanoparticles, photons as the probe medium affect the bandgap-a fundamental semiconductor property.

Published
2020
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42. Detection of gamma-ray emission from the Vela pulsar wind nebula with AGILE.

Author

Pellizzoni A, Trois A, Tavani M, Pilia M, Giuliani A, Pucella G, Esposito P, Sabatini S, Piano G, Argan A, Barbiellini G, Bulgarelli A, Burgay M, Caraveo P, Cattaneo PW, Chen AW, Cocco V, Contessi T, Costa E, D'Ammando F, Del Monte E, De Paris G, Di Cocco G, Di Persio G, Donnarumma I, Evangelista Y, Feroci M, Ferrari A, Fiorini M, Fuschino F, Galli M, Gianotti F, Hotan A, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mastropietro M, Mereghetti S, Moretti E, Morselli A, Pacciani L, Palfreyman J, Perotti F, Picozza P, Pittori C, Possenti A, Prest M, Rapisarda M, Rappoldi A, Rossi E, Rubini A, Santolamazza P, Scalise E, Soffitta P, Striani E, Trifoglio M, Vallazza E, Vercellone S, Verrecchia F, Vittorini V, Zambra A, Zanello D, Giommi P, Colafrancesco S, Antonelli A, Salotti L, D'Amico N, and Bignami GF

Abstract

Pulsars are known to power winds of relativistic particles that can produce bright nebulae by interacting with the surrounding medium. These pulsar wind nebulae are observed by their radio, optical, and x-ray emissions, and in some cases also at TeV (teraelectron volt) energies, but the lack of information in the gamma-ray band precludes drawing a comprehensive multiwavelength picture of their phenomenology and emission mechanisms. Using data from the AGILE satellite, we detected the Vela pulsar wind nebula in the energy range from 100 MeV to 3 GeV. This result constrains the particle population responsible for the GeV emission and establishes a class of gamma-ray emitters that could account for a fraction of the unidentified galactic gamma-ray sources.

Published
2010
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43. Extreme particle acceleration in the microquasar Cygnus X-3.

Author

Tavani M, Bulgarelli A, Piano G, Sabatini S, Striani E, Evangelista Y, Trois A, Pooley G, Trushkin S, Nizhelskij NA, McCollough M, Koljonen KI, Pucella G, Giuliani A, Chen AW, Costa E, Vittorini V, Trifoglio M, Gianotti F, Argan A, Barbiellini G, Caraveo P, Cattaneo PW, Cocco V, Contessi T, D'Ammando F, Del Monte E, De Paris G, Di Cocco G, Di Persio G, Donnarumma I, Feroci M, Ferrari A, Fuschino F, Galli M, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Mattaini E, Marisaldi M, Mastropietro M, Mauri A, Mereghetti S, Morelli E, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Picozza P, Pilia M, Prest M, Rapisarda M, Rappoldi A, Rossi E, Rubini A, Scalise E, Soffitta P, Vallazza E, Vercellone S, Zambra A, Zanello D, Pittori C, Verrecchia F, Giommi P, Colafrancesco S, Santolamazza P, Antonelli A, and Salotti L

Abstract

Super-massive black holes in active galaxies can accelerate particles to relativistic energies, producing jets with associated gamma-ray emission. Galactic 'microquasars', which are binary systems consisting of a neutron star or stellar-mass black hole accreting gas from a companion star, also produce relativistic jets, generally together with radio flares. Apart from an isolated event detected in Cygnus X-1, there has hitherto been no systematic evidence for the acceleration of particles to gigaelectronvolt or higher energies in a microquasar, with the consequence that we are as yet unsure about the mechanism of jet energization. Here we report four gamma-ray flares with energies above 100 MeV from the microquasar Cygnus X-3 (an exceptional X-ray binary that sporadically produces radio jets). There is a clear pattern of temporal correlations between the gamma-ray flares and transitional spectral states of the radio-frequency and X-ray emission. Particle acceleration occurred a few days before radio-jet ejections for two of the four flares, meaning that the process of jet formation implies the production of very energetic particles. In Cygnus X-3, particle energies during the flares can be thousands of times higher than during quiescent states.

Published
2009
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