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1. Discovery of strongly variable X-ray polarization in the neutron star low-mass X-ray binary transient XTE J1701$-$462

Author: Cocchi, M., Gnarini, A., Fabiani, S., Ursini, F., Poutanen, J., Capitanio, F., Bobrikova, A., Farinelli, R., Paizis, A., Sidoli, L., Veledina, A., Bianchi, S., Di Marco, A., Ingram, A., Kajava, J. J. E., La Monaca, F., Matt, G., Malacaria, C., Mikusincova, R., Rankin, J., Zane, S., Agudo, I., Antonelli, L. A., Bachetti, M., Baldini, L., Baumgartner, W. H., Bellazzini, R., Bongiorno, S. D., Bonino, R., Brez, A., Bucciantini, N., Castellano, S., Cavazzuti, E., Chen, C. -T., Ciprini, S., Costa, E., De Rosa, A., Del Monte, E., Di Gesu, L., Di Lalla, N., Donnarumma, I., Doroshenko, V., Dovciak, M., Ehlert, S. R., Enoto, T., Evangelista, Y., Ferrazzoli, R., Garcia, J. A., Gunji, S., Hayashida, K., Heyl, J., Iwakiri, W., Jorstad, S. G., Kaaret, P., Karas, V., Kislat, F., Kitaguchi, T., Kolodziejczak, J. J., Krawczynski, H., Latronico, L., Liodakis, I., Maldera, S., Manfreda, A., Marin, F., Marinucci, A., Marscher, A. P., Marshall, H. L., Massaro, F., Mitsuishi, I., Mizuno, T., Muleri, F., Negro, M., C. -Y., Ng, O'Dell, S. L., Omodei, N., Oppedisano, C., Papitto, A., Pavlov, G. G., Peirson, A. L., Perri, M., Pesce-Rollins, M., Petrucci, P. -O., Pilia, M., Possenti, A., Puccetti, S., Ramsey, B. D., Ratheesh, A., Roberts, O. J., Romani, R. W., Sgro, C., Slane, P., Soffitta, P., Spandre, G., Swartz, D. A., Tamagawa, T., Tavecchio, F., Taverna, R., Tawara, Y., Tennant, A. F., Thomas, N. E., Tombesi, F., Trois, A., Tsygankov, S. S., Turolla, R., Vink, J., Weisskopf, M. C., Wu, K., Xie, F., Cocchi, M., Gnarini, A., Fabiani, S., Ursini, F., Poutanen, J., Capitanio, F., Bobrikova, A., Farinelli, R., Paizis, A., Sidoli, L., Veledina, A., Bianchi, S., Di Marco, A., Ingram, A., Kajava, J. J. E., La Monaca, F., Matt, G., Malacaria, C., Mikusincova, R., Rankin, J., Zane, S., Agudo, I., Antonelli, L. A., Bachetti, M., Baldini, L., Baumgartner, W. H., Bellazzini, R., Bongiorno, S. D., Bonino, R., Brez, A., Bucciantini, N., Castellano, S., Cavazzuti, E., Chen, C. -T., Ciprini, S., Costa, E., De Rosa, A., Del Monte, E., Di Gesu, L., Di Lalla, N., Donnarumma, I., Doroshenko, V., Dovciak, M., Ehlert, S. R., Enoto, T., Evangelista, Y., Ferrazzoli, R., Garcia, J. A., Gunji, S., Hayashida, K., Heyl, J., Iwakiri, W., Jorstad, S. G., Kaaret, P., Karas, V., Kislat, F., Kitaguchi, T., Kolodziejczak, J. J., Krawczynski, H., Latronico, L., Liodakis, I., Maldera, S., Manfreda, A., Marin, F., Marinucci, A., Marscher, A. P., Marshall, H. L., Massaro, F., Mitsuishi, I., Mizuno, T., Muleri, F., Negro, M., Ng, C. -Y., O'Dell, S. L., Omodei, N., Oppedisano, C., Papitto, A., Pavlov, G. G., Peirson, A. L., Perri, M., Pesce-Rollins, M., Petrucci, P. -O., Pilia, M., Possenti, A., Puccetti, S., Ramsey, B. D., Ratheesh, A., Roberts, O. J., Romani, R. W., Sgro, C., Slane, P., Soffitta, P., Spandre, G., Swartz, D. A., Tamagawa, T., Tavecchio, F., Taverna, R., Tawara, Y., Tennant, A. F., Thomas, N. E., Tombesi, F., Trois, A., Tsygankov, S. S., Turolla, R., Vink, J., Weisskopf, M. C., Wu, K., and Xie, F.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: After about 16 years since its first outburst, the transient neutron star low-mass X-ray binary XTE J1701$-$462 turned on again in September 2022, allowing for the first study of its X-ray polarimetric characteristics by a dedicated observing program with the Imaging X-ray Polarimeter Explorer (IXPE). Polarimetric studies of XTE J1701$-$462 have been expected to improve our understanding of accreting weakly magnetized neutron stars, in particular, the physics and the geometry of the hot inner regions close to the compact object. The IXPE data of two triggered observations were analyzed using time-resolved spectroscopic and polarimetric techniques, following the source along its Z-track of the color-color diagram. During the first pointing on 2022 September 29, an average 2-8 keV polarization degree of 4.6$\pm$ 0.4\% was measured, the highest value found up to now for this class of sources. Conversely, only a $\sim$0.6\% average degree was obtained during the second pointing ten days later. The polarimetric signal appears to be strictly related to the higher energy blackbody component associated with the boundary layer (BL) emission and its reflection from the inner accretion disk, and it is as strong as 6.1\% and 1.2\% ($>95\%$ significant) above 3-4 keV for the two measurements, respectively. The variable polarimetric signal is apparently related to the spectral characteristics of XTE J1701$-$462, which is the strongest when the source was in the horizontal branch of its Z-track and the weakest in the normal branch. These IXPE results provide new important observational constraints on the physical models and geometry of the Z-sources. Here, we discuss the possible reasons for the presence of strong and variable polarization among these sources., 7 pages, 8 figures; published in A&A 674, L10 (2023)
Published: 2023
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2. X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator?

Author: Mushtukov, A A, Tsygankov, S S, Poutanen, J, Doroshenko, V, Salganik, A, Costa, E, Marco, A Di, Heyl, J, Monaca, F La, Lutovinov, A A, Mereminsky, I A, Papitto, A, Semena, A N, Shtykovsky, A E, Suleimanov, V F, Forsblom, S V, González-Caniulef, D, Malacaria, C, Sunyaev, R A, Agudo, I, Antonelli, L A, Bachetti, M, Baldini, L, Baumgartner, W H, Bellazzini, R, Bianchi, S, Bongiorno, S D, Bonino, R, Brez, A, Bucciantini, N, Capitanio, F, Castellano, S, Cavazzuti, E, Chen, C-T, Ciprini, S, De&nbsp, Rosa, A, Del Monte, E, Gesu, L Di, Lalla, N Di, Donnarumma, I, Dovčiak, M, Ehlert, S R, Enoto, T, Evangelista, Y, Fabiani, S, Ferrazzoli, R, Garcia, J A, Gunji, S, Hayashida, K, Iwakiri, W, Jorstad, S G, Kaaret, P, Karas, V, Kislat, F, Kitaguchi, T, Kolodziejczak, J J, Krawczynski, H, Latronico, L, Liodakis, I, Maldera, S, Manfreda, A, Marin, F, Marscher, A P, Marshall, H L, Massaro, F, Matt, G, Mitsuishi, I, Mizuno, T, Muleri, F, Negro, M, Ng, C-Y, O’Dell, S L, Omodei, N, Oppedisano, C, Pavlov, G G, Peirson, A L, Perri, M, Pesce-Rollins, M, Petrucci, P-O, Pilia, M, Possenti, A, Puccetti, S, Ramsey, B D, Rankin, J, Ratheesh, A, Roberts, O J, Romani, R W, Sgrò, C, Slane, P, Soffitta, P, Spandre, G, Swartz, D A, Tamagawa, T, Tavecchio, F, Taverna, R, Tawara, Y, Tennant, A F, Thomas, N E, Tombesi, F, Trois, A, Turolla, R, Vink, J, Weisskopf, M C, Wu, K, Xie, F, Zane, S, Mushtukov, A A, Tsygankov, S S, Poutanen, J, Doroshenko, V, Salganik, A, Costa, E, Marco, A Di, Heyl, J, Monaca, F La, Lutovinov, A A, Mereminsky, I A, Papitto, A, Semena, A N, Shtykovsky, A E, Suleimanov, V F, Forsblom, S V, González-Caniulef, D, Malacaria, C, Sunyaev, R A, Agudo, I, Antonelli, L A, Bachetti, M, Baldini, L, Baumgartner, W H, Bellazzini, R, Bianchi, S, Bongiorno, S D, Bonino, R, Brez, A, Bucciantini, N, Capitanio, F, Castellano, S, Cavazzuti, E, Chen, C-T, Ciprini, S, De&nbsp, Rosa, A, Del Monte, E, Gesu, L Di, Lalla, N Di, Donnarumma, I, Dovčiak, M, Ehlert, S R, Enoto, T, Evangelista, Y, Fabiani, S, Ferrazzoli, R, Garcia, J A, Gunji, S, Hayashida, K, Iwakiri, W, Jorstad, S G, Kaaret, P, Karas, V, Kislat, F, Kitaguchi, T, Kolodziejczak, J J, Krawczynski, H, Latronico, L, Liodakis, I, Maldera, S, Manfreda, A, Marin, F, Marscher, A P, Marshall, H L, Massaro, F, Matt, G, Mitsuishi, I, Mizuno, T, Muleri, F, Negro, M, Ng, C-Y, O’Dell, S L, Omodei, N, Oppedisano, C, Pavlov, G G, Peirson, A L, Perri, M, Pesce-Rollins, M, Petrucci, P-O, Pilia, M, Possenti, A, Puccetti, S, Ramsey, B D, Rankin, J, Ratheesh, A, Roberts, O J, Romani, R W, Sgrò, C, Slane, P, Soffitta, P, Spandre, G, Swartz, D A, Tamagawa, T, Tavecchio, F, Taverna, R, Tawara, Y, Tennant, A F, Thomas, N E, Tombesi, F, Trois, A, Turolla, R, Vink, J, Weisskopf, M C, Wu, K, Xie, F, and Zane, S
Published: 2023

3. The X-ray polarisation of the Seyfert 1 galaxy IC 4329A

Author: Ingram, A., Ewing, M., Marinucci, A., Tagliacozzo, D., Rosario, D. J., Veledina, A., Kim, D. E., Marin, F., Bianchi, S., Poutanen, J., Matt, G., Marshall, H. L., Ursini, F., De Rosa, A., Petrucci, P-O., Madejski, G., Barnouin, T., Di Gesu, L., Dovvciak, M., Gianolli, V. E., Krawczynski, H., Loktev, V., Middei, R., Podgorny, J., Puccetti, S., Ratheesh, A., Soffitta, P., Tombesi, F., Ehlert, S. R., Massaro, F., Agudo, I., Antonelli, L. A., Bachetti, M., Baldini, L., Baumgartner, W. H., Bellazzini, R., Bongiorno, S. D., Bonino, R., Brez, A., Bucciantini, N., Capitanio, F., Castellano, S., Cavazzuti, E., Chen, C. -T., Ciprini, S., Costa, E., Del Monte, E., Di Lalla, N., Di Marco, A., Donnarumma, I., Doroshenko, V., Enoto, T., Evangelista, Y., Fabiani, S., Ferrazzoli, R., Garcia, J. A., Gunji, S., Heyl, J., Iwakiri, W., Jorstad, S. G., Kaaret, P., Karas, V., Kislat, F., Kitaguchi, T., Kolodziejczak, J. J., La Monaca, F., Latronico, L., Liodakis, I., Maldera, S., Manfreda, A., Marscher, A. P., Mitsuishi, I., Mizuno, T., Muleri, F., Negro, M., Ng, C. -Y., ODell, S. L., Omodei, N., Oppedisano, C., Papitto, A., Pavlov, G. G., Peirson, A. L., Perri, M., Pesce-Rollins, M., Pilia, M., Possenti, A., Ramsey, B. D., Rankin, J., Roberts, O. J., Romani, R. W., Sgro, C., Slane, P., Spandre, G., Swartz, D. A., Tamagawa, T., Tavecchio, F., Taverna, R., Tawara, Y., Tennant, A. F., Thomas, N. E., Trois, A., Tsygankov, S. S., Turolla, R., Vink, J., Weisskopf, M. C., Wu, K., Xie, F., and Zane, S.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present an X-ray spectro-polarimetric analysis of the bright Seyfert galaxy IC 4329A. The Imaging X-ray Polarimetry Explorer (IXPE) observed the source for ~500 ks, supported by XMM-Newton (~60 ks) and NuSTAR (~80 ks) exposures. We detect polarisation in the 2-8 keV band with 2.97 sigma confidence. We report a polarisation degree of $3.3\pm1.1$ per cent and a polarisation angle of $78\pm10$ degrees (errors are 1 sigma confidence). The X-ray polarisation is consistent with being aligned with the radio jet, albeit partially due to large uncertainties on the radio position angle. We jointly fit the spectra from the three observatories to constrain the presence of a relativistic reflection component. From this, we obtain constraints on the inclination angle to the inner disc (< 39 degrees at 99 per cent confidence) and the disc inner radius (< 11 gravitational radii at 99 per cent confidence), although we note that modelling systematics in practice add to the quoted statistical error. Our spectro-polarimetric modelling indicates that the 2-8 keV polarisation is consistent with being dominated by emission directly observed from the X-ray corona, but the polarisation of the reflection component is completely unconstrained. Our constraints on viewer inclination and polarisation degree tentatively favour more asymmetric, possibly out-flowing, coronal geometries that produce more highly polarised emission, but the coronal geometry is unconstrained at the 3 sigma level., Submitted to MNRAS, 12 pages, 7 figures
Published: 2023
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4. The geometry of the hot corona in MCG-05-23-16 constrained by X-ray polarimetry

Author: Tagliacozzo, D., Marinucci, A., Ursini, F., Matt, G., Bianchi, S., Baldini, L., Barnouin, T., Rodriguez, N. Cavero, De Rosa, A., Di Gesu, L., Dovciak, M., Harper, D., Ingram, A., Karas, V., Kim, D. E., Krawczynski, H., Madejski, G., Marin, F., Middei, R., Marshall, H. L., Muleri, F., Panagiotou, C., Petrucci, P. O., Podgorny, J., Poutanen, J., Puccetti, S., Soffitta, P., Tombesi, F., Veledina, A., Zhang, W., Agudo, I., Antonelli, L. A., Bachetti, M., Baumgartner, W. H., Bellazzini, R., Bongiorno, S. D., Bonino, R., Brez, A., Bucciantini, N., Capitanio, F., Castellano, S., Cavazzuti, E., Chen, C. T., Ciprini, S., Costa, E., Del Monte, E., Di Lalla, N., Di Marco, A., Donnarumma, I., Doroshenko, V., Ehlert, S. R., Enoto, T., Evangelista, Y., Fabiani, S., Ferrazzoli, R., Garcia, J. A., Gunji, S., Heyl, J., Iwakiri, W., Jorstad, S. G., Kaaret, P., Kislat, F., Kitaguchi, T., Kolodziejczak, J. J., La Monaca, F., Latronico, L., Liodakis, I., Maldera, S., Manfreda, A., Marscher, A. P., Massaro, F., Mitsuishi, I., Mizuno, T., Negro, M., Ng, C. Y., O'Dell, S. L., Omodei, N., Oppedisano, C., Papitto, A., Pavlov, G. G., Peirson, A. L., Perri, M., Rollins, M. Pesce, Pilia, M., Possenti, A., Ramsey, B. D., Rankin, J., Ratheesh, A., Roberts, O. J., Romani, R. W., Sgrò, C., Slane, P., Spandre, G., Swartz, D. A., Tamagawa, T., Tavecchio, F., Taverna, R., Tawara, Y., Tennant, A. F., Thomas, N. E., Trois, A., Tsygankov, S. S., Turolla, R., Vink, J., Weisskopf, M. C., Wu, K., Xie, F., and Zane, S.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the second observation of the radio-quiet active galactic nucleus (AGN) MCG-05-23-16 performed with the Imaging X-ray Polarimetry Explorer (IXPE). The observation started on 2022 November 6 for a net observing time of 640 ks, and was partly simultaneous with NuSTAR (86 ks). After combining these data with those obtained in the first IXPE pointing on May 2022 (simultaneous with XMM-Newton and NuSTAR) we find a 2-8 keV polarization degree $\Pi$ = 1.6 $\pm$ 0.7 (at 68 per cent confidence level), which corresponds to an upper limit $\Pi$ = 3.2 per cent (at 99 per cent confidence level). We then compare the polarization results with Monte Carlo simulations obtained with the MONK code, with which different coronal geometries have been explored (spherical lamppost, conical, slab and wedge). Furthermore, the allowed range of inclination angles is found for each geometry. If the best fit inclination value from a spectroscopic analysis is considered, a cone-shaped corona along the disc axis is disfavoured., Comment: 9 pages, 8 figures, 3 table. Submitted to MNRAS
Published: 2023
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5. IXPE observations of the quintessential wind-accreting X-ray pulsar Vela X-1

Author: Forsblom, Sv, Poutanen, J, Tsygankov, Ss, Bachetti, M, Marco, Ad, Doroshenko, V, Heyl, J, Monaca, Fl, Malacaria, C, Marshall, Hl, Muleri, F, Mushtukov, Aa, Pilia, M, Rogantini, D, Suleimanov, Vf, Taverna, R, Xie, F, Agudo, I, Antonelli, La, Baldini, L, Baumgartner, Wh, Bellazzini, R, Bianchi, S, Bongiorno, Sd, Bonino, R, Brez, A, Bucciantini, N, Capitanio, F, Castellano, S, Cavazzuti, E, Chen, Ct, Ciprini, S, Costa, E, De Rosa, A, Del Monte, E, Di Gesu, L, Di Lalla, N, Donnarumma, I, Dovciak, M, Ehlert, Sr, Enoto, T, Evangelista, Y, Fabiani, S, Ferrazzoli, R, Garcia, Ja, Gunji, S, Hayashida, K, Iwakiri, W, Jorstad, Sg, Kaaret, P, Karas, V, Kitaguchi, T, Kolodziejczak, Jj, Krawczynski, H, Latronico, L, Liodakis, I, Maldera, S, Manfreda, A, Marin, F, Marinucci, A, Marscher, Ap, Matt, G, Mitsuishi, I, Mizuno, T, Negro, M, Cy, Ng, O'Dell, Sl, Omodei, N, Oppedisano, C, Papitto, A, Pavlov, Gg, Peirson, Al, Perri, M, Pesce-Rollins, M, Petrucci, Po, Possenti, A, Puccetti, S, Ramsey, Bd, Rankin, J, Ratheesh, A, Roberts, Oj, Romani, Rw, Sgro, C, Slane, P, Soffitta, P, Spandre, G, Sunyaev, Ra, Swartz, Da, Tamagawa, T, Tavecchio, F, Tawara, Y, Tennant, Af, Thomas, Ne, Tombesi, F, Trois, A, Turolla, R, Vink, J, Weisskopf, Mc, Kw, Wu, Zane, S, Ixpe, Collaboration, Ministerio de Ciencia e Innovación (España), Academy of Finland, German Research Foundation, Forsblom, Sofia V., Poutanen, Juri, Tsygankov, Sergey S., Bachetti, Matteo, Marco, Alessandro Di, Doroshenko, Victor, Heyl, Jeremy, Monaca, Fabio La, Malacaria, Christian, Marshall, Herman L., Muleri, Fabio, Mushtukov, Alexander A., Pilia, Maura, Rogantini, Daniele, Suleimanov, Valery F., Taverna, Roberto, Xie, Fei, Agudo, Iván, Antonelli, Lucio A., Baldini, Luca, Baumgartner, Wayne H., Bellazzini, Ronaldo, Bianchi, Stefano, Bongiorno, Stephen D., Bonino, Raffaella, Brez, Alessandro, Bucciantini, Niccolò, Capitanio, Fiamma, Castellano, Simone, Cavazzuti, Elisabetta, Chen, Chien-Ting, Ciprini, Stefano, Costa, Enrico, De Rosa, Alessandra, Del Monte, Ettore, Di Gesu, Laura, Di Lalla, Niccolò, Donnarumma, Immacolata, Dovčiak, Michal, Ehlert, Steven R., Enoto, Teruaki, Evangelista, Yuri, Fabiani, Sergio, Ferrazzoli, Riccardo, Garcia, Javier A., Gunji, Shuichi, Hayashida, Kiyoshi, Iwakiri, Wataru, Jorstad, Svetlana G., Kaaret, Philip, Karas, Vladimir, Kitaguchi, Takao, Kolodziejczak, Jeffery J., Krawczynski, Henric, Latronico, Luca, Liodakis, Ioanni, Maldera, Simone, Manfreda, Alberto, Marin, Frédéric, Marinucci, Andrea, Marscher, Alan P., Matt, Giorgio, Mitsuishi, Ikuyuki, Mizuno, Tsunefumi, Negro, Michela, Ng, Chi-Yung, O’Dell, Stephen L., Omodei, Nicola, Oppedisano, Chiara, Papitto, Alessandro, Pavlov, George G., Peirson, Abel L., Perri, Matteo, Pesce-Rollins, Melissa, Petrucci, Pierre-Olivier, Possenti, Andrea, Puccetti, Simonetta, Ramsey, Brian D., Rankin, John, Ratheesh, Ajay, Roberts, Oliver J., Romani, Roger W., Sgrò, Carmelo, Slane, Patrick, Soffitta, Paolo, Spandre, Gloria, Sunyaev, Rashid A., Swartz, Douglas A., Tamagawa, Toru, Tavecchio, Fabrizio, Tawara, Yuzuru, Tennant, Allyn F., Thomas, Nicholas E., Tombesi, Francesco, Trois, Alessio, Turolla, Roberto, Vink, Jacco, Weisskopf, Martin C., Wu, Kinwah, and Zane, Silvia
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Full list of authors: Forsblom, Sofia; Poutanen, Juri S.; Tsygankov, Sergey; Bachetti, Matteo; Marco, Alessandro Di; Doroshenko, Victor; Heyl, Jeremy; Monaca, Fabio La; Malacaria, Christian L.; Marshall, Herman; Muleri, Fabio A.; Mushtukov, Alexander; Pilia, Maura; Rogantini, Daniele F.; Suleimanov, Valery; Taverna, Roberto; Xie, Fei; Agudo, Ivan A.; Antonelli, Lucio; Baldini, Luca H.; Baumgartner, Wayne; Bellazzini, Ronaldo; Bianchi, Stefano D.; Bongiorno, Stephen; Bonino, Raffaella; Brez, Alessandro; Bucciantini, Niccolo; Capitanio, Fiamma; Castellano, Simone; Cavazzuti, Elisabetta; Chen, Chien-Ting; Ciprini, Stefano; Costa, Enrico; De Rosa, Alessandra; Del Monte, Ettore; Di Gesu, Laura; Di Lalla, Niccolo; Donnarumma, Immacolata; Dovciak, Michal R.; Ehlert, Steven; Enoto, Teruaki; Evangelista, Yuri; Fabiani, Sergio; Ferrazzoli, Riccardo A.; Garcia, Javier; Gunji, Shuichi; Hayashida, Kiyoshi; Iwakiri, Wataru G.; Jorstad, Svetlana; Kaaret, Philip; Karas, Vladimir; Kitaguchi, Takao J.; Kolodziejczak, Jeffery; Krawczynski, Henric; Latronico, Luca; Liodakis, Ioannis; Maldera, Simone; Manfreda, Alberto; Marin, Frederic; Marinucci, Andrea P.; Marscher, Alan; Matt, Giorgio; Mitsuishi, Ikuyuki; Mizuno, Tsunefumi; Negro, Michela; Ng, Chi-Yung L.; O'Dell, Stephen; Omodei, Nicola; Oppedisano, Chiara; Papitto, Alessandro G.; Pavlov, George L.; Peirson, Abel; Perri, Matteo; Pesce-Rollins, Melissa; Petrucci, Pierre-Olivier; Possenti, Andrea; Puccetti, Simonetta D.; Ramsey, Brian; Rankin, John; Ratheesh, Ajay J.; Roberts, Oliver W.; Romani, Roger; Sgro, Carmelo; Slane, Patrick; Soffitta, Paolo; Spandre, Gloria A.; Sunyaev, Rashid A.; Swartz, Douglas; Tamagawa, Toru; Tavecchio, Fabrizio; Tawara, Yuzuru F.; Tennant, Allyn E.; Thomas, Nicholas; Tombesi, Francesco; Trois, Alessio; Turolla, Roberto; Vink, Jacco C.; Weisskopf, Martin; Wu, Kinwah; Zane, Silvia; IXPE Collaboration.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., The radiation from accreting X-ray pulsars was expected to be highly polarized, with some estimates for the polarization degree of up to 80%. However, phase-resolved and energy-resolved polarimetry of X-ray pulsars is required in order to test different models and to shed light on the emission processes and the geometry of the emission region. Here we present the first results of the observations of the accreting X-ray pulsar Vela X-1 performed with the Imaging X-ray Polarimetry Explorer. Vela X-1 is considered to be the archetypal example of a wind-accreting, high-mass X-ray binary system, consisting of a highly magnetized neutron star accreting matter from its supergiant stellar companion. The spectropolarimetric analysis of the phase-averaged data for Vela X-1 reveals a polarization degree (PD) of 2.3% ± 0.4% at the polarization angle (PA) of −47fdg3 ± 5fdg4. A low PD is consistent with the results obtained for other X-ray pulsars and is likely related to the inverse temperature structure of the neutron star atmosphere. The energy-resolved analysis shows the PD above 5 keV reaching 6%–10% and a ∼90° difference in the PA compared to the data in the 2–3 keV range. The phase-resolved spectropolarimetric analysis finds a PD in the range 0%–9% with the PA varying between −80° and 40°. © 2023. The Author(s). Published by the American Astronomical Society., The Imaging X-ray Polarimetry Explorer (IXPE) is a joint US and Italian mission. The US contribution is supported by the National Aeronautics and Space Administration (NASA) and led and managed by its Marshall Space Flight Center (MSFC), with industry partner Ball Aerospace (contract NNM15AA18C). The Italian contribution is supported by the Italian Space Agency (Agenzia Spaziale Italiana, ASI) through contract ASI-OHBI-2017-12-I.0, agreements ASI-INAF-2017-12-H0 and ASI-INFN-2017.13-H0, and its Space Science Data Center (SSDC) with agreements ASI-INAF-2022-14-HH.0 and ASI-INFN 2021-43-HH.0, and by the Istituto Nazionale di Astrofisica (INAF) and the Istituto Nazionale di Fisica Nucleare (INFN) in Italy. This research used data products provided by the IXPE Team (MSFC, SSDC, INAF, and INFN) and distributed with additional software tools by the High-Energy Astrophysics Science Archive Research Center (HEASARC), at NASA Goddard Space Flight Center (GSFC). We acknowledge support from the RSF grant 19-12-00423 (SST), the Academy of Finland grants 333112, 349144, 349373, and 349906 (JP, SST), the German Academic Exchange Service (DAAD) travel grant 57525212 (VD, VFS), and the German Research Foundation (DFG) grant WE 1312/53-1 (VFS)., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).
Published: 2023
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6. WIDE-BANDSUZAKUANALYSIS OF THE PERSISTENT EMISSION FROM SGR 0501+4516 DURING THE 2008 OUTBURST

Author: Rea, N., Esposito, P., Gotz, D., Hurley, K., Israel, G. L., Mereghetti, S., Stella, L., Tiengo, A., Turolla, R., Zane, S., Enoto, T., Nakagawa, Y. E., Makishima, K., Sakamoto, T., Kokubun, Motohide, Murakami, H., Nakazawa, K., Yamada, S., Yamaoka, K., and Yoshida, A.
Subjects: Physics, Spectrometer, Pulsar, Space and Planetary Science, Soft gamma repeater, Imaging spectrometer, Astronomy, Flux, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Magnetar, Spectral line
Abstract: 著者人数: 20名, Accepted: 2010-04-09, 資料番号: SA1002850000
Published: 2010

7. X-ray spectra from magnetar candidates - III. Fitting SGR/AXP soft X-ray emission with non-relativistic Monte Carlo models

Author: Turolla, R., Zane, S., Nobili, L., Rea, N., and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Soft x ray, Photon, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, FOS: Physical sciences, Magnetosphere, Astronomy and Astrophysics, Astrophysics, Magnetar, Astrophysics - Astrophysics of Galaxies, Spectral line, Pulsar, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Thermal, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Within the magnetar scenario, the "twisted magnetosphere" model appears very promising in explaining the persistent X-ray emission from the Soft Gamma Repeaters and the Anomalous X-ray Pulsars (SGRs and AXPs). In the first two papers of the series, we have presented a 3D Monte Carlo code for solving radiation transport as soft, thermal photons emitted by the star surface are resonantly upscattered by the magnetospheric particles. A spectral model archive has been generated and implemented in XSPEC. Here we report on the systematic application of our spectral model to different XMM-Newton and Integral observations of SGRs and AXPs. We find that the synthetic spectra provide a very good fit to the data for the nearly all the source (and source states) we have analyzed., 13 Pages, 7 Figures, 4 Tables, accepted for publication in MNRAS
Published: 2009

8. Unifying neutron stars: getting to GUNS

Author: Igoshev, A. P., Sergei Popov, and Turolla, R.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Pulsars: general, Space and Planetary Science, Magnetic fields, Astrophysics::High Energy Astrophysical Phenomena, Stars: neutron, Astronomy and Astrophysics, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The variety of the observational appearance of young isolated neutron stars must find an explanation in the framework of some unifying approach. Nowadays it is believed that such scenario must include magnetic field decay, the possibility of magnetic field emergence on a time scale $\lesssim 10^4$--$10^5$ yrs, significant contribution of non-dipolar fields, and appropriate initial parameter distributions. We present our results on the initial spin period distribution, and suggest that inconsistences between distributions derived by different methods for samples with different average ages can uncover field decay or/and emerging field. We describe a new method to probe the magnetic field decay in normal pulsars. The method is a modified pulsar current approach, where we study pulsar flow along the line of increasing characteristic age for constant field. Our calculations, performed with this method, can be fitted with an exponential decay for ages in the range $8\times 10^4$--$3.5 \times 10^5$ yrs with a time scale $\sim 5 \times 10^5$ yrs. We discuss several issues related to the unifying scenario. At first, we note that the dichotomy, among local thermally emitting neutron stars, between normal pulsars and the Magnificent Seven remains unexplained. Then we discuss the role of high-mass X-ray binaries in the unification of neutron star evolution. We note, that such systems allow to check evolutionary effects on a time scale longer than what can be probed with normal pulsars alone. We conclude with a brief discussion of importance of discovering old neutron stars accreting from the interstellar medium., Comment: 6 pages, submitted to AN, proceedings of the workshop "The Fast and the Furious: Energetic Phenomena in Isolated Neutron Stars, Pulsar Wind Nebulae and Supernova Remnants" ESAC, Madrid, Spain 22nd - 24th May 2013
Published: 2013
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9. A study of the long term variability of RX J1856.5-3754 with XMM-Newton

Author: Mereghetti, S., Sartore, N., Tiengo, A., Andrea De Luca, Turolla, R., and Haberl, F.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on a detailed spectral analysis of all the available XMM-Newton data of RX J1856.5-3754, the brightest and most extensively observed nearby, thermally emitting neutron star. Very small variations (~1-2%) in the single-blackbody temperature are detected, but are probably due to an instrumental effect, since they correlate with the position of the source on the detector. Restricting the analysis to a homogeneous subset of observations, with the source at the same detector position, we place strong limits on possible spectral or flux variations from March 2005 to present-day. A slightly higher temperature (kT~61.5 eV, compared to the average value kT~61 eV) was instead measured in April 2002. If this difference is not of instrumental origin, it implies a rate of variation of about 0.15 eV/yr between April 2002 and March 2005. The high-statistics spectrum from the selected observations is well fit by the sum of two blackbody models, which extrapolate to an optical flux level in agreement with the observed value., Comment: 4 pages, to appear in the proceedings of the ERPM conference, Zielona Gora, April 2012
Published: 2012
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10. SXP 1062: an Evolved Magnetar in a BeXB ?

Author: Turolla, R. and Popov, S. B.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: SXP 1062, a newly discovered Be/X-ray binary in the Small Magellanic Cloud, provides the first example of a robust association with a supernova remnant (SNR). The short age estimated for the SNR qualifies SXP 1062 as the youngest known source in its class, ~ 10^4 yr. Here we discuss possible evolutionary scenarios for SXP 1062 in the attempt to reconcile its long spin period, P=1062 s, and short age. Our results indicate that SXP 1062 may host a neutron star born with a large initial magnetic field, typically in excess of ~ 10^14 G, which then decayed to ~ 10^13 G., Comment: 4 pages, to appear in the proceedings of the ERPM conference, Zielona Gora, April 2012
Published: 2012
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11. The log N-log S distributions of accreting and cooling isolated neutron stars

Author: Sergei Popov, Colpi, M., Prokhorov, Me, Treves, A., Turolla, R., Popov, S, Colpi, M, Prokhorov, M, Treves, A, and Turolla, R
Subjects: stars : kinematic, X-rays : stars, stars : magnetic field, accretion, accretion disk, stars : neutron, stars : statistic
Abstract: We model populations of isolated neutron stars in the Galaxy following their orbital and magnetorotational evolution. It is shown that accretors become more abundant than coolers at fluxes below similar to 10(-13) ergs cm(-2) s(-1), and one can predict that about one accreting neutron star per square degree should be observed at the Chandra and Newton flux limits of similar to 10(-16) ergs cm(-2) s(-1). The soft ROSAT sources associated with isolated neutron stars can be relatively young cooling objects only if the neutron star birthrate in the solar vicinity during the last similar to 10(6) yr is higher than that inferred from radio pulsar observations.
Published: 2000

12. The first observation of optical pulsations from a soft gamma repeater: SGR 0501+4516

Author: Dhillon, V. S., Marsh, T. R., Littlefair, S. P., Copperwheat, C. M., Hickman, R. D. G., Kerry, P., Levan, A. J., Rea, N., Savoury, C. D. J., Tanvir, N. R., Turolla, R., and Wiersema, K.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We present high-speed optical photometry of the soft gamma repeater SGR 0501+4516, obtained with ULTRACAM on two consecutive nights approximately 4 months after the source was discovered via its gamma-ray bursts. We detect SGR 0501+4516 at a magnitude of i' = 24.4+/-0.1. We present the first measurement of optical pulsations from an SGR, deriving a period of 5.7622+/-0.0003 s, in excellent agreement with the X-ray spin period of the neutron star. We compare the morphologies of the optical pulse profile with the X-ray and infrared pulse profiles; we find that the optical, infrared and harder X-rays share similar double-peaked morphologies, but the softer X-rays exhibit only a single-peaked morphology, indicative of a different origin. The optical pulsations appear to be in phase with the X-ray pulsations and exhibit a root-mean-square pulsed fraction of 52+/-7%, approximately a factor of two greater than in the X-rays. Our results find a natural explanation within the context of the magnetar model for SGRs., Comment: 5 pages, 3 figures, accepted for publication in MNRAS Letters
Published: 2011
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13. A time-variable, phase-dependent emission line in the X-ray spectrum of the isolated neutron star RX J0822-4300

Author: De Luca, A., Salvetti, D., Sartori, A., Esposito, P., Tiengo, A., Zane, S., Turolla, R., Pizzolato, F., Mignani, R. P., Caraveo, P. A., Mereghetti, S., and Bignami, G. F.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: RX J0822-4300 is the Central Compact Object associated with the Puppis A supernova remnant. Previous X-ray observations suggested RX J0822-4300 to be a young neutron star with a weak dipole field and a peculiar surface temperature distribution dominated by two antipodal spots with different temperatures and sizes. An emission line at 0.8 keV was also detected. We performed a very deep (130 ks) observation with XMM-Newton, which allowed us to study in detail the phase-resolved properties of RX J0822-4300. Our new data confirm the existence of a narrow spectral feature, best modelled as an emission line, only seen in the `Soft' phase interval - when the cooler region is best aligned to the line of sight. Surprisingly, comparison of our recent observations to the older ones yields evidence for a variation in the emission line component, which can be modelled as a decrease in the central energy from ~0.80 keV in 2001 to ~0.73 keV in 2009--2010. The line could be generated via cyclotron scattering of thermal photons in an optically thin layer of gas, or - alternatively - it could originate in low-rate accretion by a debris disk. In any case, a variation in energy, pointing to a variation of the magnetic field in the line emitting region, cannot be easily accounted for., Comment: Accepted for publication in MNRAS Letters. 5 pages, 4 figures
Published: 2011
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14. Long-term spectral and timing properties of the soft gamma-ray repeater SGR 1833-0832 and detection of extended X-ray emission around the radio pulsar PSR B1830-08

Author: Esposito, P., Israel, G. L., Turolla, R., Mattana, F., Tiengo, A., Possenti, A., Zane, S., Rea, N., Burgay, M., Götz, D., Mereghetti, S., Stella, L., Wieringa, M. H., Sarkissian, J. M., Enoto, T., Romano, P., Sakamoto, T., Nakagawa, Y. E., Makishima, K., Nakazawa, K., Nishioka, H., and François-Martin, C.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: SGR 1833-0832 was discovered on 2010 March 19 thanks to the Swift detection of a short hard X-ray burst and follow-up X-ray observations. Since then, it was repeatedly observed with Swift, Rossi X-ray Timing Explorer, and XMM-Newton. Using these data, which span about 225 days, we studied the long-term spectral and timing characteristics of SGR 1833-0832. We found evidence for diffuse emission surrounding SGR 1833-0832, which is most likely a halo produced by the scattering of the point source X-ray radiation by dust along the line of sight, and we show that the source X-ray spectrum is well described by an absorbed blackbody, with temperature kT=1.2 keV and absorbing column nH=(10.4+/-0.2)E22 cm^-2, while different or more complex models are disfavoured. The source persistent X-ray emission remained fairly constant at about 3.7E-12 erg/cm^2/s for the first 20 days after the onset of the bursting episode, then it faded by a factor 40 in the subsequent 140 days, following a power-law trend with index alpha=-0.5. We obtained a phase-coherent timing solution with the longest baseline (225 days) to date for this source which, besides period P=7.5654084(4) s and period derivative dP/dt=3.5(3)E-12 s/s, includes higher order period derivatives. We also report on our search of the counterpart to the SGR at radio frequencies using the Australia Telescope Compact Array and the Parkes radio telescope. No evidence for radio emission was found, down to flux densities of 0.9 mJy (at 1.5 GHz) and 0.09 mJy (at 1.4 GHz) for the continuum and pulsed emissions, respectively, consistently with other observations at different epochs., Comment: 12 pages, 7 colour figures and 3 tables, accepted for publication in MNRAS. Figure 6 in reduced quality and abstract abridged for astro-ph submission
Published: 2011
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15. Probing the neutron star spin evolution in the young SMC Be/X-ray binary SXP 1062

Author: Popov, S. B. and Turolla, R.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: The newly discovered Be/X-ray binary in the Small Magellanic Cloud, SXP 1062, provides the first example of a robust association with a supernova remnant (SNR). The short age estimated for the SNR qualifies SXP 1062 as the youngest known source in its class, tau ~ 1e4 yr. As such, it allows to test current models of magneto-rotational evolution of neutron stars ina still unexplored regime. Here we discuss possible evolutionary scenarios for SXP 1062 in the attempt to reconcile its long spin period, P=1062 s, and short age. Although several options can be considered, like an anomalously long initial period or the presence of a fossil disc, our results indicate that SXP 1062 may host a neutron star born with a large initial magnetic field, typically in excess of ~ 1e14 G, which then decayed to ~ 1e13 G., Comment: 5 pages, 1 figure, modified to incorporate referee's points, accepted for publication in MNRAS
Published: 2011
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16. Discovery of 59ms Pulsations from 1RXS J141256.0+792204 (Calvera)

Author: Zane, S., Haberl, F., Israel, G. L., Pellizzoni, A., Burgay, M., Mignani, R. P., Turolla, R., Possenti, A., Esposito, P., Champion, D., Eatough, R. P., Barr, E., and Kramer, M.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on a multi-wavelength study of the compact object candidate 1RXS J141256.0+792204 (Calvera). Calvera was observed in the X-rays with XMM/EPIC twice for a total exposure time of ~50 ks. The source spectrum is thermal and well reproduced by a two component model composed of either two hydrogen atmosphere models, or two blackbodies (kT_1~ 55/150 eV, kT_2~ 80/250 eV, respectively, as measured at infinity). Evidence was found for an absorption feature at ~0.65 keV; no power-law high-energy tail is statistically required. Using pn and MOS data we discovered pulsations in the X-ray emission at a period P=59.2 ms. The detection is highly significant (> 11 sigma), and unambiguously confirms the neutron star nature of Calvera. The pulse profile is nearly sinusoidal, with a pulsed fraction of ~18%. We looked for the timing signature of Calvera in the Fermi Large Area Telescope (LAT) database and found a significant (~5 sigma) pulsed signal at a period coincident with the X-ray value. The gamma-ray timing analysis yielded a tight upper limit on the period derivative, dP/dt < 5E-18 s/s (dE_rot/dt, 20 pages, 15 figures and 4 tables. Accepted for publication in MNRAS
Published: 2010
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17. From outburst to quiescence: the decay of the transient Anomalous X-ray Pulsar XTE J1810-197

Author: Bernardini, F., Israel, G. L., Dall'Osso, S., Stella, L., Rea, N., Zane, S., Turolla, R., Perna, R., Falanga, M., Campana, S., Götz, D., Mereghetti, S., and Tiengo, A.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: XTE J1810-197 is the first transient Anomalous X-ray Pulsar ever discovered. Its highly variable X-ray flux allowed us to study the timing and spectral emission properties of a magnetar candidate over a flux range of about two orders of magnitude. We analyzed nine XMM-Newton observations of XTE J1810-197 collected over a four years baseline (September 2003 - September 2007). EPIC PN and MOS data were reduced and used for detailed timing and spectral analysis. Pulse phase spectroscopic studies were also carried out for observations with sufficiently high signal to noise. We find that: (i) a three blackbodies model reproduces the spectral properties of the source over the entire outburst statistically better than the two blackbodies model previously used in the literature, (ii) the coldest blackbody is consistent with the thermal emission from the whole surface, and has temperature and radius similar to those inferred from ROSAT observations before the outburst onset, (iii) there is a spectral feature around 1.1 keV during six consecutive observations (since March 2005); if due to proton resonant cyclotron scattering, it would imply a magnetic field of around 2E14 G. This is in a very good agreement with the value from the spin period measurements., Comment: 16 pages, 11 figures, accepted for publication on A&A on 10/1/2009
Published: 2009
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18. Observations of Isolated Neutron Stars with the ESO Multi-Conjugate Adaptive Optics Demonstrator

Author: Mignani, R. P., Falomo, R., Moretti, A., Treves, A., Turolla, R., Sartore, N., Zane, S., Arcidiacono, C., Lombini, M., Farinato, J., Baruffolo, A., Ragazzoni, R., and Marchetti, E.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: High-energy observations have unveiled peculiar classes of isolated neutron stars which, at variance with radio pulsars, are mostly radio silent and not powered by the star rotation. Among these objects are the magnetars, hyper-magnetized neutron stars characterized by transient X-ray/gamma-ray emission, and neutron stars with purely thermal, and in most cases stationary, X-ray emission (a.k.a., X-ray dim isolated neutron stars or XDINSs). While apparently dissimilar in their high-energy behavior and age, both magnetars and XDINSs have similar periods and unusually high magnetic fields. This suggests a tantalizing scenario where the former evolve into the latter.Discovering so far uninvestigated similarities between the multi-wavelength properties of these two classes would be a further step forward to establish an evolutionary scenario. A most promising channels is the near infrared (NIR) one, where magnetars are characterized by a distinctive spectral flattening with respect to the extrapolation of the soft X-ray spectrum.We observed the two XDINSs RX J0420.0-5022 and RX J1856.5-3754 with the Multi-Conjugate Adaptive Optics Demonstrator (MAD) at the Very Large Telescope (VLT) as part of the instrument guaranteed time observations program, to search for their NIR counterparts. Both RX J1856.5-3754 and RX J0420.0-5022 were not detected down to K_s ~20 and Ks ~21.5, respectively. In order to constrain the relation between XDINSs and magnetars it would be of importance to perform deeper NIR observations. A good candidate is 1RXS J214303.7+065419 which is the XDINS with the highest inferred magnetic field., Comment: Accepted for publication in Astronomy and Astrophysics
Published: 2008
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19. X-ray Spectra from Magnetar Candidates. I. Monte Carlo Simulations in the Non-relativistic Regime

Author: Nobili, L., Zane, S., and Turolla, R.
Subjects: Physics, Photon, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, Astrophysics (astro-ph), Magnetosphere, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Rest frame, Magnetar, Spectral line, Neutron star, Pulsar, Space and Planetary Science
Abstract: The anomalous X-ray pulsars and soft gamma-repeaters are peculiar high-energy sources believed to host a magnetar, i.e. an ultra-magnetized neutron star. Their persistent, soft X-ray emission (~1-10 keV)is usually modeled by the superposition of a blackbody and a power-law tail. It has been suggested that this spectrum forms as the thermal photons emitted by the star surface traverse the magnetosphere. Magnetar magnetospheres are likely different from those of ordinary radio-pulsars, since the external magnetic field may acquire a toroidal component as a consequence of the deformation of the star crust induced by the super-strong interior field. In turn, the magnetosphere will be permeated by currents that can boost primary photons through repeated scatterings. Here we present 3D Monte Carlo simulations of photon propagation in a twisted magnetosphere. Our model is based on a simplified treatment of the charge carriers velocity distribution which, however, accounts for the particle collective motion, in addition to the thermal one. Present treatment is restricted to conservative (Thomson) scattering in the electron rest frame. The code, nonetheless, is completely general and inclusion of the relativistic QED resonant cross section, which is required in the modeling of the hard (~20-200 keV) spectral tails observed in the magnetar candidates, is under way. The properties of emerging spectra have been assessed under different conditions, by exploring the model parameter space, including effects arising from the viewing geometry. Monte Carlo runs have been collected into a spectral archive. Two tabulated XSPEC spectral models, with and without viewing angles, have been produced and applied to the 0.1-10 keV XMM-Newton EPIC-pn spectrum of the AXP CXOU J1647-4552., Comment: 37 pages, 14 figures, 1 table; corrected typos; accepted for publication in MNRAS
Published: 2008

20. Evidence for precession of the isolated Netron star RX J0720.4-3125

Author: Haberl, F., Turolla, R., de Vries, C.P., Zane, S., Vink, J., Mendez, M., Verbunt, F.W.M., Astrophysics, and Dep Natuurkunde
Abstract: The XMM-Newton spectra of the isolated neutron star RXJ0720.4−3125 obtained over 4.5 years can be described by sinusoidal variations in the inferred blackbody temperature, the size of the emitting area and the depth of the absorption line with a period of 7.1 ± 0.5 years, which we suggest to be the precession period of the neutron star. Precession of a neutron star with two hot spots of different temperature and size, probably not located exactly in antipodal positions, may account for the variations in the X-ray spectra, changes in the pulsed fraction, shape of the light curve and the phase-lag between soft and hard energy bands observed from RXJ0720.4−3125. An independent sinusoidal fit to published and new pulse timing residuals from a coherent analysis covering ∼12 years yields a consistent period of 7.7 ± 0.6 years supporting the precession model.
Published: 2006

21. Intensity-hardness correlation and deep infrared observation of the anomalous X-ray pulsar 1RXS J170849-400910

Author: Rea, N., Israel, G. L., Oosterbroek, T., Campana, S., Zane, S., Turolla, R., Testa, V., Mendez, M., and Stella, L.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We report here on X-ray and IR observations of the Anomalous X-ray Pulsar 1RXS J170849-400910. First, we report on new XMM-Newton, Swift-XRT and Chandra observations of this AXP, which confirm the intensity-hardness correlation observed in the long term X-ray monitoring of this source by Rea et al. (2005). These new X-ray observations show that the AXP flux is rising again, and the spectrum hardening. If the increase in the source intensity is indeed connected with the glitches and a possible bursting activity, we expect this source to enter in a bursting active phase around 2006-2007. Second, we report on deep IR observations of 1RXS J170849-400910, taken with the VLT-NACO adaptive optics, showing that there are many weak sources consistent with the AXP position. Neither star A or B, previously proposed by different authors, might yet be conclusively recognised as the IR counterpart of 1RXS J170849-400910. Third, using Monte Carlo simulations, we re-address the calculation of the significance of the absorption line found in a phase-resolved spectrum of this source by Rea et al. (2003), and interpreted as a resonant scattering cyclotron feature., Comment: 7 pages, 5 color figures; Astrophysics & Space Science, in press ("Isolated Neutron Stars"; London, UK)
Published: 2006
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22. Young close isolated compact objects

Author: Popov, S. B., Prokhorov, M. E., Colpi, M., Treves, A., and Turolla, R.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We suggest that the seven radio-quiet isolated neutron stars observed with ROSAT are young cooling objects associated to recent near-by supernova explosions which formed runaway stars and the Local Bubble, affecting the topology of the interstellar medium in the vicinity of the Sun (within a few hundred parsecs). In the aftermath of these explosions, a few black holes might have been formed, according to the local initial mass function. We thus discuss the possibility of determining approximate positions of close-by isolated black holes using data on runaway stars and simple calculations of binary evolution and disruption., Comment: 4 pages, no figures, to appear in proceedings of the conference ICGA-V in Gravitation & Cosmology (2002)
Published: 2002
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23. Isolated Neutron Stars in the Galaxy

Author: Popov, S. B., Prokhorov, M. E., Colpi, M., Treves, A., Turolla, R., and Lipunov, V. M.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: In this article we briefly review our recent results on evolution and properties of isolated neutron stars (INSs) in the Galaxy. As the first step we calculate a {\it census} of INSs in our Galaxy. We infer a lower bound for the mean kick velocity of NSs, $ \sim $(200-300) ${\rm km s^{-1}}$. The same conclusion is reached for both a constant magnetic field ($B\sim 10^{12}$ G) and for a magnetic field decaying exponentially with a timescale $\sim 10^9$ yr. These results, moreover, constrain the fraction of low velocity stars, which could have escaped pulsar statistics, to $\sim$few percents. Then we show that the range of minimum value of magnetic moment, $\mu_b$: $\sim 10^{29.5}\ge \mu_b \ge 10^{28} {\rm G} {\rm cm}^3$, and the characteristic decay time, $t_d$: $\sim 10^8\ge t_d \ge 10^7 {\rm yrs}$, can be excluded assuming the standard initial magnetic momentum, $\mu_0=10^{30} {\rm G} {\rm cm}^3$, if accreting INSs are observed. For these parameters an INS would never reach the stage of accretion from the interstellar medium even for a low space velocity of the star and high density of the ambient plasma. The range of excluded parameters increases for lower values of $\mu_0$. It is shown that old accreting INSs become more abundant than young cooling INSs at X-ray fluxes below $\sim 10^{-13}$ erg cm$^{-2}$ s$^{-1}$. We can predict that about one accreting INS per square degree should be observed at the {\it Chandra} and {\it Newton} flux limits of $\sim 10^{-16}$ erg cm$^{-2}$ s$^{-1}.$ The weak {\it ROSAT} sources, associated with INSs, can be young cooling objects, if the NSs birth rate in the solar vicinity during the last $\sim 10^6$ yr was much higher than inferred from radiopulsar observations., Comment: 7 pages, 3 PostScript figures, to be presented at the conference "Hot points in astrophysics", Dubna, August 22-26, 2000
Published: 2000
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24. The neutron star census

Author: Colpi, M., Lipunov, V. M., Sergei Popov, Prokhorov, M. E., Treves, A., and Turolla, R.
Published: 2000

25. Log N -- Log S distributions of accreting and cooling isolated neutron stars

Author: Popov, S. B., Colpi, M., Prokhorov, M. E., Treves, A., and Turolla, R.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We model populations of isolated neutron stars in the Galaxy following their orbital and magneto-rotational evolution. It is shown that accretors become more abundant than coolers at fluxes below $\sim 10^{-13}$ erg cm$^{-2}$ s$^{-1},$ and one can predict that about one accreting neutron star per square degree should be observed at the {\it Chandra} and {\it Newton} flux limits of $\sim 10^{-16}$ erg cm$^{-2}$ s$^{-1}.$ The soft ROSAT sources associated with isolated neutron stars can be relatively young cooling objects only if the neutron star birth rate in the Solar vicinity during the last $\sim 10^6$ yr is higher than that inferred from radiopulsar observations., Comment: 5 pages, 3 PostScript figures, accepted to ApJ, new figures 2,3
Published: 2000
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26. X--ray Emission from Old, Isolated, Accreting Neutron Stars

Author: Turolla, R.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: Accretion onto old, isolated neutron stars is reviewed. The detection of their X--ray emission with ROSAT is discussed and a summary of the current status of observations is presented., Comment: 5 pages, uses scprol.sty (included). Talk presented at the 2nd Sakharov Conference on Physics, Moscow May 20-25, 1996. To appear in the Proceedings
Published: 1996
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27. Science with e-ASTROGAM

Author: Angelis, A., Tatischeff, V., Grenier, I. A., Mcenery, J., Mallamaci, M., Tavani, M., Oberlack, U., Hanlon, L., Walter, R., Argan, A., Ballmoos, P., Bulgarelli, A., Bykov, A., Hernanz, M., Kanbach, G., Kuvvetli, I., Pearce, M., Zdziarski, A., Conrad, J., Ghisellini, G., Harding, A., Isern, J., Leising, M., Longo, F., Madejski, G., Martinez, M., Mazziotta, M. N., Paredes, J. M., Pohl, M., Rando, R., Razzano, M., Aboudan, A., Ackermann, M., Addazi, A., Ajello, M., Albertus, C., Alvarez, J. M., Ambrosi, G., Anton, S., Antonelli, L. A., Babic, A., Baibussinov, B., Balbo, M., Baldini, L., Balman, S., Bambi, C., Barres Almeida, U., Barrio, J. A., Bartels, R., Bastieri, D., Bednarek, W., Bernard, D., Bernardini, E., Bernasconi, T., Bertucci, B., Biland, A., Bissaldi, E., Boettcher, M., Bonvicini, V., Bosch Ramon, V., Bottacini, E., Bozhilov, V., Bretz, T., Branchesi, M., Brdar, V., Bringmann, T., Brogna, A., Budtz Jorgensen, C., Busetto, G., Buson, S., Busso, M., Caccianiga, A., Camera, S., Campana, R., Caraveo, P., Cardillo, M., Carlson, P., Celestin, S., Cermeno, M., Chen, A., Cheung, C. C., Churazov, E., Ciprini, S., Coc, A., Colafrancesco, S., Coleiro, A., Collmar, W., Coppi, P., Curado Da Silva, R., Cutini, S., Dammando, F., Lotto, B., Martino, D., Rosa, A., Del Santo, M., Delgado, L., Diehl, R., Dietrich, S., Dolgov, A. D., Dominguez, A., Dominis Prester, D., Donnarumma, I., Dorner, D., Doro, M., Dutra, M., Elsaesser, D., Fabrizio, M., Fernandezbarral, A., Fioretti, V., Foffano, L., Formato, V., Fornengo, N., Foschini, L., Franceschini, A., Franckowiak, A., Funk, S., Fuschino, F., Gaggero, D., Galanti, G., Gargano, F., Gasparrini, D., Gehrz, R., Giammaria, P., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Ghirlanda, G., Godinovic, N., Gouiffes, C., Grove, J. E., Hamadache, C., Hartmann, D. H., Hayashida, M., Hryczuk, A., Jean, P., Johnson, T., Jose, J., Kaufmann, S., Khelifi, B., Kiener, J., Knodlseder, J., Kole, M., Kopp, J., Kozhuharov, V., Labanti, C., Lalkovski, S., Laurent, P., Limousin, O., Linares, M., Lindfors, E., Lindner, M., Liu, J., Lombardi, S., Loparco, F., Lopezcoto, R., Lopez Moya, M., Lott, B., Lubrano, P., Malyshev, D., Mankuzhiyil, N., Mannheim, K., Marcha, M. J., Marciano, A., Marcote, B., Mariotti, M., Marisaldi, M., Mcbreen, S., Mereghetti, S., Merle, A., Mignani, R., Minervini, G., Moiseev, A., Morselli, A., Moura, F., Nakazawa, K., Nava, L., Nieto, D., Orienti, M., Orio, M., Orlando, E., Orleanski, P., Paiano, S., Paoletti, R., Papitto, A., Pasquato, M., Patricelli, B., Perezgarcia, M. A., Persic, M., Piano, G., Pichel, A., Pimenta, M., Pittori, C., Porter, T., Poutanen, J., Prandini, E., Prantzos, N., Produit, N., Profumo, S., Queiroz, F. S., Raino, S., Raklev, A., Regis, M., Reichardt, I., Rephaeli, Y., Rico, J., Rodejohann, W., Rodriguez Fernandez, G., Roncadelli, M., Roso, L., Rovero, A., Ruffini, R., Sala, G., Sanchezconde, M. A., Santangelo, A., Saz Parkinson, P., Sbarrato, T., Shearer, A., Shellard, R., Short, K., Siegert, T., Siqueira, C., Spinelli, P., Stamerra, A., Starrfield, S., Strong, A., Strumke, I., Tavecchio, F., Taverna, R., Terzic, T., Thompson, D. J., Tibolla, O., Diego F. Torres, Turolla, R., Ulyanov, A., Ursi, A., Vacchi, A., Den Abeele, J., Vankova Kirilovai, G., Venter, C., Verrecchia, F., Vincent, P., Wang, X., Weniger, C., Wu, X., Zaharijas, G., Zampieri, L., Zane, S., Zimmer, S., Zoglauer, A., The E, Astrogam Collaboration, Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (INFN, Sezione di Bologna), National Institute for Nuclear Physics (INFN), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), NASA Goddard Space Flight Center (GSFC), I.C.R.E, PRISMA Cluster of Excellence & Institute for Physics (THEP), Johannes Gutenberg - University of Mainz (JGU), School of Physics, University College Dublin, Ireland, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Max-Planck-Institut für Plasmaphysik [Garching] (IPP), National Space Institute [Lyngby] (DTU Space), Technical University of Denmark [Lyngby] (DTU), INAF - Osservatorio Astronomico di Brera (OAB), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Laboratoire de Mécanique des Systèmes et des Procédés (LMSP), Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Deutsches Elektronen-Synchrotron [Zeuthen] (DESY), Helmholtz-Gemeinschaft, Centro di Ateneo di Studi e Attività Spaziali 'Giuseppe Colombo' (CISAS), Universita degli Studi di Padova, Istituto Nazionale di Fisica Nucleare, Sezione di Perugia (INFN, Sezione di Perugia), Faculdade de Ciências da Universidade do Porto, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, CEA Cadarache, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Istituto Nazionale di Fisica Nucleare [Pisa] (INFN), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Max Planck Institute for Astrophysics, Max-Planck-Gesellschaft, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Agenzia Spaziale Italiana (ASI) Science Data Center, Istituto di Radioastronomia INAF, Dipartimento di Odontostomatologia, Seconda Università degli studi di Napoli, Max-Planck-Institut für Extraterrestrische Physik (MPE), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Institut für Theoretische Physik und Astrophysik [Wurzburg], Julius-Maximilians-Universität Würzburg [Wurtzbourg, Allemagne] (JMU), Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona [Barcelona] (UAB), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (INFN, Sezione di Torino), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Laboratoire Colloïdes et Matériaux Divisés (LCMD), ESPCI ParisTech-Centre National de la Recherche Scientifique (CNRS), Humboldt Universität zu Berlin, GRAPPA and Institute of Physics, Agenzia Spaziale Italiana (ASI), Istituto Nazionale di Fisica Nucleare, sezione di Bari (INFN, sezione di Bari), INAF - Osservatorio Astronomico di Bologna (OABO), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Institut de biologie et chimie des protéines [Lyon] (IBCP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Centre Scientifique et Technique du Bâtiment (CSTB Saint Martin d'Hères), Centre Scientifique et Technique du Bâtiment (CSTB), Linköpings universitet, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Smiths Detection (SH), Departament d'Astronomia i Meteorologia [Barcelona] (DAM), Universitat de Barcelona (UB), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Racah Institute of Physics (Racah Institute of Physics), The Hebrew University of Jerusalem (HUJ)-Racah Institute of Physics, Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 (LASIR), Centre National de la Recherche Scientifique (CNRS)-Université de Lille, INAF - Osservatorio Astronomico di Trieste (OAT), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], Università degli studi di Torino (UNITO), Istituto Nazionale di Fisica Nucleare, Sezione di Torino, Université Nice Sophia Antipolis - Faculté des Sciences (UNS UFR Sciences), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Universitat Politècnica de Catalunya [Barcelona] (UPC), University of Arizona, INAF-OAB, Max-Planck-Institut für Kernphysik (MPIK), Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (INFN, Sezione di Trieste), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Bioénergétique et Ingénierie des Protéines (BIP ), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Istituto Nazionale di Fisica Nucleare (INFN), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Johannes Gutenberg - Universität Mainz = Johannes Gutenberg University (JGU), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Helmholtz-Gemeinschaft = Helmholtz Association, Università degli Studi di Padova = University of Padua (Unipd), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto, Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Istituto di Radioastronomia [Bologna] (IRA), Seconda Università degli Studi di Napoli = Second University of Naples, Institut für Theoretische Physik und Astrophysik [Würzburg], Julius-Maximilians-Universität Würzburg (JMU), Universitat Autònoma de Barcelona (UAB), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Humboldt University Of Berlin, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Università degli studi di Torino = University of Turin (UNITO), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), De Angelis, A., Tatischeff, V., Grenier, I. A., Mcenery, J., Mallamaci, M., Tavani, M., Oberlack, U., Hanlon, L., Walter, R., Argan, A., Von Ballmoos, P., Bulgarelli, A., Bykov, A., Hernanz, M., Kanbach, G., Kuvvetli, I., Pearce, M., Zdziarski, A., Conrad, J., Ghisellini, G., Harding, A., Isern, J., Leising, M., Longo, F., Madejski, G., Martinez, M., Mazziotta, M. N., Paredes, J. M., Pohl, M., Rando, R., Razzano, M., Aboudan, A., Ackermann, M., Addazi, A., Ajello, M., Albertus, C., Álvarez, J. M., Ambrosi, G., Antón, S., Antonelli, L. A., Babic, A., Baibussinov, B., Balbo, M., Baldini, L., Balman, S., Bambi, C., Barres de Almeida, U., Barrio, J. A., Bartels, R., Bastieri, D., Bednarek, W., Bernard, D., Bernardini, E., Bernasconi, T., Bertucci, B., Biland, A., Bissaldi, E., Boettcher, M., Bonvicini, V., Bosch-Ramon, V., Bottacini, E., Bozhilov, V., Bretz, T., Branchesi, M., Brdar, V., Bringmann, T., Brogna, A., Budtz Jørgensen, C., Busetto, G., Buson, S., Busso, M., Caccianiga, A., Camera, S., Campana, R., Caraveo, P., Cardillo, M., Carlson, P., Celestin, S., Cermeño, M., Chen, A., Cheung, C. C., Churazov, E., Ciprini, S., Coc, A., Colafrancesco, S., Coleiro, A., Collmar, W., Coppi, P., Curado da Silva, R., Cutini, S., D'Ammando, F., De Lotto, B., de Martino, D., De Rosa, A., Del Santo, M., Delgado, L., Diehl, R., Dietrich, S., Dolgov, A. D., Domínguez, A., Dominis Prester, D., Donnarumma, I., Dorner, D., Doro, M., Dutra, M., Elsaesser, D., Fabrizio, M., Fernández-Barral, A., Fioretti, V., Foffano, L., Formato, V., Fornengo, N., Foschini, L., Franceschini, A., Franckowiak, A., Funk, S., Fuschino, F., Gaggero, D., Galanti, G., Gargano, F., Gasparrini, D., Gehrz, R., Giammaria, P., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Ghirlanda, G., Godinovic, N., Gouiffés, C., Grove, J. E., Hamadache, C., Hartmann, D. H., Hayashida, M., Hryczuk, A., Jean, P., Johnson, T., José, J., Kaufmann, S., Khelifi, B., Kiener, J., Knödlseder, J., Kole, M., Kopp, J., Kozhuharov, V., Labanti, C., Lalkovski, S., Laurent, P., Limousin, O., Linares, M., Lindfors, E., Lindner, M., Liu, J., Lombardi, S., Loparco, F., López-Coto, R., López Moya, M., Lott, B., Lubrano, P., Malyshev, D., Mankuzhiyil, N., Mannheim, K., Marchã, M. J., Marcianò, A., Marcote, B., Mariotti, M., Marisaldi, M., Mcbreen, S., Mereghetti, S., Merle, A., Mignani, R., Minervini, G., Moiseev, A., Morselli, A., Moura, F., Nakazawa, K., Nava, L., Nieto, D., Orienti, M., Orio, M., Orlando, E., Orleanski, P., Paiano, S., Paoletti, R., Papitto, A., Pasquato, M., Patricelli, B., Pérez-García, M. Ã ., Persic, M., Piano, G., Pichel, A., Pimenta, M., Pittori, C., Porter, T., Poutanen, J., Prandini, E., Prantzos, N., Produit, N., Profumo, S., Queiroz, F. S., Rainó, S., Raklev, A., Regis, M., Reichardt, I., Rephaeli, Y., Rico, J., Rodejohann, W., Rodriguez Fernandez, G., Roncadelli, M., Roso, L., Rovero, A., Ruffini, R., Sala, G., Sánchez-Conde, M. A., Santangelo, A., Saz Parkinson, P., Sbarrato, T., Shearer, A., Shellard, R., Short, K., Siegert, T., Siqueira, C., Spinelli, P., Stamerra, A., Starrfield, S., Strong, A., Strümke, I., Tavecchio, F., Taverna, R., Terzić, T., Thompson, D. J., Tibolla, O., Torres, D. F., Turolla, R., Ulyanov, A., Ursi, A., Vacchi, A., Van den Abeele, J., Vankova-Kirilovai, G., Venter, C., Verrecchia, F., Vincent, P., Wang, X., Weniger, C., Wu, X., Zaharijaš, G., Zampieri, L., Zane, S., Zimmer, S., Zoglauer, A., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Johannes Gutenberg - Universität Mainz (JGU), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Universidade do Porto, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Humboldt-Universität zu Berlin, and Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL)
Subjects: MeV-GeV gamma-ray, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, astro-ph.SR, hep-ex, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Institut für Physik und Astronomie, e-ASTROGAM, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy and Astrophysic, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], ddc:530, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), astro-ph.IM
Abstract: e-ASTROGAM (enhanced ASTROGAM) is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV - the lower energy limit can be pushed to energies as low as 150 keV for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and LISA., Published on Journal of High Energy Astrophysics (Elsevier)

28. Living in a loft

Author: Feroci, M., Stella, L., Klis, M., Courvoisier, T. J. -L, Hernanz, M., Hudec, R., Santangelo, A., Walton, D., Zdziarski, A., Barret, D., Belloni, T., Braga, J., Brandt, S., Budtz-Jørgensen, C., Campana, S., Den Herder, J. -W, Huovelin, J., Israel, G. L., Pohl, M., Ray, P., Vacchi, A., Zane, S., Argan, A., Attinà, P., Bertuccio, G., Bozzo, E., Campana, R., Chakrabarty, D., Costa, E., Rosa, A., Del Monte, E., Di Cosimo, S., Donnarumma, I., Evangelista, Y., Haas, D., Jonker, P., Korpela, S., Labanti, C., Malcovati, P., Mignani, R., Muleri, F., Rapisarda, M., Rashevski, A. R., Rea, N., Rubini, A., Tenzer, C., Wilson-Hodge, C., Winter, B., Wood, K., Zampa, G., Zampa, N., Abramowicz, M. A., Alpar, M. A., Altamirano, D., Alvarez, J. M., Amati, L., Amoros, C., Antonelli, L. A., Artigue, R., Azzarello, P., Bachetti, M., Baldazzi, G., Barbera, M., Barbieri, C., Basa, S., Baykal, A., Belmont, R., Boirin, L., Bonvicini, V., Burderi, L., Bursa, M., Cabanac, C., Cackett, E., Caliandro, G. A., Casella, P., Chaty, S., Chenevez, J., Coe, M. J., Collura, A., Corongiu, A., Covino, S., Cusumano, G., D’amico, F., Dall’osso, S., Martino, D., Paris, G., Di Persio, G., Di Salvo, T., chris done, Dovčiak, M., Drago, A., Ertan, U., Fabiani, S., Falanga, M., Fender, R., Ferrando, P., Della Monica Ferreira, D., Fraser, G., Frontera, F., Fuschino, F., Galvez, J. L., Ghandi, P., Giommi, P., Godet, O., Göğüş, E., Goldwurm, A., Götz, D., Grassi, M., Guttridge, P., Hakala, P., Henri, G., Hermsen, W., Horak, J., Hornstrup, A., In’t Zand, J. J. M., Isern, J., Kalemci, E., Kanbach, G., Karas, V., Kataria, D., Kennedy, T., Klochkov, D., Kluźniak, W., Kokkotas, K., Kreykenbohm, I., Krolik, J., Kuiper, L., Kuvvetli, I., Kylafis, N., Lattimer, J. M., Lazzarotto, F., Leahy, D., Lebrun, F., Lin, D., Lund, N., Maccarone, T., Malzac, J., Marisaldi, M., Martindale, A., Mastropietro, M., Mcclintock, J., Mchardy, I., Mendez, M., Mereghetti, S., Miller, M. C., Mineo, T., Morelli, E., Morsinck, S., Motch, C., Motta, S., Muñoz-Darias, T., Naletto, A., Neustroev, V., Nevalainen, J., Olive, J. F., Orio, M., Orlandini, M., Orleanski, P., Ozel, F., Pacciani, L., Paltani, S., Papadakis, I., Papitto, A., Patruno, A., Pellizzoni, A., Petráček, V., Petri, J., Petrucci, P. O., Phlips, B., Picolli, L., Possenti, A., Psaltis, D., Rambaud, D., Reig, P., Remillard, R., Rodriguez, J., Romano, P., Romanova, M., Schanz, T., Schmid, C., Segreto, A., Shearer, A., Smith, A., Smith, P. J., Soffitta, P., Stergioulas, N., Stolarski, M., Stuchlik, Z., Tiengo, A., Török, G., Torres, D., Turolla, R., Uttley, P., Vaughan, S., Vercellone, S., Waters, R., Watts, A., Wawrzaszek, R., Webb, N., Wilms, J., Zampieri, L., Zezas, A., Ziolkowski, J., PoS, Feroci M., Stella L., van der Klis M., Courvoisier T.J.-L., Hernanz M., Hudec R., Santangelo A., Walton D., Zdziarski A., Barret D., Belloni T., Braga J., Brandt S., Budtz-Jorgensen C., Campana S., den Herder J.-W., Huovelin J., Israel G.L., Pohl M., Ray P., Vacchi A., Zane S., Argan A., Attina P., Bertuccio G., Bozzo E., Campana R., Chakrabarty D., Costa E., De Rosa A., Del Monte E., Di Cosimo S., Donnarumma I., Evangelista Y., Haas D., Jonker P., Korpela S., Labanti C., Malcovati P., Mignani R., Muleri F., Rapisarda M., Rashevski A.R., Rea N., Rubini A., Tenzer C., Wilson-Hodge C., Winter B., Wood K., Zampa G., Zampa N., Abramowicz M.A., Alpar M.A., Altamirano D., Alvarez J.M., Amati L., Amoros C., Antonelli L.A., Artigue R., Azzarello P., Bachetti M., Baldazzi G., Barbera M., Barbieri C., Basa S., Baykal A., Belmont R., Boirin L., Bonvicini V., Burderi L., Bursa M., Cabanac C., Cackett E., Caliandro G.A., Casella P., Chaty S., Chenevez J., Coe M.J., Collura A., Corongiu A., Covino S., Cusumano G., D'Amico F., Dall'Osso S., De Martino D., De Paris G., Di Persio G., Di Salvo T., Done C., Dovciak M., Drago A., Ertan U., Fabiani S., Falanga M., Fender R., Ferrando P., Della Monica Ferreira D., Fraser G., Frontera F., Fuschino F., Galvez J.L., Ghandi P., Giommi P., Godet O., Gogus E., Goldwurm A., Gotz D., Grassi M., Guttridge P., Hakala P., Henri G., Hermsen W., Horak J., Hornstrup A., in't Zand J.J.M., Isern J., Kalemci E., Kanbach G., Karas V., Kataria D., Kennedy T., Klochkov D., Kluzniak W., Kokkotas K., Kreykenbohm I., Krolik J., Kuiper L., Kuvvetli I., Kylafis N., Lattimer J.M., Lazzarotto F., Leahy D., Lebrun F., Lin D., Lund N., Maccarone T., Malzac J., Marisaldi M., Martindale A., Mastropietro M., McClintock J., McHardy I., Mendez M., Mereghetti S., Miller M.C., Mineo T., Morelli E., Morsinck S., Motch C., Motta S., Munoz-Darias T., Naletto A., Neustroev V., Nevalainen J., Olive J.F., Orio M., Orlandini M., Orleanski P., Ozel F., Pacciani L., Paltani S., Papadakis I., Papitto A., Patruno A., Pellizzoni A., Petracek V., Petri J., Petrucci P.O., Phlips B., Picolli L., Possenti A., Psaltis D., Rambaud D., Reig P., Remillard R., Rodriguez J., Romano P., Romanova M., Schanz T., Schmid C., Segreto A., Shearer A., Smith A., Smith P.J., Soffitta P., Stergioulas N., Stolarski M., Stuchlik Z., Tiengo A., Torok G., Torres D., Turolla R., Uttley P., Vaughan S., Vercellone S., Waters R., Watts A., Wawrzaszek R., Webb N., Wilms J., Zampieri L., Zezas A., and Ziolkowski J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, LOFT (Large area Observatory For x-ray Timing), Matter under extreme condition, Large Area Detector (LAD), Wide Field Monitor (WFM), Silicon Drift Detector (SDD)
Abstract: LOFT (Large area Observatory For x-ray Timing) is an innovative mission concept for the next generation of X-ray experiments, submitted to the ESA Call for Medium size missions “M3”. Recent developments in the field of Silicon detectors allowed us to design a realistic observatory devoted to X-ray timing studies with an effective area above 10 m2, operating in the energy range 2-30 keV with an energy resolution of ∼250 eV. Such an exceedingly large area (20 times that of RXTE/PCA), with a time resolution better than 10 µs, will enable unprecedently fast and accurate time variability studies related to accreting collapsed objects (e.g. fast coherent pulsations and QPOs). The scientific payload is complemented by a coded-mask wide field monitor based on similar detectors. In this paper we present the mission concept, the payload design and the expected performances.

29. LOFT: A large observatory for x-ray timing

Author: Muleri, F., Feroci, M., Belloni, T., Braga, J., Campana, S., Courvousier, T., Hernanz, M., Hudec, R., Israel, G. L., Ray, P. S., Santangelo, A., Stella, L., Vacchi, A., Klis, M., Walton, D., Zdziarski, A., Alvarez, J. M., Argan, A., Baldazzi, G., Barbera, M., Bertuccio, G., Bonvicini, V., Bozzo, E., Campana, R., Collura, A., Cusumano, G., Del Monte, E., Den Herder, J. W., Di Cosimo, S., Di Persio, G., Evangelista, Y., Fuschino, F., Galvez, J. L., Giommi, P., Grassi, M., Guttridge, P., In T Zand, J. J. M., Kataria, D., Klochkov, D., Labanti, C., Lazzarotto, F., Malcovati, P., Marisaldi, M., Mastropietro, M., Mineo, T., Morelli, E., Orleanski, P., Phlips, B., Picolli, L., Rapisarda, M., Rashevski, A., Remillard, R., Rubini, A., Schanz, T., Segreto, A., Stolarski, M., Tenzer, C., Wawrzaszek, R., Wilson-Hodge, C., Winter, B., Zampa, G., Zampa, N., Alpar, A., Altamirano, D., Amati, L., Antonelli, L. A., Attinà, P., Barbieri, C., Burderi, L., Bursa, M., Caliandro, G. A., Casella, P., Chakrabarty, D., Corongiu, A., Costa, E., Covino, S., Dall Osso, S., D Amico, F., Done, C., Di Salvo, T., Drago, A., Martino, D., Rosa, A., Donnarumma, I., Dovciak, M., Ertan, U., Falanga, M., Fender, R., Frontera, F., Ghandi, P., Ersin Gogus, Hermsen, W., Isern, J., Horak, J., Jonker, P., Kalemci, E., Kanbach, G., Karas, V., Kluzniak, W., Kokkotas, K., Krolik, J., Kylafis, N., Lattimer, J., Leahy, D., Maccarone, T., Mcclintock, J., Mendez, M., Mereghetti, S., Mignani, R., Miller, C., Mornick, S., Motta, S., Muñoz-Darias, T., Naletto, A., Orio, M., Orlandini, M., Ozel, F., Pacciani, L., Paltani, S., Papadakis, I., Papitto, A., Patruno, A., Pellizzoni, A., Possenti, A., Psaltis, D., Rea, N., Reig, P., Romano, P., Romanova, M., Shearer, A., Soffitta, P., Stergioulas, N., Stuchlik, Z., Tiengo, A., Torres, D., Turolla, R., Vercellone, S., Watts, A., Wood, K., Zampieri, L., Zane, S., Zezas, A., Ziolkowski, J., Muleri, Fabio, Feroci, M., Belloni, T., Braga, J., Campana, S., Courvousier, T., Hernanz, M., Hudec, R., Israel, G. L., Ray, P. S., Santangelo, A., Stella, L., Vacchi, A., Van Der Klis, M., Walton, D., Zdziarski, A., Alvarez, J. M., Argan, A., Baldazzi, Giuseppe, Barbera, M., Bertuccio, G., Bonvicini, V., Bozzo, E., Campana, R., Collura, A., Cusumano, G., Del Monte, E., Den Herder, J. W., Di Cosimo, S., Di Persio, G., Evangelista, Y., Fuschino, F., Galvez, J. L., Giommi, P., Grassi, M., Guttridge, P., In'T Zand, J. J. M., Kataria, D., Klochkov, D., Labanti, C., Lazzarotto, F., Malcovati, P., Marisaldi, M., Mastropietro, M., Mineo, T., Morelli, E., Muleri, F., Orleanski, P., Phlips, B., Picolli, L., Rapisarda, M., Rashevski, A., Remillard, R., Rubini, A., Schanz, T., Segreto, A., Stolarski, M., Tenzer, C., Wawrzaszek, R., Wilson Hodge, C., Winter, B., Zampa, G., Zampa, N., Alpar, A., Altamirano, D., Amati, L., Antonelli, L. A., Attinà, P., Barbieri, C., Burderi, L., Bursa, M., Caliandro, G. A., Casella, P., Chakrabarty, D., Corongiu, A., Costa, E., Covino, S., Dall'Osso, S., D'Amico, F., Done, C., Di Salvo, T., Drago, A., De Martino, D., De Rosa, A., Donnarumma, I., Dovciak, M., Ertan, U., Falanga, M., Fender, R., Frontera, F., Ghandi, P., Gogus, E., Hermsen, W., Isern, J., Horak, J., Jonker, P., Kalemci, E., Kanbach, G., Karas, V., Kluzniak, W., Kokkotas, K., Krolik, J., Kylafis, N., Lattimer, J., Leahy, D., Maccarone, T., Mcclintock, J., Mendez, M., Mereghetti, S., Mignani, R., Miller, C., Mornick, S., Motta, S., Muñoz Darias, T., Naletto, A., Orio, M., Orlandini, M., Ozel, F., Pacciani, L., Paltani, S., Papadakis, I., Papitto, A., Patruno, A., Pellizzoni, A., Possenti, A., Psaltis, D., Rea, N., Reig, P., Romano, P., Romanova, M., Shearer, A., Soffitta, P., Stergioulas, N., Stuchlik, Z., Tiengo, A., Torres, D., Turolla, R., Vercellone, S., Watts, A., Wood, K., Zampieri, L., Zane, S., Zezas, A., and Ziolkowski, J.
Subjects: Multidisciplinary
Abstract: LOFT (Large area Observatory For x-ray Timing) is an innovative mission submitted in response to the Cosmic Vision "Call for a Medium-size mission opportunity for a launch in 2022" recently issued by ESA. LOFT is an ideal candidate for the next generation of (extremely) large experiments for X-ray timing dedicated to the study of the physics of compact objects and to the understanding of the behavior of matter in strong gravitational fields. Recent developments in the field of large area monolithic silicon detectors allowed us to reach an effective area ∼12 m2 (15 m2 goal), more than a order of magnitude larger that RXTE/PCA, in the energy range 2-30 keV (1-40 keV goal). This Large Area Detector (LAD) will have both high timing resolution (

30. GTC optical observations of SGR 0418+5729

Author: Mignani, R. P., Rea, N., Vincenzo Testa, Israel, G. L., Covino, S., Stella, L., Mereghetti, S., Burgay, M., Possenti, A., Chaty, S., Jonker, P., Lo Curto, G., Perna, R., Turolla, R., Zane, S., and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Abstract: We observed the field containing the new SGR 0418+5729 (ATel #2076, #2077) in the i'-band on 2009 September 15 with the OSIRIS camera (0.25"/pixel) mounted at the 10.4m Gran Telescopio Canarias (GTC) in the La Palma Observatory, as a part of our magnetar ToO observing program.

31. Detection of the second period derivative in the timing evolution of SGR 1833-0832

Author: Esposito, P., GianLuca Israel, Turolla, R., Rea, N., Burgay, M., Possenti, A., Tiengo, A., Mereghetti, S., Gotz, D., Stella, L., and Zane, S.

32. A time-variable, phase-dependent emission line in the isolated neutron star RX J0822-4300

Author: Sartori, A., Luca, A., Salvetti, D., Esposito, P., Andrea Tiengo, Zane, S., Turolla, R., Pizzolato, F., Mignani, R. P., Caraveo, P. A., Mereghetti, S., and Bignami, G. F.

33. Strong evidence for precession of the isolated neutron star RX J0720.4-3125

Author: Haberl, F., Turolla, R., Vries, C. P., Zane, S., Vink, J., Mariano Mendez, and Verbunt, F.

34. Period derivative of the Soft Gamma-ray Repeater SGR 1627-41

Author: Esposito, P., Andrea Tiengo, Mereghetti, S., Luca, A., Israel, G. L., Gotz, D., Rea, N., Turolla, R., Zane, S., Romano, P., Burgay, M., Possenti, A., and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Abstract: After nearly a decade of quiescence, the soft gamma-ray repeater SGR 1627-41 reactivated on 2008 May 28 with a bursting episode (Esposito et al. 2008, MNRAS, 390, L34). On 2008 September 27-28 we performed an XMM-Newton target of opportunity observation of the source and discovered its long-sought spin period at 2.594578(6) s (Esposito et al. 2009, ApJ, 690, L105). We searched in the archival Chandra data of SGR 1627-41 taken on 2008 June 03 (obsID 9126, ATEL #1564 by Woods et al.) for the presence of a periodic signal over a period range extrapolated from our XMM-Newton data, assuming a period derivative dP/dt < 10-9 s s-1.

35. ATCA observations of the soft gamma-ray repeater SGR 1833-0832

Author: Wieringa, M. H., Possenti, A., Burgay, M., Esposito, P., Israel, G. L., Rea, N., Andrea Tiengo, Turolla, R., Zane, S., Gotz, D., Mereghetti, S., and Stella, L.

36. An analytical approach to the problem of mass loss from Wolf-Rayet stars

Author: Rino Bandiera and Turolla, R.

37. XMM-Newton Observations of the Two Anomalous X-ray pulsars 1RXS J170849.0-400910 and 1E 1048.1-5937

Author: Zane, S., Rea, N., Israel, G. L., Tiengo, A., Mereghetti, S., Stella, L., Mariano Mendez, Turolla, R., Oosterbroek, T., and Haberl, F.

38. Detection of pulsations and a spectral feature in the X-ray emission of the isolated neutron star 1RXS J214303.7+065419/RBS 1774

Author: Turolla, R., Zane, S., Cropper, M., Zampieri, L., Chieregato, M., Drake, J., and Treves, A.
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Resolution (electron density), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Spectral line, Neutron star, Pulsar, Space and Planetary Science, Feature (computer vision), ROSAT, Absorption (electromagnetic radiation), Spin-½
Abstract: We report on the results of a deep XMM-Newton observation of RBS 1774, the most recent dim isolated neutron star candidate found in the ROSAT archive data. Spectral and timing analysis of the high-quality PN and MOS data confirm the association of this source with an isolated neutron star. The spectrum is thermal and blackbody-like, and there is evidence at a significance level > 4sigma that the source is an X-ray pulsar, with spin period of 9.437 s. Spectral fitting reveils the presence of an absorption feature at ~0.7 keV, but at this level data do not have enough resolution to allow us to discriminate between an absorption line or an edge. We compare the newly measured properties of RBS 1774 with those of other known dim isolated neutron stars, and discuss possible interpretations for the absorption feature., 21 pages, 5 figures, ApJ accepted

39. LOFT: A large observatory for x-ray timing

Author: Muleri, F., Feroci, M., Belloni, T., Braga, J., Campana, S., Courvousier, T., Hernanz, M., Hudec, R., Israel, G. L., Ray, P. S., Santangelo, A., Stella, L., Vacchi, A., Klis, M., Walton, D., Zdziarski, A., Alvarez, J. M., Argan, A., Baldazzi, G., Barbera, M., Bertuccio, G., Bonvicini, V., Bozzo, E., Campana, R., Collura, A., Cusumano, G., Del Monte, E., Den Herder, J. W., Di Cosimo, S., Di Persio, G., Evangelista, Y., Fuschino, F., Galvez, J. L., Giommi, P., Grassi, M., Guttridge, P., In ’t Zand, J. J. M., Kataria, D., Klochkov, D., Labanti, C., Lazzarotto, F., Malcovati, P., Marisaldi, M., Mastropietro, M., Mineo, T., Morelli, E., Orleanski, P., Phlips, B., Picolli, L., Rapisarda, M., Rashevski, A., Remillard, R., Rubini, A., Schanz, T., Segreto, A., Stolarski, M., Tenzer, C., Wawrzaszek, R., Wilson-Hodge, C., Winter, B., Zampa, G., Zampa, N., Alpar, A., Altamirano, D., Amati, L., Antonelli, L. A., Primo Attinà, Barbieri, C., Burderi, L., Bursa, M., Caliandro, G. A., Casella, P., Chakrabarty, D., Corongiu, A., Costa, E., Covino, S., Dall’osso, S., D’amico, F., Done, C., Di Salvo, T., Drago, A., Martino, D., Rosa, A., Donnarumma, I., Dovciak, M., Ertan, U., Falanga, M., Fender, R., Frontera, F., Ghandi, P., Gogus, E., Hermsen, W., Isern, J., Horak, J., Jonker, P., Kalemci, E., Kanbach, G., Karas, V., Kluzniak, W., Kokkotas, K., Krolik, J., Kylafis, N., Lattimer, J., Leahy, D., Maccarone, T., Mcclintock, J., Mendez, M., Mereghetti, S., Mignani, R., Miller, C., Mornick, S., Motta, S., Muñoz-Darias, T., Naletto, A., Orio, M., Orlandini, M., Ozel, F., Pacciani, L., Paltani, S., Papadakis, I., Papitto, A., Patruno, A., Pellizzoni, A., Possenti, A., Psaltis, D., Rea, N., Reig, P., Romano, P., Romanova, M., Shearer, A., Soffitta, P., Stergioulas, N., Stuchlik, Z., Tiengo, A., Torres, D., Turolla, R., Vercellone, S., Watts, A., Wood, K., Zampieri, L., Zane, S., Zezas, A., and Ziolkowski, J.

40. Upper limit on the radio emission from the soft gamma-ray repeater SGR 1833-0832

Author: Burgay, M., Possenti, A., Esposito, P., Israel, G. L., Rea, N., Sarkissian, J., Andrea Tiengo, Turolla, R., Zane, S., Gotz, D., Stella, L., and Mereghetti, S.

41. The Twin Magnetars: SGR 1627-41 and 1E 1547-5408

Author: Mereghetti, S., Tiengo, A., Esposito, P., Vianello, G., Luca, A., Gotz, D., Weidenspointner, G., Kienlin, A., Israel, G. L., Stella, L., Nanda Rea, Turolla, R., and Zane, S.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: We report on recent results obtained thanks to Target of Opportunity observations of the two galactic sources SGR 1627-41 and 1E 1547-5408. These two transient sources present several similarities which support the interpretation of Anomalous X-ray Pulsars and Soft Gamma-ray Repeaters as a single class of strongly magnetized neutron stars., Comment: To be published in the proceedings of the conference "Neutron Stars and Gamma Ray Bursts: Recent Developments and Future Directions" - March 30 - April 4, 2009 (Cairo and Alexandria, Egypt)

42. Measuring the strongest magnetic fields in the Universe

Author: Andrea Tiengo, Esposito, P., Mereghetti, S., Turolla, R., Nobili, L., Gotz, D., Israel, G., Rea, N., Stella, L., and Zane, S.

43. On the spin-down rate of Swift J1822.3-1606

Author: Israel, G. L., Esposito, P., Nanda Rea, Turolla, R., Zane, S., Mereghetti, S., and Tieng, A.

44. Discovery of 59ms Pulsations from 1RXS J141256.0+792204 (Calvera)

Author: Champion, D., Zane, S., Haberl, F., Israel, G., Pellizzoni, A., Burgay, M., Mignani, R., Turolla, R., Possenti, A., Esposito, P., Eatough, R., Barr, E., and Kramer, M.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: We report on a multi-wavelength study of the compact object candidate 1RXS J141256.0+792204 (Calvera). Calvera was observed in the X-rays with XMM/EPIC twice for a total exposure time of ~50 ks. The source spectrum is thermal and well reproduced by a two component model composed of either two hydrogen atmosphere models, or two blackbodies (kT_1~ 55/150 eV, kT_2~ 80/250 eV, respectively, as measured at infinity). Evidence was found for an absorption feature at ~0.65 keV; no power-law high-energy tail is statistically required. Using pn and MOS data we discovered pulsations in the X-ray emission at a period P=59.2 ms. The detection is highly significant (> 11 sigma), and unambiguously confirms the neutron star nature of Calvera. The pulse profile is nearly sinusoidal, with a pulsed fraction of ~18%. We looked for the timing signature of Calvera in the Fermi Large Area Telescope (LAT) database and found a significant (~5 sigma) pulsed signal at a period coincident with the X-ray value. The gamma-ray timing analysis yielded a tight upper limit on the period derivative, dP/dt < 5E-18 s/s (dE_rot/dt

45. Ultraluminous X-ray sources in nearby galaxies: Clues on their nature from X-ray timing and new optical data

Author: Luca Zampieri, Mucciarelli, P., Falomo, R., Casella, P., Belloni, T., Turolla, R., Treves, A., and Ranalli, P.

46. Ten years of XMM-Newton observations of RX J1856.5-3754

Author: Sartore, N., Mereghetti, S., Andrea Tiengo, Luca, A., Turolla, R., and Haberl, F.

47. Spin down rate and inferred dipole magnetic field of the new soft gamma-ray repeater Sgr 1833-0832

Author: Esposito, P., Israel, G. L., Burgay, M., Possenti, A., Gotz, D., Rea, N., Mereghetti, S., Andrea Tiengo, Stella, L., Turolla, R., and Zane, S.

48. Ultra-strong electric fields and vacuum breakdown: Search for an astrophysical scenario

Author: Treves, A., Turolla, R., and Sergei Popov

49. X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho’s Supernova Remnant

Author: Riccardo Ferrazzoli, Patrick Slane, Dmitry Prokhorov, Ping Zhou, Jacco Vink, Niccolò Bucciantini, Enrico Costa, Niccolò Di Lalla, Alessandro Di Marco, Paolo Soffitta, Martin C. Weisskopf, Kazunori Asakura, Luca Baldini, Jeremy Heyl, Philip E. Kaaret, Frédéric Marin, Tsunefumi Mizuno, C.-Y. Ng, Melissa Pesce-Rollins, Stefano Silvestri, Carmelo Sgrò, Douglas A. Swartz, Toru Tamagawa, Yi-Jung Yang, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Fabian Kislat, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Giorgio Matt, Ikuyuki Mitsuishi, Fabio Muleri, Michela Negro, Stephen L. O’Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver Roberts, Roger W. Romani, Gloria Spandre, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Kinwah Wu, Fei Xie, Silvia Zane, Ferrazzoli, R., Slane, P., Prokhorov, D., Zhou, P., Vink, J., Bucciantini, N., Costa, E., Di Lalla, N., Di Marco, A., Soffitta, P., Weisskopf, M. C., Asakura, K., Baldini, L., Heyl, J., Kaaret, P. E., Marin, F., Mizuno, T., Ng, C. -Y., Pesce-Rollins, M., Silvestri, S., Sgro, C., Swartz, D. A., Tamagawa, T., Yang, Y. -J., Agudo, I., Antonelli, L. A., Bachetti, M., Baumgartner, W. H., Bellazzini, R., Bianchi, S., Bongiorno, S. D., Bonino, R., Brez, A., Capitanio, F., Castellano, S., Cavazzuti, E., Chen, C. -T., Ciprini, S., De Rosa, A., Del Monte, E., Di Gesu, L., Donnarumma, I., Doroshenko, V., Dovciak, M., Ehlert, S. R., Enoto, T., Evangelista, Y., Fabiani, S., Garcia, J. A., Gunji, S., Hayashida, K., Iwakiri, W., Jorstad, S. G., Kislat, F., Karas, V., Kitaguchi, T., Kolodziejczak, J. J., Krawczynski, H., La Monaca, F., Latronico, L., Liodakis, I., Maldera, S., Manfreda, A., Marinucci, A., Marscher, A. P., Marshall, H. L., Matt, G., Mitsuishi, I., Muleri, F., Negro, M., O'Dell, S. L., Omodei, N., Oppedisano, C., Papitto, A., Pavlov, G. G., Peirson, A. L., Perri, M., Petrucci, P. -O., Pilia, M., Possenti, A., Poutanen, J., Puccetti, S., Ramsey, B. D., Rankin, J., Ratheesh, A., Roberts, O., Romani, R. W., Spandre, G., Tavecchio, F., Taverna, R., Tawara, Y., Tennant, A. F., Thomas, N. E., Tombesi, F., Trois, A., Tsygankov, S. S., Turolla, R., Wu, K., Xie, F., Zane, S., Ministerio de Ciencia e Innovación (España), and European Commission
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Full list of authors: Ferrazzoli, Riccardo; Slane, Patrick; Prokhorov, Dmitry; Zhou, Ping; Vink, Jacco; Bucciantini, Niccolo; Costa, Enrico; Di Lalla, Niccolo; Di Marco, Alessandro; Soffitta, Paolo; Weisskopf, Martin C.; Asakura, Kazunori; Baldini, Luca; Heyl, Jeremy; Kaaret, Philip E.; Marin, Frederic; Mizuno, Tsunefumi; Ng, C. -Y.; Pesce-Rollins, Melissa; Silvestri, Stefano; Sgro, Carmelo; Swartz, Douglas A.; Tamagawa, Toru; Yang, Yi-Jung; Agudo, Ivan; Antonelli, Lucio A.; Bachetti, Matteo; Baumgartner, Wayne H.; Bellazzini, Ronaldo; Bianchi, Stefano; Bongiorno, Stephen D.; Bonino, Raffaella; Brez, Alessandro; Capitanio, Fiamma; Castellano, Simone; Cavazzuti, Elisabetta; Chen, Chien-Ting; Ciprini, Stefano; De Rosa, Alessandra; Del Monte, Ettore; Di Gesu, Laura; Donnarumma, Immacolata; Doroshenko, Victor; Dovciak, Michal; Ehlert, Steven R.; Enoto, Teruaki; Evangelista, Yuri; Fabiani, Sergio; Garcia, Javier A.; Gunji, Shuichi; Hayashida, Kiyoshi; Iwakiri, Wataru; Jorstad, Svetlana G.; Kislat, Fabian; Karas, Vladimir; Kitaguchi, Takao; Kolodziejczak, Jeffery J.; Krawczynski, Henric; La Monaca, Fabio; Latronico, Luca; Liodakis, Ioannis; Maldera, Simone; Manfreda, Alberto; Marinucci, Andrea; Marscher, Alan P.; Marshall, Herman L.; Matt, Giorgio; Mitsuishi, Ikuyuki; Muleri, Fabio; Negro, Michela; O'Dell, Stephen L.; Omodei, Nicola; Oppedisano, Chiara; Papitto, Alessandro; Pavlov, George G.; Peirson, Abel L.; Perri, Matteo; Petrucci, Pierre-Olivier; Pilia, Maura; Possenti, Andrea; Poutanen, Juri; Puccetti, Simonetta; Ramsey, Brian D.; Rankin, John; Ratheesh, Ajay; Roberts, Oliver; Romani, Roger W.; Spandre, Gloria; Tavecchio, Fabrizio; Taverna, Roberto; Tawara, Yuzuru; Tennant, Allyn F.; Thomas, Nicholas E.; Tombesi, Francesco; Trois, Alessio; Tsygankov, Sergey S.; Turolla, Roberto; Wu, Kinwah; Xie, Fei; Zane, Silvia.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., Supernova remnants are commonly considered to produce most of the Galactic cosmic rays via diffusive shock acceleration. However, many questions regarding the physical conditions at shock fronts, such as the magnetic-field morphology close to the particle acceleration sites, remain open. Here we report the detection of a localized polarization signal from some synchrotron X-ray emitting regions of Tycho's supernova remnant made by the Imaging X-ray Polarimetry Explorer. The derived degree of polarization of the X-ray synchrotron emission is 9% ± 2% averaged over the whole remnant, and 12% ± 2% at the rim, higher than the value of polarization of 7%–8% observed in the radio band. In the west region, the degree of polarization is 23% ± 4%. The degree of X-ray polarization in Tycho is higher than for Cassiopeia A, suggesting a more ordered magnetic field or a larger maximum turbulence scale. The measured tangential direction of polarization corresponds to the radial magnetic field, and is consistent with that observed in the radio band. These results are compatible with the expectation of turbulence produced by an anisotropic cascade of a radial magnetic field near the shock, where we derive a magnetic-field amplification factor of 3.4 ± 0.3. The fact that this value is significantly smaller than those expected from acceleration models is indicative of highly anisotropic magnetic-field turbulence, or that the emitting electrons either favor regions of lower turbulence, or accumulate close to where the orientation of the magnetic field is preferentially radially oriented due to hydrodynamical instabilities. © 2023. The Author(s). Published by the American Astronomical Society., J. Vink & D.Prokhorov are supported by funding from the European Union's Horizon 2020 research and innovation program under grant agreement No. 101004131 (SHARP). P.S. acknowledges support from NASA contract NAS8-03060. P.Z. acknowledges the support from NWO Veni Fellowship grant No. 639.041.647 and NSFC grant No. 12273010 C.-Y.N. and Y.J.Y. are supported by a GRF grant of the Hong Kong Government under HKU 17305419., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).
Published: 2023

50. Polarization properties of the weakly magnetized neutron star X-ray binary GS 1826-238 in the high soft state

Author: Fiamma Capitanio, Sergio Fabiani, Andrea Gnarini, Francesco Ursini, Carlo Ferrigno, Giorgio Matt, Juri Poutanen, Massimo Cocchi, Romana Mikusincova, Ruben Farinelli, Stefano Bianchi, Jari J. E. Kajava, Fabio Muleri, Celia Sanchez-Fernandez, Paolo Soffitta, Kinwah Wu, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccolò Di Lalla, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O’Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Fei Xie, Silvia Zane, Ministerio de Ciencia e Innovación (España), Russian Science Foundation, Academy of Finland, Capitanio, F., Fabiani, S., Gnarini, A., Ursini, F., Ferrigno, C., Matt, G., Poutanen, J., Cocchi, M., Mikusincova, R., Farinelli, R., Bianchi, S., Kajava, J. J. E., Muleri, F., Sanchez-Fernandez, C., Soffitta, P., Wu, K., Agudo, I., Antonelli, L. A., Bachetti, M., Baldini, L., Baumgartner, W. H., Bellazzini, R., Bongiorno, S. D., Bonino, R., Brez, A., Bucciantini, N., Castellano, S., Cavazzuti, E., Ciprini, S., Costa, E., De Rosa, A., Del Monte, E., Di Gesu, L., Di Lalla, N., Di Marco, A., Donnarumma, I., Doroshenko, V., Dovciak, M., Ehlert, S. R., Enoto, T., Evangelista, Y., Ferrazzoli, R., Garcia, J. A., Gunji, S., Hayashida, K., Heyl, J., Iwakiri, W., Jorstad, S. G., Karas, V., Kitaguchi, T., Kolodziejczak, J. J., Krawczynski, H., La Monaca, F., Latronico, L., Liodakis, I., Maldera, S., Manfreda, A., Marin, F., Marinucci, A., Marscher, A. P., Marshall, H. L., Mitsuishi, I., Mizuno, T., Ng, C. -Y., O'Dell, S. L., Omodei, N., Oppedisano, C., Papitto, A., Pavlov, G. G., Peirson, A. L., Perri, M., Pesce-Rollins, M., Petrucci, P. -O., Pilia, M., Possenti, A., Puccetti, S., Ramsey, B. D., Rankin, J., Ratheesh, A., Romani, R. W., Sgro, C., Slane, P., Spandre, G., Tamagawa, T., Tavecchio, F., Taverna, R., Tawara, Y., Tennant, A. F., Thomas, N. E., Tombesi, F., Trois, A., Tsygankov, S. S., Turolla, R., Vink, J., Weisskopf, M. C., Xie, F., and Zane, S.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, Settore FIS/05, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Full list of authors: Capitanio, Fiamma; Fabiani, Sergio; Gnarini, Andrea; Ursini, Francesco; Ferrigno, Carlo; Matt, Giorgio; Poutanen, Juri; Cocchi, Massimo; Mikusincova, Romana; Farinelli, Ruben; Bianchi, Stefano; Kajava, Jari J. E.; Muleri, Fabio; Sanchez-Fernandez, Celia; Soffitta, Paolo; Wu, Kinwah; Agudo, Ivan; Antonelli, Lucio A.; Bachetti, Matteo; Baldini, Luca; Baumgartner, Wayne H.; Bellazzini, Ronaldo; Bongiorno, Stephen D.; Bonino, Raffaella; Brez, Alessandro; Bucciantini, Niccolo; Castellano, Simone; Cavazzuti, Elisabetta; Ciprini, Stefano; Costa, Enrico; De Rosa, Alessandra; Del Monte, Ettore; Di Gesu, Laura; Di Lalla, Niccolo; Di Marco, Alessandro; Donnarumma, Immacolata; Doroshenko, Victor; Dovciak, Michal; Ehlert, Steven R.; Enoto, Teruaki; Evangelista, Yuri; Ferrazzoli, Riccardo; Garcia, Javier A.; Gunji, Shuichi; Hayashida, Kiyoshi; Heyl, Jeremy; Iwakiri, Wataru; Jorstad, Svetlana G.; Karas, Vladimir; Kitaguchi, Takao; Kolodziejczak, Jeffery J.; Krawczynski, Henric; La Monaca, Fabio; Latronico, Luca; Liodakis, Ioannis; Maldera, Simone; Manfreda, Alberto; Marin, Frederic; Marinucci, Andrea; Marscher, Alan P.; Marshall, Herman L.; Mitsuishi, Ikuyuki; Mizuno, Tsunefumi; Ng, C. -Y.; O'Dell, Stephen L.; Omodei, Nicola; Oppedisano, Chiara; Papitto, Alessandro; Pavlov, George G.; Peirson, Abel L.; Perri, Matteo; Pesce-Rollins, Melissa; Petrucci, Pierre-Olivier; Pilia, Maura; Possenti, Andrea; Puccetti, Simonetta; Ramsey, Brian D.; Rankin, John; Ratheesh, Ajay; Romani, Roger W.; Sgro, Carmelo; Slane, Patrick; Spandre, Gloria; Tamagawa, Toru; Tavecchio, Fabrizio; Taverna, Roberto; Tawara, Yuzuru; Tennant, Allyn F.; Thomas, Nicholas E.; Tombesi, Francesco; Trois, Alessio; Tsygankov, Sergey S.; Turolla, Roberto; Vink, Jacco; Weisskopf, Martin C.; Xie, Fei; Zane, Silvia.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., The launch of the Imaging X-ray Polarimetry Explorer (IXPE) on 2021 December 9 has opened a new window in X-ray astronomy. We report here the results of the first IXPE observation of a weakly magnetized neutron star, GS 1826−238, performed on 2022 March 29–31 when the source was in a high soft state. An upper limit (99.73% confidence level) of 1.3% for the linear polarization degree is obtained over the IXPE 2–8 keV energy range. Coordinated INTEGRAL and NICER observations were carried out simultaneously with IXPE. The spectral parameters obtained from the fits to the broadband spectrum were used as inputs for Monte Carlo simulations considering different possible geometries of the X-ray emitting region. Comparing the IXPE upper limit with these simulations, we can put constraints on the geometry and inclination angle of GS 1826–238. © 2023. The Author(s). Published by the American Astronomical Society., J.P. and S.S.T. acknowledge support from Russian Science Foundation grant 20-12-00364 and Academy of Finland travel grants 349144, 349373, and 349906. J.P. and J.J.E.K. were supported by Academy of Finland grant 333112., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).
Published: 2022
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