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99 results on '"Coti Zelati, F."'

1. A long-period radio transient active for three decades

Author

Hurley-Walker, N., Rea, N., McSweeney, S. J., Meyers, B. W., Lenc, E., Heywood, I., Hyman, S. D., Men, Y. P., Clarke, T. E., Coti Zelati, F., Price, D. C., Horváth, C., Galvin, T. J., Anderson, G. E., Bahramian, A., Barr, E. D., Bhat, N. D. R., Caleb, M., Dall’Ora, M., de Martino, D., Giacintucci, S., Morgan, J. S., Rajwade, K. M., Stappers, B., and Williams, A.

Published
2023
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2. Long-term Study of the 2020 Magnetar-like Outburst of the Young Pulsar PSR J1846-0258 in Kes 75.

Author

Sathyaprakash, R., Rea, N., Coti Zelati, F., Borghese, A., Pilia, M., Trudu, M., Burgay, M., Turolla, R., Zane, S., Esposito, P., Mereghetti, S., Campana, S., Götz, D., Ibrahim, A. Y., Israel, G. L., Possenti, A., and Tiengo, A.

Subjects
STELLAR rotation, NEUTRON stars, SUPERNOVA remnants, X-ray bursts, PULSARS, MAGNETARS
Abstract

Magnetar-like activity has been observed in a large variety of neutron stars. PSR J1846−0258 is a young 327 ms radio-quiet pulsar with a large rotational power (∼8 × 1036 erg s−1), and resides at the center of the supernova remnant Kes 75. It is one of the rare examples of a high-magnetic-field pulsar showing characteristics both of magnetars and radio pulsars, and can thus provide important clues on the differences in the emission mechanisms between these two classes. In 2006, PSR J1846−0258 was detected to undergo an outburst for the first time, accompanied by a large flux increase, millisecond X-ray bursts, significant spectral changes, and a large timing glitch. In the period between 2020 May and June, after 14 yr of quiescent stable emission, the source underwent a second magnetar-like outburst, which was followed up with several observations by Neutron Star Interior Composition Explorer, XMM-Newton, NuSTAR, and Swift. In this work, we report on the long-term timing and X-ray spectral properties of the source following the 2020 outburst, and place upper limits on any source activity at radio wavelengths. We demonstrate that the pulsed flux increased by a factor >6 during the outburst, followed by nontrivial variability in the spin-down rate. Our timing analysis shows that the spin frequency and its derivative are clearly affected by magnetospheric activity due to the outburst. We find hints for an oscillation in the frequency derivative with a timescale of 50–60 days, recovering later on to stable quiescence. [ABSTRACT FROM AUTHOR]

Published
2024
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3. Spectral and timing properties of the accreting millisecond X-ray pulsar IGR J17498−2921 during its 2023 outburst.

Author

Illiano, G., Papitto, A., Marino, A., Strohmayer, T. E., Sanna, A., Di Salvo, T., La Placa, R., Ambrosino, F., Miraval Zanon, A., Coti Zelati, F., Ballocco, C., Malacaria, C., Ghedina, A., Cecconi, M., Gonzales, M., and Leone, F.

Abstract

We present a comprehensive study of the spectral properties of the accreting millisecond X-ray pulsar IGR J17498−2921 during its 2023 outburst. Similar to other accreting millisecond X-ray pulsars, the broadband spectral emission observed quasi-simultaneously by NICER and NuSTAR is well described by an absorbed Comptonized emission with an electron temperature of ∼17 keV plus a disk reflection component. The broadening of the disk reflection spectral features, such as a prominent iron emission line at 6.4–6.7 keV, is consistent with the relativistic motion of matter in a disk truncated at ∼21 Rg from the source, near the Keplerian corotation radius. From the high-cadence monitoring data obtained with NICER, we observed that the evolution of the photon index and the temperature of seed photons tracks variations in the X-ray flux. This is particularly evident close to a sudden ∼–0.25 cycle jump in the pulse phase, which occurs immediately following an X-ray flux flare and a drop in the pulse amplitude below the 3σ detection threshold. We also report on the non-detection of optical pulsations with TNG/SiFAP2 from the highly absorbed optical counterpart. [ABSTRACT FROM AUTHOR]

Published
2024
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4. X-ray and optical observations of the millisecond pulsar binary PSR J1431–4715.

Author

de Martino, D., Phosrisom, A., Dhillon, V. S., Torres, D. F., Coti Zelati, F., Breton, R. P., Marsh, T. R., Miraval Zanon, A., Rea, N., and Papitto, A.

Abstract

We present the first X-ray observation of the energetic millisecond pulsar binary PSR J1431−4715, performed with XMM-Newton and complemented with fast optical multi-band photometry acquired with the ULTRACAM instrument at ESO-NTT. It is found as a faint X-ray source without a significant orbital modulation. This contrasts with the majority of systems that instead display substantial X-ray orbital variability. The X-ray spectrum is dominated by non-thermal emission and, due to the lack of orbital modulation, does not favour an origin in an intrabinary shock between the pulsar and companion star wind. While thermal emission from the neutron star polar cap cannot be excluded in the soft X-rays, the dominance of synchrotron emission favours an origin in the pulsar magnetosphere that we describe at both X-ray and gamma-ray energies with a synchro-curvature model. The optical multi-colour light curve folded at the 10.8 h orbital period is double-humped and dominated by ellipsoidal effects, but also affected by irradiation. The ULTRACAM light curves are fit with several models encompassing direct heating and a cold spot, or heat redistribution after irradiation either through convection or convection plus diffusion. Despite the inability to constrain the best irradiation models, the fits provide consistent system parameters, giving an orbital inclination of 59 ± 6° and a distance of 3.1 ± 0.3 kpc. The companion is found to be an F-type star, underfilling its Roche lobe (fRL = 73 ± 4%) with a mass of 0.20 ± 0.04 M⊙, confirming the redback status, but hotter than the majority of redbacks. The stellar dayside and nightside temperatures of 7500 K and 7400 K, respectively, indicate a weak irradiation effect on the companion, likely due to its high intrinsic luminosity. Although the pulsar mass cannot be precisely derived, a heavy (1.8−2.2 M⊙) neutron star is favoured. [ABSTRACT FROM AUTHOR]

Published
2024
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5. Short-term variability of the transitional pulsar candidate CXOU J110926.4−650224 from X-rays to infrared.

Author

Coti Zelati, F., de Martino, D., Dhillon, V. S., Marsh, T. R., Vincentelli, F., Campana, S., Torres, D. F., Papitto, A., Baglio, M. C., Miraval Zanon, A., Rea, N., Brink, J., Buckley, D. A. H., D'Avanzo, P., Illiano, G., Manca, A., and Marino, A.

Subjects
*ACCRETION disks, *X-rays, *DATA analysis, *PULSARS, *PHENOMENOLOGY
Abstract

CXOU J110926.4−650224 is a candidate transitional millisecond pulsar (tMSP) with X-ray and radio emission properties reminiscent of those observed in confirmed tMSPs in their X-ray 'subluminous' disc state. We present the results of observing campaigns that, for the first time, characterise the optical and near-infrared variability of this source and establish a connection with the mode-switching phenomenon observed in X-rays. The optical emission exhibited flickering activity, frequent dipping episodes where it appeared redder, and a multi-peaked flare where it was bluer. The variability pattern was strongly correlated with that of the X-ray emission. Each dip matched an X-ray low-mode episode, indicating that a significant portion of the optical emission originates from nearly the same region as the X-ray emission. The near-infrared emission also displayed remarkable variability, including a dip of 20 min in length during which it nearly vanished. Time-resolved optical spectroscopic observations reveal significant changes in the properties of emission lines from the disc and help infer the spectral type of the companion star to be between K0 and K5. We compare the properties of CXOU J110926.4−650224 with those of other tMSPs in the X-ray subluminous disc state and discuss our findings within the context of a recently proposed scenario that explains the phenomenology exhibited by the prototypical tMSP PSR J1023+0038. [ABSTRACT FROM AUTHOR]

Published
2024
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6. High-temporal-resolution optical spectroscopic observations of the transitional millisecond pulsar PSR J1023+0038.

Author

Messa, M. M., D'Avanzo, P., Coti Zelati, F., Baglio, M. C., and Campana, S.

Subjects
NEUTRON stars, ACCRETION disks, PULSARS
Abstract

Transitional millisecond pulsars (tMSPs) represent a dynamic category of celestial sources that establish a crucial connection between low-mass X-ray binaries and millisecond radio pulsars. These systems exhibit transitions from rotation-powered states to accretion-powered ones and vice versa, highlighting the tight evolutionary link expected by the so-called recycling scenario. In their active phase, these sources manifest two distinct emission modes named high and low, occasionally punctuated by sporadic flares. Here, we present high-time-resolution spectroscopic observations of the binary tMSP J1023+0038, in the sub-luminous disc state. This is the first short-timescale (∼1 min) optical spectroscopic campaign ever conducted on a tMSP. The campaign was carried out over the night of June 10, 2021 using the Gran Telescopio Canarias. The optical continuum shows erratic variability, without clear evidence of high and low modes or of orbital modulation. Besides, the analysis of these high-temporal-cadence spectroscopic observations reveals, for the first time, evidence for a significant (up to a factor of ∼2) variability in the emission line properties (equivalent width and full width half maximum) over a timescale of minutes. Intriguingly, the variability episodes observed in the optical continuum and in the emission line properties seem uncorrelated, making their origin unclear. [ABSTRACT FROM AUTHOR]

Published
2024
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7. An X-Ray and Radio View of the 2022 Reactivation of the Magnetar SGR J1935+2154

Author

Ibrahim, A. Y., primary, Borghese, A., additional, Coti Zelati, F., additional, Parent, E., additional, Marino, A., additional, Ould-Boukattine, O. S., additional, Rea, N., additional, Ascenzi, S., additional, Pacholski, D. P., additional, Mereghetti, S., additional, Israel, G. L., additional, Tiengo, A., additional, Possenti, A., additional, Burgay, M., additional, Turolla, R., additional, Zane, S., additional, Esposito, P., additional, Götz, D., additional, Campana, S., additional, Kirsten, F., additional, Gawroński, M. P., additional, and Hessels, J. W. T., additional

Published
2024
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8. Optical and ultraviolet pulsed emission from an accreting millisecond pulsar

Author

Ambrosino, F., Miraval Zanon, A., Papitto, A., Coti Zelati, F., Campana, S., D’Avanzo, P., Stella, L., Di Salvo, T., Burderi, L., Casella, P., Sanna, A., de Martino, D., Cadelano, M., Ghedina, A., Leone, F., Meddi, F., Cretaro, P., Baglio, M. C., Poretti, E., Mignani, R. P., Torres, D. F., Israel, G. L., Cecconi, M., Russell, D. M., Gonzalez Gomez, M. D., Riverol Rodriguez, A. L., Perez Ventura, H., Hernandez Diaz, M., San Juan, J. J., Bramich, D. M., and Lewis, F.

Published
2021
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9. An X-Ray and Radio View of the 2022 Reactivation of the Magnetar SGR J1935+2154

Author

Ibrahim, A, Borghese, A, Coti Zelati, F, Parent, E, Marino, A, Ould-Boukattine, O, Rea, N, Ascenzi, S, Pacholski, D, Mereghetti, S, Israel, G, Tiengo, A, Possenti, A, Burgay, M, Turolla, S, Zane, S, Esposito, P, Götz, D, Campana, S, Kirsten, F, Gawroński, M, Hessels, J, Ibrahim, AY, Ould-Boukattine, OS, Pacholski, DP, Israel, GL, Gawroński, MP, Hessels, JWT, Ibrahim, A, Borghese, A, Coti Zelati, F, Parent, E, Marino, A, Ould-Boukattine, O, Rea, N, Ascenzi, S, Pacholski, D, Mereghetti, S, Israel, G, Tiengo, A, Possenti, A, Burgay, M, Turolla, S, Zane, S, Esposito, P, Götz, D, Campana, S, Kirsten, F, Gawroński, M, Hessels, J, Ibrahim, AY, Ould-Boukattine, OS, Pacholski, DP, Israel, GL, Gawroński, MP, and Hessels, JWT

Abstract

Recently, the Galactic magnetar SGR J1935+2154 has garnered attention due to its emission of an extremely luminous radio burst, reminiscent of fast radio bursts (FRBs). SGR J1935+2154 is one of the most active magnetars, displaying flaring events nearly every year, including outbursts as well as short and intermediate bursts. Here, we present our results on the properties of the persistent and bursting X-ray emission from SGR J1935+2154 during the initial weeks following its outburst on 2022 October 10. The source was observed with XMM-Newton and NuSTAR (quasi-)simultaneously during two epochs, separated by ∼5 days. The persistent emission spectrum is well described by an absorbed blackbody plus power-law model up to an energy of ∼25 keV. No significant changes were observed in the blackbody temperature (kT BB ∼ 0.4 keV) and emitting radius (R BB ∼ 1.9 km) between the two epochs. However, we observed a slight variation in the power-law parameters. Moreover, we detected X-ray pulsations in all the data sets and derived a spin-period derivative of P ̇ = 5.52 ( 5 ) × 10 − 11 s s−1. This is 3.8 times larger than the value measured after the first recorded outburst in 2014. Additionally, we performed quasi-simultaneous radio observations using three 25-32 m class radio telescopes for a total of 92.5 hr to search for FRB-like radio bursts and pulsed emission. However, our analysis did not reveal any radio bursts or periodic emission.

Published
2024

10. The INTEGRAL view of the pulsating hard X-ray sky: from accreting and transitional millisecond pulsars to rotation-powered pulsars and magnetars

Author

Papitto, A., Falanga, M., Hermsen, W., Mereghetti, S., Kuiper, L., Poutanen, J., Bozzo, E., Ambrosino, F., Coti Zelati, F., De Falco, V., de Martino, D., Di Salvo, T., Esposito, P., Ferrigno, C., Forot, M., Götz, D., Gouiffes, C., Iaria, R., Laurent, P., Li, J., Li, Z., Mineo, T., Moran, P., Neronov, A., Paizis, A., Rea, N., Riggio, A., Sanna, A., Savchenko, V., Słowikowska, A., Shearer, A., Tiengo, A., and Torres, D.F.

Published
2020
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11. The accretion/ejection link in the neutron star X-ray binary 4U 1820-30 I: a boundary layer-jet coupling?

Author

Marino, A, Russell, T D, Del Santo, M, Beri, A, Sanna, A, Coti Zelati, F, Degenaar, N, Altamirano, D, Ambrosi, E, Anitra, A, Carotenuto, F, D'Aì, A, Di Salvo, T, Manca, A, Motta, S E, Pinto, C, Pintore, F, Rea, N, and van den Eijnden, J

Subjects
NEUTRON stars, X-ray binaries, X-ray spectra, BLACK holes, HARD X-rays, BOUNDARY layer (Aerodynamics), SUPERCONDUCTING quantum interference devices
Abstract

The accretion flow/jet correlation in neutron star (NS) low-mass X-ray binaries (LMXBs) is far less understood when compared to black hole (BH) LMXBs. In this paper we will present the results of a dense multiwavelength observational campaign on the NS LMXB 4U 1820-30, including X-ray (NICER, NuSTAR , and AstroSat) and quasi-simultaneous radio (ATCA) observations in 2022. 4U 1820-30 shows a peculiar 170 d super-orbital accretion modulation, during which the system evolves between 'modes' of high and low X-ray flux. During our monitoring, the source did not show any transition to a full hard state. X-ray spectra were well described using a disc blackbody, a Comptonization spectrum along with a Fe K emission line at ∼6.6 keV. Our results show that the observed X-ray flux modulation is almost entirely produced by changes in the size of the region providing seed photons for the Comptonization spectrum. This region is large (∼15 km) in the high mode and likely coincides with the whole boundary layer, while it shrinks significantly (≲10 km) in low mode. The electron temperature of the corona and the observed rms variability in the hard X-rays also exhibit a slight increase in low mode. As the source moves from high to low mode, the radio emission due to the jet becomes ∼5 fainter. These radio changes appear not to be strongly connected to the hard-to-soft transitions as in BH systems, while they seem to be connected mostly to variations observed in the boundary layer. [ABSTRACT FROM AUTHOR]

Published
2023
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12. Discovery of a magnetar candidate X-ray pulsar in the Large Magellanic Cloud.

Author

Imbrogno, M, Israel, G L, Rodríguez Castillo, G A, Buckley, D A H, Coti Zelati, F, Rea, N, Monageng, I M, Casella, P, Stella, L, Haberl, F, Esposito, P, Tombesi, F, De Luca, A, and Tiengo, A

Subjects
LARGE magellanic cloud, MAGNETARS, PULSARS, MAGELLANIC clouds, X-rays, NEUTRON stars, SUPERCONDUCTING quantum interference devices
Abstract

During a systematic search for new X-ray pulsators in the XMM–Newton archive, we discovered a high amplitude (⁠|$PF\simeq 86~{{\ \rm per\ cent}}$|⁠) periodic (⁠|$P\simeq 7.25\, \mathrm{s}$|⁠) modulation in the X-ray flux of 4XMM J045626.3–694723 (J0456 hereafter), a previously unclassified source in the Large Magellanic Cloud (LMC). The period of the modulation is strongly suggestive of a spinning neutron star (NS). The source was detected only during one out of six observations in 2018–2022. Based on an absorbed power-law spectral model with photon slope of Γ ≃ 1.9, we derive a 0.3–10 keV luminosity of |$L_\mathrm{X}\simeq 2.7\times 10^{34}\, \mathrm{erg}\, \mathrm{s}^{-1}$| for a distance of 50 kpc. The X-ray properties of J0456 are at variance with those of variable LMC X-ray pulsars hosted in high-mass X-ray binary systems with a Be-star companion. Based on Southern African Large Telescope (SALT) spectroscopic observations of the only optical object that matches the X-ray uncertainty region, we cannot completely rule out that J0456 is an NS accreting from a late-type (G8-K3) star, an as-yet-unobserved binary evolutionary outcome in the Magellanic Clouds (MCs). We show that the source properties are in better agreement with those of magnetars. J0456 may thus be the second known magnetar in the LMC after SGR 0526–66. [ABSTRACT FROM AUTHOR]

Published
2023
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13. Investigating the origin of optical and X-ray pulsations of the transitional millisecond pulsar PSR J1023+0038

Author

Illiano, G., primary, Papitto, A., additional, Ambrosino, F., additional, Miraval Zanon, A., additional, Coti Zelati, F., additional, Stella, L., additional, Zampieri, L., additional, Burtovoi, A., additional, Campana, S., additional, Casella, P., additional, Cecconi, M., additional, de Martino, D., additional, Fiori, M., additional, Ghedina, A., additional, Gonzales, M., additional, Hernandez Diaz, M., additional, Israel, G. L., additional, Leone, F., additional, Naletto, G., additional, Perez Ventura, H., additional, Riverol, C., additional, Riverol, L., additional, Torres, D. F., additional, and Turchetta, M., additional

Published
2023
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14. Matter ejections behind the highs and lows of the transitional millisecond pulsar PSR J1023+0038.

Author

Baglio, M. C., Coti Zelati, F., Campana, S., Busquet, G., D'Avanzo, P., Giarratana, S., Giroletti, M., Ambrosino, F., Crespi, S., Miraval Zanon, A., Hou, X., Li, D., Li, J., Wang, P., Russell, D. M., Torres, D. F., Alabarta, K., Casella, P., Covino, S., and Bramich, D. M.

Subjects
*PULSARS, *BINARY pulsars, *SPECTRAL energy distribution, *SURVEILLANCE radar, *OPTICAL disks, *X-ray binaries, *POLARIMETRY, *ACCRETION disks
Abstract

Transitional millisecond pulsars are an emerging class of sources that link low-mass X-ray binaries to millisecond radio pulsars in binary systems. These pulsars alternate between a radio pulsar state and an active low-luminosity X-ray disc state. During the active state, these sources exhibit two distinct emission modes (high and low) that alternate unpredictably, abruptly, and incessantly. X-ray to optical pulsations are observed only during the high mode. The root cause of this puzzling behaviour remains elusive. This paper presents the results of the most extensive multi-wavelength campaign ever conducted on the transitional pulsar prototype, PSR J1023+0038, covering from the radio to X-rays. The campaign was carried out over two nights in June 2021 and involved 12 different telescopes and instruments, including XMM-Newton, HST, VLT/FORS2 (in polarimetric mode), ALMA, VLA, and FAST. By modelling the broadband spectral energy distributions in both emission modes, we show that the mode switches are caused by changes in the innermost region of the accretion disc. These changes trigger the emission of discrete mass ejections, which occur on top of a compact jet, as testified by the detection of at least one short-duration millimetre flare with ALMA at the high-to-low mode switch. The pulsar is subsequently re-enshrouded, completing our picture of the mode switches. [ABSTRACT FROM AUTHOR]

Published
2023
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17. eXTP: Enhanced X-Ray Timing and Polarimetry Mission

Author

Zhang, S. N, Feroci, M, Santangelo, A, Dong, Y. W, Feng, H, Lu, F. J, Nandra, K, Wang, Z. S, Zhang, S, Bozzo, E, Brandt, S, De Rosa, A, Gou, L. J, Hernanz, M, Van der Klis, M, LI, X. D, Liu, Y, Orleanski, P, Pareschi, G, Pohl, M, Poutanen, J, Qu, J. L, Schanne, S, Stella, L, Uttley, P, Watts, A, Xu, R. X, Yu, W. F, In 't Zand, J. J. M, Zane, S, Alvarez, L, Amati, L, Baldini, L, Bambi, C, Basso, S, Bhattacharyya, S, Bellazzini, R, Belloni, T, Bellutti, P, Bianchi, S, Brez, A, Bursa, M, Burwitz, V, Tagliaferri, G, Budtz-Jorgensen, C, Caiazzo, I, Campana, R, Cao, X. L, Casella, P, Chen, C. Y, Chen, L, Chen, T. X, Chen, Y, Chen, Y. P, Civitani, M, Coti Zelati, F, Cui, W, Cui, W. W, Dai, Z. G, Del Monte, E, De Martino, D, Di Cosimo, S, Diebold, S, Dovciak, M, Donnarumma, I, Doroshenko, V, Esposito, P, Evangelista, Y, Favre, Y, Friedrich, P, Fuschino, F, Galvez, J. L, Gao, Z. L, Ge, M. Y, Gevin, O, Goetz, D, Han, D. W, Heyl, J, Horak, J, Hu, W, Huang, F, Huang, Q. S, Hudec, R, Huppenkothen. D, Israel, G. L, Ingram, A, Karas, V, Karelin, D, Jenke, P. A, Ji, L, Kennedy, T, Korpela, S, Kunneriath, D, Labanti, C, Li, G, Li, X, Li, Z. S, Liang, E. W, Limousin, O, Lin, L, Ling, Z. X, Liu, H. B, Liu, H. W, Liu, Z, Lu, B, Lund, N, Lai, D, Luo, B, Luo, T, Ma, B, Mahmoodifar, S, Marisaldi, M, Martindale, A, Meidinger, N, Men, Y. P, Michalska, M, Mignani, R, Minuti, M, Motta, S, Muleri, F, Neilsen, J, Orlandini, M, Pan, A. T, Patruno, A, Perinati, E, Picciotto, A, Piemonte, C, Pinchera, M, Rachevski, A, Rapisarda, M, Rea, N, Rossi, E. M. R, Rubini, A, Sala, G, Shu, X. W, Sgro, C, Shen, Z. X, Soffitta, P, Song, L. M, Spandre, G, Stratta, G, Strohmayer, T. E, Sun, L, Svoboda, J, Tenzer, C, Tong, H, Taverna, R, Torok, G, Turolla, R, Vacchi, A, Wang, J, Wang, J. X, Walton, D, Wang, K, Wang, J. F, Wang, R. J, Wang, Y. F, Weng, S. S, Wilms, J, Winter, B, Wu, X, Wu, X. F, Xiong, S. L, Xu, Y. P, Xue, Y. Q, Yan, Z, Yang, S, Yang, X, Yang, Y. J, Yuan, F, Yuan, W. M, Yuan, Y. F, Zampa, G, Zampa, N, Zdziarski, A, Zhang, C, Zhang, C. L, Zhang, L, Zhang, X, Zhang, Z, Zhang, W. D, Zheng, S. J, Zhou, P, and Zhou, X. L

Subjects
Astrophysics
Abstract

eXTP is a science mission designed to study the state of matter under extreme conditions of density, gravity and magnetism. Primary goals are the determination of the equation of state of matter at supra-nuclear density, the measurement of QED effects in highly magnetized star, and the study of accretion in the strong-field regime of gravity. Primary targets include isolated and binary neutron stars, strong magnetic field systems like magnetars, and stellar-mass and supermassive black holes. The mission carries a unique and unprecedented suite of state-of-the-art scientific instruments enabling for the first time ever the simultaneous spectral-timing-polarimetry studies of cosmic sources in the energy range from 0.5-30 keV (and beyond). Key elements of the payload are: the Spectroscopic Focusing Array (SFA) - a set of 11 X-ray optics for a total effective area of approx. 0.9 m(exp. 2) and 0.6 m(exp. 2) at 2 keV and 6 keV respectively, equipped with Silicon Drift Detectors offering less than 180 eV spectral resolution; the Large Area Detector (LAD) - a deployable set of 640 Silicon Drift Detectors, for a total effective area of approx. 3.4 m(exp. 2), between 6 and 10 keV, and spectral resolution better than 250 eV; the Polarimetry Focusing Array (PFA) - a set of 2 X-ray telescope, for a total effective area of 250 cm(exp. 2) at 2 keV, equipped with imaging gas pixel photoelectric polarimeters; the Wide Field Monitor (WFM) - a set of 3 coded mask wide field units, equipped with position-sensitive Silicon Drift Detectors, each covering a 90 degrees x 90 degrees field of view. The eXTP international consortium includes major institutions of the Chinese Academy of Sciences and Universities in China, as well as major institutions in several European countries and the United States. The predecessor of eXTP, the XTP mission concept, has been selected and funded as one of the so-called background missions in the Strategic Priority Space Science Program of the Chinese Academy of Sciences since 2011. The strong European participation has significantly enhanced the scientific capabilities of eXTP. The planned launch date of the mission is earlier than 2025.

Published
2016
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18. Simultaneous X-ray and radio observations of the transitional millisecond pulsar candidate CXOU J110926.4–650224

Author

Coti Zelati, F., primary, Hugo, B., additional, Torres, D. F., additional, de Martino, D., additional, Papitto, A., additional, Buckley, D. A. H., additional, Russell, T. D., additional, Campana, S., additional, Van Rooyen, R., additional, Bozzo, E., additional, Ferrigno, C., additional, Li, J., additional, Migliari, S., additional, Monageng, I., additional, Rea, N., additional, Serylak, M., additional, Stappers, B. W., additional, and Titus, N., additional

Published
2021
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20. Evidence of intra-binary shock emission from the redback pulsar PSR J1048+2339

Author

Miraval Zanon, A., primary, D’Avanzo, P., additional, Ridolfi, A., additional, Coti Zelati, F., additional, Campana, S., additional, Tiburzi, C., additional, de Martino, D., additional, Muñoz Darias, T., additional, Bassa, C. G., additional, Zampieri, L., additional, Possenti, A., additional, Ambrosino, F., additional, Papitto, A., additional, Baglio, M. C., additional, Burgay, M., additional, Burtovoi, A., additional, Michilli, D., additional, Ochner, P., additional, and Zucca, P., additional

Published
2021
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21. The X-ray evolution and geometry of the 2018 outburst of XTE J1810−197

Author

Borghese, A, primary, Rea, N, additional, Turolla, R, additional, Rigoselli, M, additional, Alford, J A J, additional, Gotthelf, E V, additional, Burgay, M, additional, Possenti, A, additional, Zane, S, additional, Coti Zelati, F, additional, Perna, R, additional, Esposito, P, additional, Mereghetti, S, additional, Viganò, D, additional, Tiengo, A, additional, Götz, D, additional, Ibrahim, A, additional, Israel, G L, additional, Pons, J, additional, and Sathyaprakash, R, additional

Published
2021
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22. X-ray and radio follow-up observations of the X-ray transient Swift J0840.7-3516

Author

Borghese, A., Coti Zelati, F., Rea, N., Russell, T., Kennea, J.A., Evans, P., Iwakiri, W., Esposito, P., Israel, G.L., Vigano', D., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

We report on follow-up X-ray and radio observations of the transientsource Swift J0840.7-3516, which triggered the Swift BAT on February 5th (GCN 26982). Swift XRT is monitoring the source on a daily cadence.

Published
2020

23. The X-Ray Outburst of the Galactic Center Magnetar over Six Years of Chandra Observations

Author

Rea, N., primary, Coti Zelati, F., additional, Viganò, D., additional, Papitto, A., additional, Baganoff, F., additional, Borghese, A., additional, Campana, S., additional, Esposito, P., additional, Haggard, D., additional, Israel, G. L., additional, Mereghetti, S., additional, Mignani, R. P., additional, Perna, R., additional, Pons, J. A., additional, Ponti, G., additional, Stella, L., additional, Torres, D. F., additional, Turolla, R., additional, and Zane, S., additional

Published
2020
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25. Pulsating in Unison at Optical and X-Ray Energies : Simultaneous High Time Resolution Observations of the Transitional Millisecond Pulsar PSR J1023+0038

Author

Papitto, A., Ambrosino, F., Stella, L., Torres, D., Coti Zelati, F., Ghedina, A., Meddi, F., Sanna, A., Casella, P., Dallilar, Y., Eikenberry, S., Israel, G. L., Onori, F., Piranomonte, S., Bozzo, E., Burderi, L., Campana, S., de Martino, D., Di Salvo, T., Ferrigno, C., Rea, N., Riggio, A., Serrano, S., Veledina, Alexandra, Zampieri, L., Papitto, A., Ambrosino, F., Stella, L., Torres, D., Coti Zelati, F., Ghedina, A., Meddi, F., Sanna, A., Casella, P., Dallilar, Y., Eikenberry, S., Israel, G. L., Onori, F., Piranomonte, S., Bozzo, E., Burderi, L., Campana, S., de Martino, D., Di Salvo, T., Ferrigno, C., Rea, N., Riggio, A., Serrano, S., Veledina, Alexandra, and Zampieri, L.

Abstract

PSR J1023+0038 is the first millisecond pulsar discovered to pulsate in the visible band; such a detection took place when the pulsar was surrounded by an accretion disk and also showed X-ray pulsations. We report on the first high time resolution observational campaign of this transitional pulsar in the disk state, using simultaneous observations in the optical (Telescopio Nazionale Galileo, Nordic Optical Telescope, Telescopi Joan Oro), X-ray (XMM-Newton, NuSTAR, NICER), infrared (Gran Telescopio Canarias), and UV (Swift) bands. Optical and X-ray pulsations were detected simultaneously in the X-ray high-intensity mode in which the source spends similar to 70% of the time, and both disappeared in the low mode, indicating a common underlying physical mechanism. In addition, optical and X-ray pulses were emitted within a few kilometers and had similar pulse shapes and distributions of the pulsed flux density compatible with a power-law relation F-nu proportional to nu(-0.7) connecting the optical and the 0.3-45 keV X-ray band. Optical pulses were also detected during flares with a pulsed flux reduced by one-third with respect to the high mode; the lack of a simultaneous detection of X-ray pulses is compatible with the lower photon statistics. We show that magnetically channeled accretion of plasma onto the surface of the neutron star cannot account for the optical pulsed luminosity (similar to 10(31) erg s(-1)). On the other hand, magnetospheric rotation-powered pulsar emission would require an extremely efficient conversion of spin-down power into pulsed optical and X-ray emission. We then propose that optical and X-ray pulses are instead produced by synchrotron emission from the intrabinary shock that forms where a striped pulsar wind meets the accretion disk, within a few light cylinder radii away, similar to 100 km, from the pulsar., QC 20191007

Published
2019
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26. Renewed activity from the magnetar CXOU J164710.2-455216

Author

Borghese, A., Coti Zelati, F., Rea, N., Esposito, P., Mereghetti, S., Pintore, F., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

On 2018 February 5 at 19:27:11 UT, Swift BAT detected a new burst from a direction consistent with the magnetar CXOU J164710.2-455216 (trigger=808755; Barthelmy et al. 2018, GCN #22389).

Published
2018

29. Long X-ray flares from the central source in RCW 103

Author

Esposito, P., primary, De Luca, A., additional, Turolla, R., additional, Coti Zelati, F., additional, Hummel, W., additional, Tiengo, A., additional, Israel, G. L., additional, Rea, N., additional, Mignani, R. P., additional, and Borghese, A., additional

Published
2019
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30. Detailed X-ray spectroscopy of the magnetar 1E 2259+586

Author

Pizzocaro, D., primary, Tiengo, A., additional, Mereghetti, S., additional, Turolla, R., additional, Esposito, P., additional, Stella, L., additional, Zane, S., additional, Rea, N., additional, Coti Zelati, F., additional, and Israel, G., additional

Published
2019
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31. The multi-outburst activity of the magnetar in Westerlund I

Author

Borghese, A, primary, Rea, N, additional, Turolla, R, additional, Pons, J A, additional, Esposito, P, additional, Coti Zelati, F, additional, Savchenko, V, additional, Bozzo, E, additional, Perna, R, additional, Zane, S, additional, Mereghetti, S, additional, Campana, S, additional, Mignani, R P, additional, Bachetti, M, additional, Rodríguez, G, additional, Pintore, F, additional, Tiengo, A, additional, Götz, D, additional, Israel, G L, additional, and Stella, L, additional

Published
2019
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32. XIPE: the x-ray imaging polarimetry explorer

Author

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

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

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

Published
2016

33. A Wildly Flickering Jet in the Black Hole X-Ray Binary MAXI J1535-571

Author

Cristina Baglio, M., Russell, D., Casella, P., Al Noori, H., Al Yazeedi, A., Belloni, T., Buckley, D., Cadolle Bel, M., Ceccobello, C., Corbel, S., Coti Zelati, F., Díaz Trigo, M., Fender, R., Gallo, E., Gandhi, P., Homan, J., Koljonen, K., Lewis, F., Maccarone, T., Malzac, J., Markoff, S., Miller-Jones, James, O'Brien, K., Russell, T., Saikia, P., Shahbaz, T., Sivakoff, G., Soria, Roberto, Testa, V., Tetarenko, A., Van Den Ancker, M., Vincentelli, F., Cristina Baglio, M., Russell, D., Casella, P., Al Noori, H., Al Yazeedi, A., Belloni, T., Buckley, D., Cadolle Bel, M., Ceccobello, C., Corbel, S., Coti Zelati, F., Díaz Trigo, M., Fender, R., Gallo, E., Gandhi, P., Homan, J., Koljonen, K., Lewis, F., Maccarone, T., Malzac, J., Markoff, S., Miller-Jones, James, O'Brien, K., Russell, T., Saikia, P., Shahbaz, T., Sivakoff, G., Soria, Roberto, Testa, V., Tetarenko, A., Van Den Ancker, M., and Vincentelli, F.

Abstract

We report on the results of optical, near-infrared (NIR), and mid-infrared observations of the black hole X-ray binary candidate (BHB) MAXI J1535-571 during its 2017/2018 outburst. During the first part of the outburst (MJD 58004-58012), the source shows an optical-NIR spectrum that is consistent with an optically thin synchrotron power law from a jet. After MJD 58015, however, the source faded considerably, the drop in flux being much more evident at lower frequencies. Before the fading, we measure a dereddened flux density of 100 mJy in the mid-infrared, making MAXI J1535-571 one of the brightest mid-infrared BHBs known so far. A significant softening of the X-ray spectrum is evident contemporaneous with the infrared fade. We interpret it as being due to the suppression of the jet emission, similar to the accretion-ejection coupling seen in other BHBs. However, MAXI J1535-571 did not transition smoothly to the soft state, instead showing X-ray hardness deviations associated with infrared flaring. We also present the first mid-IR variability study of a BHB on minute timescales, with a fractional rms variability of the light curves of ~15%-22%, which is similar to that expected from the internal shock jet model, and much higher than the optical fractional rms (?7%). These results represent an excellent case of multiwavelength jet spectral timing and demonstrate how rich, multiwavelength time-resolved data of X-ray binaries over accretion state transitions can help in refining models of the disk-jet connection and jet launching in these systems.

Published
2018

36. XIPE

Author

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

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

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

Published
2016

37. Chandra monitoring of the Galactic Centre magnetar SGR J1745−2900 during the initial 3.5 years of outburst decay

Author

Coti Zelati, F., primary, Rea, N., additional, Turolla, R., additional, Pons, J. A., additional, Papitto, A., additional, Esposito, P., additional, Israel, G. L., additional, Campana, S., additional, Zane, S., additional, Tiengo, A., additional, Mignani, R. P., additional, Mereghetti, S., additional, Baganoff, F. K., additional, Haggard, D., additional, Ponti, G., additional, Torres, D. F., additional, Borghese, A., additional, and Elfritz, J., additional

Published
2017
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39. XIPE: the x-ray imaging polarimetry explorer

Author

Soffitta, Paolo, primary, Bellazzini, Ronaldo, additional, Bozzo, Enrico, additional, Burwitz, Vadim, additional, Castro Tirado, Alberto, additional, Costa, Enrico, additional, Courvoisier, Thierry, additional, Feng, Hua, additional, Gburek, Szymon, additional, Goosmann, Rene', additional, Karas, Vladimir, additional, Matt, Giorgio, additional, Muleri, Fabio, additional, Nandra, Kirpal, additional, Pearce, Mark, additional, Poutanen, Juri, additional, Reglero, Victor, additional, Graziati, Maria Dolores, additional, Santangelo, Andrea, additional, Tagliaferri, Gianpiero, additional, Tenzer, Christopher, additional, Vink, Jacco, additional, Weisskopf, Martin, additional, Zane, Silvia, additional, Agudo, I., additional, Antonelli, A., additional, Attina, P., additional, Baldini, L., additional, Bykov, A., additional, Carpentiero, R., additional, Cavazzuti, E., additional, Churazov, E., additional, Del Monte, E., additional, De Martino, D., additional, Donnarumma, I., additional, Doroshenko, V., additional, Evangelista, Y., additional, Ferreira, I., additional, Gallo, E., additional, Grosso, N., additional, Kaaret, P., additional, Kuulkers, E., additional, Laranaga, J., additional, Latronico, L., additional, Lumb, D. H., additional, Macian, J., additional, Malzac, J., additional, Marin, F., additional, Massaro, E., additional, Minuti, M., additional, Mundell, C., additional, Ness, J. U., additional, Oosterbroek, T., additional, Paltani, S., additional, Pareschi, G., additional, Perna, R., additional, Petrucci, P.-O., additional, Pinazo, H. B., additional, Pinchera, M., additional, Rodriguez, J. P., additional, Roncadelli, M., additional, Santovincenzo, A., additional, Sazonov, S., additional, Sgro, C., additional, Spiga, D., additional, Svoboda, J., additional, Theobald, C., additional, Theodorou, T., additional, Turolla, R., additional, Wilhelmi de Ona, E., additional, Winter, B., additional, Akbar, A. M., additional, Allan, H., additional, Aloisio, R., additional, Altamirano, D., additional, Amati, L., additional, Amato, E., additional, Angelakis, E., additional, Arezu, J., additional, Atteia, J.-L., additional, Axelsson, M., additional, Bachetti, M., additional, Ballo, L., additional, Balman, S., additional, Bandiera, R., additional, Barcons, X., additional, Basso, S., additional, Baykal, A., additional, Becker, W., additional, Behar, E., additional, Beheshtipour, B., additional, Belmont, R., additional, Berger, E., additional, Bernardini, F., additional, Bianchi, S., additional, Bisnovatyi-Kogan, G., additional, Blasi, P., additional, Blay, P., additional, Bodaghee, A., additional, Boer, M., additional, Boettcher, M., additional, Bogdanov, S., additional, Bombaci, I., additional, Bonino, R., additional, Braga, J., additional, Brandt, W., additional, Brez, A., additional, Bucciantini, N., additional, Burderi, L., additional, Caiazzo, I., additional, Campana, R., additional, Campana, S., additional, Capitanio, F., additional, Cappi, M., additional, Cardillo, M., additional, Casella, P., additional, Catmabacak, O., additional, Cenko, B., additional, Cerda-Duran, P., additional, Cerruti, C., additional, Chaty, S., additional, Chauvin, M., additional, Chen, Y., additional, Chenevez, J., additional, Chernyakova, M., additional, Cheung, C. C. T., additional, Christodoulou, D., additional, Connell, P., additional, Corbet, R., additional, Coti Zelati, F., additional, Covino, S., additional, Cui, W., additional, Cusumano, G., additional, D’Ai, A., additional, D’Ammando, F., additional, Dadina, M., additional, Dai, Z., additional, De Rosa, A., additional, de Ruvo, L., additional, Degenaar, N., additional, Del Santo, M., additional, Del Zanna, L., additional, Dewangan, G., additional, Di Cosimo, S., additional, Di Lalla, N., additional, Di Persio, G., additional, Di Salvo, T., additional, Dias, T., additional, Done, C., additional, Dovciak, M., additional, Doyle, G., additional, Ducci, L., additional, Elsner, R., additional, Enoto, T., additional, Escada, J., additional, Esposito, P., additional, Eyles, C., additional, Fabiani, S., additional, Falanga, M., additional, Falocco, S., additional, Fan, Y., additional, Fender, R., additional, Feroci, M., additional, Ferrigno, C., additional, Forman, W., additional, Foschini, L., additional, Fragile, C., additional, Fuerst, F., additional, Fujita, Y., additional, Gasent-Blesa, J. L., additional, Gelfand, J., additional, Gendre, B., additional, Ghirlanda, G., additional, Ghisellini, G., additional, Giroletti, M., additional, Goetz, D., additional, Gogus, E., additional, Gomez, J.-L., additional, Gonzalez, D., additional, Gonzalez-Riestra, R., additional, Gotthelf, E., additional, Gou, L., additional, Grandi, P., additional, Grinberg, V., additional, Grise, F., additional, Guidorzi, C., additional, Gurlebeck, N., additional, Guver, T., additional, Haggard, D., additional, Hardcastle, M., additional, Hartmann, D., additional, Haswell, C., additional, Heger, A., additional, Hernanz, M., additional, Heyl, J., additional, Ho, L., additional, Hoormann, J., additional, Horak, J., additional, Huovelin, J., additional, Huppenkothen, D., additional, Iaria, R., additional, Inam Sitki, C., additional, Ingram, A., additional, Israel, G., additional, Izzo, L., additional, Burgess, M., additional, Jackson, M., additional, Ji, L., additional, Jiang, J., additional, Johannsen, T., additional, Jones, C., additional, Jorstad, S., additional, Kajava, J. J. E., additional, Kalamkar, M., additional, Kalemci, E., additional, Kallman, T., additional, Kamble, A., additional, Kislat, F., additional, Kiss, M., additional, Klochkov, D., additional, Koerding, E., additional, Kolehmainen, M., additional, Koljonen, K., additional, Komossa, S., additional, Kong, A., additional, Korpela, S., additional, Kowalinski, M., additional, Krawczynski, H., additional, Kreykenbohm, I., additional, Kuss, M., additional, Lai, D., additional, Lan, M., additional, Larsson, J., additional, Laycock, S., additional, Lazzati, D., additional, Leahy, D., additional, Li, H., additional, Li, J., additional, Li, L., additional, Li, T., additional, Li, Z., additional, Linares, M., additional, Lister, M., additional, Liu, H., additional, Lodato, G., additional, Lohfink, A., additional, Longo, F., additional, Luna, G., additional, Lutovinov, A., additional, Mahmoodifar, S., additional, Maia, J., additional, Mainieri, V., additional, Maitra, C., additional, Maitra, D., additional, Majczyna, A., additional, Maldera, S., additional, Malyshev, D., additional, Manfreda, A., additional, Manousakis, A., additional, Manuel, R., additional, Margutti, R., additional, Marinucci, A., additional, Markoff, S., additional, Marscher, A., additional, Marshall, H., additional, Massaro, F., additional, McLaughlin, M., additional, Medina-Tanco, G., additional, Mehdipour, M., additional, Middleton, M., additional, Mignani, R., additional, Mimica, P., additional, Mineo, T., additional, Mingo, B., additional, Miniutti, G., additional, Mirac, S. M., additional, Morlino, G., additional, Motlagh, A. V., additional, Motta, S., additional, Mushtukov, A., additional, Nagataki, S., additional, Nardini, F., additional, Nattila, J., additional, Navarro, G. J., additional, Negri, B., additional, Negro, Matteo, additional, Nenonen, S., additional, Neustroev, V., additional, Nicastro, F., additional, Norton, A., additional, Nucita, A., additional, O’Brien, P., additional, O’Dell, S., additional, and Turriziani, S., additional

Published
2016
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43. The discovery, monitoring and environment of SGR J1935+2154

Author

Israel, G. L., primary, Esposito, P., additional, Rea, N., additional, Coti Zelati, F., additional, Tiengo, A., additional, Campana, S., additional, Mereghetti, S., additional, Rodriguez Castillo, G. A., additional, Götz, D., additional, Burgay, M., additional, Possenti, A., additional, Zane, S., additional, Turolla, R., additional, Perna, R., additional, Cannizzaro, G., additional, and Pons, J., additional

Published
2016
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45. Gazing at the ultraslow magnetar in RCW 103 with <italic>NuSTAR</italic> and <italic>Swift</italic>.

Author

Borghese, A, Coti Zelati, F, Esposito, P, Rea, N, De Luca, A, Bachetti, M, Israel, G L, Perna, R, and Pons, J A

Subjects
*MAGNETARS, *TELESCOPES, *BLACK body (Physics), *ASTRONOMICAL observations, *RADIOACTIVE decay
Abstract

We report on a new NuSTAR observation and on the ongoing Swift X-Ray Telescope monitoring campaign of the peculiar source 1E 161348–5055, located at the centre of the supernova remnant RCW 103, which is recovering from its last outburst in 2016 June. The X-ray spectrum at the epoch of the NuSTAR observation can be described by either two absorbed blackbodies ( $kT_{\rm BB_1}$  ∼ 0.5 keV, $kT_{\rm BB_2}$  ∼ 1.2 keV) or an absorbed blackbody plus a power law ( $kT_{\rm BB_1}$  ∼ 0.6 keV, Γ ∼ 3.9). The observed flux was ∼9 × 10−12 erg s−1 cm−2, ∼3 times lower than what observed at the outburst onset, but about one order of magnitude higher than the historical quiescent level. A periodic modulation was detected at the known 6.67 h periodicity. The spectral decomposition and evolution along the outburst decay are consistent with 1E 161348–5055 being a magnetar, the slowest ever detected. [ABSTRACT FROM AUTHOR]

Published
2018
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46. The X-ray outburst of the Galactic Centre magnetar SGR J1745−2900 during the first 1.5 year

Author

Coti Zelati, F., primary, Rea, N., additional, Papitto, A., additional, Viganò, D., additional, Pons, J. A., additional, Turolla, R., additional, Esposito, P., additional, Haggard, D., additional, Baganoff, F. K., additional, Ponti, G., additional, Israel, G. L., additional, Campana, S., additional, Torres, D. F., additional, Tiengo, A., additional, Mereghetti, S., additional, Perna, R., additional, Zane, S., additional, Mignani, R. P., additional, Possenti, A., additional, and Stella, L., additional

Published
2015
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47. Multiband study of RX J0838-2827 and XMM J083850.4-282759: a new asynchronous magnetic cataclysmic variable and a candidate transitional millisecond pulsar.

Author

Rea, N., Coti Zelati, F., Esposito, P., D'Avanzo, P., de Martino, D., Israel, G. L., Torres, D. F., Campana, S., Belloni, T. M., Papitto, A., Masetti, N., Carrasco, L., Possenti, A., Wieringa, M., De Oña Wilhelmi, E., Li, J., Bozzo, E., Ferrigno, C., Linares, M., and Tauris, T. M.

Subjects
*CATACLYSMIC variable stars, *PULSARS, *ACCRETION (Astrophysics), *X-ray emission spectroscopy, *WHITE dwarf stars
Abstract

In a search for the counterpart to the Fermi-LAT source 3FGL J0838.8-2829, we performed a multiwavelength campaign: in the X-ray band with Swift and XMM–Newton; in the infrared and optical with OAGH, ESO-NTT and IAC80; and in the radio with ATCA observations. We also used archival hard X-ray data obtained by INTEGRAL. We report on three X-ray sources consistent with the position of the Fermi-LAT source. We confirm the identification of the brightest object, RX J0838-2827, as a magnetic cataclysmic variable that we recognize as an asynchronous system (not associated with the Fermi-LAT source). RX J0838-2827 is extremely variable in the X-ray and optical bands, and timing analysis reveals the presence of several periodicities modulating its X-ray and optical emission. The most evident modulations are interpreted as being caused by the binary system orbital period of ∼1.64 h and the white dwarf spin period of ∼1.47 h. A strong flux modulation at ∼15 h is observed at all energy bands, consistent with the beat frequency between spin and orbital periods. Optical spectra show prominent Hβ, He I and He II emission lines that are Doppler-modulated at the orbital period and at the beat period. Therefore, RX J0838-2827 accretes through a disc-less configuration and could be either a strongly asynchronous polar or a rare example of a pre-polar system on its way to reaching synchronism. Regarding the other two X-ray sources, XMM J083850.4-282759 showed a variable X-ray emission, with a powerful flare lasting for ∼600 s, similar to what is observed in transitional millisecond pulsars during the subluminous disc state: this observation possibly means that this source can be associated with the Fermi-LAT source. [ABSTRACT FROM AUTHOR]

Published
2017
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48. Chandra monitoring of the Galactic Centre magnetar SGR J1745–2900 during the initial 3.5 years of outburst decay.

Author

Coti Zelati, F., Rea, N., Turolla, R., Pons, J. A., Papitto, A., Esposito, P., Israel, G. L., Campana, S., Zane, S., Tiengo, A., Mignani, R. P., Mereghetti, S., Baganoff, F. K., Haggard, D., Ponti, G., Torres, D. F., Borghese, A., and Elfritz, J.

Subjects
*GALACTIC center, *X-ray bursts, *RADIOACTIVE decay, *MAGNETARS, *MAGNETIC stars
Abstract

We report on 3.5 yr of Chandra monitoring of the Galactic Centre magnetar SGR J1745–2900 since its outburst onset in 2013 April. Themagnetar spin-down has shown at least two episodes of period derivative increases so far, and it has slowed down regularly in the past year or so. We observed a slightly increasing trend in the time evolution of the pulsed fraction, up to ~55 per cent in the most recent observations. SGR J1745–2900 has not reached the quiescent level yet, and so far the overall outburst evolution can be interpreted in terms of a cooling hot region on the star surface. We discuss possible scenarios, showing in particular how the presence of a shrinking hotspot in this source is hardly reconcilable with internal crustal cooling and favours the untwisting bundle model for this outburst. Moreover, we also show how the emission from a single uniform hotspot is incompatible with the observed pulsed fraction evolution for any pair of viewing angles, suggesting an anisotropic emission pattern. [ABSTRACT FROM AUTHOR]

Published
2017
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49. Engulfing a radio pulsar: the case of PSR J1023+0038

Author

Coti Zelati, F., primary, Baglio, M. C., additional, Campana, S., additional, D'Avanzo, P., additional, Goldoni, P., additional, Masetti, N., additional, Muñoz-Darias, T., additional, Covino, S., additional, Fender, R. P., additional, Jiménez Bailón, E., additional, Otí-Floranes, H., additional, Palazzi, E., additional, and Ramón-Fox, F. G., additional

Published
2014
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