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101. ART-XC / SRG overview

Author

Pavlinsky, Mikhail N., primary, Levin, Vasiliy, primary, Akimov, Valeriy V., primary, Krivchenko, Alexander, primary, Rotin, Alexey, primary, Kuznetsova, Maria M., primary, Lapshov, Igor Y., primary, Tkachenko, Alexey, primary, Krivonos, Roman, primary, Semena, Nikolay P., primary, Buntov, Mikhail, primary, Glushenko, Alexander, primary, Arefiev, Vadim A., primary, Yaskovich, Alexander, primary, Grebenev, Sergei, primary, Sazonov, Sergey, primary, Lutovinov, Alexander A., primary, Molkov, Sergey, primary, Serbinov, Dmitry, primary, Kudelin, Mikhail, primary, Drozdova, Tatyana, primary, Voronkov, Sergey, primary, Sunyaev, Rashid, primary, Churazov, Eugene, primary, Gilfanov, Marat, primary, Ramsey, Brian D., primary, O'Dell, Stephen L., primary, Kolodziejczak, Jeffrey, primary, Zavlin, Vyacheslav E., primary, and Swartz, Douglas A., primary

Published
2018
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107. INTEGRAL IBIS, SPI, and JEM-X observations of LVT151012

Author

Savchenko, V., Bazzano, A., Bozzo, E., Brandt, Søren, Chenevez, Jérôme, Courvoisier, T. J. L., Diehl, R., Ferrigno, C., Hanlon, L., von Kienlin, A., Kuulkers, E., Laurent, P., Lebrun, F., Lutovinov, Alexander A., Martin-Carrillo, A., Mereghetti, S., Natalucci, L., Roques, J. P., Siegert, T., Sunyaev, R., Ubertini, P., Savchenko, V., Bazzano, A., Bozzo, E., Brandt, Søren, Chenevez, Jérôme, Courvoisier, T. J. L., Diehl, R., Ferrigno, C., Hanlon, L., von Kienlin, A., Kuulkers, E., Laurent, P., Lebrun, F., Lutovinov, Alexander A., Martin-Carrillo, A., Mereghetti, S., Natalucci, L., Roques, J. P., Siegert, T., Sunyaev, R., and Ubertini, P.

Abstract

During the first observing run of LIGO, two gravitational wave events and one lower-significance trigger (LVT151012) were reported by the LIGO/Virgo collaboration. At the time of LVT151012, the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) was pointing at a region of the sky coincident with the high localization probability area of the event and thus permitted us to search for its electromagnetic counterpart (both prompt and afterglow emission). The imaging instruments on-board INTEGRAL (IBIS/ISGRI, IBIS/PICsIT, SPI, and the two JEM-X modules)have been exploited to attempt the detection of any electromagnetic emission associated with LVT151012 over 3 decades in energy (from 3 keV to 8 MeV). The omni-directional instruments on-board the satellite, i.e. the SPI-ACSand the IBIS/Veto, complemented the capabilities of the IBIS/ISGRI and IBIS/PICsIT for detections outside their imaging field of view in order to provide an efficient monitoring of the entire LVT151012 localization region at energies above 75 keV. We did not find any significant transient source that was spatially and/or temporally coincident withLVT151012, obtaining tight upper limits on the associated hard X-ray and Υ-ray radiation. For typical spectral models,the upper limits on the fluence of the emission from any 1 s long-lasting counterpart of LVT151012 ranges from FΥ =3.5×10−8 erg cm−2 (20 – 200 keV), within the field of view of the imaging instruments, to FΥ =7.1×10−7 erg cm−2 (75 – 2000 keV), considering the least favorable location of the counterpart for a detection by the omni-directionalinstruments. These results can be interpreted as a tight constrain on the ratio of the isotropic equivalent energy releasedin the electromagnetic emission to the total energy of the gravitational waves: E75−2000 keV /EGW <4.4×10−5.Finally, we provide an exhaustive summary of the capabilities of all in

Published
2017

108. INTEGRAL Observations of GW170104

Author

Savchenko, V., Ferrigno, C., Bozzo, E., Bazzano, A., Brandt, Søren, Chenevez, Jérôme, Courvoisier, T. J.-L., Diehl, R., Hanlon, L., von Kienlin, A., Kuulkers, E., Laurent, P, Lebrun, F., Lutovinov, Alexander A., Martin-Carillo, A., Mereghetti, S., Roques, J.-P., Sunyaev, R., Ubertini, P., Savchenko, V., Ferrigno, C., Bozzo, E., Bazzano, A., Brandt, Søren, Chenevez, Jérôme, Courvoisier, T. J.-L., Diehl, R., Hanlon, L., von Kienlin, A., Kuulkers, E., Laurent, P, Lebrun, F., Lutovinov, Alexander A., Martin-Carillo, A., Mereghetti, S., Roques, J.-P., Sunyaev, R., and Ubertini, P.

Abstract

We used data from the International Gamma-Ray Astrophysics Laboratory (INTEGRAL) to set upper limits on the γ-ray and hard X-ray prompt emission associated with the gravitational-wave event GW170104, discovered by the Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo collaboration. The unique omnidirectional viewing capability of the instruments on board INTEGRAL allowed us to examine the full 90% confidence level localization region of the LIGO trigger. Depending on the particular spectral model assumed and the specific position within this region, the upper limits inferred from the INTEGRAL observations range from F γ = 1.9 × 10−7 erg cm−2 to F γ = 10−6 erg cm−2 (75 keV–2 MeV energy range). This translates into a ratio between the prompt energy released in γ-rays along the direction to the observer and the gravitational-wave energy of E γ /E GW < 2.6 × 10−5. Using the INTEGRAL results, we cannot confirm the γ-ray proposed counterpart to GW170104 by the Astro—Rivelatore Gamma a Immagini Leggero (AGILE) team with the mini-Calorimeter (MCAL) instrument. The reported flux of the AGILE/MCAL event, E2, is not compatible with the INTEGRAL upper limits within most of the 90% LIGO localization region. There is only a relatively limited portion of the sky where the sensitivity of the INTEGRAL instruments was not optimal and the lowest-allowed fluence estimated for E2 would still be compatible with the INTEGRAL results. This region was also observed independently by Fermi/Gamma-ray Burst Monitor and AstroSAT, from which, as far as we are aware, there are no reports of any significant detection of a prompt high-energy event.

Published
2017

109. Luminosity dependence of the cyclotron line and evidence for the accretion regime transition in V 0332+53

Author

Doroshenko, Victor, Tsygankov, Sergey S., Mushtukov, Alexander A., Lutovinov, Alexander A., Santangelo, Andrea, Suleimanov, Valery F., Poutanen, Juri, Doroshenko, Victor, Tsygankov, Sergey S., Mushtukov, Alexander A., Lutovinov, Alexander A., Santangelo, Andrea, Suleimanov, Valery F., and Poutanen, Juri

Abstract

We report on the analysis of NuSTAR observations of the Be-transient X-ray pulsar V 0332+ 53 during the giant outburst in 2015 and another minor outburst in 2016. We confirm the cyclotronline energy-luminosity correlation previously reported in the source and the line energy decrease during the giant outburst. Based on 2016 observations, we find that a year later the line energy has increased again essentially reaching the pre-outburst values. We discuss this behaviour and conclude that it is likely caused by a change of the emission region geometry rather than previously suggested accretion-induced decay of the neutron stars magnetic field. At lower luminosities, we find for the first time a hint of departure from the anticorrelation of line energy with flux, which we interpret as a transition from super-to sub-critical accretion associated with the disappearance of the accretion column. Finally, we confirm and briefly discuss the orbital modulation observed in the outburst light curve of the source., QC 20170522

Published
2017
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110. PROPELLER EFFECT IN THE TRANSIENT X-RAY PULSAR SMC X-2

Author

Lutovinov, Alexander A., Tsygankov, Sergey S., Krivonos, Roman A., Molkov, Sergey V., Poutanen, Juri, Lutovinov, Alexander A., Tsygankov, Sergey S., Krivonos, Roman A., Molkov, Sergey V., and Poutanen, Juri

Abstract

We report the results of the monitoring campaign of the transient X-ray pulsar SMC X-2 performed with the Swift/XRT telescope over the period of 2015 September-2016 January during the Type II outburst. During this event, the bolometric luminosity of the source ranged from similar or equal to 10(39) down to several x 10(34) erg s(-1). Moreover, we discovered its dramatic drop by a factor of more than 100 below the limiting value of L-lim similar or equal to 4 x 10(36) erg s(-1), which can be interpreted as a transition to the propeller regime. These measurements make SMC X-2 the sixth pulsating X-ray source where such a transition is observed and allow us to estimate the magnetic field of the neutron star in the system B similar or equal to 3 x 10(12) G, which is in agreement with independent results of the spectral analysis.

Published
2017
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111. Towards a medium-scale axion helioscope and haloscope

Author

Anastassopoulos, Vassilis, Fischer, Horst, Gangapshev, A., Gardikiotis, Antonios, Gninenko, Sergei, Golubev, N., Hoffmann, Dieter D.H.H., Karuza, Marin, Kravchuk, Leonid, Libanov, Maxim, Lutovinov, Alexander, Avignone, Frank, Maroudas, Marios, Matveev, Viktor, Molkov, Sergey, Muratova, Valentina, Pantuev, V., Pavlinsky, Mikhail, Ptitsyna, Ksenia, Rubtsov, Grigory, Semenov, D., Sikivie, Pierre, Bykov, A., Spiridonov, A., Tiniakov, Petr, Tkachev, Igor, Troitsky, Sergey, Unzhakov, E., Zioutas, Konstantin, Cantatore, Giovanni, Cetin, Serkant Ali, Derbin, A., Drachnev, I., Djilkibaev, Rashid, Eremin, Vladimir, Anastassopoulos, Vassilis, Fischer, Horst, Gangapshev, A., Gardikiotis, Antonios, Gninenko, Sergei, Golubev, N., Hoffmann, Dieter D.H.H., Karuza, Marin, Kravchuk, Leonid, Libanov, Maxim, Lutovinov, Alexander, Avignone, Frank, Maroudas, Marios, Matveev, Viktor, Molkov, Sergey, Muratova, Valentina, Pantuev, V., Pavlinsky, Mikhail, Ptitsyna, Ksenia, Rubtsov, Grigory, Semenov, D., Sikivie, Pierre, Bykov, A., Spiridonov, A., Tiniakov, Petr, Tkachev, Igor, Troitsky, Sergey, Unzhakov, E., Zioutas, Konstantin, Cantatore, Giovanni, Cetin, Serkant Ali, Derbin, A., Drachnev, I., Djilkibaev, Rashid, and Eremin, Vladimir

Abstract

We discuss the physics case for and the concept of a medium-scale axion helioscope with sensitivities in the axion-photon coupling a few times better than CERN Axion Solar Telescope (CAST). Search for an axion-like particle with these couplings is motivated by several persistent astrophysical anomalies. We present early conceptual design, existing infrastructure, projected sensitivity and timeline of such a helioscope (Troitsk Axion Solar Telescope Experiment, TASTE) to be constructed in the Institute for Nuclear Research, Troitsk, Russia. The proposed instrument may be also used for the search of dark-matter halo axions., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2017

114. NuSTAR discovery of a cyclotron absorption line in the transient X-ray pulsar 2S 1553-542

Author

Tsygankov, Sergey S., Lutovinov, Alexander A., Krivonos, Roman A., Molkov, Sergey V., Jenke, Peter J., Finger, Mark H., Poutanen, Juri, Tsygankov, Sergey S., Lutovinov, Alexander A., Krivonos, Roman A., Molkov, Sergey V., Jenke, Peter J., Finger, Mark H., and Poutanen, Juri

Abstract

We report the results of a spectral and timing analysis of the poorly studied transient X-ray pulsar 2S 1553-542 using data collected with the NuSTAR and Chandra observatories and the Fermi/GBM instrument during an outburst in 2015. The properties of the source at high energies (>30 keV) are studied for the first time and the sky position has been essentially improved. The source broad-band spectrum has a quite complicated shape and can be reasonably described by a composite model with two continuum components - a blackbody emission with the temperature about 1 keV at low energies and a power law with an exponential cut-off at high energies. Additionally, an absorption feature at similar to 23.5 keV is discovered both in phase-averaged and phase-resolved spectra and interpreted as the cyclotron resonance scattering feature corresponding to the magnetic field strength of the neutron star B similar to 3 x 10(12) G. Based on the Fermi/ GBM data, the orbital parameters of the system were substantially improved, which allowed us to determine the spin period of the neutron star P = 9.27880(3) s and a local spin-up. (P) over dot similar or equal to -7.5 x 10(-10) s s(-1) due to the mass accretion during the NuSTAR observations. Assuming accretion from the disc and using standard torque models, we estimated the distance to the system as d = 20 +/- 4 kpc., QC 20160421

Published
2016
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120. Dramatic spectral transition of X-ray pulsar GX 304−1 in low luminous state.

Author

Tsygankov, Sergey S, Rouco Escorial, Alicia, Suleimanov, Valery F, Mushtukov, Alexander A, Doroshenko, Victor, Lutovinov, Alexander A, Wijnands, Rudy, and Poutanen, Juri

Subjects
PULSARS, NEUTRON stars, CYCLOTRONS, HEAT radiation & absorption, PULSATING stars
Abstract

We report on the discovery of a dramatic change in the energy spectrum of the X-ray pulsar GX 304−1 appearing at low luminosity. Particularly, we found that the cut-off power-law spectrum typical for accreting pulsars, including GX 304−1 at higher luminosities of L X ∼ 1036–1037 erg s−1, transformed at lower luminosity of L X ∼ 1034 erg s−1 to a two-component spectrum peaking around 5 and 40 keV. We suggest that the observed transition corresponds to a change of the dominant mechanism responsible for the deceleration of the accretion flow. We argue that the accretion flow energy at low accretion rates is released in the atmosphere of the neutron star, and the low-energy component in the source spectrum corresponds to the thermal emission of the optically thick, heated atmospheric layers. The most plausible explanations for the high-energy component are either the cyclotron emission reprocessed by the magnetic Compton scattering or the thermal radiation of deep atmospheric layers partly Comptonized in the overheated upper layers. Alternative scenarios are also discussed. [ABSTRACT FROM AUTHOR]

Published
2019
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121. Studying temporal variability of GRS 1739–278 during the 2014 outburst.

Author

Mereminskiy, Ilya A, Semena, Andrey N, Bykov, Sergey D, Filippova, Ekaterina V, Lutovinov, Alexander A, and Poutanen, Juri

Subjects
BLACK holes, GAMMA ray bursts, ACCRETION (Astrophysics), RELATIVISTIC mechanics, X-ray binaries
Abstract

We report a discovery of low-frequency quasi-periodic oscillation at 0.3–0.7 Hz in the power spectra of the accreting black hole GRS 1739–278 in the hard-intermediate state during its 2014 outburst based on the NuSTAR and Swift /XRT data. The QPO frequency strongly evolved with the source flux during the NuSTAR observation. The source spectrum became softer with rising QPO frequency and simultaneous increasing of the power-law index and decreasing of the cut-off energy. In the power spectrum, a prominent harmonic is clearly seen together with the main QPO peak. The fluxes in the soft and the hard X-ray bands are coherent, however, the coherence drops for the energy bands separated by larger gaps. The phase lags are generally positive (hard) in the 0.1–3 Hz frequency range, and negative below 0.1 Hz. The accretion disc inner radius estimated with the relativistic reflection spectral model appears to be R in < 7.3 R g. In the framework of the relativistic precession model, in order to satisfy the constraints from the observed QPO frequency and the accretion disc truncation radius, a massive black hole with M BH ≈ 100 M⊙ is required. [ABSTRACT FROM AUTHOR]

Published
2019
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122. On the radiation beaming of bright X-ray pulsars and constraints on neutron star mass–radius relation.

Author

Mushtukov, Alexander A., Verhagen, Patrick A., Tsygankov, Sergey S., van der Klis, Michiel, Lutovinov, Alexander A., and Larchenkova, Tatiana I.

Subjects
NEUTRON stars, LUMINOSITY, EDDINGTON mass limit, COSMIC magnetic fields, PULSARS
Abstract

The luminosity of accreting magnetized neutron stars can largely exceed the Eddington value due to appearance of accretion columns. The height of the columns can be comparable to the neutron star radius. The columns produce the X-rays detected by the observer directly and illuminate the stellar surface, which reprocesses the X-rays and causes additional component of the observed flux. The geometry of the column and the illuminated part of the surface determine the radiation beaming. Curved space–time affects the angular flux distribution. We construct a simple model of the beam patterns formed by direct and reflected flux from the column. We take into account the possibility of appearance of accretion columns, whose height is comparable to the neutron star radius. We argue that depending on the compactness of the star, the flux from the column can be either strongly amplified due to gravitational lensing, or significantly reduced due to column eclipse by the star. The eclipses of high accretion columns result in specific features in pulse profiles. Their detection can put constraints on the neutron star radius. We speculate that column eclipses are observed in X-ray pulsar V 0332+53, leading us to the conclusion of large neutron star radius in this system (∼15 km if M ∼ 1.4 M⊙). We point out that the beam pattern can be strongly affected by scattering in the accretion channel at high luminosity, which has to be taken into account in the models reproducing the pulse profiles. [ABSTRACT FROM AUTHOR]

Published
2018
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124. NuSTARDISCOVERY OF AN UNUSUALLY STEADY LONG-TERM SPIN-UP OF THE Be BINARY 2RXP J130159.6–635806

Author

Krivonos, Roman A., primary, Tsygankov, Sergey S., additional, Lutovinov, Alexander A., additional, Tomsick, John A., additional, Chakrabarty, Deepto, additional, Bachetti, Matteo, additional, Boggs, Steven E., additional, Chernyakova, Masha, additional, Christensen, Finn E., additional, Craig, William W., additional, Fürst, Felix, additional, Hailey, Charles J., additional, Harrison, Fiona A., additional, Lansbury, George B., additional, Rahoui, Farid, additional, Stern, Daniel, additional, and Zhang, William W., additional

Published
2015
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126. Observatory science with eXTP

Author

in ’t Zand, Jean, Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen, Hernanz, Margarita, Jenke, Peter, Maccarone, Thomas, Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena, Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas, Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils, Baglio, M., Ballantyne, David, Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward, Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward, Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert, Feroci, Marco, Fraschetti, Federico, Galloway, Duncan, Gambino, Angelo, Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig, Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter, José, Jordi, Kaastra, Jelle, Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander, Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto, Mikusincova, Romana, Miller, M., Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul, Orlandini, Mauro, Osborne, Julian, Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif, Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel, Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven, Stappers, Ben, Strohmayer, Tod, Suleimanov, Valery, Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego, Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna, Weng, ShanShan, Weinberg, Nevin, Wheatley, Peter, Wijnands, Rudy, Woods, Tyrone, Woosley, Stan, Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej, Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, and Zingale, Michael

Abstract

In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.

Published
2019
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130. Galactic survey of 44Ti sources with the IBIS telescope onboard INTEGRAL.

Author

Tsygankov, Sergey S., Krivonos, Roman A., Lutovinov, Alexander A., Revnivtsev, Mikhail G., Churazov, Eugene M., Sunyaev, Rashid A., and Grebenev, Sergey A.

Subjects
NUCLEAR excitation, TITANIUM isotopes, SUPERNOVA remnants, TELESCOPES
Abstract

We report the results of the deepest Galactic plane (|b| < 17. . 5) survey in the 67.9 and 78.4 keV nuclear de-excitation lines of titanium-44 (44Ti) performed using the data acquired with the IBIS/ISGRI instrument onboard the INTEGRAL satellite during 12 yr of operation. The peak sensitivity of our survey reached an unprecedented level of 4.8 ? 10-6 ph cm-2 s-1 (3σ) that improves the sensitivity of the survey done by Compton Gamma-Ray Observatory/COMPTEL by a factor of ~5. As a result, constraining upper limits for all sources from the catalogue of Galactic supernova remnants (SNRs; Green 2014) are derived. These upper limits can be used to estimate the exposure needed to detect 44Ti emission from any known SNR using existing and prospective X- and gamma-ray telescopes. Among the youngest Galactic SNRs, only Cas A shows significant 44Ti emission flux in good agreement with the NuSTAR measurements. We did not detect any other sources of titanium emission in the Galactic plane at significance level higher than 5σ confirming previous claims of the rarity of such 44Ti-producing SNRs. [ABSTRACT FROM AUTHOR]

Published
2016
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139. Catching Element Formation In The Act

Author

Fryer, Chris L., Timmes, Frank, Hungerford, Aimee L., Couture, Aaron, Adams, Fred, Aoki, Wako, Arcones, Almudena, Arnett, David, Auchettl, Katie, Avila, Melina, Badenes, Carles, Baron, Eddie, Bauswein, Andreas, Beacom, John, Blackmon, Jeff, Blondin, Stéphane, Bloser, Peter, Boggs, Steve, Boss, Alan, Brandt, Terri, Bravo, Eduardo, Brown, E., Brown, Peter, Bruenn, Steve, Budtz-Jørgensen, Carl, Burns, Eric, Calder, Alan, Caputo, Regina, Champagne, Art, Chevalier, Roger, Chieffi, Alessandro, Chipps, Kelly, Cinabro, David, Clarkson, Ondrea, Clayton, Don, Coc, Alain, Connolly, Devin, Conroy, Charlie, Côté, Benoit, Couch, Sean, Dauphas, Nicolas, deBoer, Richard James, Deibel, Catherine, Denisenkov, Pavel, Desch, Steve, Dessart, Luc, Diehl, Roland, Doherty, Carolyn, Domínguez, Inma, Dong, Subo, Dwarkadas, Vikram, Fan, Doreen, Fields, Brian, Fields, Carl, Filippenko, Alex, Fisher, Robert, Foucart, Francois, Fransson, Claes, Fröhlich, Carla, Fuller, George, Gibson, Brad, Giryanskaya, Viktoriya, Görres, Joachim, Goriely, Stéphane, Grebenev, Sergei, Grefenstette, Brian, Grohs, Evan, Guillochon, James, Harpole, Alice, Harris, Chelsea, Austin Harris, J., Harrison, Fiona, Hartmann, Dieter, Hashimoto, Masa-aki, Heger, Alexander, Hernanz, Margarita, Herwig, Falk, Hirschi, Raphael, Hix, Raphael William, Höflich, Peter, Hoffman, Robert, Holcomb, Cole, Hsiao, Eric, Iliadis, Christian, Janiuk, Agnieszka, Janka, Thomas, Jerkstrand, Anders, Johns, Lucas, Jones, Samuel, José, Jordi, Kajino, Toshitaka, Karakas, Amanda, Karpov, Platon, Kasen, Dan, Kierans, Carolyn, Kippen, Marc, Korobkin, Oleg, Kobayashi, Chiaki, Kozma, Cecilia, Krot, Saha, Kumar, Pawan, Kuvvetli, Irfan, Laird, Alison, Laming, (John) Martin, Larsson, Josefin, Lattanzio, John, Lattimer, James, Leising, Mark, Lennarz, Annika, Lentz, Eric, Limongi, Marco, Lippuner, Jonas, Livne, Eli, Lloyd-Ronning, Nicole, Longland, Richard, Lopez, Laura A., Lugaro, Maria, Lutovinov, Alexander, Madsen, Kristin, Malone, Chris, Matteucci, Francesca, McEnery, Julie, Meisel, Zach, Messer, Bronson, Metzger, Brian, Meyer, Bradley, Meynet, Georges, Mezzacappa, Anthony, Miller, Jonah, Miller, Richard, Milne, Peter, Misch, Wendell, Mitchell, Lee, Mösta, Philipp, Motizuki, Yuko, Müller, Bernhard, Mumpower, Matthew, Murphy, Jeremiah, Nagataki, Shigehiro, Nakar, Ehud, Nomoto, Ken'ichi, Nugent, Peter, Nunes, Filomena, O'Shea, Brian, Oberlack, Uwe, Pain, Steven, Parker, Lucas, Perego, Albino, Pignatari, Marco, Pinedo, Gabriel Martínez, Plewa, Tomasz, Poznanski, Dovi, Priedhorsky, William, Pritychenko, Boris, Radice, David, Ramirez-Ruiz, Enrico, Rauscher, Thomas, Reddy, Sanjay, Rehm, Ernst, Reifarth, Rene, Richman, Debra, Ricker, Paul, Rijal, Nabin, Roberts, Luke, Röpke, Friedrich, Rosswog, Stephan, Ruiter, Ashley J., Ruiz, Chris, Savin, Daniel Wolf, Schatz, Hendrik, Schneider, Dieter, Schwab, Josiah, Seitenzahl, Ivo, Shen, Ken, Siegert, Thomas, Sim, Stuart, Smith, David, Smith, Karl, Smith, Michael, Sollerman, Jesper, Sprouse, Trevor, Spyrou, Artemis, Starrfield, Sumner, Steiner, Andrew, Strong, Andrew W., Sukhbold, Tuguldur, Suntzeff, Nick, Surman, Rebecca, Tanimori, Toru, The, Lih-Sin, Thielemann, Friedrich-Karl, Tolstov, Alexey, Tominaga, Nozomu, Tomsick, John, Townsley, Dean, Tsintari, Pelagia, Tsygankov, Sergey, Vartanyan, David, Venters, Tonia, Vestrand, Tom, Vink, Jacco, Waldman, Roni, Wang, Lifang, Wang, Xilu, Warren, MacKenzie, West, Christopher, Craig Wheeler, J., Wiescher, Michael, Winkler, Christoph, Winter, Lisa, Wolf, Bill, Woolf, Richard, Woosley, Stan, Wu, Jin, Wrede, Chris, Yamada, Shoichi, Young, Patrick, Zegers, Remco, Zingale, Michael, and Portegies Zwart, Simon

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Astrophysics and Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

Gamma-ray astronomy explores the most energetic photons in nature to address some of the most pressing puzzles in contemporary astrophysics. It encompasses a wide range of objects and phenomena: stars, supernovae, novae, neutron stars, stellar-mass black holes, nucleosynthesis, the interstellar medium, cosmic rays and relativistic-particle acceleration, and the evolution of galaxies. MeV gamma-rays provide a unique probe of nuclear processes in astronomy, directly measuring radioactive decay, nuclear de-excitation, and positron annihilation. The substantial information carried by gamma-ray photons allows us to see deeper into these objects, the bulk of the power is often emitted at gamma-ray energies, and radioactivity provides a natural physical clock that adds unique information. New science will be driven by time-domain population studies at gamma-ray energies. This science is enabled by next-generation gamma-ray instruments with one to two orders of magnitude better sensitivity, larger sky coverage, and faster cadence than all previous gamma-ray instruments. This transformative capability permits: (a) the accurate identification of the gamma-ray emitting objects and correlations with observations taken at other wavelengths and with other messengers; (b) construction of new gamma-ray maps of the Milky Way and other nearby galaxies where extended regions are distinguished from point sources; and (c) considerable serendipitous science of scarce events -- nearby neutron star mergers, for example. Advances in technology push the performance of new gamma-ray instruments to address a wide set of astrophysical questions., 14 pages including 3 figures

140. High-mass X-ray binaries in the Milky Way: A closer look with INTEGRAL

Author

Walter, Roland, Lutovinov, Alexander, Bozzo, Enrico, Tsygankov, Sergey, Walter, Roland, Lutovinov, Alexander, Bozzo, Enrico, and Tsygankov, Sergey

Abstract

High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, whose number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified into three categories: classical/obscured, eccentric and fast transient. The classical systems feature low eccentricity and variability factor of $${\sim }10^3$$ ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood. Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind clumps, magnetic fields, neutron star rotation and eccentricity ought to be included in future modelling work. Observations with INTEGRAL in combination with other observatories were also important for detecting cyclotron resonant scattering features in spectra of X-ray pulsars, probing their variations and the geometry of the accretion column and emission regions. Finally, the unique characteristics of INTEGRAL and its long life time played a fundamental role for building a complete catalogue of HXMBs, to study the different populations of these systems in our Galaxy and to constrain some of the time scales and processes driving t

141. RX J0440.9+4431: another supercritical X-ray pulsar.

Author

Salganik, Alexander, Tsygankov, Sergey S, Doroshenko, Victor, Molkov, Sergey V, Lutovinov, Alexander A, Mushtukov, Alexander A, and Poutanen, Juri

Subjects
*PULSARS, *MAGNETIC flux density, *NEUTRON stars, *X-rays, *STELLAR magnetic fields, *ACCRETION (Astrophysics)
Abstract

In the beginning of 2023, the Be transient X-ray pulsar RX J0440.9+4431 underwent a first-ever giant outburst observed from the source peaking in the beginning of February and reaching peak luminosity of ≈4.3 × 1037 erg s−1. Here, we present the results of a detailed spectral and temporal study of the source based on NuSTAR, Swift, INTEGRAL , and NICER observations performed during this period and covering wide range of energies and luminosities. We find that both the pulse profile shape and spectral hardness change abruptly around ≈2.8 × 1037 erg s−1, which we associate with a transition to supercritical accretion regime and erection of the accretion column. The observed pulsed fraction decreases gradually with energy up to 20 keV (with a local minimum around fluorescence iron line), which is unusual for an X-ray pulsar, and then rises rapidly at higher energies with the pulsations significantly detected up to ≈120 keV. The broad-band energy spectra of RX J0440.9+4431 at different luminosity states can be approximated with a two-hump model with peaks at energies of about 10–20 and 50–70 keV previously suggested for other pulsars without additional features. In particular, an absorption feature around 30 keV previously reported and interpreted as a cyclotron line in the literature appears to be absent when using this model, so the question regarding the magnetic field strength of the neutron star remains open. Instead, we attempted to estimate field using several indirect methods and conclude that all of them point to a relatively strong field of around B ∼ 1013 G. [ABSTRACT FROM AUTHOR]

Published
2023
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142. A polarimetrically oriented X-ray stare at the accreting pulsar EXO 2030+375

Author

Christian Malacaria, Jeremy Heyl, Victor Doroshenko, Sergey S. Tsygankov, Juri Poutanen, Sofia V. Forsblom, Fiamma Capitanio, Alessandro Di Marco, Yujia Du, Lorenzo Ducci, Fabio La Monaca, Alexander A. Lutovinov, Herman L. Marshall, Ilya A. Mereminskiy, Sergey V. Molkov, Alexander A. Mushtukov, Mason Ng, Pierre-Olivier Petrucci, Andrea Santangelo, Andrey E. Shtykovsky, Valery F. Suleimanov, Iv??n Agudo, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccol?? Bucciantini, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Niccol?? Di Lalla, Immacolata Donnarumma, Michal Dov??iak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Wataru Iwakiri, Svetlana G. Jorstad, Philip Kaaret, Vladimir Karas, Fabian Kislat, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Luca Latronico, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Fr??d??ric Marin, Andrea Marinucci, Alan P. Marscher, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Chi-Yung Ng, Stephen L. O???Dell, Nicola Omodei, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Roger W. Romani, Carmelo Sgr??, Patrick Slane, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane, Malacaria, Christian, Heyl, Jeremy, Doroshenko, Victor, Tsygankov, Sergey S., Poutanen, Juri, Forsblom, Sofia V., Capitanio, Fiamma, Di Marco, Alessandro, Du, Yujia, Ducci, Lorenzo, La Monaca, Fabio, Lutovinov, Alexander A., Marshall, Herman L., Mereminskiy, Ilya A., Molkov, Sergey V., Mushtukov, Alexander A., Ng, Mason, Petrucci, PIERRE-OLIVIER, Santangelo, Andrea, Shtykovsky, Andrey E., Suleimanov, Valery F., Agudo, Iv??n, Antonelli, Lucio A., Bachetti, Matteo, Baldini, Luca, Baumgartner, Wayne H., Bellazzini, Ronaldo, Bianchi, Stefano, Bongiorno, Stephen D., Bonino, Raffaella, Brez, Alessandro, Bucciantini, Niccol??, Castellano, Simone, Cavazzuti, Elisabetta, Chen, Chien-Ting, Ciprini, Stefano, Costa, Enrico, DE ROSA, Alessandra, Del Monte, Ettore, Di Gesu, Laura, Di Lalla, Niccol??, Donnarumma, Immacolata, Dov??iak, 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, Kislat, Fabian, Kitaguchi, Takao, Kolodziejczak, Jeffery J., Krawczynski, Henric, Latronico, Luca, Liodakis, Ioanni, Maldera, Simone, Manfreda, Alberto, Marin, Fr??d??ric, Marinucci, Andrea, Marscher, Alan P., Massaro, Francesco, Matt, Giorgio, Mitsuishi, Ikuyuki, Mizuno, Tsunefumi, Muleri, Fabio, 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, Pilia, Maura, Possenti, Andrea, Puccetti, Simonetta, Ramsey, Brian D., Rankin, John, Ratheesh, Ajay, Roberts, Oliver J., Romani, Roger W., Sgr??, Carmelo, Slane, Patrick, Soffitta, Paolo, Spandre, Gloria, Swartz, Douglas A., Tamagawa, Toru, Tavecchio, Fabrizio, Taverna, Roberto, Tawara, Yuzuru, Tennant, Allyn F., Thomas, Nicholas E., Tombesi, Francesco, Trois, Alessio, Turolla, Roberto, Vink, Jacco, Weisskopf, Martin C., Wu, Kinwah, Xie, Fei, and Zane, Silvia

Published
2023

143. Polarized x-rays constrain the disk-jet geometry in the black hole x-ray binary Cygnus X-1

Author

Henric Krawczynski, Fabio Muleri, Michal Dovčiak, Alexandra Veledina, Nicole Rodriguez Cavero, Jiri Svoboda, Adam Ingram, Giorgio Matt, Javier A. Garcia, Vladislav Loktev, Michela Negro, Juri Poutanen, Takao Kitaguchi, Jakub Podgorný, John Rankin, Wenda Zhang, Andrei Berdyugin, Svetlana V. Berdyugina, Stefano Bianchi, Dmitry Blinov, Fiamma Capitanio, Niccolò Di Lalla, Paul Draghis, Sergio Fabiani, Masato Kagitani, Vadim Kravtsov, Sebastian Kiehlmann, Luca Latronico, Alexander A. Lutovinov, Nikos Mandarakas, Frédéric Marin, Andrea Marinucci, Jon M. Miller, Tsunefumi Mizuno, Sergey V. Molkov, Nicola Omodei, Pierre-Olivier Petrucci, Ajay Ratheesh, Takeshi Sakanoi, Andrei N. Semena, Raphael Skalidis, Paolo Soffitta, Allyn F. Tennant, Phillipp Thalhammer, Francesco Tombesi, Martin C. Weisskopf, Joern Wilms, Sixuan Zhang, 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, Alessandro Di Marco, Immacolata Donnarumma, Victor Doroshenko, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Jeffery J. Kolodziejczak, Fabio La Monaca, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Alan P. Marscher, Herman L. Marshall, Ikuyuki Mitsuishi, Chi-Yung Ng, Stephen L. O’Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Nicholas E. Thomas, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie, Silvia Zane, Krawczynski, Henric, Muleri, Fabio, Dovčiak, Michal, Veledina, Alexandra, Rodriguez Cavero, Nicole, Svoboda, Jiri, Ingram, Adam, Matt, Giorgio, Garcia, Javier A., Loktev, Vladislav, Negro, Michela, Poutanen, Juri, Kitaguchi, Takao, Podgorný, Jakub, Rankin, John, Zhang, Wenda, Berdyugin, Andrei, Berdyugina, Svetlana V., Bianchi, Stefano, Blinov, Dmitry, Capitanio, Fiamma, Di Lalla, Niccolò, Draghis, Paul, Fabiani, Sergio, Kagitani, Masato, Kravtsov, Vadim, Kiehlmann, Sebastian, Latronico, Luca, Lutovinov, Alexander A., Mandarakas, Niko, Marin, Frédéric, Marinucci, Andrea, Miller, Jon M., Mizuno, Tsunefumi, Molkov, Sergey V., Omodei, Nicola, Petrucci, Pierre-Olivier, Ratheesh, Ajay, Sakanoi, Takeshi, Semena, Andrei N., Skalidis, Raphael, Soffitta, Paolo, Tennant, Allyn F., Thalhammer, Phillipp, Tombesi, Francesco, Weisskopf, Martin C., Wilms, Joern, Zhang, Sixuan, Agudo, Iván, Antonelli, Lucio A., Bachetti, Matteo, Baldini, Luca, Baumgartner, Wayne H., Bellazzini, Ronaldo, Bongiorno, Stephen D., Bonino, Raffaella, Brez, Alessandro, Bucciantini, Niccolò, Castellano, Simone, Cavazzuti, Elisabetta, Ciprini, Stefano, Costa, Enrico, De Rosa, Alessandra, Del Monte, Ettore, Di Gesu, Laura, Di Marco, Alessandro, Donnarumma, Immacolata, Doroshenko, Victor, Ehlert, Steven R., Enoto, Teruaki, Evangelista, Yuri, Ferrazzoli, Riccardo, Gunji, Shuichi, Hayashida, Kiyoshi, Heyl, Jeremy, Iwakiri, Wataru, Jorstad, Svetlana G., Karas, Vladimir, Kolodziejczak, Jeffery J., La Monaca, Fabio, Liodakis, Ioanni, Maldera, Simone, Manfreda, Alberto, Marscher, Alan P., Marshall, Herman L., Mitsuishi, Ikuyuki, Ng, Chi-Yung, O’Dell, Stephen L., Oppedisano, Chiara, Papitto, Alessandro, Pavlov, George G., Peirson, Abel L., Perri, Matteo, Pesce-Rollins, Melissa, Pilia, Maura, Possenti, Andrea, Puccetti, Simonetta, Ramsey, Brian D., Romani, Roger W., Sgrò, Carmelo, Slane, Patrick, Spandre, Gloria, Tamagawa, Toru, Tavecchio, Fabrizio, Taverna, Roberto, Tawara, Yuzuru, Thomas, Nicholas E., Trois, Alessio, Tsygankov, Sergey, Turolla, Roberto, Vink, Jacco, Wu, Kinwah, Xie, Fei, Zane, Silvia, High Energy Astrophys. & Astropart. Phys (API, FNWI), Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, and Natural Sciences and Engineering Research Council of Canada

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Multidisciplinary, Settore FIS/05, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, General Relativity and Quantum Cosmology
Abstract

Full list of authors: Krawczynski, Henric; Muleri, Fabio; Dovciak, Michal; Veledina, Alexandra; Cavero, Nicole Rodriguez; Svoboda, Jiri; Ingram, Adam; Matt, Giorgio; Garcia, Javier A.; Loktev, Vladislav; Negro, Michela; Poutanen, Juri; Kitaguchi, Takao; Podgorny, Jakub; Rankin, John; Zhang, Wenda; Berdyugin, Andrei; Berdyugina, Svetlana, V; Bianchi, Stefano; Blinov, Dmitry; Capitanio, Fiamma; Di Lalla, Niccolo; Draghis, Paul; Fabiani, Sergio; Kagitani, Masato; Kravtsov, Vadim; Kiehlmann, Sebastian; Latronico, Luca; Lutovinov, Alexander A.; Mandarakas, Nikos; Marin, Frederic; Marinucci, Andrea; Miller, Jon; Mizuno, Tsunefumi; Molkov, Sergey, V; Omodei, Nicola; Petrucci, Pierre-Olivier; Ratheesh, Ajay; Sakanoi, Takeshi; Semena, Andrei N.; Skalidis, Raphael; Soffitta, Paolo; Tennant, Allyn F.; Thalhammer, Phillipp; Tombesi, Francesco; Weisskopf, Martin C.; Wilms, Joern; Zhang, Sixuan; 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 Marco, Alessandro; Donnarumma, Immacolata; Doroshenko, Victor; Ehlert, Steven R.; Enoto, Teruaki; Evangelista, Yuri; Ferrazzoli, Riccardo; Gunji, Shuichi; Hayashida, Kiyoshi; Heyl, Jeremy; Iwakiri, Wataru; Jorstad, Svetlana G.; Karas, Vladimir; Kolodziejczak, Jeffery J.; La Monaca, Fabio; Liodakis, Ioannis; Maldera, Simone; Manfreda, Alberto; Marscher, Alan P.; Marshall, Herman L.; Massaro, Francesco; Mitsuishi, Ikuyuki; Ng, Chi-Yung; O'Dell, Stephen L.; Oppedisano, Chiara; Papitto, Alessandro; Pavlov, George G.; Peirson, Abel L.; Perri, Matteo; Pesce-Rollins, Melissa; Pilia, Maura; Possenti, Andrea; Puccetti, Simonetta; Ramsey, Brian D.; Romani, Roger W.; Sgro, Carmelo; Slane, Patrick; Spandre, Gloria; Tamagawa, Toru; Tavecchio, Fabrizio; Taverna, Roberto; Tawara, Yuzuru; Thomas, Nicholas E.; Trois, Alessio; Tsygankov, Sergey; Turolla, Roberto; Vink, Jacco; Wu, Kinwah; Xie, Fei; Zane, Silvia., A black hole x-ray binary (XRB) system forms when gas is stripped from a normal star and accretes onto a black hole, which heats the gas sufficiently to emit x-rays. We report a polarimetric observation of the XRB Cygnus X-1 using the Imaging X-ray Polarimetry Explorer. The electric field position angle aligns with the outflowing jet, indicating that the jet is launched from the inner x-ray–emitting region. The polarization degree is 4.01 ± 0.20% at 2 to 8 kiloelectronvolts, implying that the accretion disk is viewed closer to edge-on than the binary orbit. These observations reveal that hot x-ray–emitting plasma is spatially extended in a plane perpendicular to, not parallel to, the jet axis. © 2022 The Authors., H.K. acknowledges NASA support under grants 80NSSC18K0264, 80NSSC22K1291, 80NSSC21K1817, and NNX16AC42G. F.Mu., J.R., S.B., S.F., A.R., P.So., E.D.M., E.Co., A.D.M., G.M., Y.E., R.F., F.L.M., M.Pe., and A.T. were funded through contract ASI-INAF-2017-12-H0. L.B., R.Bo., R.Be., A.Br., L.L., S.Ca., S.M., A.Man., C.O., M.P.-R., C.S., and G.S. were funded by the ASI through contracts ASI-INFN-2017.13-H0 and ASI-INFN 2021-43-HH.0. M.Pi. was funded through contract ASI-INAF-2022-14-HH.0. I.A. acknowledges support from MICINN (Ministerio de Ciencia e Innovación) Severo Ochoa award for the IAA-CSIC (SEV-2017-0709) and through grants AYA2016-80889-P and PID2019-107847RB-C44. M.D., J.S., and V.Ka. acknowledge support from GACR (Grantová agentura České republiky) project 21-06825X and institutional support from the Astronomical Institute of the Czech Academy of Sciences (RVO:67985815). J.A.G. acknowledges support from NASA grant 80NSSC20K0540. J.Pod. acknowledges support from Charles University project GA UK No. 174121 and from the Barrande Fellowship Programme of the Czech and French governments. A.V., J.Pou., and S.S.T. acknowledge support from Russian Science Foundation grant 20-12-00364 and the Academy of Finland grants 333112, 347003, 349144, and 349906. M.N. acknowledges support from NASA under award number 80GSFC21M0002. T.K. is supported by JSPS KAKENHI Grant Number JP19K03902. P.-O.P. acknowledges support from the High Energy National Programme (PNHE) of Centre national de la recherche scientifique (CNRS) and from the French space agency (CNES) as well as from the Barrande Fellowship Programme of the Czech and French governments. D.B., S.K., N.M., and R.S. acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program under grant agreement no. 771282. V.Kr. thanks Vilho, Yrjö and Kalle Väisälä Foundation. P.T. and J.W. acknowledge funding from Bundesministerium für Wirtschaft and Klimaschutz under Deutsches Zentrum für Luft- und Raumfahrt grant 50 OR 1909. A.I. acknowledges support from the Royal Society. J.H. acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC), funding reference number 5007110, and the Canadian Space Agency. S.G.J. and A.P.M. are supported in part by National Science Foundation grant AST-2108622, by NASA Fermi Guest Investigator grant 80NSSC21K1917, and by NASA Swift Guest Investigator grant 80NSSC22K0537. C.-Y.N. is supported by a General Research Fund of the Hong Kong Government under grant number HKU 17305419. P.Sl. acknowledges support from NASA Contract NAS8-03060.

Published
2022

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