1,315 results on '"Markoff, S"'
Search Results
202. A new lepto-hadronic model applied to the first simultaneous multiwavelength data set for Cygnus X–1
- Author
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Kantzas, D, primary, Markoff, S, additional, Beuchert, T, additional, Lucchini, M, additional, Chhotray, A, additional, Ceccobello, C, additional, Tetarenko, A J, additional, Miller-Jones, J C A, additional, Bremer, M, additional, Garcia, J A, additional, Grinberg, V, additional, Uttley, P, additional, and Wilms, J, additional
- Published
- 2020
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203. Spectral and imaging properties of Sgr A* from high-resolution 3D GRMHD simulations with radiative cooling
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Yoon, D, primary, Chatterjee, K, additional, Markoff, S B, additional, van Eijnatten, D, additional, Younsi, Z, additional, Liska, M, additional, and Tchekhovskoy, A, additional
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- 2020
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204. Observational signatures of disc and jet misalignment in images of accreting black holes
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Chatterjee, K, primary, Younsi, Z, additional, Liska, M, additional, Tchekhovskoy, A, additional, Markoff, S B, additional, Yoon, D, additional, van Eijnatten, D, additional, Hesp, C, additional, Ingram, A, additional, and van der Klis, M B M, additional
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- 2020
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205. Rapid compact jet quenching in the Galactic black hole candidate X-ray binary MAXI J1535−571
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Russell, T D, primary, Lucchini, M, additional, Tetarenko, A J, additional, Miller-Jones, J C A, additional, Sivakoff, G R, additional, Krauß, F, additional, Mulaudzi, W, additional, Baglio, M C, additional, Russell, D M, additional, Altamirano, D, additional, Ceccobello, C, additional, Corbel, S, additional, Degenaar, N, additional, van den Eijnden, J, additional, Fender, R, additional, Heinz, S, additional, Koljonen, K I I, additional, Maitra, D, additional, Markoff, S, additional, Migliari, S, additional, Parikh, A S, additional, Plotkin, R M, additional, Rupen, M, additional, Sarazin, C, additional, Soria, R, additional, and Wijnands, R, additional
- Published
- 2020
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206. Relativistic AGN jets – III. Synthesis of synchrotron emission from double-double radio galaxies
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Walg, S, primary, Achterberg, A, additional, Markoff, S, additional, Keppens, R, additional, and Porth, O, additional
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- 2020
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207. SYMBA: An end-to-end VLBI synthetic data generation pipeline
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Roelofs, F., primary, Janssen, M., additional, Natarajan, I., additional, Deane, R., additional, Davelaar, J., additional, Olivares, H., additional, Porth, O., additional, Paine, S. N., additional, Bouman, K. L., additional, Tilanus, R. P. J., additional, van Bemmel, I. M., additional, Falcke, H., additional, Akiyama, K., additional, Alberdi, A., additional, Alef, W., additional, Asada, K., additional, Azulay, R., additional, Baczko, A., additional, Ball, D., additional, Baloković, M., additional, Barrett, J., additional, Bintley, D., additional, Blackburn, L., additional, Boland, W., additional, Bower, G. C., additional, Bremer, M., additional, Brinkerink, C. D., additional, Brissenden, R., additional, Britzen, S., additional, Broderick, A. E., additional, Broguiere, D., additional, Bronzwaer, T., additional, Byun, D., additional, Carlstrom, J. E., additional, Chael, A., additional, Chan, C., additional, Chatterjee, S., additional, Chatterjee, K., additional, Chen, M., additional, Chen, Y., additional, Cho, I., additional, Christian, P., additional, Conway, J. E., additional, Cordes, J. M., additional, Crew, G. B., additional, Cui, Y., additional, De Laurentis, M., additional, Dempsey, J., additional, Desvignes, G., additional, Dexter, J., additional, Doeleman, S. S., additional, Eatough, R. P., additional, Fish, V. L., additional, Fomalont, E., additional, Fraga-Encinas, R., additional, Friberg, P., additional, Fromm, C. M., additional, Gómez, J. L., additional, Galison, P., additional, Gammie, C. F., additional, García, R., additional, Gentaz, O., additional, Georgiev, B., additional, Goddi, C., additional, Gold, R., additional, Gu, M., additional, Gurwell, M., additional, Hada, K., additional, Hecht, M. H., additional, Hesper, R., additional, Ho, L. C., additional, Ho, P., additional, Honma, M., additional, Huang, C. L., additional, Huang, L., additional, Hughes, D. H., additional, Ikeda, S., additional, Inoue, M., additional, Issaoun, S., additional, James, D. J., additional, Jannuzi, B. T., additional, Jeter, B., additional, Jiang, W., additional, Johnson, M. D., additional, Jorstad, S., additional, Jung, T., additional, Karami, M., additional, Karuppusamy, R., additional, Kawashima, T., additional, Keating, G. K., additional, Kettenis, M., additional, Kim, J., additional, Kino, M., additional, Koay, J. Y., additional, Koch, P. M., additional, Koyama, S., additional, Kramer, M., additional, Kramer, C., additional, Krichbaum, T. P., additional, Kuo, C., additional, Lauer, T. R., additional, Lee, S., additional, Li, Y., additional, Li, Z., additional, Lindqvist, M., additional, Lico, R., additional, Liu, K., additional, Liuzzo, E., additional, Lo, W., additional, Lobanov, A. P., additional, Loinard, L., additional, Lonsdale, C., additional, Lu, R., additional, MacDonald, N. R., additional, Mao, J., additional, Markoff, S., additional, Marrone, D. P., additional, Marscher, A. P., additional, Martí-Vidal, I., additional, Matsushita, S., additional, Matthews, L. D., additional, Medeiros, L., additional, Menten, K. M., additional, Mizuno, Y., additional, Mizuno, I., additional, Moran, J. M., additional, Moriyama, K., additional, Moscibrodzka, M., additional, Müller, C., additional, Nagai, H., additional, Nagar, N. M., additional, Nakamura, M., additional, Narayan, R., additional, Narayanan, G., additional, Neri, R., additional, Ni, C., additional, Noutsos, A., additional, Okino, H., additional, Ortiz-León, G. N., additional, Oyama, T., additional, Özel, F., additional, Palumbo, D. C. M., additional, Patel, N., additional, Pen, U., additional, Pesce, D. W., additional, Piétu, V., additional, Plambeck, R., additional, PopStefanija, A., additional, Prather, B., additional, Preciado-López, J. A., additional, Psaltis, D., additional, Pu, H., additional, Ramakrishnan, V., additional, Rao, R., additional, Rawlings, M. G., additional, Raymond, A. W., additional, Rezzolla, L., additional, Ripperda, B., additional, Rogers, A., additional, Ros, E., additional, Rose, M., additional, Roshanineshat, A., additional, Rottmann, H., additional, Roy, A. L., additional, Ruszczyk, C., additional, Ryan, B. R., additional, Rygl, K. L. J., additional, Sánchez, S., additional, Sánchez-Arguelles, D., additional, Sasada, M., additional, Savolainen, T., additional, Schloerb, F. P., additional, Schuster, K., additional, Shao, L., additional, Shen, Z., additional, Small, D., additional, Won Sohn, B., additional, SooHoo, J., additional, Tazaki, F., additional, Tiede, P., additional, Titus, M., additional, Toma, K., additional, Torne, P., additional, Traianou, E., additional, Trent, T., additional, Trippe, S., additional, Tsuda, S., additional, van Langevelde, H. J., additional, van Rossum, D. R., additional, Wagner, J., additional, Wardle, J., additional, Weintroub, J., additional, Wex, N., additional, Wharton, R., additional, Wielgus, M., additional, Wong, G. N., additional, Wu, Q., additional, Young, A., additional, Young, K., additional, Younsi, Z., additional, Yuan, F., additional, Yuan, Y., additional, Zensus, J. A., additional, Zhao, G., additional, Zhao, S., additional, and Zhu, Z., additional
- Published
- 2020
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208. The Chandra High-resolution X-Ray Spectrum of Quiescent Emission from Sgr A*
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Corrales, Lia, primary, Baganoff, F. K., additional, Wang, Q. D., additional, Nowak, M., additional, Neilsen, J., additional, Markoff, S., additional, Haggard, D., additional, Davis, J., additional, Houck, J., additional, and Principe, D., additional
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- 2020
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209. High-energy cosmic ray production in X-ray binary jets
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Cooper, A J, primary, Gaggero, D, additional, Markoff, S, additional, and Zhang, S, additional
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- 2020
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210. A radio parallax to the black hole X-ray binary MAXI J1820+070
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Atri, P, primary, Miller-Jones, J C A, additional, Bahramian, A, additional, Plotkin, R M, additional, Deller, A T, additional, Jonker, P G, additional, Maccarone, T J, additional, Sivakoff, G R, additional, Soria, R, additional, Altamirano, D, additional, Belloni, T, additional, Fender, R, additional, Koerding, E, additional, Maitra, D, additional, Markoff, S, additional, Migliari, S, additional, Russell, D, additional, Russell, T, additional, Sarazin, C L, additional, Tetarenko, A J, additional, and Tudose, V, additional
- Published
- 2020
- Full Text
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211. Disc-jet Coupling in the 2009 Outburst of the Black Hole Candidate H1743-322
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Miller-Jones, J. C. A, Sivakoff, G. R, Altamirano, D, Coriat, M, Corbel, S, Dhawan, V, Krimm, H. A, Remillard, R. A, Rupen, M. P, Russell, D. M, Fender, R. P, Heinz, S, Kording, E. G, Maitra, D, Markoff, S, Migliari, S, Sarazin, C. L, and Tudose, V
- Subjects
Astrophysics - Abstract
We present an intensive radio and X-ray monitoring campaign on the 2009 outburst of the Galactic black hole candidate X-ray binary H1743-322. With the high angular resolution of the Very Long Baseline Array, we resolve the jet ejection event and measure the proper motions of the jet ejecta relative to the position of the compact core jets detected at the beginning of the outburst. This allows us to accurately couple the moment when the jet ejection event occurred with X-ray spectral and timing signatures. We find that X-ray timing signatures are the best diagnostic of the jet ejection event in this outburst, which occurred as the X-ray variability began to decrease and the Type C quasi-periodic oscillations disappeared from the X-ray power density spectrum. However, this sequence of events does not appear to be replicated in all black hole X-ray binary outbursts, even within an individual source. In our observations of H1743-322, the ejection was contemporaneous with a quenching of the radio emission, prior to the start of the major radio flare. This contradicts previous assumptions that the onset of the radio flare marks the moment of ejection. The jet speed appears to vary between outbursts with a positive correlation outburst luminosity. The compact core radio jet reactivated on transition to the hard intermediate state at the end of the outburst and not when the source reached the low hard spectral state. Comparison with the known near-infrared behaviour of the compact jets suggests a gradual evolution of the compact jet power over a few days near beginning the and end of an outburst
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- 2012
212. The Microquasar Cyg X-1: A Short Review
- Author
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Nowak, M. A, Wilms, J, Hanke, M, Pottschmidt, K, and Markoff, S
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Astrophysics - Abstract
We review the spectral properties of the black hole candidate Cygnus X-I. Specifically, we discuss two recent sets of multi-satellite observations. One comprises a 0.5-500 keY spectrum, obtained with eve!)' flying X-ray satellite at that time, that is among the hardest Cyg X-I spectra observed to date. The second set is comprised of 0.5-40 keV Chandra-HETG plus RXTE-PCA spectra from a radio-quiet, spectrally soft state. We first discuss the "messy astrophysics" often neglected in the study of Cyg X-I, i.e., ionized absorption from the wind of the secondary and the foreground dust scattering halo. We then discuss components common to both state extremes: a low temperature accretion disk, and a relativistically broadened Fe line and reflection. Hard state spectral models indicate that the disk inner edge does not extend beyond > or approx.= 40 GM/sq c , and may even approach as close as approx. = 6GM/sq c. The soft state exhibits a much more prominent disk component; however, its very low normalization plausibly indicates a spinning black hole in the Cyg X-I system. Key words. accretion, accretion disks - black hole physics - X-rays:binaries
- Published
- 2011
213. prototype X-ray binary GX 339–4: using TeV γ-rays to assess LMXBs as Galactic cosmic ray accelerators.
- Author
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Kantzas, D, Markoff, S, Lucchini, M, Ceccobello, C, Grinberg, V, Connors, R M T, and Uttley, P
- Subjects
- *
GALACTIC cosmic rays , *COSMIC rays , *X-ray binaries , *STELLAR black holes , *SUPERMASSIVE black holes , *RELATIVISTIC particles - Abstract
Since the discovery of cosmic rays (CRs) over a century ago, their origin remains an open question. Galactic CRs with energy up to the knee (1015 eV) are considered to originate from supernova remnants, but this scenario has recently been questioned due to lack of TeV γ-ray counterparts in many cases. Extragalactic CRs, on the other hand, are thought to be associated with accelerated particles in the relativistic jets launched by supermassive accreting black holes at the centre of galaxies. Scaled down versions of such jets have been detected in X-ray binaries hosting a stellar black hole (BHXBs). In this work, we investigate the possibility that the smaller scale jets in transient outbursts of low-mass BHXBs could be sources of Galactic CRs. To better test this scenario, we model the entire electromagnetic spectrum of such sources focusing on the potential TeV regime, using the 'canonical' low-mass BHXB GX 339–4 as a benchmark. Taking into account both the leptonic radiative processes and the γ-rays produced via neutral pion decay from inelastic hadronic interactions, we predict the GeV and TeV γ-ray spectrum of GX 339–4 using lower frequency emission as constraints. Based on this test-case of GX 339–4, we investigate whether other, nearby low-mass BHXBs could be detected by the next-generation very-high-energy γ-ray facility the Cherenkov Telescope Array, which would establish them as additional and numerous potential sources of CRs in the Galaxy. [ABSTRACT FROM AUTHOR]
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- 2022
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214. A Swift study of long-term changes in the X-ray flaring properties of Sagittarius A.
- Author
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Andrés, A, van den Eijnden, J, Degenaar, N, Evans, P A, Chatterjee, K, Reynolds, M, Miller, J M, Kennea, J, Wijnands, R, Markoff, S, Altamirano, D, Heinke, C O, Bahramian, A, Ponti, G, and Haggard, D
- Subjects
SOLAR flares ,SUPERMASSIVE black holes ,X-rays - Abstract
The radiative counterpart of the supermassive black hole at the Galactic Centre, Sagittarius A*, displays flaring emission in the X-ray band atop a steady, quiescent level. Flares are also observed in the near-infrared band. The physical process producing the flares is not fully understood and it is unclear if the flaring rate varies, although some recent works suggest it has reached unprecedented variability in recent years. Using over a decade of regular X-ray monitoring of Neil Gehrels Swift Observatory, we studied the variations in count rate of Sgr A* on time-scales of years. We decomposed the X-ray emission into quiescent and flaring emission, modelled as a constant and power-law process, respectively. We found that the complete, multiyear data set cannot be described by a stationary distribution of flare fluxes, while individual years follow this model better. In three of the ten studied years, the data is consistent with a purely Poissonian quiescent distribution, while for 5 yr, only an upper limit of the flare flux distribution parameter could be determined. We find that these possible changes cannot be explained fully by the different number of observations per year. Combined, these results are instead consistent with a changing flaring rate of Sgr A*, appearing more active between 2006–2007 and 2017–2019, than between 2008–2012. Finally, we discuss this result in the context of flare models and the passing of gaseous objects, and discuss the extra statistical steps taken, for instance, to deal with the background in the Swift observations. [ABSTRACT FROM AUTHOR]
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- 2022
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215. Flares from a candidate Galactic magnetar suggest a missing link to dim isolated neutron stars
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Castro-Tirado, A. J., Postigo, A. de Ugarte, Gorosabel, J., Jelínek, M., Fatkhullin, T. A., Sokolov, V. V., Ferrero, P., Kann, D. A., Klose, S., Sluse, D., Bremer, M., Winters, J. M., Nuernberger, D., Pérez-Ramírez, D., Guerrero, M. A., French, J., Melady, G., Hanlon, L., McBreen, B., Leventis, K., Markoff, S. B., Leon, S., Kraus, A., Aceituno, F. J., Cunniffe, R., Kubánek, P., Vítek, S., Schulze, S., Wilson, A. C., Hudec, R., Durant, M., González-Pérez, J. M., Shahbaz, T., Guziy, S., Pandey, S. B., Pavlenko, L., Sonbas, E., Trushkin, S. A., Bursov, N. N., Nizhelskij, N. A., Sánchez-Fernández, C., and Sabau-Graziati, L.
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- 2008
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216. Corrigendum: A large light-mass component of cosmic rays at 10171017.5 electronvolts from radio observations
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Buitink, S., Corstanje, A., Falcke, H., Hrandel, J. R., Huege, T., Nelles, A., Rachen, J. P., Rossetto, L., Schellart, P., Scholten, O., ter Veen, S., Thoudam, S., Trinh, T. N. G., Anderson, J., Asgekar, A., Avruch, I. M., Bell, M. E., Bentum, M. J., Bernardi, G., Best, P., Bonafede, A., Breitling, F., Broderick, J. W., Brouw, W. N., Brggen, M., Butcher, H. R., Carbone, D., Ciardi, B., Conway, J. E., de Gasperin, F., de Geus, E., Deller, A., Dettmar, R.-J., van Diepen, G., Duscha, S., Eislffel, J., Engels, D., Enriquez, J. E., Fallows, R. A., Fender, R., Ferrari, C., Frieswijk, W., Garrett, M. A., Griemeier, J. M., Gunst, A. W., van Haarlem, M. P., Hassall, T. E., Heald, G., Hessels, J. W. T., Hoeft, M., Horneffer, A., Iacobelli, M., Intema, H., Juette, E., Karastergiou, A., Kondratiev, V. I., Kramer, M., Kuniyoshi, M., Kuper, G., van Leeuwen, J., Loose, G. M., Maat, P., Mann, G., Markoff, S., McFadden, R., McKay-Bukowski, D., McKean, J. P., Mevius, M., Mulcahy, D. D., Munk, H., Norden, M. J., Orru, E., Paas, H., Pandey-Pommier, M., Pandey, V. N., Pietka, M., Pizzo, R., Polatidis, A. G., Reich, W., Rttgering, H. J. A., Scaife, A. M. M., Schwarz, D. J., Serylak, M., Sluman, J., Smirnov, O., Stappers, B. W., Steinmetz, M., Stewart, A., Swinbank, J., Tagger, M., Tang, Y., Tasse, C., Toribio, M. C., Vermeulen, R., Vocks, C., Vogt, C., van Weeren, R. J., Wijers, R. A. M. J., Wijnholds, S. J., Wise, M. W., Wucknitz, O., Yatawatta, S., Zarka, P., and Zensus, J. A.
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Environmental issues ,Science and technology ,Zoology and wildlife conservation - Abstract
Author(s): S. Buitink; A. Corstanje; H. Falcke; J. R. Hrandel; T. Huege; A. Nelles; J. P. Rachen; L. Rossetto; P. Schellart; O. Scholten; S. ter Veen; S. Thoudam; T. N. [...]
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- 2016
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217. The unique case of the active galactic nucleus core of M87: a misaligned low-power blazar?
- Author
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Lucchini, M., Krauß, F., Markoff, S., High Energy Astrophys. & Astropart. Phys (API, FNWI), GRAPPA (ITFA, IoP, FNWI), and Gravitation and Astroparticle Physics Amsterdam
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Cosmology and Extragalactic Astrophysics - Abstract
M87 hosts one of the closest jetted active galactic nuclei (AGN) to Earth. Thanks to its vicinity and to the large mass of its central black hole, M87 is the only source in which the jet can be directly imaged down to near-event horizon scales with radio very large baseline interferometry. This property makes M87 a unique source to isolate and study jet launching, acceleration, and collimation. In this paper, we employ a multizone model designed as a parametrization of general relativistic magnetohydrodynamics (GRMHD); for the first time, we reproduce the jet’s observed shape and multiwavelength spectral energy distribution simultaneously. We find strong constraints on key physical parameters of the jet, such as the location of particle acceleration and the kinetic power. However, we underpredict the (unresolved) gamma-ray flux of the source, implying that the high-energy emission does not originate in the magnetically dominated inner jet regions. Our results have important implications both for comparisons of GRMHD simulations with observations and for unified models of AGN classes.
- Published
- 2019
218. X-Ray Imaging of the Jet From the Supermassive Black Hole M87
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Anczarski, J., Nielsen, J., Markoff, S., Nowak, M., Haggard, D., Baganoff, F.K., and High Energy Astrophys. & Astropart. Phys (API, FNWI)
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
The supermassive black hole, M87, has long been a target of interest for the study of black hole physics and relativistic jets across the electromagnetic spectrum. In April 2017, the Event Horizon Telescope and many ground- and space-based observatories undertook a campaign to study nearby supermassive black holes, including M87, at many wavelengths. With the inclusion of phased ALMA, the EHT data should have sufficient resolution to image the event horizon of the black hole. As part of this campaign, we observed M87 with the Chandra X-ray Observatory for a total of 26.24 ks over two exposures, enabling us to study M87 at high energy. We report the results of imaging and spectroscopy of the X-ray jet, focusing on the X-ray nucleus, which includes emission from both the core and a bright knot in the jet called HST-1. We present a deconvolved image to explore the relative intensity of the core and HST-1. Our analysis of this deconvolved image suggests that HST-1 was significantly fainter than the core. We found no evidence of strong variability in the X-ray brightness during our observation, but compared to the historically recorded spectra of the core, we discovered a slight decrease in the photon index (to Γ=2.05+0.06/-0.07, compared to a typical value of Γ=2.25+/-0.10 in the recent past). M87 was also fainter than in recent observations (LX~1.25x1041 erg s-1). In light of the historical variability of HST-1, we explore the possibility that the lower photon index may be due to a smaller HST-1 contribution to the nuclear emission.
- Published
- 2019
219. Exploring the role of jets in X-ray binaries and low-luminosity AGN
- Author
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Markoff, S., Nowak, M., Falcke, H., Maccarone, T., and Fender, R.
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- 2004
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220. ALMA observations of A0620–00: Fresh clues on the nature of quiescent black hole X-ray binary jets
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Gallo, E., Teague, R., Plotkin, Richard, Miller-Jones, James, Russell, D.M., Dinçer, T., Bailyn, C., Maccarone, T.J., Markoff, S., Fender, R.P., Gallo, E., Teague, R., Plotkin, Richard, Miller-Jones, James, Russell, D.M., Dinçer, T., Bailyn, C., Maccarone, T.J., Markoff, S., and Fender, R.P.
- Abstract
© 2019 The Author(s). We report on Atacama Large Millimeter Array (ALMA) continuum observations of the black hole X-ray binary A0620–00 at an X-ray luminosity nine orders of magnitude sub-Eddington. The system was significantly detected at 98 GHz (at 44 ± 7 μJy) and only marginally at 233 GHz (20 ± 8 μJy), about 40 d later. These results suggest either an optically thin sub-mm synchrotron spectrum, or highly variable sub-mm jet emission on month time-scales. Although the latter appears more likely, we note that, at the time of the ALMA observations, A0620–00 was in a somewhat less active optical-IR state than during all published multiwavelength campaigns when a flat-spectrum, partially self-absorbed jet has been suggested to extend from the radio to the mid-IR regime. Either interpretation is viable in the context of an internal shock model, where the jet’s spectral shape and variability are set by the power density spectrum of the shells’ Lorentz factor fluctuations. While strictly simultaneous radio–mm-IR observations are necessary to draw definitive conclusions for A0620–00, the data presented here, in combination with recent radio and sub-mm results from higher luminosity systems, demonstrate that jets from black hole X-ray binaries exhibit a high level of variability – either in flux density or intrinsic spectral shape, or both – across a wide spectrum of Eddington ratios. This is not in contrast with expectations from an internal shock model, where lower jet power systems can be expected to exhibit larger fractional variability owing to an overall decrease in synchrotron absorption.
- Published
- 2019
221. A black hole X-ray binary at similar to 100 Hz : multiwavelength timing of MAXIJ1820+070 with HiPERCAM and NICER
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Paice, J. A., Gandhi, P., Shahbaz, T., Uttley, P., Arzoumanian, Z., Charles, P. A., Dhillon, V. S., Gendreau, K. C., Littlefair, S. P., Malzac, J., Markoff, S., Marsh, T. R., Misra, R., Russell, D. M., Veledina, Alexandra, Paice, J. A., Gandhi, P., Shahbaz, T., Uttley, P., Arzoumanian, Z., Charles, P. A., Dhillon, V. S., Gendreau, K. C., Littlefair, S. P., Malzac, J., Markoff, S., Marsh, T. R., Misra, R., Russell, D. M., and Veledina, Alexandra
- Abstract
We report on simultaneous sub-second optical and X-ray timing observations of the low-mass X-ray binary black hole candidate MAXI J1820+070. The bright 2018 outburst rise allowed simultaneous photometry in five optical bands (ugrizs) with HiPERCAM/GTC (Optical) at frame rates over 100 Hz, together with NICER/ISS observations (X-rays). Intense (factor of 2) red flaring activity in the optical is seen over a broad range of time-scales down to similar to 10 ms. Cross-correlating the bands reveals a prominent anticorrelation on time-scales of similar to seconds, and a narrow sub-second correlation at a lag of approximate to+165 ms (optical lagging X-rays). This lag increases with optical wavelength, and is approximately constant over Fourier frequencies of similar to 0.3-10 Hz. These features are consistent with an origin in the inner accretion flow and jet base within similar to 5000 Gravitational radii. An additional similar to+5 s lag feature may be ascribable to disc reprocessing. MAXI J1820+070 is the third black hole transient to display a clear similar to 0.1 s optical lag, which may be common feature in such objects. The sub-second lag variation with wavelength is novel, and may allow constraints on internal shock jet stratification models., QC 20200324
- Published
- 2019
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222. Introduction to CTA Science
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Acharya, B. S., Agudo, I., Al Samarai, I., Alfaro, R., Alfaro, J., Alispach, C., Batista, R. Alves, Amans, J. -P, Amato, E., Ambrosi, G., Antolini, E., Antonelli, L. A., Aramo, C., Araya, M., Armstrong, T., Arqueros, F., Arrabito, L., Asano, K., Ashley, M., Backes, M., Balazs, C., Balbo, M., Ballester, O., Ballet, J., Bamba, A., Barkov, M., Barres de Almeida, U., Barrio, J. A., Bastieri, D., Becherini, Yvonne, Belfiore, A., Benbow, W., Berge, D., Bernardini, E., Bernardini, M. G., Bernardos, M., Bernloehr, K., Bertucci, B., Biasuzzi, B., Bigongiari, C., Biland, A., Bissaldi, E., Biteau, J., Blanch, O., Blazek, J., Boisson, C., Bolmont, J., Bonanno, G., Bonardi, A., Bonavolonta, C., Bonnoli, G., Bosnjak, Z., Bottcher, M., Braiding, C., Bregeon, J., Brill, A., Brown, A. 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A., Wischnewski, R., Wood, M., Yamamoto, T., Yamazaki, R., Yanagita, S., Yang, L., Yoshida, T., Yoshiike, S., Yoshikoshi, T., Zacharias, M., Zaharijas, G., Zampieri, L., Zandanel, F., Zanin, R., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. I., Ziegler, A., and Zorn, J.
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- 2019
- Full Text
- View/download PDF
223. Disk-Jet Coupling in the 2017/2018 Outburst of the Galactic Black Hole Candidate X-Ray Binary MAXI J1535-571
- Author
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Russell, T.D., Tetarenko, A.J., Miller-Jones, James, Sivakoff, G.R., Parikh, A.S., Rapisarda, S., Wijnands, R., Corbel, S., Tremou, E., Altamirano, D., Baglio, M.C., Ceccobello, C., Degenaar, N., Eijnden, J.V.D., Fender, R., Heywood, I., Krimm, H.A., Lucchini, M., Markoff, S., Russell, D.M., Soria, Roberto, Woudt, P.A., Russell, T.D., Tetarenko, A.J., Miller-Jones, James, Sivakoff, G.R., Parikh, A.S., Rapisarda, S., Wijnands, R., Corbel, S., Tremou, E., Altamirano, D., Baglio, M.C., Ceccobello, C., Degenaar, N., Eijnden, J.V.D., Fender, R., Heywood, I., Krimm, H.A., Lucchini, M., Markoff, S., Russell, D.M., Soria, Roberto, and Woudt, P.A.
- Abstract
MAXI J1535-571 is a Galactic black hole candidate X-ray binary that was discovered going into outburst in 2017 September. In this paper, we present comprehensive radio monitoring of this system using the Australia Telescope Compact Array, as well as the MeerKAT radio observatory, showing the evolution of the radio jet during its outburst. Our radio observations show the early rise and subsequent quenching of the compact jet as the outburst brightened and then evolved toward the soft state. We constrain the compact jet quenching factor to be more than 3.5 orders of magnitude. We also detected and tracked (for 303 days) a discrete, relativistically moving jet knot that was launched from the system. From the motion of the apparently superluminal knot, we constrain the jet inclination (at the time of ejection) and speed to ≤45° and ≥0.69 c, respectively. Extrapolating its motion back in time, our results suggest that the jet knot was ejected close in time to the transition from the hard intermediate state to soft intermediate state. The launching event also occurred contemporaneously with a short increase in X-ray count rate, a rapid drop in the strength of the X-ray variability, and a change in the type-C quasi-periodic oscillation (QPO) frequency that occurs >2.5 days before the first appearance of a possible type-B QPO.
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- 2019
224. The Event Horizon General Relativistic Magnetohydrodynamic Code Comparison Project
- Author
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National Science Foundation (US), Netherlands Organization for Scientific Research, European Research Council, Gauss Centre for Supercomputing, Department of Energy (US), Academy of Finland, European Commission, John Templeton Foundation, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Consejo Nacional de Ciencia y Tecnología (México), Universidad Nacional Autónoma de México, Generalitat Valenciana, Gordon and Betty Moore Foundation, National Radio Astronomy Observatory (US), Japanese Government, Japan Society for the Promotion of Science, Chinese Academy of Sciences, Leverhulme Trust, MIT International Science and Technology Initiatives, Ministry of Science and Technology (Taiwan), National Aeronautics and Space Administration (US), National Key Research and Development Program (China), National Research Foundation of Korea, Spinoza Prize, South African Radio Astronomy Observatory, Swedish Research Council, Government of Canada, Russian Science Foundation, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Ministero dell'Istruzione, dell'Università e della Ricerca, Chandra X-ray Observatory, CyVerse, Compute Ontario, Calcul Québec, Compute Canada, Porth, O., Chatterjee, K., Narayan, Ramesh, Gammie, C.F, Mizuno, Yosuke, Anninos, P., Baker, J. G., Bugli, M, Chan, C. K., Davelaar, J., Zanna, L. D., Zensus, J. A., Tilanus, R. P. J., Koay, J. Y., Young, K., Boland, W., Gentaz, O., Rao, R., Kino, Motoki, Nagar, Neil M., Rygl, K. L. J., Matthews, L. D., Palumbo, Daniel C. M., Ros, E., Psaltis, D, Medeiros, L., Jiang, Wu, Natarajan, I., Fish, Vincent L., Honma, M., Lauer, T. R., Schuster, K. F., Koch, P. M., Zhao, G., Issaoun, Sara, Roy, A. L., Schloerb, F. P., Kim, J., Azulay, Rebecca, Akiyama, Kazunori, Oyama, T., Alberdi, Antxón, Wagner, J., Stone, J. M., Menten, K. M., Ripperda, B., Narayanan, Gopal, Karuppusamy, R., Piétu, V., Broguiere, D., Roelofs, Freek, Noble, S. C., Baczko, A. K., Ball, D., Yuan, Y. F., Sánchez-Arguelles, D., Wu, Q., Ho, P., Lindqvist, M., Koyama, S., Sánchez, S., Keating, G. K., Plambeck, R., Li, Y. R., Kelly, B. J., Markoff, S., Kramer, Michael, van Rossum, D. R., Marscher, Alan P., Yuan, F., Patel, Nimesh, Wardle, J., Alef, W., Lobanov, A. P., Rezzolla, L., PopStefanija, A., Bintley, D, Conway, J. E., van Langevelde, H. J., Bremer, M., Sasada, Mahito, Moscibrodzka, M., Toma, K., Raymond, A. W., Wielgus, Maciek, Titus, Michael A., Hecht, M. H., Rogers, A., Fomalont, E., Carlstrom, J. E., Savolainen, T., Britzen, S., Loinard, Laurent, Özel, F., Nagai, H., Zhao, Shan-Shan, Brinkerink, C. D., Ryan, B. R., Trent, T., Jannuzi, B. T., SooHoo, J., Tiede, Paul, Ikeda, S., Lo, W. P., McKinney, J. C., Byun, D. Y., Tazaki, F., Crew, Geoffrey B., De Laurentis, M., Blackburn, Lindy, Chen, Y., Pesce, Dominic W., Broderick, Avery E., Trippe, S., Deane, Roger, Inoue, M., Baloković, M., Tsuda, S, Doeleman, Sheperd S., Janssen, M., Rottmann, H., Rose, M., Falcke, H., Preciado-López, J. A, Lee, S.-S, Kramer, C., Wong, G. N., Krichbaum, Thomas P., Hesper, R., Fragile, P. C., Chael, A., Mishra, B., Shao, L., Gómez, José L., Marrone, Daniel P., Gurwell, M., Kim, J. Y., Christian, P., Neri, Roberto, Friberg, P., Hughes, D. H., Gu, M., Chatterjee, S., Zhu, Z., Desvignes, Gregory, Shen, Z., Wex, N., Prather, B., Karami, M., Tomei, N., Hada, Kazuhiro, Young, A., James, D. J., Kawashima, T., Olivares, Hector, Ni, C., Kuo, C. Y., Fraga-Encinas, R., Etienne, Z. B., Liu, K., Moriyama, K., Chen, M. T., Lonsdale, Colin J., Dempsey, J., Liska, M., García, Roberto, Ramakrishnan, V., Huang, C. W. L., Galison, P., Noutsos, A., Okino, H., Matsushita, S., Johnson, M. D., MacDonald, N. R., Wharton, R., Barrett, John, White, C.J, Jeter, B., Lu, Ru-Sen, Georgiev, B., Ruszczyk, Chester A., Freeman, B., Eatough, R. P., Younsi, Z., Weintroub, Jonathan, Bronzwaer, T., Martí-Vidal, Iván, Fromm, Christian M., Müller, C., Liuzzo, Elisabetta, Mizuno, I., Bouman, Katherine L., Mao, J., Goddi, Ciriaco, Nakamura, M., Roshanineshat, A., Li, Z., Gold, R., Jorstad, S., Cordes, J. M., Cho, I., Ho, Luis C., Brissenden, R., van Bemmel, I., Torne, P., Huang, L., Small, D., Rawlings, M. G., Jung, T., Kettenis, Mark, Bower, G. C., Pen, U. L., Cui, Y., Pu, H. Y., Sohn, B. W., Morán, J. M., Asada, Keiichi, National Science Foundation (US), Netherlands Organization for Scientific Research, European Research Council, Gauss Centre for Supercomputing, Department of Energy (US), Academy of Finland, European Commission, John Templeton Foundation, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Consejo Nacional de Ciencia y Tecnología (México), Universidad Nacional Autónoma de México, Generalitat Valenciana, Gordon and Betty Moore Foundation, National Radio Astronomy Observatory (US), Japanese Government, Japan Society for the Promotion of Science, Chinese Academy of Sciences, Leverhulme Trust, MIT International Science and Technology Initiatives, Ministry of Science and Technology (Taiwan), National Aeronautics and Space Administration (US), National Key Research and Development Program (China), National Research Foundation of Korea, Spinoza Prize, South African Radio Astronomy Observatory, Swedish Research Council, Government of Canada, Russian Science Foundation, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Ministero dell'Istruzione, dell'Università e della Ricerca, Chandra X-ray Observatory, CyVerse, Compute Ontario, Calcul Québec, Compute Canada, Porth, O., Chatterjee, K., Narayan, Ramesh, Gammie, C.F, Mizuno, Yosuke, Anninos, P., Baker, J. G., Bugli, M, Chan, C. K., Davelaar, J., Zanna, L. D., Zensus, J. A., Tilanus, R. P. J., Koay, J. Y., Young, K., Boland, W., Gentaz, O., Rao, R., Kino, Motoki, Nagar, Neil M., Rygl, K. L. J., Matthews, L. D., Palumbo, Daniel C. M., Ros, E., Psaltis, D, Medeiros, L., Jiang, Wu, Natarajan, I., Fish, Vincent L., Honma, M., Lauer, T. R., Schuster, K. F., Koch, P. M., Zhao, G., Issaoun, Sara, Roy, A. L., Schloerb, F. P., Kim, J., Azulay, Rebecca, Akiyama, Kazunori, Oyama, T., Alberdi, Antxón, Wagner, J., Stone, J. M., Menten, K. M., Ripperda, B., Narayanan, Gopal, Karuppusamy, R., Piétu, V., Broguiere, D., Roelofs, Freek, Noble, S. C., Baczko, A. K., Ball, D., Yuan, Y. F., Sánchez-Arguelles, D., Wu, Q., Ho, P., Lindqvist, M., Koyama, S., Sánchez, S., Keating, G. K., Plambeck, R., Li, Y. R., Kelly, B. J., Markoff, S., Kramer, Michael, van Rossum, D. R., Marscher, Alan P., Yuan, F., Patel, Nimesh, Wardle, J., Alef, W., Lobanov, A. P., Rezzolla, L., PopStefanija, A., Bintley, D, Conway, J. E., van Langevelde, H. J., Bremer, M., Sasada, Mahito, Moscibrodzka, M., Toma, K., Raymond, A. W., Wielgus, Maciek, Titus, Michael A., Hecht, M. H., Rogers, A., Fomalont, E., Carlstrom, J. E., Savolainen, T., Britzen, S., Loinard, Laurent, Özel, F., Nagai, H., Zhao, Shan-Shan, Brinkerink, C. D., Ryan, B. R., Trent, T., Jannuzi, B. T., SooHoo, J., Tiede, Paul, Ikeda, S., Lo, W. P., McKinney, J. C., Byun, D. Y., Tazaki, F., Crew, Geoffrey B., De Laurentis, M., Blackburn, Lindy, Chen, Y., Pesce, Dominic W., Broderick, Avery E., Trippe, S., Deane, Roger, Inoue, M., Baloković, M., Tsuda, S, Doeleman, Sheperd S., Janssen, M., Rottmann, H., Rose, M., Falcke, H., Preciado-López, J. A, Lee, S.-S, Kramer, C., Wong, G. N., Krichbaum, Thomas P., Hesper, R., Fragile, P. C., Chael, A., Mishra, B., Shao, L., Gómez, José L., Marrone, Daniel P., Gurwell, M., Kim, J. Y., Christian, P., Neri, Roberto, Friberg, P., Hughes, D. H., Gu, M., Chatterjee, S., Zhu, Z., Desvignes, Gregory, Shen, Z., Wex, N., Prather, B., Karami, M., Tomei, N., Hada, Kazuhiro, Young, A., James, D. J., Kawashima, T., Olivares, Hector, Ni, C., Kuo, C. Y., Fraga-Encinas, R., Etienne, Z. B., Liu, K., Moriyama, K., Chen, M. T., Lonsdale, Colin J., Dempsey, J., Liska, M., García, Roberto, Ramakrishnan, V., Huang, C. W. L., Galison, P., Noutsos, A., Okino, H., Matsushita, S., Johnson, M. D., MacDonald, N. R., Wharton, R., Barrett, John, White, C.J, Jeter, B., Lu, Ru-Sen, Georgiev, B., Ruszczyk, Chester A., Freeman, B., Eatough, R. P., Younsi, Z., Weintroub, Jonathan, Bronzwaer, T., Martí-Vidal, Iván, Fromm, Christian M., Müller, C., Liuzzo, Elisabetta, Mizuno, I., Bouman, Katherine L., Mao, J., Goddi, Ciriaco, Nakamura, M., Roshanineshat, A., Li, Z., Gold, R., Jorstad, S., Cordes, J. M., Cho, I., Ho, Luis C., Brissenden, R., van Bemmel, I., Torne, P., Huang, L., Small, D., Rawlings, M. G., Jung, T., Kettenis, Mark, Bower, G. C., Pen, U. L., Cui, Y., Pu, H. Y., Sohn, B. W., Morán, J. M., and Asada, Keiichi
- Abstract
Recent developments in compact object astrophysics, especially the discovery of merging neutron stars by LIGO, the imaging of the black hole in M87 by the Event Horizon Telescope, and high- precision astrometry of the Galactic Center at close to the event horizon scale by the GRAVITY experiment motivate the development of numerical source models that solve the equations of general relativistic magnetohydrodynamics (GRMHD). Here we compare GRMHD solutions for the evolution of a magnetized accretion flow where turbulence is promoted by the magnetorotational instability from a set of nine GRMHD codes: Athena++, BHAC, Cosmos++, ECHO, H-AMR, iharm3D, HARM-Noble, IllinoisGRMHD, and KORAL. Agreement among the codes improves as resolution increases, as measured by a consistently applied, specially developed set of code performance metrics. We conclude that the community of GRMHD codes is mature, capable, and consistent on these test problems. © 2019. The American Astronomical Society. All rights reserved.
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- 2019
225. A rapidly changing jet orientation in the stellar-mass black-hole system V404 Cygni
- Author
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Miller-Jones, James, Tetarenko, A.J., Sivakoff, G.R., Middleton, M.J., Altamirano, D., Anderson, Gemma, Belloni, T.M., Fender, R.P., Jonker, P.G., Körding, E.G., Krimm, H.A., Maitra, D., Markoff, S., Migliari, S., Mooley, K.P., Rupen, M.P., Russell, D.M., Russell, T.D., Sarazin, C.L., Soria, R., Tudose, V., Miller-Jones, James, Tetarenko, A.J., Sivakoff, G.R., Middleton, M.J., Altamirano, D., Anderson, Gemma, Belloni, T.M., Fender, R.P., Jonker, P.G., Körding, E.G., Krimm, H.A., Maitra, D., Markoff, S., Migliari, S., Mooley, K.P., Rupen, M.P., Russell, D.M., Russell, T.D., Sarazin, C.L., Soria, R., and Tudose, V.
- Abstract
© 2019, The Author(s), under exclusive licence to Springer Nature Limited. Powerful relativistic jets are one of the main ways in which accreting black holes provide kinetic feedback to their surroundings. Jets launched from or redirected by the accretion flow that powers them are expected to be affected by the dynamics of the flow, which for accreting stellar-mass black holes has shown evidence for precession1 due to frame-dragging effects that occur when the black-hole spin axis is misaligned with the orbital plane of its companion star2. Recently, theoretical simulations have suggested that the jets can exert an additional torque on the accretion flow3, although the interplay between the dynamics of the accretion flow and the launching of the jets is not yet understood. Here we report a rapidly changing jet orientation—on a time scale of minutes to hours—in the black-hole X-ray binary V404 Cygni, detected with very-long-baseline interferometry during the peak of its 2015 outburst. We show that this changing jet orientation can be modelled as the Lense–Thirring precession of a vertically extended slim disk that arises from the super-Eddington accretion rate4. Our findings suggest that the dynamics of the precessing inner accretion disk could play a role in either directly launching or redirecting the jets within the inner few hundred gravitational radii. Similar dynamics should be expected in any strongly accreting black hole whose spin is misaligned with the inflowing gas, both affecting the observational characteristics of the jets and distributing the black-hole feedback more uniformly over the surrounding environment5,6.
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- 2019
226. LOFAR 150-MHz observations of SS 433 and W50
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Broderick, JW, Fender, RP, Miller-Jones, JCA, Trushkin, SA, Stewart, AJ, Anderson, GE, Staley, TD, Blundell, KM, Pietka, M, Markoff, S, Rowlinson, A, Swinbank, JD, van der Horst, AJ, Bell, ME, Breton, RP, Carbone, D, Corbel, S, Eislöffel, J, Falcke, H, Grießmeier, JM, Hessels, JWT, Kondratiev, VI, Law, CJ, Molenaar, GJ, Serylak, M, Stappers, BW, van Leeuwen, J, Wijers, RAMJ, Wijnands, R, Wise, MW, and Zarka, P
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
© 2017 The Author(s). We present Low-Frequency Array (LOFAR) high-band data over the frequency range 115-189 MHz for the X-ray binary SS 433, obtained in an observing campaign from 2013 February to 2014 May. Our results include a deep, wide-field map, allowing a detailed view of the surrounding supernova remnant W50 at low radio frequencies, as well as a light curve for SS 433 determined from shorter monitoring runs. The complex morphology of W50 is in excellent agreement with previously published higher frequency maps; we find additional evidence for a spectral turnover in the eastern wing, potentially due to foreground free-free absorption. Furthermore, SS 433 is tentatively variable at 150 MHz, with both a debiased modulation index of 11 per cent and a Χ2 probability of a flat light curve of 8.2 × 10-3. By comparing the LOFAR flux densities with contemporaneous observations carried out at 4800 MHz with the RATAN-600 telescope, we suggest that an observed ~0.5-1 Jy rise in the 150-MHz flux density may correspond to sustained flaring activity over a period of approximately 6 months at 4800 MHz. However, the increase is too large to be explained with a standard synchrotron bubble model. We also detect a wealth of structure along the nearby Galactic plane, including the most complete detection to date of the radio shell of the candidate supernova remnant G38.7-1.4. This further demonstrates the potential of supernova remnant studies with the current generation of low-frequency radio telescopes.
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- 2018
227. A bright mid-infrared excess in MAXI J1820+070
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Russell, D.M., Baglio, M.C., Bright, J., Fender, R., Al Qaissieh, T., Palado, A., Gabuya, A., Asmus, D., Belloni, T., Bel, M.C., Casella, P., Ceccobello, C., Corbel, S., Diaz Trigo, M., Gallo, E., Gandhi, P., Homan, J., Koljonen, K., Lewis, F., Markoff, S., Miller-Jones, J.C.A., O'Brien, K., Russell, T.D., Saikia, P., Sivakoff, G., Shahbaz, T., Soria, R., Tetarenko, A., van den Ancker, M., and High Energy Astrophys. & Astropart. Phys (API, FNWI)
- Abstract
MAXI J1820+070 (ASASSN-18ey) is a black hole candidate X-ray binary (e.g. ATel #11399, #11418, #11420). It is currently in a bright, hard spectral state (ATel #11423, #11427, #11439).
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- 2018
228. Relativistic Jets in Active Galactic Nuclei and Microquasars
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Romero, G.E., Boettcher, M., Markoff, S., Tavecchio, F., Bykov, A., Amato, E., Arons, J., Falanga, M., Lemoine, M., Stella, L., von Steiger, R., and High Energy Astrophys. & Astropart. Phys (API, FNWI)
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Galaxy Astrophysics - Abstract
Collimated outflows (jets) appear to be a ubiquitous phenomenon associated with the accretion of material onto a compact object. Despite this ubiquity, many fundamental physics aspects of jets are still poorly understood and constrained. These include the mechanism of launching and accelerating jets, the connection between these processes and the nature of the accretion flow, and the role of magnetic fields; the physics responsible for the collimation of jets over tens of thousands to even millions of gravitational radii of the central accreting object; the matter content of jets; the location of the region(s) accelerating particles to TeV (possibly even PeV and EeV) energies (as evidenced by γ-ray emission observed from many jet sources) and the physical processes responsible for this particle acceleration; the radiative processes giving rise to the observed multi-wavelength emission; and the topology of magnetic fields and their role in the jet collimation and particle acceleration processes. This chapter reviews the main knowns and unknowns in our current understanding of relativistic jets, in the context of the main model ingredients for Galactic and extragalactic jet sources. It discusses aspects specific to active Galactic nuclei (especially blazars) and microquasars, and then presents a comparative discussion of similarities and differences between them.
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- 2018
229. Disk–Jet Coupling in the 2017/2018 Outburst of the Galactic Black Hole Candidate X-Ray Binary MAXI J1535–571
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Russell, T. D., primary, Tetarenko, A. J., additional, Miller-Jones, J. C. A., additional, Sivakoff, G. R., additional, Parikh, A. S., additional, Rapisarda, S., additional, Wijnands, R., additional, Corbel, S., additional, Tremou, E., additional, Altamirano, D., additional, Baglio, M. C., additional, Ceccobello, C., additional, Degenaar, N., additional, Eijnden, J. van den, additional, Fender, R., additional, Heywood, I., additional, Krimm, H. A., additional, Lucchini, M., additional, Markoff, S., additional, Russell, D. M., additional, Soria, R., additional, and Woudt, P. A., additional
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- 2019
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230. A black hole X-ray binary at ∼100 Hz: multiwavelength timing of MAXI J1820+070 with HiPERCAM and NICER
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Paice, J A, primary, Gandhi, P, additional, Shahbaz, T, additional, Uttley, P, additional, Arzoumanian, Z, additional, Charles, P A, additional, Dhillon, V S, additional, Gendreau, K C, additional, Littlefair, S P, additional, Malzac, J, additional, Markoff, S, additional, Marsh, T R, additional, Misra, R, additional, Russell, D M, additional, and Veledina, A, additional
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- 2019
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231. Accelerating AGN jets to parsec scales using general relativistic MHD simulations
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Chatterjee, K, primary, Liska, M, additional, Tchekhovskoy, A, additional, and Markoff, S B, additional
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- 2019
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232. The unique case of the AGN core of M87: a misaligned low power blazar?
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Lucchini, M, primary, Krauß, F, additional, and Markoff, S, additional
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- 2019
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233. Discovery of a radio transient in M81
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Anderson, G E, primary, Miller-Jones, J C A, additional, Middleton, M J, additional, Soria, R, additional, Swartz, D A, additional, Urquhart, R, additional, Hurley-Walker, N, additional, Hancock, P J, additional, Fender, R P, additional, Gandhi, P, additional, Markoff, S, additional, and Roberts, T P, additional
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- 2019
- Full Text
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234. Combining timing characteristics with physical broad-band spectral modelling of black hole X-ray binary GX 339–4
- Author
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Connors, R M T, primary, van Eijnatten, D, primary, Markoff, S, primary, Ceccobello, C, primary, Grinberg, V, primary, Heil, L, primary, Kantzas, D, primary, Lucchini, M, primary, and Crumley, P, primary
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- 2019
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235. Kinetic simulations of mildly relativistic shocks – I. Particle acceleration in high Mach number shocks
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Crumley, P, primary, Caprioli, D, additional, Markoff, S, additional, and Spitkovsky, A, additional
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- 2019
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236. Simultaneous X-Ray and Infrared Observations of Sagittarius A*'s Variability
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Boyce, H., primary, Haggard, D., additional, Witzel, G., additional, Willner, S. P., additional, Neilsen, J., additional, Hora, J. L., additional, Markoff, S., additional, Ponti, G., additional, Baganoff, F., additional, Becklin, E. E., additional, Fazio, G. G., additional, Lowrance, P., additional, Morris, M. R., additional, and Smith, H. A., additional
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- 2019
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237. The Size, Shape, and Scattering of Sagittarius A* at 86 GHz: First VLBI with ALMA
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Issaoun, S., primary, Johnson, M. D., additional, Blackburn, L., additional, Brinkerink, C. D., additional, Mościbrodzka, M., additional, Chael, A., additional, Goddi, C., additional, Martí-Vidal, I., additional, Wagner, J., additional, Doeleman, S. S., additional, Falcke, H., additional, Krichbaum, T. P., additional, Akiyama, K., additional, Bach, U., additional, Bouman, K. L., additional, Bower, G. C., additional, Broderick, A., additional, Cho, I., additional, Crew, G., additional, Dexter, J., additional, Fish, V., additional, Gold, R., additional, Gómez, J. L., additional, Hada, K., additional, Hernández-Gómez, A., additional, Janßen, M., additional, Kino, M., additional, Kramer, M., additional, Loinard, L., additional, Lu, R.-S., additional, Markoff, S., additional, Marrone, D. P., additional, Matthews, L. D., additional, Moran, J. M., additional, Müller, C., additional, Roelofs, F., additional, Ros, E., additional, Rottmann, H., additional, Sanchez, S., additional, Tilanus, R. P. J., additional, Vicente, P. de, additional, Wielgus, M., additional, Zensus, J. A., additional, and Zhao, G.-Y., additional
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- 2019
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238. XIPE: the x-ray imaging polarimetry explorer
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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. 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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.
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- 2016
239. LOFAR 150-MHz observations of SS 433 and W 50
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Broderick, J.W., Fender, R.P., Miller-Jones, J.C.A., Trushkin, S.A., Stewart, A.J., Anderson, G.E., Staley, T.D., Blundell, K.M., Pietka, M., Markoff, S., Rowlinson, A., Swinbank, J.D., Horst, A.J.v.d., Bell, M.E., Breton, R.P., Carbone, D., Corbel, S., Eislöffel, J., Falcke, H., Grießmeier, J.M., Hessels, J.W.T., Kondratiev, V.I., Law, C.J., Molenaar, G.J., Serylak, M, Stappers, B.W., Leeuwen, J. van, Wijers, R.A.M.J., Wijnands, R., Wise, M.W., Zarka, P., Broderick, J.W., Fender, R.P., Miller-Jones, J.C.A., Trushkin, S.A., Stewart, A.J., Anderson, G.E., Staley, T.D., Blundell, K.M., Pietka, M., Markoff, S., Rowlinson, A., Swinbank, J.D., Horst, A.J.v.d., Bell, M.E., Breton, R.P., Carbone, D., Corbel, S., Eislöffel, J., Falcke, H., Grießmeier, J.M., Hessels, J.W.T., Kondratiev, V.I., Law, C.J., Molenaar, G.J., Serylak, M, Stappers, B.W., Leeuwen, J. van, Wijers, R.A.M.J., Wijnands, R., Wise, M.W., and Zarka, P.
- Abstract
Contains fulltext : 184318.pdf (publisher's version ) (Open Access)
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- 2018
240. Simultaneous X-ray and Infrared Observations of Sagittarius A*'s Variability
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Boyce, H., Haggard, D., Witzel, G., Willner, S. P., Neilsen, J., Hora, J. L., Markoff, S., Ponti, G., Baganoff, F., Becklin, E., Fazio, G., Lowrance, P., Morris, M. R., Smith, H. A., Boyce, H., Haggard, D., Witzel, G., Willner, S. P., Neilsen, J., Hora, J. L., Markoff, S., Ponti, G., Baganoff, F., Becklin, E., Fazio, G., Lowrance, P., Morris, M. R., and Smith, H. A.
- Abstract
Emission from Sgr A* is highly variable at both X-ray and infrared (IR) wavelengths. Observations over the last ~20 years have revealed X-ray flares that rise above a quiescent thermal background about once per day, while faint X-ray flares from Sgr A* are undetectable below the constant thermal emission. In contrast, the IR emission of Sgr A* is observed to be continuously variable. Recently, simultaneous observations have indicated a rise in IR flux density around the same time as every distinct X-ray flare, while the opposite is not always true (peaks in the IR emission may not be coincident with an X-ray flare). Characterizing the behaviour of these simultaneous X-ray/IR events and measuring any time lag between them can constrain models of Sgr A*'s accretion flow and the flare emission mechanism. Using 100+ hours of data from a coordinated campaign between the Spitzer Space Telescope and the Chandra X-ray Observatory, we present results of the longest simultaneous IR and X-ray observations of Sgr A* taken to date. The cross-correlation between the IR and X-ray light curves in this unprecedented dataset, which includes four modest X-ray/IR flares, indicates that flaring in the X-ray may lead the IR by approximately 10-20 minutes with 68% confidence. However, the 99.7% confidence interval on the time-lag also includes zero, i.e., the flaring remains statistically consistent with simultaneity. Long duration and simultaneous multiwavelength observations of additional bright flares will improve our ability to constrain the flare timing characteristics and emission mechanisms, and must be a priority for Galactic Center observing campaigns., Comment: 12 pages, 6 figures, 3 tables, accepted for publication in ApJ
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- 2018
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241. Breaking degeneracy in jet dynamics: multi-epoch joint modelling of the BL Lac PKS 2155-304
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Lucchini, M., Markoff, S., Crumley, P., Krauß, F., Connors, R. M. T., Lucchini, M., Markoff, S., Crumley, P., Krauß, F., and Connors, R. M. T.
- Abstract
Supermassive black holes can launch powerful jets which can be some of the most luminous multi-wavelength sources; decades after their discovery their physics and energetics are still poorly understood. The past decade has seen a dramatic improvement in the quality of available data, but despite this improvement the semi-analytical modelling of jets has advanced slowly: simple one-zone models are still the most commonly employed method of interpreting data, in particular for AGN jets. These models can roughly constrain the properties of jets but they cannot unambiguously couple their emission to the launching regions and internal dynamics, which can be probed with simulations. However, simulations are not easily comparable to observations because they cannot yet self-consistently predict spectra. We present an advanced semi-analytical model which accounts for the dynamics of the whole jet, starting from a simplified parametrization of Relativistic Magnetohydrodynamics in which the magnetic flux is converted into bulk kinetic energy. To benchmark the model we fit six quasisimultaneous, multi-wavelength spectral energy distributions of the BL Lac PKS 2155-304 obtained by the TANAMI program, and we address the degeneracies inherent to such a complex model by employing a state-of-the-art exploration of parameter space, which so far has been mostly neglected in the study of AGN jets. We find that this new approach is much more effective than a single-epoch fit in providing meaningful constraints on model parameters., Comment: Accepted for publication on MNRAS
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- 2018
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242. Tracking the variable jets of V404 Cygni during its 2015 outburst
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Tetarenko, A. J., Sivakoff, G. R., Miller-Jones, J. C. A., Bremer, M., Mooley, K. P., Fender, R. P., Rumsey, C., Bahramian, A., Altamirano, D., Heinz, S., Maitra, D., Markoff, S. B., Migliari, S., Rupen, M. P., Russell, D. M., Russell, T. D., Sarazin, C. L., Tetarenko, A. J., Sivakoff, G. R., Miller-Jones, J. C. A., Bremer, M., Mooley, K. P., Fender, R. P., Rumsey, C., Bahramian, A., Altamirano, D., Heinz, S., Maitra, D., Markoff, S. B., Migliari, S., Rupen, M. P., Russell, D. M., Russell, T. D., and Sarazin, C. L.
- Abstract
We present multi-frequency monitoring observations of the black hole X-ray binary V404 Cygni throughout its June 2015 outburst. Our data set includes radio and mm/sub-mm photometry, taken with the Karl G. Jansky Very Large Array, Arc-Minute MicroKelvin Imager Large Array, Sub-millimeter Array, James Clerk Maxwell Telescope, and the Northern Extended Millimetre Array, combined with publicly available infrared, optical, UV, and X-ray measurements. With these data, we report detailed diagnostics of the spectral and variability properties of the jet emission observed during different stages of this outburst. These diagnostics show that emission from discrete jet ejecta dominated the jet emission during the brightest stages of the outburst. We find that the ejecta became fainter, slower, less frequent, and less energetic, before the emission transitioned (over 1--2 days) to being dominated by a compact jet, as the outburst decayed toward quiescence. While the broad-band spectrum of this compact jet showed very little evolution throughout the outburst decay (with the optically thick to thin synchrotron jet spectral break residing in the near-infrared/optical bands; $\sim2-5\times10^{14}$ Hz), the emission still remained intermittently variable at mm/sub-mm frequencies. Additionally, we present a comparison between the radio jet emission throughout the 2015 and previous 1989 outbursts, confirming that the radio emission in the 2015 outburst decayed significantly faster than in 1989. Lastly, we detail our sub-mm observations taken during the December 2015 mini-outburst of V404 Cygni, which demonstrate that, similar to the main outburst, the source was likely launching jet ejecta during this short period of renewed activity., Comment: 24 pages, 12 Figures, Accepted to MNRAS
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- 2018
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243. A wildly flickering jet in the black hole X-ray binary MAXI J1535-571
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Baglio, M. C., Russell, D. M., Casella, P., Noori, H. Al, Yazeedi, A. Al, Belloni, T., Buckley, D. A. H., Bel, M. Cadolle, Ceccobello, C., Corbel, S., Zelati, F. Coti, Trigo, M. Diaz, Fender, R. P., Gallo, E., Gandhi, P., Homan, J., koljonen, K. I. I., lewis, F., Maccarone, T. J., Malzac, J., Markoff, S., Miller-Jones, J. C. A., O'Brien, K., Russell, T. D., Saikia, P., Shahbaz, T., Sivakoff, G. R., Soria, R., Testa, V., Tetarenko, A. J., Ancker, M. E. van den, Vincentelli, F. M., Baglio, M. C., Russell, D. M., Casella, P., Noori, H. Al, Yazeedi, A. Al, Belloni, T., Buckley, D. A. H., Bel, M. Cadolle, Ceccobello, C., Corbel, S., Zelati, F. Coti, Trigo, M. Diaz, Fender, R. P., Gallo, E., Gandhi, P., Homan, J., koljonen, K. I. I., lewis, F., Maccarone, T. J., Malzac, J., Markoff, S., Miller-Jones, J. C. A., O'Brien, K., Russell, T. D., Saikia, P., Shahbaz, T., Sivakoff, G. R., Soria, R., Testa, V., Tetarenko, A. J., Ancker, M. E. van den, and Vincentelli, F. M.
- 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 de-reddened flux density of $\gtrsim$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 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 $\sim 15-22 \%$, which is similar to that expected from the internal shock jet model, and much higher than the optical fractional rms ($\lesssim 7 \%$). These results represent an excellent case of multi-wavelength jet spectral-timing and demonstrate how rich, multi-wavelength time-resolved data of X-ray binaries over accretion state transitions can help refining models of the disk-jet connection and jet launching in these systems., Comment: 20 pages, 8 figures. Accepted for publication in the ApJ
- Published
- 2018
- Full Text
- View/download PDF
244. LOFAR 150-MHz observations of SS 433 and W 50
- Author
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Broderick, J. W., Fender, R. P., Miller-Jones, J. C. A., Trushkin, S. A., Stewart, A. J., Anderson, G. E., Staley, T. D., Blundell, K. M., Pietka, M., Markoff, S., Rowlinson, A., Swinbank, J. D., van der Horst, A. J., Bell, M. E., Breton, R. P., Carbone, D., Corbel, S., Eislöffel, J., Falcke, H., Grießmeier, J. -M., Hessels, J. W. T., Kondratiev, V. I., Law, C. J., Molenaar, G. J., Serylak, M., Stappers, B. W., van Leeuwen, J., Wijers, R. A. M. J., Wijnands, R., Wise, M. W., Zarka, P., Broderick, J. W., Fender, R. P., Miller-Jones, J. C. A., Trushkin, S. A., Stewart, A. J., Anderson, G. E., Staley, T. D., Blundell, K. M., Pietka, M., Markoff, S., Rowlinson, A., Swinbank, J. D., van der Horst, A. J., Bell, M. E., Breton, R. P., Carbone, D., Corbel, S., Eislöffel, J., Falcke, H., Grießmeier, J. -M., Hessels, J. W. T., Kondratiev, V. I., Law, C. J., Molenaar, G. J., Serylak, M., Stappers, B. W., van Leeuwen, J., Wijers, R. A. M. J., Wijnands, R., Wise, M. W., and Zarka, P.
- Abstract
We present LOFAR high-band data over the frequency range 115-189 MHz for the X-ray binary SS 433, obtained in an observing campaign from 2013 February - 2014 May. Our results include a deep, wide-field map, allowing a detailed view of the surrounding supernova remnant W 50 at low radio frequencies, as well as a light curve for SS 433 determined from shorter monitoring runs. The complex morphology of W 50 is in excellent agreement with previously published higher-frequency maps; we find additional evidence for a spectral turnover in the eastern wing, potentially due to foreground free-free absorption. Furthermore, SS 433 is tentatively variable at 150 MHz, with both a debiased modulation index of 11 per cent and a $\chi^2$ probability of a flat light curve of $8.2 \times 10^{-3}$. By comparing the LOFAR flux densities with contemporaneous observations carried out at 4800 MHz with the RATAN-600 telescope, we suggest that an observed $\sim$0.5-1 Jy rise in the 150-MHz flux density may correspond to sustained flaring activity over a period of approximately six months at 4800 MHz. However, the increase is too large to be explained with a standard synchrotron bubble model. We also detect a wealth of structure along the nearby Galactic plane, including the most complete detection to date of the radio shell of the candidate supernova remnant G 38.7-1.4. This further demonstrates the potential of supernova remnant studies with the current generation of low-frequency radio telescopes., Comment: 19 pages, 8 figures, 4 tables, accepted for publication in MNRAS
- Published
- 2018
- Full Text
- View/download PDF
245. VLBA polarimetric monitoring of 3C 111
- Author
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Ministerio de Economía y Competitividad (España), European Commission, Generalitat Valenciana, Russian Foundation for Basic Research, Alexander von Humboldt Foundation, Academy of Finland, Junta de Andalucía, Beuchert, T., Kadler, M., Perucho, M., Großberger, C., Schulz, R., Agudo, Iván, Casadio, Carolina, Gómez, José L., Gurwell, M., Homan, D., Kovalev, Y. Y., Lister, Matthew L., Markoff, S., Molina, Sol, Pushkarev, A.B., Ros, E., Savolainen, T., Steinbring, T., Thum, C., Wilms, J., Ministerio de Economía y Competitividad (España), European Commission, Generalitat Valenciana, Russian Foundation for Basic Research, Alexander von Humboldt Foundation, Academy of Finland, Junta de Andalucía, Beuchert, T., Kadler, M., Perucho, M., Großberger, C., Schulz, R., Agudo, Iván, Casadio, Carolina, Gómez, José L., Gurwell, M., Homan, D., Kovalev, Y. Y., Lister, Matthew L., Markoff, S., Molina, Sol, Pushkarev, A.B., Ros, E., Savolainen, T., Steinbring, T., Thum, C., and Wilms, J.
- Abstract
Context. While studies of large samples of jets of active galactic nuclei (AGN) are important in order to establish a global picture, dedicated single-source studies are an invaluable tool for probing crucial processes within jets on parsec scales. These processes involve in particular the formation and geometry of the jet magnetic field as well as the flow itself. Aims. We aim to better understand the dynamics within relativistic magneto-hydrodynamical flows in the extreme environment and close vicinity of supermassive black holes. Methods. We analyze the peculiar radio galaxy 3C 111, for which long-Term polarimetric observations are available. We make use of the high spatial resolution of the VLBA network and the MOJAVE monitoring program, which provides high data quality also for single sources and allows us to study jet dynamics on parsec scales in full polarization with an evenly sampled time-domain. While electric vectors can probe the underlying magnetic field, other properties of the jet such as the variable (polarized) flux density, feature size, and brightness temperature, can give valuable insights into the flow itself. We complement the VLBA data with data from the IRAM 30-m Telescope as well as the SMA. Results. We observe a complex evolution of the polarized jet. The electric vector position angles (EVPAs) of features traveling down the jet perform a large rotation of &180across a distance of about 20 pc. As opposed to this smooth swing, the EVPAs are strongly variable within the first parsecs of the jet.We find an overall tendency towards transverse EVPAs across the jet with a local anomaly of aligned vectors in between. The polarized flux density increases rapidly at that distance and eventually saturates towards the outermost observable regions. The transverse extent of the flow suddenly decreases simultaneously to a jump in brightness temperature around where we observe the EVPAs to turn into alignment with the jet flow. Also the gradient of the fe
- Published
- 2018
246. Tracking of an electron beam through the solar corona with LOFAR
- Author
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Mann, G, Breitling, F, Vocks, C, Aurass, H, Steinmetz, M, Strassmeier, KG, Bisi, MM, Fallows, RA, Gallagher, P, Kerdraon, A, Mackinnon, A, Magdalenic, J, Rucker, H, Anderson, J, Asgekar, A, Avruch, IM, Bell, ME, Bentum, MJ, Bernardi, G, Best, P, Bîrzan, L, Bonafede, A, Broderick, JW, Brüggen, M, Butcher, HR, Ciardi, B, Corstanje, A, Gasperin, FD, Geus, ED, Deller, A, Duscha, S, Eislöffel, J, Engels, D, Falcke, H, Fender, R, Ferrari, C, Frieswijk, W, Garrett, MA, Grießmeier, J, Gunst, AW, Haarlem, MV, Hassall, TE, Heald, G, Hessels, JWT, Hoeft, M, Hörandel, J, Horneffer, A, Juette, E, Karastergiou, A, Klijn, WFA, Kondratiev, VI, Kramer, M, Kuniyoshi, M, Kuper, G, Maat, P, Markoff, S, McFadden, R, McKay-Bukowski, D, McKean, JP, Mulcahy, DD, Munk, H, Nelles, A, Norden, MJ, Orru, E, Paas, H, Pandey-Pommier, M, Pandey, VN, Pizzo, R, Polatidis, AG, Rafferty, D, Reich, W, Röttgering, H, Scaife, AMM, Schwarz, DJ, Serylak, M, Sluman, J, Smirnov, O, Stappers, BW, Tagger, M, Tang, Y, Tasse, C, Veen, ST, Thoudam, S, Toribio, MC, Vermeulen, R, Weeren, RJV, Wise, MW, Wucknitz, O, Yatawatta, S, Zarka, P, Zensus, JA, Mann, G, Breitling, F, Vocks, C, Aurass, H, Steinmetz, M, Strassmeier, KG, Bisi, MM, Fallows, RA, Gallagher, P, Kerdraon, A, Mackinnon, A, Magdalenic, J, Rucker, H, Anderson, J, Asgekar, A, Avruch, IM, Bell, ME, Bentum, MJ, Bernardi, G, Best, P, Bîrzan, L, Bonafede, A, Broderick, JW, Brüggen, M, Butcher, HR, Ciardi, B, Corstanje, A, Gasperin, FD, Geus, ED, Deller, A, Duscha, S, Eislöffel, J, Engels, D, Falcke, H, Fender, R, Ferrari, C, Frieswijk, W, Garrett, MA, Grießmeier, J, Gunst, AW, Haarlem, MV, Hassall, TE, Heald, G, Hessels, JWT, Hoeft, M, Hörandel, J, Horneffer, A, Juette, E, Karastergiou, A, Klijn, WFA, Kondratiev, VI, Kramer, M, Kuniyoshi, M, Kuper, G, Maat, P, Markoff, S, McFadden, R, McKay-Bukowski, D, McKean, JP, Mulcahy, DD, Munk, H, Nelles, A, Norden, MJ, Orru, E, Paas, H, Pandey-Pommier, M, Pandey, VN, Pizzo, R, Polatidis, AG, Rafferty, D, Reich, W, Röttgering, H, Scaife, AMM, Schwarz, DJ, Serylak, M, Sluman, J, Smirnov, O, Stappers, BW, Tagger, M, Tang, Y, Tasse, C, Veen, ST, Thoudam, S, Toribio, MC, Vermeulen, R, Weeren, RJV, Wise, MW, Wucknitz, O, Yatawatta, S, Zarka, P, and Zensus, JA
- Abstract
© ESO 2018. The Sun's activity leads to bursts of radio emission, among other phenomena. An example is type-III radio bursts. They occur frequently and appear as short-lived structures rapidly drifting from high to low frequencies in dynamic radio spectra. They are usually interpreted as signatures of beams of energetic electrons propagating along coronal magnetic field lines. Here we present novel interferometric LOFAR (LOw Frequency ARray) observations of three solar type-III radio bursts and their reverse bursts with high spectral, spatial, and temporal resolution. They are consistent with a propagation of the radio sources along the coronal magnetic field lines with nonuniform speed. Hence, the type-III radio bursts cannot be generated by a monoenergetic electron beam, but by an ensemble of energetic electrons with a spread distribution in velocity and energy. Additionally, the density profile along the propagation path is derived in the corona. It agrees well with three-fold coronal density model by (1961, ApJ, 133, 983).
- Published
- 2018
247. 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
248. LOFAR 150-MHz observations of SS 433 and W50
- Author
-
Broderick, J., Fender, R., Miller-Jones, James, Trushkin, S., Stewart, A., Anderson, Gemma, Staley, T., Blundell, K., Pietka, M., Markoff, S., Rowlinson, A., Swinbank, J., van der Horst, A., Bell, M., Breton, R., Carbone, D., Corbel, S., Eislöffel, J., Falcke, H., Grießmeier, J., Hessels, J., Kondratiev, V., Law, C., Molenaar, G., Serylak, M., Stappers, B., van Leeuwen, J., Wijers, R., Wijnands, R., Wise, M., Zarka, P., Broderick, J., Fender, R., Miller-Jones, James, Trushkin, S., Stewart, A., Anderson, Gemma, Staley, T., Blundell, K., Pietka, M., Markoff, S., Rowlinson, A., Swinbank, J., van der Horst, A., Bell, M., Breton, R., Carbone, D., Corbel, S., Eislöffel, J., Falcke, H., Grießmeier, J., Hessels, J., Kondratiev, V., Law, C., Molenaar, G., Serylak, M., Stappers, B., van Leeuwen, J., Wijers, R., Wijnands, R., Wise, M., and Zarka, P.
- Abstract
We present Low-Frequency Array (LOFAR) high-band data over the frequency range 115-189 MHz for the X-ray binary SS 433, obtained in an observing campaign from 2013 February to 2014 May. Our results include a deep, wide-field map, allowing a detailed view of the surrounding supernova remnant W50 at low radio frequencies, as well as a light curve for SS 433 determined from shorter monitoring runs. The complex morphology of W50 is in excellent agreement with previously published higher frequency maps; we find additional evidence for a spectral turnover in the eastern wing, potentially due to foreground free-free absorption. Furthermore, SS 433 is tentatively variable at 150 MHz, with both a debiased modulation index of 11 per cent and a Χ 2 probability of a flat light curve of 8.2 × 10 -3 . By comparing the LOFAR flux densities with contemporaneous observations carried out at 4800 MHz with the RATAN-600 telescope, we suggest that an observed ~0.5-1 Jy rise in the 150-MHz flux density may correspond to sustained flaring activity over a period of approximately 6 months at 4800 MHz. However, the increase is too large to be explained with a standard synchrotron bubble model. We also detect a wealth of structure along the nearby Galactic plane, including the most complete detection to date of the radio shell of the candidate supernova remnant G38.7-1.4. This further demonstrates the potential of supernova remnant studies with the current generation of low-frequency radio telescopes.
- Published
- 2018
249. Disc–jet coupling changes as a possible indicator for outbursts from GX 339−4 remaining within the X-ray hard state.
- Author
-
de Haas, S E M, Russell, T D, Degenaar, N, Markoff, S, Tetarenko, A J, Tetarenko, B E, van den Eijnden, J, Miller-Jones, J C A, Parikh, A S, Plotkin, R M, and Sivakoff, G R
- Subjects
HARD X-rays ,BINARY black holes ,GALACTIC X-ray sources ,JETS (Fluid dynamics) ,JETS (Nuclear physics) - Abstract
We present quasi-simultaneous radio, (sub-)millimetre, and X-ray observations of the Galactic black hole X-ray binary GX 339−4, taken during its 2017–2018 outburst, where the source remained in the hard X-ray spectral state. During this outburst, GX 339−4 showed no atypical X-ray behaviour that may act as an indicator for an outburst remaining within the hard state. However, quasi-simultaneous radio and X-ray observations showed a flatter than expected coupling between the radio and X-ray luminosities (with a best-fitting relation of |$L_{\rm radio} \propto L_{\rm X}^{0.39 \pm 0.06}$|), when compared to successful outbursts from this system (|$L_{\rm radio} \propto L_{\rm X}^{0.62 \pm 0.02}$|). While our 2017–2018 outburst data only span a limited radio and X-ray luminosity range (∼1 order of magnitude in both, where more than 2 orders of magnitude in L
X is desired), including data from other hard-only outbursts from GX 339−4 extends the luminosity range to ∼1.2 and ∼2.8 orders of magnitude, respectively, and also results in a flatter correlation (where |$L_{\rm radio} \propto L_{\rm X}^{0.46 \pm 0.04}$|). This result is suggestive that for GX 339−4 a flatter radio–X-ray correlation, implying a more inefficient coupling between the jet and accretion flow, could act as an indicator for a hard-only outburst. However, further monitoring of both successful and hard-only outbursts over larger luminosity ranges with strictly simultaneous radio and X-ray observations is required from different single sources to explore if this applies generally to the population of black hole X-ray binaries, or even GX 339−4 at higher hard-state luminosities. [ABSTRACT FROM AUTHOR]- Published
- 2021
- Full Text
- View/download PDF
250. Correlating spectral and timing properties in the evolving jet of the microblazar MAXI J1836−194.
- Author
-
Lucchini, M, Russell, T D, Markoff, S B, Vincentelli, F, Gardenier, D, Ceccobello, C, and Uttley, P
- Subjects
BINARY black holes ,X-ray spectra ,HARD X-rays ,JETS (Nuclear physics) ,ACCRETION (Astrophysics) ,BLACK holes ,POWER spectra - Abstract
During outbursts, the observational properties of black hole X-ray binaries vary on time-scales of days to months. These relatively short time-scales make these systems ideal laboratories to probe the coupling between accreting material and outflowing jets as the accretion rate varies. In particular, the origin of the hard X-ray emission is poorly understood and highly debated. This spectral component, which has a power-law shape, is due to Comptonization of photons near the black hole, but it is unclear whether it originates in the accretion flow itself, or at the base of the jet, or possibly the interface region between them. In this paper, we explore the disc–jet connection by modelling the multiwavelength emission of MAXI J1836−194 during its 2011 outburst. We combine radio through X-ray spectra, X-ray timing information, and a robust joint-fitting method to better isolate the jet's physical properties. Our results demonstrate that the jet base can produce power-law hard X-ray emission in this system/outburst, provided that its base is fairly compact and that the temperatures of the emitting electrons are subrelativistic. Because of energetic considerations, our model favours mildly pair-loaded jets carrying at least 20 pairs per proton. Finally, we find that the properties of the X-ray power spectrum are correlated with the jet properties, suggesting that an underlying physical process regulates both. [ABSTRACT FROM AUTHOR]
- Published
- 2021
- Full Text
- View/download PDF
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