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153 results on '"van den Eijnden, J."'

1. A shared accretion instability for black holes and neutron stars

Author

Vincentelli, F. M., Neilsen, J., Tetarenko, A. J., Cavecchi, Y., Castro Segura, N., del Palacio, S., van den Eijnden, J., Vasilopoulos, G., Altamirano, D., Armas Padilla, M., Bailyn, C. D., Belloni, T., Buisson, D. J. K., Cúneo, V. A., Degenaar, N., Knigge, C., Long, K. S., Jiménez-Ibarra, F., Milburn, J., Muñoz Darias, T., Özbey Arabacı, M., Remillard, R., and Russell, T.

Published
2023
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2. Multiwavelength coverage of the 2024 periastron passage of PSR B1259–63/LS 2883.

Author

Chernyakova, M, Malyshev, D, van Soelen, B, Finn Gallagher, A, Matchett, N, Russell, T D, van den Eijnden, J, Lower, M E, Johnston, S, Tsygankov, S, Salganik, A, and Shebalkova, Iu

Subjects
STELLAR winds, STARS, X-ray binaries, ORBITS (Astronomy), PULSARS
Abstract

PSR B1259 |$-$| 63is a gamma-ray binary system with a 48 ms radio pulsar orbiting around an O9.5Ve star, LS 2883, in a highly eccentric |${\sim} 3.4$|  yr long orbit. Close to the periastron the system is detected from radio up to the TeV energies due to the interaction of the stellar wind from LS 2883 and the pulsar's relativistic outflow. Observations of the last four periastron passages, taken in 2010–2021, demonstrate periastron-to-periastron variability at all wavelengths, probably linked to the state of the Be star's decretion disc. In this paper, we present the results of our optical, radio and X-ray observational campaigns on PSR B1259 |$-$| 63 performed in 2024 accompanied with the analysis of the publicly available GeV Fermi /LAT data. We show that this periastron passage was characterized by the early flaring of X-rays before the periastron passage and GeV emission after the periastron passage, which can be explained by a larger size of the decretion disc as supported by the optical observations. The structure of the GeV flare is also in agreement with the disruption of the large dense disc. The possible X-ray/radio correlation was observed only during the post-periastron rise of X-ray and radio emission. [ABSTRACT FROM AUTHOR]

Published
2025
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3. A persistent ultraviolet outflow from an accreting neutron star binary transient

Author

Castro Segura, N., Knigge, C., Long, K. S., Altamirano, D., Armas Padilla, M., Bailyn, C., Buckley, D. A. H., Buisson, D. J. K., Casares, J., Charles, P., Combi, J. A., Cúneo, V. A., Degenaar, N. D., del Palacio, S., Díaz Trigo, M., Fender, R., Gandhi, P., Georganti, M., Gutiérrez, C., Hernandez Santisteban, J. V., Jiménez-Ibarra, F., Matthews, J., Méndez, M., Middleton, M., Muñoz-Darias, T., Özbey Arabacı, M., Pahari, M., Rhodes, L., Russell, T. D., Scaringi, S., van den Eijnden, J., Vasilopoulos, G., Vincentelli, F. M., and Wiseman, P.

Published
2022
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4. Radio observations of the 2022 outburst of the transitional Z-Atoll source XTE J1701−462.

Author

Gasealahwe, K V S, Monageng, I M, Fender, R P, Woudt, P A, Hughes, A K, Motta, S E, van den Eijnden, J, Saikia, P, and Tremou, E

Subjects
BINARY black holes, NEUTRON stars, RADIO telescopes, X-ray detection, LIGHT curves, X-ray binaries
Abstract

XTE J1701−462 is a neutron star low-mass X-ray binary (NS LMXB) discovered in 2006 as the first system to demonstrate unambiguously that the 'Atoll' and 'Z' classes of accreting neutron stars are separated by accretion rate. Radio observations during the 2006/7 outburst provided evidence for the formation of a relativistic jet, as now expected for all accreting neutron star and black hole X-ray binaries at high-accretion rates. The source entered a new outburst in 2022, and we report 29 observations made with the MeerKAT radio telescope. The first radio detection was on the 16th September 2022, we continued detecting the source until mid-December 2022. Thereafter, establishing radio upper limits till 25 March 2023. We present the radio analysis alongside analysis of contemporaneous X-ray observations from MAXI. The radio light curve shows evidence for at least three flare-like events over the first hundred days, the most luminous of which has an associated minimum energy of |$1\times 10^{38}$|  erg. We provide a detailed comparison with the 2006/7 outburst, and demonstrate that we detected radio emission from the source for considerably longer in the more recent outburst, although this is probably a function of sampling. We further constrain the radio emission from the source to have a polarization of less than 9 per cent at the time of 2022 IXPE detection of X-ray polarization. Finally, we place the source in the radio–X-ray plane, demonstrating that when detected in radio it sits in a comparable region of parameter space to the other Z-sources. [ABSTRACT FROM AUTHOR]

Published
2024
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5. The variable radio jet of the accreting neutron star the Rapid Burster.

Author

van den Eijnden, J, Robins, D, Sharma, R, Sánchez-Fernández, C, Russell, T D, Degenaar, N, Miller-Jones, J C A, and Maccarone, T

Subjects
*X-ray bursts, *NEUTRON stars, *LIGHT curves, *ASTROPHYSICS, *ACCRETION disks, *X-ray binaries
Abstract

The Rapid Burster is a unique neutron star low-mass X-ray binary system, showing both thermonuclear v-I and accretion-driven Type-II X-ray bursts. Recent studies have demonstrated how coordinated observations of X-ray and radio variability can constrain jet properties of accreting neutron stars – particularly when the X-ray variability is dominated by discrete changes. We present a simultaneous very large array, Swift , and INTErnational Gamma-Ray Astrophysics Laboratory observing campaign of the Rapid Burster to investigate whether its jet responds to Type-II bursts. We observe the radio counterpart of the X-ray binary at its faintest-detected radio luminosity, while the X-ray observations reveal prolific, fast X-ray bursting. A time-resolved analysis reveals that the radio counterpart varies significantly between observing scans, displaying a fractional variability of |$38 \pm 5$|  per cent. The radio faintness of the system prevents the robust identification of a causal relation between individual Type-II bursts and the evolution of the radio jet. However, based on a comparison of its low-radio luminosity with archival Rapid Burster observations and other accreting neutron stars, and on a qualitative assessment of the X-ray and radio light curves, we explore the presence of a tentative connection between bursts and jet: i.e. the Type-II bursts may weaken or strengthen the jet. The former of those two scenarios would fit with magnetorotational jet models; we discuss three lines of future research to establish this potential relation between Type-II bursts and jets more confidently. [ABSTRACT FROM AUTHOR]

Published
2024
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8. Particle acceleration at the bow shock of runaway star LS 2355: non-thermal radio emission but no γ-ray counterpart.

Author

van den Eijnden, J, Mohamed, S, Carotenuto, F, Motta, S, Saikia, P, and Williams-Baldwin, D R A

Subjects
*PARTICLE acceleration, *MAGNETIC flux density, *SUPERGIANT stars, *INTERSTELLAR medium, *SOLAR radio emission, *STELLAR winds
Abstract

Massive stars that travel at supersonic speeds can create bow shocks as their stellar winds interact with the surrounding interstellar medium (ISM). These bow shocks – prominent sites for mechanical feedback of individual massive stars – are predominantly observed in the infrared (IR) band. Confirmed high-energy emission from stellar bow shocks has remained elusive and confirmed radio counterparts, while rising in recent years, remain rare. Here, we present an in-depth multiwavelength exploration of the bow shock driven by LS 2355, focusing on its non-thermal properties. Using the most recent Fermi source catalogue, we rule out its previously proposed association with an unidentified γ-ray source. Furthermore, we use deep Australian Square Kilometre Array Pathfinder (ASKAP) observations from the Rapid ASKAP Continuum Survey and the Evolutionary Map of the Universe survey to identify a non-thermal radio counterpart: the third spectrally confirmed non-thermal bow shock counterpart after BD+43°3654 and BD+60°2522. We finally use Wide-field Infrared Survey Explorer (WISE) IR data and Gaia to study the surrounding ISM and update the motion of LS 2355. Specifically, we derive a substantially reduced stellar velocity, |$v_* = 7.0\pm 2.5$| km s−1, compared to previous estimates. The observed non-thermal properties of the bow shock can be explained by an interaction between the wind of LS 2355 and a dense H  ii region, at a magnetic field close to the maximum magnetic field strength allowed by the compressibility of the ISM. Similar to earlier works, we find that the thermal radio emission of the shocked ISM is likely to be substantially suppressed for it to be consistent with the observed radio spectrum. [ABSTRACT FROM AUTHOR]

Published
2024
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9. The high energy X-ray probe (HEX-P): a new window into neutron star accretion

Author

Ludlam, R. M., primary, Malacaria, C., additional, Sokolova-Lapa, E., additional, Fuerst, F., additional, Pradhan, P., additional, Shaw, A. W., additional, Pottschmidt, K., additional, Pike, S., additional, Vasilopoulos, G., additional, Wilms, J., additional, García, J. A., additional, Madsen, K., additional, Stern, D., additional, Maitra, C., additional, Del Santo, M., additional, Walton, D. J., additional, Brumback, M. C., additional, and van den Eijnden, J., additional

Published
2023
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12. The first mm detection of a neutron star high-mass X-ray binary

Author

van den Eijnden, J, primary, Sidoli, L, additional, Díaz Trigo, M, additional, Degenaar, N, additional, El Mellah, I, additional, Fürst, F, additional, Grinberg, V, additional, Kretschmar, P, additional, Martínez-Núñez, S, additional, Miller-Jones, J C A, additional, Postnov, K, additional, and Russell, T D, additional

Published
2023
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13. The accretion/ejection link in the neutron star X-ray binary 4U 1820-30 I: A boundary layer-jet coupling?

Author

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

Published
2023
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14. SAX J1810.8−2609: an outbursting neutron star X-ray binary with persistent spatially coincident radio emission.

Author

Hughes, A K, Sivakoff, G R, van den Eijnden, J, Fender, R, Miller-Jones, J C A, and Tremou, E

Subjects
X-ray binaries, NEUTRON stars, X-rays, RADIO programs, STELLAR radiation, SPATIAL resolution, HARD X-rays
Abstract

Here, we report on joint X-ray and radio monitoring of the neutron star low-mass X-ray binary SAX J1810.8−2609. Our monitoring covered the entirety of its |${\sim }\, 5\,$| month outburst in 2021, revealing a temporal correlation between its radio and X-ray luminosity and X-ray spectral properties consistent with a 'hard-only' outburst. During the outburst, the best-fitting radio position shows significant variability, suggesting emission from multiple locations on the sky. Furthermore, our 2023 follow-up observations revealed a persistent, unresolved, steep spectrum radio source |${\sim }\, 2\,$| yr after SAX J1810.8−2609 returned to X-ray quiescence. We investigated potential origins of the persistent emission, which included an unrelated background source, long-lasting jet ejection(s), and SAX J1810 as a transitional millisecond pulsar. While the chance coincidence probability is low (⁠|${\lesssim }\, 0.16~{{\ \rm per\ cent}}$|⁠), an unrelated background source remains the most likely scenario. SAX J1810.8−2609 goes into outburst every |${\sim }\, 5\,$| yr, so monitoring of the source during its next outburst at higher sensitivities and improved spatial resolutions (e.g. with the Karl G. Jansky Very Large Array or Square Kilometre Array) should be able to identify two components (if the persistent emission originates from a background source). If only one source is observed, this would be strong evidence that the persistent emission is local SAX J1810.8−2609, and future monitoring campaigns should focus on understanding the underlying physical mechanisms, as no neutron star X-ray binary has shown a persistent radio signal absent any simultaneous X-ray emission. [ABSTRACT FROM AUTHOR]

Published
2024
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16. The 2019 outburst of AMXP SAX J1808.4–3658 and radio follow up of MAXI J0911–655 and XTE J1701–462

Author

Gasealahwe, K V S, primary, Monageng, I M, additional, Fender, R P, additional, Woudt, P A, additional, Motta, S E, additional, van den Eijnden, J, additional, Williams, D R A, additional, Heywood, I, additional, Bloemen, S, additional, Groot, P J, additional, Vreeswijk, P, additional, McBride, V, additional, Klein-Wolt, M, additional, Körding, E, additional, Le Poole, R, additional, Pieterse, D, additional, and de Wet, S, additional

Published
2023
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21. Vela X-1 in depth: a review article on outstanding object

Author

Martínez-Núñez, Silvia, Kretschmar, Peter, El Mellah, I., Fuerst, F., Grinberg, V., Sander, A. A. C, van den Eijnden, J., Degenaar, N., Maíz Apellániz, J., Jiménez Esteban, F., Ramos-Lerate, M, and Utrilla, E.

Subjects
X-rays: individuals: Vela X-1, X-rays: binaries, stars: winds, outflows, accretion, accretion disks, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

In this poster, we will summarise the review paper entitled: "Revisiting the archetypical wind accretor Vela X-1 in depth. Case study of a well-known X-ray binary and the limits of our knowledge." The paper, published in late 2021 in Astronomy and Astrophysics journal, triggered a discussion amongst the editors of Astronomy and Astrophysics leading to the creation of a new type of review article on uniquely interesting objects. In the paper we have: provided a thoughtful compilation of the knowledge of the Vela X-1 system and its modelling published over decades; added new information derived from public data or catalogues, including an updated distance and spectral classification based on the Gaia EDR3 release; and identified specific avenues of future research that could help to clarify open questions.

Published
2022
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22. Vela X-1 in depth: a review article on an outstanding object

Author

Martínez-Núñez, Silvia, Kretschmar, Peter, El Mellah, I., Fuerst, F., Grinberg, V., Sander, A. A. C, van den Eijnden, J., Degenaar, N., Maíz Apellániz, J., Jiménez Esteban, F., Ramos-Lerate, M, and Utrilla, E.

Subjects
X-rays: individuals: Vela X-1, X-rays: binaries, stars: winds, outflows, accretion, accretion disks, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

In this poster, we will summarise the review paper entitled: "Revisiting the archetypical wind accretor Vela X-1 in depth. Case study of a well-known X-ray binary and the limits of our knowledge." The paper, published in late 2021 in Astronomy and Astrophysics journal, triggered a discussion amongst the editors of Astronomy and Astrophysics leading to the creation of a new type of review article on uniquely interesting objects. In the paper we have: provided a thoughtful compilation of the knowledge of the Vela X-1 system and its modelling published over decades; added new information derived from public data or catalogues, including an updated distance and spectral classification based on the Gaia EDR3 release; and identified specific avenues of future research that could help to clarify open questions., SMN acknowledges funding by the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER, UE), co-funded by FEDER funds and by the Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765.

Published
2022
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24. Forskolin induced swelling (FIS) assay in intestinal organoids to guide eligibility for compassionate use treatment in a CF patient with a rare genotype

Author

Onderzoek Longziekten, Infection & Immunity, Longziekten patientenzorg, Speerpunt Child Health, Child Health, Longziekten onderzoek 2, Onderzoek, Regenerative Medicine and Stem Cells, Longziekten, Aalbers, B L, Brunsveld, J E, van der Ent, C K, van den Eijnden, J C, Beekman, J M, Heijerman, H G M, Onderzoek Longziekten, Infection & Immunity, Longziekten patientenzorg, Speerpunt Child Health, Child Health, Longziekten onderzoek 2, Onderzoek, Regenerative Medicine and Stem Cells, Longziekten, Aalbers, B L, Brunsveld, J E, van der Ent, C K, van den Eijnden, J C, Beekman, J M, and Heijerman, H G M

Published
2022

27. A Swift study of long-term changes in the X-ray flaring properties of Sagittarius A

Author

Andrés, A, primary, van den Eijnden, J, additional, Degenaar, N, additional, Evans, P A, additional, Chatterjee, K, additional, Reynolds, M, additional, Miller, J M, additional, Kennea, J, additional, Wijnands, R, additional, Markoff, S, additional, Altamirano, D, additional, Heinke, C O, additional, Bahramian, A, additional, Ponti, G, additional, and Haggard, D, additional

Published
2021
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30. Revisiting the archetypical wind accretor Vela X-1 in depth

Author

Kretschmar, P., primary, El Mellah, I., additional, Martínez-Núñez, S., additional, Fürst, F., additional, Grinberg, V., additional, Sander, A. A. C., additional, van den Eijnden, J., additional, Degenaar, N., additional, Maíz Apellániz, J., additional, Jiménez Esteban, F., additional, Ramos-Lerate, M., additional, and Utrilla, E., additional

Published
2021
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31. Multiwavelength observations reveal a faint candidate black hole X-ray binary in IGR J17285−2922

Author

Stoop, M, primary, van den Eijnden, J, additional, Degenaar, N, additional, Bahramian, A, additional, Swihart, S J, additional, Strader, J, additional, Jiménez-Ibarra, F, additional, Muñoz-Darias, T, additional, Armas Padilla, M, additional, Shaw, A W, additional, Maccarone, T J, additional, Wijnands, R, additional, Russell, T D, additional, Santisteban, J V Hernández, additional, Miller-Jones, J C A, additional, Russell, D M, additional, Maitra, D, additional, Heinke, C O, additional, Sivakoff, G R, additional, Lewis, F, additional, and Bramich, D M, additional

Published
2021
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32. A new radio census of neutron star X-ray binaries

Author

van den Eijnden, J, primary, Degenaar, N, additional, Russell, T D, additional, Wijnands, R, additional, Bahramian, A, additional, Miller-Jones, J C A, additional, Hernández Santisteban, J V, additional, Gallo, E, additional, Atri, P, additional, Plotkin, R M, additional, Maccarone, T J, additional, Sivakoff, G, additional, Miller, J M, additional, Reynolds, M, additional, Russell, D M, additional, Maitra, D, additional, Heinke, C O, additional, Armas Padilla, M, additional, and Shaw, A W, additional

Published
2021
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33. VLA detection of the radio counterpart of the BeXRB 1A 0535+262

Author

van den Eijnden, J., Degenaar, N., Wijnands, R., Russell, T.D., Sivakoff, G.R., Miller-Jones, J.C.A., Rouco Escorial, A., Herádez Santisteban, J., Reynolds, M., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

After the announcement of a new outburst of the transient Be/X-ray binary and X-ray pulsar 1A 0535+262 (Atel #14157), and its continuously increasing X-ray flux since then (Atel #14170, Atel #14171, Atel #14173, Atel #14179), we have observed this source with the Karl G. Jansky Very Large Array (VLA) to search for a radio counterpart.

Published
2020

34. VLA detection of a likely radio counterpart of IGR J17494-3030

Author

van den Eijnden, J., Degenaar, N., Wijnands, R., Russell, T.D., Stoop, M., Armas Padilla, M., Russell, D.M., Maitra, D., Heinke, C.O., Sivakoff, G. R., Shaw, A.W., Maccarone, T.J., Miller-Jones, J.C.A., Bahramian, A., High Energy Astrophys. & Astropart. Phys (API, FNWI), and API Other Research (FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics
Abstract

IGR J17494-3030 is a transient X-ray binary that was recently reported to be in outburst by INTEGRAL (ATel #14119). Follow-up NICER observations have subsequently shown the presence of X-ray pulsations at 376 Hz (ATel #14124), confirming the neutron star nature of the compact object and identifying IGR J17494-3030 as an accreting millisecond X-ray pulsar (AMXP).

Published
2020

35. VLA radio detection of the new X-ray transient SRGt J071522.1-191609

Author

van den Eijnden, J., Degenaar, N., Wijnands, R., Russell, T., Stoop, M., Armas Padilla, M., Russell, D.M., Maitra, D., Heinke, C.O., Sivakoff, G.R., Shaw, A.W., Maccarone, T.J., Miller-Jones, J.C.A., Bahramian, A., High Energy Astrophys. & Astropart. Phys (API, FNWI), and API Other Research (FNWI)

Abstract

Following the eROSITA discovery of the new X-ray transient SRGt J071522.1-191609 (ATel #13657) and the first follow-up observation using the X-ray telescope (XRT) on board the Neil Gehrels Swift Observatory (ATel #13661), we triggered an X-ray and radio monitoring program using Swift/XRT and the Karl G. Jansky Very Large Array (VLA).

Published
2020

36. Dips and eclipses in the X-ray binary Swift J1858.6–0814 observed with NICER

Author

Buisson, D J K, primary, Altamirano, D, additional, Armas Padilla, M, additional, Arzoumanian, Z, additional, Bult, P, additional, Castro Segura, N, additional, Charles, P A, additional, Degenaar, N, additional, Díaz Trigo, M, additional, van den Eijnden, J, additional, Fogantini, F, additional, Gandhi, P, additional, Gendreau, K, additional, Hare, J, additional, Homan, J, additional, Knigge, C, additional, Malacaria, C, additional, Mendez, M, additional, Muñoz Darias, T, additional, Ng, M, additional, Özbey Arabacı, M, additional, Remillard, R, additional, Strohmayer, T E, additional, Tombesi, F, additional, Tomsick, J A, additional, Vincentelli, F, additional, and Walton, D J, additional

Published
2021
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40. Rapid compact jet quenching in the Galactic black hole candidate X-ray binary MAXI J1535−571

Author

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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41. Soft X-ray emission lines in the X-ray binary Swift J1858.6–0814 observed with XMM–Newton Reflection Grating Spectrometer: disc atmosphere or wind?

Author

Buisson, D J K, primary, Altamirano, D, additional, Díaz Trigo, M, additional, Mendez, M, additional, Armas Padilla, M, additional, Castro Segura, N, additional, Degenaar, N D, additional, van den Eijnden, J, additional, Fogantini, F A, additional, Gandhi, P, additional, Knigge, C, additional, Muñoz-Darias, T, additional, Özbey Arabacı, M, additional, and Vincentelli, F M, additional

Published
2020
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42. The variable radio counterpart of Swift J1858.6-0814

Author

van den Eijnden, J, primary, Degenaar, N, additional, Russell, T D, additional, Buisson, D J K, additional, Altamirano, D, additional, Armas Padilla, M, additional, Bahramian, A, additional, Castro Segura, N, additional, Fogantini, F A, additional, Heinke, C O, additional, Maccarone, T, additional, Maitra, D, additional, Miller-Jones, J C A, additional, Muñoz-Darias, T, additional, Özbey Arabacı, M, additional, Russell, D M, additional, Shaw, A W, additional, Sivakoff, G, additional, Tetarenko, A J, additional, Vincentelli, F, additional, and Wijnands, R, additional

Published
2020
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44. The Changing-look Optical Wind of the Flaring X-Ray Transient Swift J1858.6-0814

Author

Muñoz-Darias, T., primary, Padilla, M. Armas, additional, Jiménez-Ibarra, F., additional, Panizo-Espinar, G., additional, Casares, J., additional, Altamirano, D., additional, Buisson, D. J. K., additional, Segura, N. Castro, additional, Cúneo, V. A., additional, Degenaar, N., additional, Fogantini, F. A., additional, Knigge, C., additional, Sánchez, D. Mata, additional, Özbey Arabaci, M., additional, Sánchez-Sierras, J., additional, Torres, M. A. P., additional, van den Eijnden, J., additional, and Vincentelli, F. M., additional

Published
2020
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45. Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: disc atmosphere or wind?

Author

Buisson, D. J. K., Altamirano, Diego, Diaz Trigo, M., Mendez, Mariano, Padilla, M. Armas, Castro Segura, N., Degenaar, Nathalie, van den Eijnden, J., Fogantini, Federico Adrián, Gandhi, Poshak, Knigge, Christian, Muñoz-Darias, T., Arabaci, M. Ozbey, and Vincentelli, F. M.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Ciencias Astronómicas, Accretion, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, neutron [Stars], Astrophysics::Cosmology and Extragalactic Astrophysics, Black hole physics, Stars: neutron, X-rays: binaries, Astrophysics::Solar and Stellar Astrophysics, binaries [X-rays], Astrophysics - High Energy Astrophysical Phenomena, Accretion discs, Astrophysics::Galaxy Astrophysics
Abstract

We find soft X-ray emission lines from the X-ray binary Swift J1858.6-0814 in data from XMM-Newton-RGS: N VII, O VII and O VIII, as well as notable residuals short of a detection at Ne IX and other higher ionisation transitions. These could be associated with the disc atmosphere, as in accretion disc corona sources, or with a wind, as has been detected in Swift J1858.6-0814 in emission lines at optical wavelengths. Indeed, the N VII line is redshifted, consistent with being the emitting component of a P-Cygni profile. We find that the emitting plasma has an ionisation parameter $\log(��)=1.35\pm0.2$ and a density $n>1.5\times10^{11}$ cm$^{-3}$. From this, we infer that the emitting plasma must be within $10^{13}$ cm of the ionising source, $\sim5\times10^{7}r_{\rm g}$ for a $1.4M_{\odot}$ neutron star, and from the line width that it is at least $10^4r_{\rm g}$ away ($2\times10^{9}(M/1.4M_{\odot})$ cm). We compare this with known classes of emission line regions in other X-ray binaries and active galactic nuclei., 10 pages, 7 figures, MNRAS accepted

Published
2020
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46. Serendipitous detection of a new outburst of the HMXB IGR J19294+1816 with XMM-Newton

Author

Domcek, V., van den Eijnden, J., Rouco Censorial, A., Hernandez Santisteban, J., Degenaar, N., Wijnands, R., Parikh, A., Zhou, P., Vink, J., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

IGR J19294+1816 is an accreting pulsar in high-mass X-ray binary thatwas discovered by Integral on 31st of March 2009 (ATel #1997). Further studies using Swift/XRT data have found pulsation period of 12.45s (ATel #1998; #2002) and that it falls within the region of pulse period vs. orbital period parameter space expected for a Be X-ray binary system(ATel #2008).

Published
2019

47. Swift Observation during the 2019 outburst of Swift J1357.2-0933

Author

Beri, A., Wijnands, R., Russell, T., Degenaar, N., van den Eijnden, J., Gandhi, P., Paice, J.A., Altamirano, D., Armas Padilla, M., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
General Relativity and Quantum Cosmology, Astrophysics::High Energy Astrophysical Phenomena
Abstract

The Galactic black-hole candidate Swift J1357.2-0933 has been reported to be in a new outburst by the Zwicky Transient Factory (ZTF; Bellm et al 2019, PASP 131, 018002).

Published
2019

48. Swift/XRT detection of the very faint X-ray binary transient IGR J17285-2922

Author

Armas Padilla, M., van den Eijnden, J., Degenaar, N., Wijnands, R., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Abstract

Following the recent detection with INTEGRAL/IBIS-ISCRI of the very faint X-ray binary IGR J17285-2922 (ATel #12646), we report on a 1 ks Swift/XRT observation taken on April 10th 2019.

Published
2019

49. Radio and X-ray monitoring of the accreting millisecond X-ray pulsar IGR J17591-2342 in outburst

Author

Gusinskaia, N.V., Russell, T.D., Hessels, J.W.T., Bogdanov, S., Degenaar, N., Deller, A.T., Van Den Eijnden, J., Jaodand, A.D., Miller-Jones, James, Wijnands, R., Gusinskaia, N.V., Russell, T.D., Hessels, J.W.T., Bogdanov, S., Degenaar, N., Deller, A.T., Van Den Eijnden, J., Jaodand, A.D., Miller-Jones, James, and Wijnands, R.

Abstract

© 2019 The Author(s). IGR J17591-2342 is a new accreting millisecond X-ray pulsar that was recently discovered in outburst in 2018. Early observations revealed that the source's radio emission is brighter than that of any other known neutron star low-mass X-ray binary (NS-LMXB) at comparable X-ray luminosity, and assuming its likely >~6 kpc distance. It is comparably radio bright to black hole LMXBs at similar X-ray luminosities. In this work, we present the results of our extensive radio and X-ray monitoring campaign of the 2018 outburst of IGR J17591-2342. In total, we collected 10 quasi-simultaneous radio (VLA, ATCA) and X-ray (Swift-XRT) observations, which make IGR J17591-2342 one of the best-sampled NS-LMXBs. We use these to fit a power-law correlation index β = 0.37+0.42-0.40 between observed radio and X-ray luminosities (LR α LXβ ). However, our monitoring revealed a large scatter in IGR J17591-2342's radio luminosity (at a similar X-ray luminosity, LX ~1036 erg s-1, and spectral state), with LR ~ 4 × 1029 erg s-1 during the first three reported observations, and up to a factor of 4 lower LR during later radio observations. None the less, the average radio luminosity of IGR J17591-2342 is still one of the highest among NS-LMXBs, and we discuss possible reasons for the wide range of radio luminosities observed in such systems during outburst.We found no evidence for radio pulsations from IGR J17591-2342 in our Green Bank Telescope observations performed shortly after the source returned to quiescence. None the less, we cannot rule out that IGR J17591-2342 becomes a radio millisecond pulsar during quiescence.

Published
2020

50. Rapid compact jet quenching in the Galactic black hole candidate X-ray binary MAXI J1535−571

Author

Russell, T.D., Lucchini, M., Tetarenko, A.J., Miller-Jones, James, Sivakoff, G.R., Krauß, F., Mulaudzi, W., Baglio, M.C., Russell, D.M., Altamirano, D., Ceccobello, C., Corbel, S., Degenaar, N., van den Eijnden, J., Fender, R., Heinz, S., Koljonen, K.I.I., Maitra, D., Markoff, S., Migliari, S., Parikh, A.S., Plotkin, Richard, Rupen, M., Sarazin, C., Soria, Roberto, Wijnands, R., Russell, T.D., Lucchini, M., Tetarenko, A.J., Miller-Jones, James, Sivakoff, G.R., Krauß, F., Mulaudzi, W., Baglio, M.C., Russell, D.M., Altamirano, D., Ceccobello, C., Corbel, S., Degenaar, N., van den Eijnden, J., Fender, R., Heinz, S., Koljonen, K.I.I., Maitra, D., Markoff, S., Migliari, S., Parikh, A.S., Plotkin, Richard, Rupen, M., Sarazin, C., Soria, Roberto, and Wijnands, R.

Abstract

We present results from six epochs of quasi-simultaneous radio, (sub-)millimetre, infrared, optical, and X-ray observations of the black hole X-ray binary MAXI J1535−571. These observations show that as the source transitioned through the hard-intermediate X-ray state towards the soft-intermediate X-ray state, the jet underwent dramatic and rapid changes. We observed the frequency of the jet spectral break, which corresponds to the most compact region in the jet where particle acceleration begins (higher frequencies indicate closer to the black hole), evolves from the infrared band into the radio band (decreasing by ≈3 orders of magnitude) in less than a day. During one observational epoch, we found evidence of the jet spectral break evolving in frequency through the radio band. Estimating the magnetic field and size of the particle acceleration region shows that the rapid fading of the high-energy jet emission was not consistent with radiative cooling; instead, the particle acceleration region seems to be moving away from the black hole on approximately dynamical time-scales. This result suggests that the compact jet quenching is not caused by local changes to the particle acceleration, rather we are observing the acceleration region of the jet travelling away from the black hole with the jet flow. Spectral analysis of the X-ray emission shows a gradual softening in the few days before the dramatic jet changes, followed by a more rapid softening ∼1-2 d after the onset of the jet quenching.

Published
2020

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