NuSTAR Hard X-Ray Observation of the Gamma-Ray Binary Candidate HESS J1832–093

Mori, Kaya; Gotthelf, E. V.; Hailey, Charles J.; Hord, Benjamin J.; Wilhelmi, E. de Oña; Rahoui, Farid; Tomsick, John A.; Zhang, Shuo; Hong, Jaesub; Garvin, Amani; Boggs, Steven E.; Christensen, Finn Erland; Craig, William W.; Harrison, Fiona A.; Stern, Daniel; Zhang, William W.

doi:10.3847/1538-4357/aa8d15

Cited by 13 publications

(17 citation statements)

References 69 publications

(105 reference statements)

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“…Since G22.7−0.2 is in a complex region with MCs, H II regions and the GLIMPSE9 stellar cluster (Su et al 2014), we consider the possibility of having a binary object related with those systems, thus at a distance of d = 4.4 ± 0.4 kpc. Assuming this distance and using the IR magnitudes from the literature of 2MASS J18324516−0921545, Mori et al (2017) derived a spectral type between B8V and B1.5V, fully compatible with the stars found in other γ-ray binaries (Dubus 2013). However, this result is only a lower limit since local dust absorption would increase their optical extinction (A V = 7.7).…”

Section: On the Optical Counterpart Issuesupporting

confidence: 67%

X-ray andγ-ray orbital variability from theγ-ray binary HESS J1832−093

Martí-Devesa

Reimer

2020

A&A

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Context. Gamma-ray binaries are systems composed of a massive star and a compact object whose interaction leads to particle acceleration up to relativistic energies. In the last fifteen years, a few binaries have been discovered to emit at high energies, but their number is still scarce. The TeV source HESS J1832−093 has been proposed as a binary candidate, although its nature is unclear. Neither a GeV counterpart nor a period was found for it. Aims. The purpose of this work is to search for a γ-ray source at GeV energies to understand the origin of the TeV signal. For an unambiguous identification of its binary nature, finding an orbital modulation is crucial. Methods. We have analysed data spanning more than 10 years from the Fermi Large Area Telescope (Fermi-LAT), together with Swift archival observations taken between 2015 and 2018, using both the X-Ray Telescope (XRT) and UltraViolet and Optical Telescope (UVOT). We searched for periodicities in both X-ray and γ-ray bands using a Lomb-Scargle periodogram. Results. We find a periodic modulation of ∼ 86 days in the X-ray source XMMU J183245−0921539, together with indications of γ-ray modulation with a compatible period in 4FGL J1832.9−0913. Neither an optical nor an UV counterpart is found at the X-ray source location. The overall spectral energy distribution strongly resembles the known γ-ray binary HESS J0632+057.Conclusions. Both the spectrum and the discovery of an orbital period allow the identification of the TeV source HESS J1832−093 as a new member of the γ-ray binary class.

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Section: On the Optical Counterpart Issuesupporting

confidence: 67%

X-ray andγ-ray orbital variability from theγ-ray binary HESS J1832−093

Martí-Devesa

Reimer

2020

A&A

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“…To the west of HESS J1834−087 is HESS J1832−093. Recent observations, strongly indicate a non-accreting binary origin for this gamma-ray emission (Eger et al 2016;Mori et al 2017). This is contrasted with initial investigations which suggested a possible association with the SNR G22.7−0.2 (HESS Collaboration et al 2015).…”

Section: The W41 Region and Hess J1832−085mentioning

confidence: 81%

A Supernova Remnant Counterpart for HESS J1832−085

Maxted¹,

Filipović²,

Hurley‐Walker³

et al. 2019

ApJ

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We examine the new Galactic supernova remnant (SNR) candidate, G23.11+0.18, as seen by the Murchison Widefield Array (MWA) radio telescope. We describe the morphology of the candidate and find a spectral index of −0.63±0.05 in the 70-170 MHz domain. A coincident TeV gamma-ray detection in High-Energy Stereoscopic System (HESS) data supports the SNR nature of G23.11+0.18 and suggests that G23.11+0.18 is accelerating particles beyond TeV energies, thus making this object a promising new cosmic ray hadron source candidate. The remnant cannot be seen in current optical, infrared and X-ray data-sets. We do find, however, a dip in CO-traced molecular gas at a line-of-sight velocity of ∼85 km s −1 , suggesting the existence of a G23.11+0.18 progenitor wind-blown bubble. Furthermore, the discovery of molecular gas clumps at a neighbouring velocity towards HESS J1832−085 adheres to the notion that a hadronic gamma-ray production mechanism is plausible towards the north of the remnant. Based on these morphological arguments, we propose an interstellar medium association for G23.11+0.18 at a kinematic distance of 4.6±0.8 kpc.

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“…Recently Mori et al (2017) reported on a NuSTAR X-ray observation of the field containing HESS J1832-093 and a reanalysis of the archival Chandra and XMM-Newton data. The data reanalysis does not confirm the same level of flux variation reported in previous work.…”

Section: Hess J1832-093mentioning

confidence: 99%

Overview of non-transientγ-ray binaries and prospects for the Cherenkov Telescope Array

Chernyakova

Malyshev

Paizis

et al. 2019

A&A

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Aims. Despite recent progress in the field, there are still many open questions regarding γ-ray binaries. In this paper we provide an overview of non-transient γ-ray binaries and discuss how observations with the Cherenkov Telescope Array (CTA) will contribute to their study. Methods. We simulate the spectral behaviour of the non-transient γ-ray binaries using archival observations as a reference. With this we test the CTA capability to measure the sources' spectral parameters and detect variability on various time scales. Results. We review the known properties of γ-ray binaries and the theoretical models that have been used to describe their spectral and timing characteristics. We show that CTA is capable of studying these sources on time scales comparable to their characteristic variability time scales. For most of the binaries, the unprecedented sensitivity of CTA will allow the spectral evolution to be studied on a time scale as short as 30 min. This will enable a direct comparison of the TeV and lower energy (radio to GeV) properties of these sources from simultaneous observations. We also review the source-specific questions that can be addressed with such high-accuracy CTA measurements.

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NuSTAR Hard X-Ray Observation of the Gamma-Ray Binary Candidate HESS J1832–093

Cited by 13 publications

References 69 publications

X-ray andγ-ray orbital variability from theγ-ray binary HESS J1832−093

X-ray andγ-ray orbital variability from theγ-ray binary HESS J1832−093

A Supernova Remnant Counterpart for HESS J1832−085

Overview of non-transientγ-ray binaries and prospects for the Cherenkov Telescope Array

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