Discovery of a new<b><i>INTEGRAL</i></b>source: IGR J19140+0951

Hannikainen, Diana; Rodríguez, J.; Cabanac, C.; Schultz, J.; Lund, N.; Vilhu, O.; Petrucci, P.-O.; Henri, G.

doi:10.1051/0004-6361:200400021

Cited by 19 publications

(21 citation statements)

References 12 publications

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“…The region of interest, which includes the microquasar GRS 1915+105 (Rodriguez et al 1995), the Integral source IGR J19140+0951 (Hannikainen et al 2004), the high spindown luminosity pulsar PSR J1913+1011 (Morris et al 2002), as well as the SNR candidate 44.6+0.1 (Kassim 1988), was first targeted in 2004 as part of the observational programme on GRS 1915+105. In 2005, dedicated observations were taken on the supernova remnant W 49B (Harris et al 1960); some of the pointings also cover the field-of-view of interest.…”

Section: Observations and Resultsmentioning

confidence: 99%

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Discovery of very-high-energy γ-ray emission from the vicinity of PSR J1913+1011 with HESS

Aharonian¹,

Akhperjanian²,

Bazer‐Bachi³

et al. 2008

A&A

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The HESS experiment, an array of four Imaging Atmospheric Cherenkov Telescopes with high sensitivity and large field-of-view, has been used to search for emitters of very-high-energy (VHE, >100 GeV) γ-rays along the Galactic plane, covering the region 30In this continuation of the HESS Galactic Plane Scan, a new extended VHE γ-ray source was discovered at α 2000 =19 h 12 m 49 s , δ 2000 =+10• 09 06 (HESS J1912+101). Its integral flux between 1-10 TeV is ∼10% of the Crab Nebula flux in the same energy range. The measured energy spectrum can be described by a power law dN/dE ∼ E −Γ with a photon index Γ = 2.7 ± 0.2 stat ± 0.3 sys . HESS J1912+101 is plausibly associated with the high spin-down luminosity pulsar PSR J1913+1011. We also discuss associations with an as yet unconfirmed SNR candidate proposed from low frequency radio observation and/or with molecular clouds found in 13 CO data.

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Section: Observations and Resultsmentioning

confidence: 99%

“…The first (Obs. Id 4590) was targeted on EXO 1912+097 (Lu et al 1996), which is coincident with and possibly the same object as IGR J19140+0951 (Hannikainen et al 2004). The overlap of this observation with HESS J1912+101 is marginal.…”

Section: Possible Associationsmentioning

confidence: 99%

Discovery of very-high-energy γ-ray emission from the vicinity of PSR J1913+1011 with HESS

Aharonian¹,

Akhperjanian²,

Bazer‐Bachi³

et al. 2008

A&A

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“…Timing analysis of the RXTE All-Sky Monitor (ASM) data showed an X-ray period of 13.55 days (Corbet et al 2004). Hannikainen et al (2004) presented high energy spectral analysis of the period of the discovery, concluding that the source manifests two distinct spectral behaviors, the first showing a thermal component in the soft X-ray and hard X-ray tail, the second being harder and possibly originating from thermal Comptonization. This second, low-luminosity, behavior was confirmed to be the preferred state of the source (Rodriguez et al 2005).…”

Section: Igr J19140+0951mentioning

confidence: 99%

Unveiling the nature of six HMXBs through IR spectroscopy

Nespoli¹,

Fabregat²,

Mennickent

2008

A&A

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Context. The International Gamma-Ray Astrophyiscs Laboratory (INTEGRAL) is discovering a large number of new hard X-ray sources, many of them being HMXBs. The identification and spectral characterization of their optical/infrared counterparts is a necessary step to undertake detailed study of these systems. In particular, the determination of the spectral type is crucial in the case of the new class of Supergiant Fast X-ray Transients (SFXTs), which show X-ray properties common to other objects. Aims. Our goal is to perform spectral analysis and classification of proposed counterparts to HMXBs in order to characterize the system they belong to. Methods. We used the ESO/NTT SofI spectrograph to observe proposed IR counterparts to HMXBs, obtaining K s medium resolution spectra (R = 1320) with a S /N 100. We classified them through comparison with published atlases. Results. We were able to spectrally classify the six sources. This allowed us to ascribe one of them to the new class of SFXTs and confirm the membership of two sources to this class. We confirmed the spectral classification, derived from optical spectroscopy, of a known system, 4U 1907-09, showing for the first time its infrared spectrum. The spectral classification was also used to estimate the distance of the sources. We compared the extinction as derived from X-ray data with effective interstellar extinction obtained from our data, discussing the absorption component due to the circumstellar environment, which we observed in four systems; in particular, intrinsic absorption seems to emerge as a typical feature of the entire class of SFXTs.

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“…IGR J19140+0951 is at a distance of ∼2−3 kpc (Rahoui et al 2008). A hard X-ray emission up to 100 keV with a spectral index 2.39 ± 0.11 is observed from this source (Hannikainen et al 2004). Its X-ray luminosity in the high state was ∼3.7 × 10 37 × (D/10 kpc) 2 erg s −1 ).…”

Section: Discussionmentioning

confidence: 86%

Gamma-rays from the vicinity of accreting neutron stars inside compact high-mass X-ray binaries

Bednarek

2009

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The dense wind of a massive star can be captured partially by a neutron star (NS) inside a compact binary system. Depending on the parameters of the NS and the wind, the matter can penetrate the inner NS magnetosphere. At some distance from the NS, a turbulent and magnetized transition region is formed due to the balance between the magnetic pressure and the pressure inserted by accreting matter. This region provides good conditions for acceleration of particles to relativistic energies. The matter at the transition region can farther accrete onto the NS surface (the accretor phase) or be expelled from the NS vicinity (the propeller phase). We consider the consequences of the acceleration of electrons at the transition region, concentrating on the situation in which at least part of the matter falls onto the NS surface. This matter creates a hot spot on the NS surface which emits thermal radiation. Relativistic electrons lose energy to the synchrotron process and the inverse Compton (IC) scattering of this thermal radiation. We calculate the synchrotron spectra (from X-rays to soft γ-rays) and IC spectra (above a few tens of MeV) expected in this scenario. We argue that a population of massive binaries discovered by the INTEGRAL observatory, which contain neutron stars hidden inside dense stellar winds of massive stars, is detectable by the Fermi LAT telescope in the GeV energy range. As an example, we predict the expected γ-ray flux from the source IGR J19140+0951.

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Discovery of a newINTEGRALsource: IGR J19140+0951

Cited by 19 publications

References 12 publications

Discovery of very-high-energy γ-ray emission from the vicinity of PSR J1913+1011 with HESS

Discovery of very-high-energy γ-ray emission from the vicinity of PSR J1913+1011 with HESS

Unveiling the nature of six HMXBs through IR spectroscopy

Gamma-rays from the vicinity of accreting neutron stars inside compact high-mass X-ray binaries

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