DETECTION OF THE ENERGETIC PULSAR PSR B1509–58 AND ITS PULSAR WIND NEBULA IN MSH 15–52 USING THE<i>FERMI</i>-LARGE AREA TELESCOPE

Abdo, A. A.; Ackermann, M.; Ajello, M.; Allafort, A.; Asano, Katsuaki; Baldini, Luca; Ballet, J.; Barbiellini, G.; Baring, Matthew G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, Pascal; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Hartog, P. R. den; Dermer, C. D.; Luca, A. De; Palma, F. de; Dormody, M.; Silva, E. Do Couto E; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Frailis, M.; Fukazawa, Yasushi; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Gotthelf, E. V.; Grenier, I. A.; Grondin, M.-H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hays, E.; Hobbs, G.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Kanai, Yoshikazu; Kanbach, G.; Katagiri, H.; Kataoka, J.; Kawai, N.; Keith, Michael; Kerr, M.; Knödlseder, J.; Kuss, M.; Landé, J.; Latronico, L.; Lemoine‐Goumard, M.; Garde, M. Llena; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Моисеев, А. А.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, Takeshi; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J.; Parent, D.; Pelassa, V.; Pepé, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Rea, N.; Reimer, O.; Reposeur, T.; Rodriguez, A. Y.; Romani, Roger W.; Roth, M.; Ryde, F.; Sadrozinski, H. F-W.; Sander, A.; Parkinson, P. M. Saz; Sgrò, C.; Siskind, E. J.; Smith, David Stanley; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, Jean-Luc; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Takahashi, Tadayuki; Tanaka, Takaaki; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T.; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Ylinen, T.; Ziegler, M.

doi:10.1088/0004-637x/714/1/927

Cited by 91 publications

(84 citation statements)

References 56 publications

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“…For better visualization we show higher-level error bands for the X-ray data and for the modeled SEDs. The data shown left are adopted from [9], [10] and [11] while data in the right panel are taken from [12], [13] and [14].…”

Section: The Modelmentioning

confidence: 99%

Unidentified VHE γ-ray sources and evolved pulsar wind nebulae - A possible connection?

Mayer¹,

Brucker²,

Holler³

et al. 2012

AIP Conference Proceedings

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Abstract. Among Galactic VHE (very high energy, E > 100 GeV) γ-ray sources, pulsar wind nebulae (PWNe) form the most abundant class. At the same time, there are numerous sources of VHE γ-rays which are still unidentified. A firm identification of such objects requires a counterpart at other wavelengths. Middle-aged PWNe may account for many of these unidentified sources. While leptons that have been injected into a PWN a long time ago can still cause the observed VHE γ-ray flux, the present energy output of the pulsar is significantly reduced with respect to former times and powers only a faint synchrotron nebula which is difficult to detect with current X-ray observatories. We present a time-dependent model to study the spectral evolution of PWNe. With this model it is possible to roughly predict the X-ray emission of PWNe based on the VHE γ-ray observations only. These predictions allow to select those unidentified VHE γ-ray sources for which, assuming an evolved PWN scenario, a detection of an X-ray counterpart seems to be feasible.

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Section: The Modelmentioning

confidence: 99%

Unidentified VHE γ-ray sources and evolved pulsar wind nebulae - A possible connection?

Mayer¹,

Brucker²,

Holler³

et al. 2012

AIP Conference Proceedings

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“…This feature could be as low as ∼ 130 keV, as has been suggested (Wang et al 2014) by an analysis of nine years of INTEGRAL/IBIS data for the bright AXP 4U 0142+61. The need for such a spectral turnover is reinforced above 100 MeV by upper limits in Fermi-LAT data for around 20 magnetars (Abdo et al 2010, Li et al 2017. We mention that Wu et al (2013) reported discovery of pulsed gamma-ray emission above 200 MeV from AXP 1E2259+586 with a targeted search of public 4-year Fermi-LAT data archive.…”

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confidence: 95%

“…A classic exemplar is the "low-field" magnetar SGR 0418+5729, with a field estimate of B p ∼ 1.2 × 10 13 Gauss ) and sporadic outburst activity that is the hallmark of magnetars. Yet it too, may present a challenge to stereotypes in that there is suggestive evidence of a variable proton cyclotron absorption feature (Tiengo et al 2013), implying that it possesses local magnetic field components of 10 14 − 10 15 G. Then there are tens of rotation-powered high-field pulsars such as PSR B1509-58 (Abdo et al 2010) and PSR J1846-0258 (Kuiper, Hermsen & Dekker 2018), whose polar fields approach or exceed 10 13 G, the latter of which has been shown to have magnetar-like outbursts (Gavriil et al 2008), as has PSR J1119-6127 (Gögüş et al 2016). Interestingly following their outbursts, the quiescent power-law spectrum of J1846-0258 developed a transient thermal-like component (Kuiper & Hermsen 2009), while the quiescent thermal spectrum of J1119-6127 at temperature ∼ 0.2 keV heated to the higher value of ∼ 1 keV, with an additional transient power-law component (Archibald et al 2016), so that each had a transient magnetar-like spectrum.…”

mentioning

confidence: 99%

Resonant Inverse Compton Scattering Spectra from Highly Magnetized Neutron Stars

Wadiasingh

Baring

Gonthier

et al. 2018

ApJ

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Hard, non-thermal, persistent pulsed X-ray emission extending between 10 keV and ∼ 150 keV has been observed in nearly ten magnetars. For inner-magnetospheric models of such emission, resonant inverse Compton scattering of soft thermal photons by ultra-relativistic charges is the most efficient production mechanism. We present angle-dependent upscattering spectra and pulsed intensity maps for uncooled, relativistic electrons injected in inner regions of magnetar magnetospheres, calculated using collisional integrals over field loops. Our computations employ a new formulation of the QED Compton scattering cross section in strong magnetic fields that is physically correct for treating important spindependent effects in the cyclotron resonance, thereby producing correct photon spectra. The spectral cut-off energies are sensitive to the choices of observer viewing geometry, electron Lorentz factor, and scattering kinematics. We find that electrons with energies < ∼ 15 MeV will emit most of their radiation below 250 keV, consistent with inferred turnovers for magnetar hard X-ray tails. More energetic electrons still emit mostly below 1 MeV, except for viewing perspectives sampling field line tangents. Pulse profiles may be singly-or doubly-peaked dependent upon viewing geometry, emission locale, and observed energy band. Magnetic pair production and photon splitting will attenuate spectra to hard X-ray energies, suppressing signals in the Fermi-LAT band. The resonant Compton spectra are strongly polarized, suggesting that hard X-ray polarimetry instruments such as X-Calibur, or a future Compton telescope, can prove central to constraining model geometry and physics.

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“…In addition, future X-ray observations could detect pulsed emission from Suzaku source A or source B. Given these detections, emission models for PWNe (e.g., Abdo et al 2010b;Tanaka & Takahara 2010;Slane et al 2010;Bucciantini et al 2011), using a broken power-law distribution of electrons, might be able to reveal that the VHE gamma-ray emission of this unidentified source originates from a PWN.…”

Section: Pwn Scenariomentioning

confidence: 99%

CANGAROO-III OBSERVATION OF TeV GAMMA RAYS FROM THE UNIDENTIFIED GAMMA-RAY SOURCE HESS J1614–518

Mizukami¹,

Kubo²,

Yoshida³

et al. 2011

ApJ

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We report the detection, with the CANGAROO-III imaging atmospheric Cherenkov telescope array, of a very high energy gamma-ray signal from the unidentified gamma-ray source HESS J1614−518, which was discovered in the H.E.S.S. Galactic plane survey. Diffuse gamma-ray emission was detected above 760 GeV at the 8.9σ level during an effective exposure of 54 hr from 2008 May to August. The spectrum can be represented by a power law: (8.2 ± 2.2 stat ± 2.5 sys ) × 10 −12 × (E/1 TeV) −γ cm −2 s −1 TeV −1 with a photon index γ of 2.4 ± 0.3 stat ± 0.2 sys , which is compatible with that of the H.E.S.S. observations. By combining our result with multiwavelength data, we discuss the possible counterparts for HESS J1614−518 and consider radiation mechanisms based on hadronic and leptonic processes for a supernova remnant (SNR), stellar winds from massive stars, and a pulsar wind nebula (PWN). Although a leptonic origin from a PWN driven by an unknown pulsar remains possible, hadronic-origin emission from an unknown SNR is preferred.

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DETECTION OF THE ENERGETIC PULSAR PSR B1509–58 AND ITS PULSAR WIND NEBULA IN MSH 15–52 USING THEFERMI-LARGE AREA TELESCOPE

Cited by 91 publications

References 56 publications

Unidentified VHE γ-ray sources and evolved pulsar wind nebulae - A possible connection?

Unidentified VHE γ-ray sources and evolved pulsar wind nebulae - A possible connection?

Resonant Inverse Compton Scattering Spectra from Highly Magnetized Neutron Stars

CANGAROO-III OBSERVATION OF TeV GAMMA RAYS FROM THE UNIDENTIFIED GAMMA-RAY SOURCE HESS J1614–518

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