RADIO AND Γ-Ray CONSTRAINTS ON THE EMISSION GEOMETRY AND BIRTHPLACE OF PSR J2043+2740

Noutsos, A.; Abdo, A. A.; Ackermann, M.; Ajello, M.; Ballet, J.; Barbiellini, G.; Baring, Matthew G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bonamente, E.; Borgland, A. W.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, Pascal; Buehler, R.; Busetto, G.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Chaty, S.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Colafrancesco, S.; Cutini, S.; Dermer, C. D.; Palma, F. de; Drell, P. S.; Dumora, D.; M., Carroll Sean; Favuzzi, C.; Ferrara, E. C.; Focke, W. B.; Frailis, M.; Freire, P. C. C.; Fukazawa, Yasushi; Funk, S.; Fusco, P.; Gargano, F.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Godfrey, G.; Grandi, P.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Harding, A. K.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Katagiri, H.; Kataoka, J.; Knödlseder, J.; Krämer, M.; Kuss, M.; Landé, J.; Lee, S.-H.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Makeev, A.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; Méhault, J.; Michelson, P. F.; Mizuno, T.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godó, M.; Nolan, P. L.; Nuss, E.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Panetta, J.; Parent, D.; Pelassa, V.; Pepé, M.; Peršić, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Ray, Paul S.; Razzano, M.; Reimer, A.; Reposeur, T.; Romani, Roger W.; Sadrozinski, H. F-W.; Sander, A.; Parkinson, P. M. Saz; Sgrò, C.; Siskind, E. J.; Smith, David A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Strickman, M. S.; Suson, D. J.; Takahashi, H.; Tanaka, Takaaki; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibolla, O.; Torres, D. F.; Tramacere, A.; Usher, T.; Vandenbroucke, J.; Vianello, G.; Vilchez, N.; Villata, M.; Vitale, V.; Kienlin, A. von; Waite, A. P.; Wang, P.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ziegler, M.

doi:10.1088/0004-637x/728/2/77

Cited by 10 publications

(3 citation statements)

References 58 publications

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“…Figure 2 also exhibits a decrease in the ratio of peaks P1 and P2 with increasing energy. Also observed in other LAT pulsars (see, e.g., Abdo et al 2010cAbdo et al , 2010dNoutsos et al 2011), this is thought to be caused by varying gamma-ray emission altitudes and curvature radii of the magnetic field lines as the pulsar rotates (Abdo et al 2010d).…”

Section: Pulse Profile and Spectral Parametersmentioning

confidence: 77%

PSR J1838–0537: Discovery of a Young, Energetic Gamma-Ray Pulsar

Pletsch

Guillemot

Allen

et al. 2012

ApJ

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We report the discovery of PSR J1838−0537, a gamma-ray pulsar found through a blind search of data from the Fermi Large Area Telescope (LAT). The pulsar has a spin frequency of 6.9 Hz and a frequency derivative of −2.2 × 10 −11 Hz s −1 , implying a young characteristic age of 4970 yr and a large spin-down power of 5.9 × 10 36 erg s −1 . Follow-up observations with radio telescopes detected no pulsations; thus PSR J1838−0537 appears radio-quiet as viewed from Earth. In 2009 September the pulsar suffered the largest glitch so far seen in any gamma-ray-only pulsar, causing a relative increase in spin frequency of about 5.5 × 10 −6 . After the glitch, during a putative recovery period, the timing analysis is complicated by the sparsity of the LAT photon data, the weakness of the pulsations, and the reduction in average exposure from a coincidental, contemporaneous change in LAT's sky-survey observing pattern. The pulsar's sky position is coincident with the spatially extended TeV source HESS J1841−055 detected by the High Energy Stereoscopic System (H.E.S.S.). The inferred energetics suggest that HESS J1841−055 contains a pulsar wind nebula powered by the pulsar.

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Section: Pulse Profile and Spectral Parametersmentioning

confidence: 77%

PSR J1838–0537: Discovery of a Young, Energetic Gamma-Ray Pulsar

Pletsch

Guillemot

Allen

et al. 2012

ApJ

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“…PSR J2043+2740 (Ps=0.096 s) is a radio loud (Ray et al 1996) γ-ray pulsar (Pellizzoni et al 2009;Abdo et al 2010;Noutsos et al 2011). Its X-ray counterpart was detected by XMM-Newton but no X-ray pulsations were detected (Becker et al 2004).…”

Section: Introductionmentioning

confidence: 99%

Observations of three young γ-ray pulsars with the Gran Telescopio Canarias

Mignani

Rea

Testa

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Pulsed GeV γ-ray emission from more than 100 pulsars 10 has been observed by the Large Area Telescope (LAT; Atwood et al 2009) aboard the Fermi satellite, launched in 2008 June (see The Second Fermi Large Area Catalog of Gamma-Ray Pulsars; Fermi LAT Collaboration 2013, hereafter 2PC). The current population of γ-ray pulsars includes objects known from independent radio or X-ray observations and detected in γ rays by folding the Fermi LAT data at the known rotational periods (e.g., Abdo et al 2009a;Noutsos et al 2011;Espinoza et al 2013), and γ-ray pulsars found through direct blind searches of the LAT data (Abdo et al 2009b;Pletsch et al 2012) or radio searches for pulsars in unassociated γ-ray sources (see Ray et al 2012, and references therein). These pulsars are energetic (spindown luminositiesĖ = 4π 2 IṖ/P 3 > 10 33 erg s −1 , where P is the spin period,Ṗ is its first time derivative, and I denotes the moment of inertia, assumed to be 10 45 g cm 2 in this work) and are typically nearby.…”

Section: Introductionmentioning

confidence: 99%

FERMILAT PULSED DETECTION OF PSR J0737–3039A IN THE DOUBLE PULSAR SYSTEM

Guillemot

Krämer

Johnson

et al. 2013

ApJ

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We report the Fermi Large Area Telescope discovery of γ-ray pulsations from the 22.7 ms pulsar A in the double pulsar system J0737−3039A/B. This is the first mildly recycled millisecond pulsar (MSP) detected in the GeV domain. The 2.7 s companion object PSR J0737−3039B is not detected in γ rays. PSR J0737−3039A is a faint γ-ray emitter, so that its spectral properties are only weakly constrained; however, its measured efficiency is typical of other MSPs. The two peaks of the γ-ray light curve are separated by roughly half a rotation and are well offset from the radio and X-ray emission, suggesting that the GeV radiation originates in a distinct part of the magnetosphere from the other types of emission. From the modeling of the radio and the γ-ray emission profiles and the analysis of radio polarization data, we constrain the magnetic inclination α and the viewing angle ζ to be close to 90 • , which is consistent with independent studies of the radio emission from PSR J0737−3039A. A small misalignment angle between the pulsar's spin axis and the system's orbital axis is therefore favored, supporting the hypothesis that pulsar B was formed in a nearly symmetric supernova explosion as has been discussed in the literature already.

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RADIO AND Γ-Ray CONSTRAINTS ON THE EMISSION GEOMETRY AND BIRTHPLACE OF PSR J2043+2740

Cited by 10 publications

References 58 publications

PSR J1838–0537: Discovery of a Young, Energetic Gamma-Ray Pulsar

PSR J1838–0537: Discovery of a Young, Energetic Gamma-Ray Pulsar

Observations of three young γ-ray pulsars with the Gran Telescopio Canarias

FERMILAT PULSED DETECTION OF PSR J0737–3039A IN THE DOUBLE PULSAR SYSTEM

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