ERRATUM: “THE FIRST FERMI LARGE AREA TELESCOPE
                    CATALOG OF GAMMA-RAY PULSARS” (2010, ApJS, 187, 460)

Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, Luca; Ballet, J.; Barbiellini, G.; Baring, Matthew G.; Bastieri, D.; Baughman, B. M.; 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; Burnett, T. H.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L.; Conrad, J.; Corbet, R. H. D.; Cutini, S.; Hartog, P. R. den; Dermer, C. D.; Angelis, A. De; Luca, A. De; Palma, F. de; Digel, S. W.; Dormody, M.; Silva, E. Do Couto E; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C. M.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Focke, W. B.; Fortin, P.; Frailis, M.; Freire, P. C. C.; Fukazawa, Yasushi; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giavitto, G.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Glanzman, T.; Godfrey, G.; Gotthelf, E. V.; Grenier, I. A.; Grondin, M.-H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Gwon, C.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jackson, M. S.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Johnston, S.; Kamae, T.; Kanbach, G.; Kaspi, V. M.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocian, M.; Krämer, M.; Kuss, M.; Landé, J.; Latronico, L.; Lemoine‐Goumard, M.; Livingstone, Margaret A.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Madejski, G.; Makeev, A.; Manchester, R. N.; Marelli, M.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mineo, T.; 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.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, Masanobu; Paneque, D.; Panetta, J.; Parent, D.; Pelassa, V.; Pepé, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Ray, Paul S.; Razzano, M.; Rea, N.; Reimer, A.; Reposeur, T.; Ritz, S.; Rodriguez, A. Y.; Romani, Roger W.; Roth, M.; Ryde, F.; Sadrozinski, H. F-W.; Sánchez, David; Sander, A.; Parkinson, P. M. Saz; Scargle, Jeffrey D.; Schalk, T.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, David A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stappers, B. W.; Starck, Jean-Luc; Striani, E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, Takaaki; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T.; Etten, A. van; Vasileiou, V.; Venter, C.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Wang, N.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.

doi:10.1088/0067-0049/193/1/22

Cited by 116 publications

(244 citation statements)

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“…As a PLE model typically describes the γ -ray spectrum of a pulsar (Abdo et al 2010b(Abdo et al , 2011, we speculate that there may be a hidden pulsar in HESS J1745-303. To test this hypothesis, we performed a blind search for coherent pulsation.…”

Section: Data Analysis and Resultsmentioning

confidence: 95%

EXPLORING THE DARK ACCELERATOR HESS J1745-303 WITH THEFERMILARGE AREA TELESCOPE

Hui

et al. 2011

ApJ

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We present a detailed analysis of the γ -ray emission from HESS J1745-303 with the data obtained by the Fermi Gamma-ray Space Telescope in its first ∼29 month observation. The source can clearly be detected at the levels of ∼18σ and ∼6σ in 1-20 GeV and 10-20 GeV, respectively. We do not find any evidence of the variability seen in the results obtained by the Compton Gamma-ray Observatory.

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Section: Data Analysis and Resultsmentioning

confidence: 95%

EXPLORING THE DARK ACCELERATOR HESS J1745-303 WITH THEFERMILARGE AREA TELESCOPE

Hui

et al. 2011

ApJ

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“…We performed LAT standard data processing using GTSELECT, GTMKTIME and GTBARY tools obtained from the HEADAS distribution of the Fermi ScienceTools (version V9R15P2) built on Scientific Linux 5 64 bit operating system. We selected E > 100 MeV events extracted within the 'region of interest' (ROI) of 2 degrees from X-ray source position (S/N ratio of Fermi-LAT pulsars is typically maximized taking ROI of ∼1 • -2 • around pulsar position; Abdo et al 2010a). We selected only events with high probability of being photons ('diffuse' event class = 3, data quality = 1) collected within 105 • maximum zenith angle (applying ROI-based zenith angle cut) and excluding data acquired during passages through the South Atlantic Anomaly.…”

Section: Gamma-ray Data Analysis and Resultsmentioning

confidence: 99%

Discovery of 59 ms pulsations from 1RXS J141256.0+792204 (Calvera)

Zane¹,

Haberl²,

Israel³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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101

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We report on the results of a multi‐wavelength study of the compact object candidate 1RXS J141256.0+792204 (Calvera). Calvera was observed in the X‐rays with XMM–Newton/EPIC twice for a total exposure time of ∼50 ks. The source spectrum is thermal and well reproduced by a two‐component model composed of either two (absorbed) hydrogen atmosphere models or two blackbodies with temperatures kT1∼ 55/150 eV, kT2∼ 80/250 eV, respectively (as measured at infinity). Evidence was found for an absorption feature at ∼0.65 keV while no power‐law high‐energy tail is statistically required. Using pn and MOS data we discovered pulsations in the X‐ray emission at a period P = 59.2 ms. The detection is highly significant (≳11σ), and unambiguously confirms the neutron star nature of Calvera. The pulse profile is nearly sinusoidal, with a pulsed fraction of ∼18 per cent. We looked for the timing signature of Calvera in the Fermi Large Area Telescope (LAT) data base and found a significant (∼5σ) pulsed signal at a period coincident with the X‐ray value. The gamma‐ray timing analysis yielded a tight upper limit on the period derivative, s s−1 ( erg s−1, B < 5 × 1010 G for magneto‐dipolar spin‐down). Radio searches at 1.36 GHz with the 100‐m Effelsberg radio telescope yielded negative results, with a deep upper limit on the pulsed flux of 0.05 mJy. Diffuse, soft (<1 keV) X‐ray emission about 13 arcmin west of the Calvera position is present both in our pointed observations and in archive ROSAT all‐sky survey images, but is unlikely associated with the X‐ray pulsar. Its spectrum is compatible with an old supernova remnant (SNR); no evidence for diffuse emission in the radio and optical bands was found. The most likely interpretations are that Calvera is either a central compact object escaped from a SNR or a mildly recycled pulsar; in both cases the source would be the first ever member of the class detected at gamma‐ray energies.

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“…Currently there is no reliable theory which can explain pulsar radio emission. The radio emission is coherent and it seems that conditions for generation of coherent emission in pulsar magnetospheres may be not always fulfilled -at least there are pulsars with periods and magnetic fields typical for radio-emitting pulsars which are visible in gamma-rays but show no detectable radio emission (Abdo et al 2010). If, at least for some range of pulsar parameters, the conditions for generation of coherent emission are very sensitive to the properties of the magnetospheric plasma -like current and plasma densities or/and their gradients -then it can be that in some of the magnetospheric states the coherent emission is not generated at all or is generated at different places.…”

Section: The Modelmentioning

confidence: 99%

A model for nulling and mode changing in pulsars

Timokhin

2010

Monthly Notices of the Royal Astronomical Society: Letters

135

113

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We propose that in some pulsars the magnetosphere has different states with different geometries or/and different distributions of currents, it occasionally switches between them. These states have different spindown rates and emission beams, in some of the states no radioemission is produced at all. Switching into a different state manifests as a mode change when we see different parts of the emission beam or the beams in different states have significantly different geometries, it manifests as nulling when we either miss the new beam or no radioemission is generated in the new state. We show that modest variations in the beam shape can be accompanied by large variations in the pulsar spindown rate W - the dependence of W on the opening angle of the emission beam $\alpha$ can be as strong as W\propto\alpha^4. We speculate about physical mechanisms which may cause reconfiguration of the magnetosphere.Comment: 5 pages, 1 figure; MNRAS, in pres

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ERRATUM: “THE FIRST FERMI LARGE AREA TELESCOPE CATALOG OF GAMMA-RAY PULSARS” (2010, ApJS, 187, 460)

Cited by 116 publications

References 1 publication

EXPLORING THE DARK ACCELERATOR HESS J1745-303 WITH THEFERMILARGE AREA TELESCOPE

EXPLORING THE DARK ACCELERATOR HESS J1745-303 WITH THEFERMILARGE AREA TELESCOPE

Discovery of 59 ms pulsations from 1RXS J141256.0+792204 (Calvera)

A model for nulling and mode changing in pulsars

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