Abstract
The Vela pulsar is the brightest persistent source in the GeV sky and thus is the traditional first target for new γ-ray observatories. We report here on initial Fermi Large Area Telescope observations during verification phase pointed exposure and early sky survey scanning. We have used the Vela signal to verify Fermi timing and angular resolution. The high-quality pulse profile, with some 32,400 pulsed photons at E ≥ 0.03GeV, shows new features, including pulse structure as fine as 0.3ms and a distinct third peak, which shifts in phase with energy. We examine the high-energy behavior of the pulsed emission; initial spectra suggest a phase-averaged power-law index of Γ = 1.51+0.05 -0.04 with an exponential cutoff at E c = 2.9 ± 0.1 GeV. Spectral fits with generalized cutoffs of the form require b ≤ 1, which is inconsistent with magnetic pair attenuation, and thus favor outer-magnetosphere emission models. Finally, we report on upper limits to any unpulsed component, as might be associated with a surrounding pulsar wind nebula.
| Original language | English |
|---|---|
| Pages (from-to) | 1084-1093 |
| Number of pages | 10 |
| Journal | Astrophysical Journal |
| Volume | 696 |
| Issue number | 2 |
| DOIs | |
| Publication status | Published - 2009 May 10 |
| Externally published | Yes |
Keywords
- gamma rays: observations
- pulsars: individual (PSR B0833-45)
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
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Fermi large area telescope observations of the vela pulsar. / Abdo, A. A.; Ackermann, M.; Atwood, W. B.; Bagagli, R.; Baldini, L.; Ballet, J.; Band, D. L.; Barbiellini, G.; Baring, M. G.; Bartelt, J.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellardi, F.; Bellazzini, R.; Berenji, B.; Bisello, D.; Blandford, R. D.; Bloom, E. D.; Bogart, J. R.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Camilo, F.; Caraveo, P. A.; Casandjian, J. M.; Ceccanti, M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cognard, I.; Cohen-Tanugi, J.; Cominsky, L. R.; Conrad, J.; Corbet, R.; Corucci, L.; Cutini, S.; Davis, D. S.; Deklotz, M.; Dermer, C. D.; De Angelis, A.; De Palma, F.; Digel, S. W.; Dormody, M.; Silva, E. Do Couto E.; Drell, P. S.; Dubois, R.; Dumora, D.; Espinoza, C.; Farnier, C.; Favuzzi, C.; Flath, D. L.; Fleury, P.; Focke, W. B.; Frailis, M.; Friere, P. C.C.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giannitrapani, R.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Gotthelf, E. V.; Grenier, I. A.; Grondin, M. H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Haller, G.; Harding, A. K.; Hart, P. A.; Hartman, R. C.; Hays, E.; Hobbs, G.; Hughes, R. E.; 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.; Kavelaars, A.; Kawai, N.; Kelly, H.; Kerr, M.; Kiziltan, B.; Klamra, W.; Knödlseder, J.; Kramer, M.; Kuehn, F.; Kuss, M.; Lande, J.; Landriu, D.; Latronico, L.; Lee, B.; Lee, S. H.; Lemoine-Goumard, M.; Livingstone, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Lyne, A. G.; Madejski, G. M.; Makeev, A.; Manchester, R. N.; Marangelli, B.; Marelli, M.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; McLaughlin, M. A.; Menon, N.; Meurer, C.; Michelson, P. F.; Mineo, T.; Mirizzi, N.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Mongelli, M.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Noutsos, A.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paccagnella, A.; Paneque, D.; Panetta, J. H.; Parent, D.; Pearce, M.; Pepe, M.; Perchiazzi, M.; Pesce-Rollins, M.; Pieri, L.; Pinchera, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Ransom, S. M.; Rapposelli, E.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, L. C.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Romani, R. W.; Roth, M.; Ryde, F.; Sacchetti, A.; Sadrozinski, H. F.W.; Saggini, N.; Sanchez, D.; Sander, A.; Parkinson, P. M.Saz; Segal, K. N.; Sellerholm, A.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Starck, J. L.; Stecker, F. W.; Stephens, T. E.; Strickman, M. S.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Tenze, A.; Thayer, J. B.; Thayer, J. G.; Theureau, G.; Thompson, D. J.; Thorsett, S. E.; Tibaldo, L.; Tibolla, O.; Torres, D. F.; Tramacere, A.; Turri, M.; Usher, T. L.; Vigiani, L.; Vilchez, N.; Vitale, V.; Waite, A. P.; Wang, P.; Watters, K.; Weltevrede, P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.
In: Astrophysical Journal, Vol. 696, No. 2, 10.05.2009, p. 1084-1093.Research output: Contribution to journal › Article › peer-review
}
TY - JOUR
T1 - Fermi large area telescope observations of the vela pulsar
AU - Abdo, A. A.
AU - Ackermann, M.
AU - Atwood, W. B.
AU - Bagagli, R.
AU - Baldini, L.
AU - Ballet, J.
AU - Band, D. L.
AU - Barbiellini, G.
AU - Baring, M. G.
AU - Bartelt, J.
AU - Bastieri, D.
AU - Baughman, B. M.
AU - Bechtol, K.
AU - Bellardi, F.
AU - Bellazzini, R.
AU - Berenji, B.
AU - Bisello, D.
AU - Blandford, R. D.
AU - Bloom, E. D.
AU - Bogart, J. R.
AU - Bonamente, E.
AU - Borgland, A. W.
AU - Bouvier, A.
AU - Bregeon, J.
AU - Brez, A.
AU - Brigida, M.
AU - Bruel, P.
AU - Burnett, T. H.
AU - Caliandro, G. A.
AU - Cameron, R. A.
AU - Camilo, F.
AU - Caraveo, P. A.
AU - Casandjian, J. M.
AU - Ceccanti, M.
AU - Cecchi, C.
AU - Charles, E.
AU - Chekhtman, A.
AU - Cheung, C. C.
AU - Chiang, J.
AU - Ciprini, S.
AU - Claus, R.
AU - Cognard, I.
AU - Cohen-Tanugi, J.
AU - Cominsky, L. R.
AU - Conrad, J.
AU - Corbet, R.
AU - Corucci, L.
AU - Cutini, S.
AU - Davis, D. S.
AU - Deklotz, M.
AU - Dermer, C. D.
AU - De Angelis, A.
AU - De Palma, F.
AU - Digel, S. W.
AU - Dormody, M.
AU - Silva, E. Do Couto E.
AU - Drell, P. S.
AU - Dubois, R.
AU - Dumora, D.
AU - Espinoza, C.
AU - Farnier, C.
AU - Favuzzi, C.
AU - Flath, D. L.
AU - Fleury, P.
AU - Focke, W. B.
AU - Frailis, M.
AU - Friere, P. C.C.
AU - Fukazawa, Y.
AU - Funk, S.
AU - Fusco, P.
AU - Gargano, F.
AU - Gasparrini, D.
AU - Gehrels, N.
AU - Germani, S.
AU - Giannitrapani, R.
AU - Giebels, B.
AU - Giglietto, N.
AU - Giordano, F.
AU - Glanzman, T.
AU - Godfrey, G.
AU - Gotthelf, E. V.
AU - Grenier, I. A.
AU - Grondin, M. H.
AU - Grove, J. E.
AU - Guillemot, L.
AU - Guiriec, S.
AU - Haller, G.
AU - Harding, A. K.
AU - Hart, P. A.
AU - Hartman, R. C.
AU - Hays, E.
AU - Hobbs, G.
AU - Hughes, R. E.
AU - Jóhannesson, G.
AU - Johnson, A. S.
AU - Johnson, R. P.
AU - Johnson, T. J.
AU - Johnson, W. N.
AU - Johnston, S.
AU - Kamae, T.
AU - Kanbach, G.
AU - Kaspi, V. M.
AU - Katagiri, H.
AU - Kataoka, J.
AU - Kavelaars, A.
AU - Kawai, N.
AU - Kelly, H.
AU - Kerr, M.
AU - Kiziltan, B.
AU - Klamra, W.
AU - Knödlseder, J.
AU - Kramer, M.
AU - Kuehn, F.
AU - Kuss, M.
AU - Lande, J.
AU - Landriu, D.
AU - Latronico, L.
AU - Lee, B.
AU - Lee, S. H.
AU - Lemoine-Goumard, M.
AU - Livingstone, M.
AU - Longo, F.
AU - Loparco, F.
AU - Lott, B.
AU - Lovellette, M. N.
AU - Lubrano, P.
AU - Lyne, A. G.
AU - Madejski, G. M.
AU - Makeev, A.
AU - Manchester, R. N.
AU - Marangelli, B.
AU - Marelli, M.
AU - Mazziotta, M. N.
AU - McEnery, J. E.
AU - McGlynn, S.
AU - McLaughlin, M. A.
AU - Menon, N.
AU - Meurer, C.
AU - Michelson, P. F.
AU - Mineo, T.
AU - Mirizzi, N.
AU - Mitthumsiri, W.
AU - Mizuno, T.
AU - Moiseev, A. A.
AU - Mongelli, M.
AU - Monte, C.
AU - Monzani, M. E.
AU - Moretti, E.
AU - Morselli, A.
AU - Moskalenko, I. V.
AU - Murgia, S.
AU - Nakamori, T.
AU - Nolan, P. L.
AU - Noutsos, A.
AU - Nuss, E.
AU - Ohsugi, T.
AU - Omodei, N.
AU - Orlando, E.
AU - Ormes, J. F.
AU - Ozaki, M.
AU - Paccagnella, A.
AU - Paneque, D.
AU - Panetta, J. H.
AU - Parent, D.
AU - Pearce, M.
AU - Pepe, M.
AU - Perchiazzi, M.
AU - Pesce-Rollins, M.
AU - Pieri, L.
AU - Pinchera, M.
AU - Piron, F.
AU - Porter, T. A.
AU - Rainò, S.
AU - Rando, R.
AU - Ransom, S. M.
AU - Rapposelli, E.
AU - Razzano, M.
AU - Reimer, A.
AU - Reimer, O.
AU - Reposeur, T.
AU - Reyes, L. C.
AU - Ritz, S.
AU - Rochester, L. S.
AU - Rodriguez, A. Y.
AU - Romani, R. W.
AU - Roth, M.
AU - Ryde, F.
AU - Sacchetti, A.
AU - Sadrozinski, H. F.W.
AU - Saggini, N.
AU - Sanchez, D.
AU - Sander, A.
AU - Parkinson, P. M.Saz
AU - Segal, K. N.
AU - Sellerholm, A.
AU - Sgrò, C.
AU - Siskind, E. J.
AU - Smith, D. A.
AU - Smith, P. D.
AU - Spandre, G.
AU - Spinelli, P.
AU - Stamatikos, M.
AU - Starck, J. L.
AU - Stecker, F. W.
AU - Stephens, T. E.
AU - Strickman, M. S.
AU - Strong, A. W.
AU - Suson, D. J.
AU - Tajima, H.
AU - Takahashi, H.
AU - Takahashi, T.
AU - Tanaka, T.
AU - Tenze, A.
AU - Thayer, J. B.
AU - Thayer, J. G.
AU - Theureau, G.
AU - Thompson, D. J.
AU - Thorsett, S. E.
AU - Tibaldo, L.
AU - Tibolla, O.
AU - Torres, D. F.
AU - Tramacere, A.
AU - Turri, M.
AU - Usher, T. L.
AU - Vigiani, L.
AU - Vilchez, N.
AU - Vitale, V.
AU - Waite, A. P.
AU - Wang, P.
AU - Watters, K.
AU - Weltevrede, P.
AU - Winer, B. L.
AU - Wood, K. S.
AU - Ylinen, T.
AU - Ziegler, M.
N1 - Copyright: Copyright 2015 Elsevier B.V., All rights reserved.
PY - 2009/5/10
Y1 - 2009/5/10
N2 - The Vela pulsar is the brightest persistent source in the GeV sky and thus is the traditional first target for new γ-ray observatories. We report here on initial Fermi Large Area Telescope observations during verification phase pointed exposure and early sky survey scanning. We have used the Vela signal to verify Fermi timing and angular resolution. The high-quality pulse profile, with some 32,400 pulsed photons at E ≥ 0.03GeV, shows new features, including pulse structure as fine as 0.3ms and a distinct third peak, which shifts in phase with energy. We examine the high-energy behavior of the pulsed emission; initial spectra suggest a phase-averaged power-law index of Γ = 1.51+0.05 -0.04 with an exponential cutoff at E c = 2.9 ± 0.1 GeV. Spectral fits with generalized cutoffs of the form require b ≤ 1, which is inconsistent with magnetic pair attenuation, and thus favor outer-magnetosphere emission models. Finally, we report on upper limits to any unpulsed component, as might be associated with a surrounding pulsar wind nebula.
AB - The Vela pulsar is the brightest persistent source in the GeV sky and thus is the traditional first target for new γ-ray observatories. We report here on initial Fermi Large Area Telescope observations during verification phase pointed exposure and early sky survey scanning. We have used the Vela signal to verify Fermi timing and angular resolution. The high-quality pulse profile, with some 32,400 pulsed photons at E ≥ 0.03GeV, shows new features, including pulse structure as fine as 0.3ms and a distinct third peak, which shifts in phase with energy. We examine the high-energy behavior of the pulsed emission; initial spectra suggest a phase-averaged power-law index of Γ = 1.51+0.05 -0.04 with an exponential cutoff at E c = 2.9 ± 0.1 GeV. Spectral fits with generalized cutoffs of the form require b ≤ 1, which is inconsistent with magnetic pair attenuation, and thus favor outer-magnetosphere emission models. Finally, we report on upper limits to any unpulsed component, as might be associated with a surrounding pulsar wind nebula.
KW - gamma rays: observations
KW - pulsars: individual (PSR B0833-45)
UR - http://www.scopus.com/inward/record.url?scp=84863115445&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84863115445&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/696/2/1084
DO - 10.1088/0004-637X/696/2/1084
M3 - Article
AN - SCOPUS:84863115445
VL - 696
SP - 1084
EP - 1093
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
ER -