A Search for TeV Gamma-Ray Emission from Pulsar Tails by VERITAS
/ Authors
W. Benbow, A. Brill, J. Buckley, M. Capasso, A. Chromey, M. Errando, A. Falcone, K. A. Farrell, Q. Feng, J. Finley
and 49 more authors
G. Foote, L. Fortson, A. Furniss, A. Gent, C. Giuri, D. Hanna, T. Hassan, O. Hervet, J. Holder, G. Hughes, T. Humensky, Weidong Jin, P. Kaaret, O. Kargaltsev, M. Kertzman, D. Kieda, N. Klingler, Sajan Kumar, M. Lang, M. Lundy, G. Maier, C. McGrath, P. Moriarty, R. Mukherjee, D. Nieto, M. Nievas-Rosillo, S. O’Brien, R. Ong, A. Otte, S. Patel, K. Pfrang, M. Pohl, R. Prado, J. Quinn, K. Ragan, P., T. Reynolds, D. Ribeiro, G. Richards, E. Roache, J. Ryan, M. Santander, G. Sembroski, R. Shang, I. Volkov, S. Wakely, A. Weinstein, P. Wilcox, D. Williams
/ Abstract
We report on the search for very-high-energy gamma-ray emission from the regions around three nearby supersonic pulsars (PSR B0355+54, PSR J0357+3205, and PSR J1740+1000) that exhibit long X-ray tails. To date there is no clear detection of TeV emission from any pulsar tail that is prominent in X-ray or radio. We provide upper limits on the TeV flux, and luminosity, and also compare these limits with other pulsar wind nebulae detected in X-rays and the tail emission model predictions. We find that at least one of the three tails is likely to be detected in observations that are a factor of 2–3 more sensitive. The analysis presented here also has implications for deriving the properties of pulsar tails, for those pulsars whose tails could be detected in TeV.
Journal: The Astrophysical Journal