2010ApJ...719L..69A

Query : 2010ApJ...719L..69A

2010ApJ...719L..69A - Astrophys. J., 719, L69-L73 (2010/August-2)

Discovery of very high energy γ-ray emission from the SNR G54.1+0.3.

ACCIARI V.A., ALIU E., ARLEN T., AUNE T., BAUTISTA M., BEILICKE M., BENBOW W., BOLTUCH D., BRADBURY S.M., BUCKLEY J.H., BUGAEV V., BUTT Y., BYRUM K., CESARINI A., CIUPIK L., CUI W., DICKHERBER R., DUKE C., FINLEY J.P., FINNEGAN G., FORTSON L., FURNISS A., GALANTE N., GALL D., GILLANDERS G.H., GODAMBE S., GOTTHELF E.V., GRUBE J., GUENETTE R., GYUK G., HANNA D., HOLDER J., HUI C.M., HUMENSKY T.B., IMRAN A., KAARET P., KARLSSON N., KERTZMAN M., KIEDA D., KONOPELKO A., KRAWCZYNSKI H., KRENNRICH F., LANG M.J., LEBOHEC S., MAIER G., McARTHUR S., McCANN A., McCUTCHEON M., MORIARTY P., MUHKERJEE R., ONG R.A., OTTE A.N., PANDEL D., PERKINS J.S., POHL M., QUINN J., RAGAN K., REYES L.C., REYNOLDS P.T., ROACHE E., ROSE H.J., SCHROEDTER M., SEMBROSKI G.H., SENTURK G.D., SLANE P., SMITH A.W., STEELE D., SWORDY S.P., TESIC G., THEILING M., THIBADEAU S., VASSILIEV V.V., VINCENT S., WAKELY S.P., WARD J.E., WEEKES T.C., WEINSTEIN A., WEISGARBER T., WILLIAMS D.A., WISSEL S., WOOD M. and ZITZER B.

Abstract (from CDS):

We report the discovery of very high energy (VHE) gamma-ray emission from the direction of the SNR G54.1+0.3 using the VERITAS ground-based gamma-ray observatory. The TeV signal has an overall significance of 6.8σ and appears pointlike given the resolution of the instrument. The integral flux above 1 TeV is 2.5% of the Crab Nebula flux and significant emission is measured between 250 GeV and 4 TeV, well described by a power-law energy spectrum dN/dE ∼ E –Γ with a photon index Γ = 2.39±0.23stat± 0.30sys. We find no evidence of time variability among observations spanning almost two years. Based on the location, the morphology, the measured spectrum, the lack of variability, and a comparison with similar systems previously detected in the TeV band, the most likely counterpart of this new VHE gamma-ray source is the pulsar wind nebula (PWN) in the SNR G54.1+0.3. The measured X-ray to VHE gamma-ray luminosity ratio is the lowest among all the nebulae supposedly driven by young rotation-powered pulsars, which could indicate a particle-dominated PWN.

Abstract Copyright: ∼

Journal keyword(s): gamma rays: general - ISM: supernova remnants - pulsars: individual (J1930+1852, J1928+1746)

Simbad objects: 16

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Number of rows : 16
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
2 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5476 0
3 NAME Vela X Psr 08 33 08.880 -45 11 24.36           ~ 302 1
4 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2446 1
5 SNR G000.9+00.1 SNR 17 47.3 -28 09           ~ 222 1
6 NAME AGPS 273.4-17.8 SNR 18 13 35.05 -17 49 58.1           ~ 145 2
7 PSR B1823-13 Psr 18 26 13.06 -13 34 48.1           ~ 460 1
8 SNR G021.5-00.9 SNR 18 33 33.612 -10 34 07.69           ~ 490 1
9 AX J1844.8-0258 HXB 18 44 53 -02 56.0           ~ 126 0
10 SNR G029.7-00.3 SNR 18 46 22.8 -02 59 47           ~ 375 2
11 3EG J1928+1746 gam 19 28.0 +17 46           ~ 2 0
12 PSR J1928+1746 Psr 19 28 42.8 +17 46 27           ~ 62 0
13 SNR G054.1+00.3 SNR 19 30 10.6 +18 50 22           ~ 271 1
14 PSR J1930+1852 Psr 19 30 30.13 +18 52 14.1           ~ 110 1
15 SNR G106.3+02.7 SNR 22 27.5 +60 50           ~ 99 1
16 PSR J2229+6114 Psr 22 29 05.262 +61 14 08.48           ~ 252 2

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