2013ApJ...764...38A

Query : 2013ApJ...764...38A

2013ApJ...764...38A - Astrophys. J., 764, 38 (2013/February-2)

Discovery of TeV gamma-ray emission from CTA 1 by VERITAS.

ALIU E., ARCHAMBAULT S., ARLEN T., AUNE T., BEILICKE M., BENBOW W., BOUVIER A., BUCKLEY J.H., BUGAEV V., CESARINI A., CIUPIK L., COLLINS-HUGHES E., CONNOLLY M.P., CUI W., DICKHERBER R., DUKE C., DUMM J., DWARKADAS V.V., ERRANDO M., FALCONE A., FEDERICI S., FENG Q., FINLEY J.P., FINNEGAN G., FORTSON L., FURNISS A., GALANTE N., GALL D., GILLANDERS G.H., GODAMBE S., GOTTHELF E.V., GRIFFIN S., GRUBE J., GYUK G., HANNA D., HOLDER J., HUGHES G., HUMENSKY T.B., KAARET P., KARGALTSEV O., KARLSSON N., KHASSEN Y., KIEDA D., KRAWCZYNSKI H., KRENNRICH F., LANG M.J., LEE K., MADHAVAN A.S., MAIER G., MAJUMDAR P., McARTHUR S., McCANN A., MORIARTY P., MUKHERJEE R., NELSON T., O'FAOLAIN DE BHROITHE A., ONG R.A., ORR M., OTTE A.N., PARK N., PERKINS J.S., POHL M., PROKOPH H., QUINN J., RAGAN K., REYES L.C., REYNOLDS P.T., ROACHE E., ROBERTS M., SAXON D.B., SCHROEDTER M., SEMBROSKI G.H., SLANE P., SMITH A.W., STASZAK D., TELEZHINSKY I., TESIC G., THEILING M., THIBADEAU S., TSURUSAKI K., TYLER J., VARLOTTA A., VASSILIEV V.V., VINCENT S., VIVIER M., WAKELY S.P., WEEKES T.C., WEINSTEIN A., WELSING R., WILLIAMS D.A. and ZITZER B.

Abstract (from CDS):

We report the discovery of TeV gamma-ray emission coincident with the shell-type radio supernova remnant (SNR) CTA 1 using the VERITAS gamma-ray observatory. The source, VER J0006+729, was detected as a 6.5 standard deviation excess over background and shows an extended morphology, approximated by a two-dimensional Gaussian of semimajor (semiminor) axis 0.°30 (0.°24) and a centroid 5' from the Fermi gamma-ray pulsar PSR J0007+7303 and its X-ray pulsar wind nebula (PWN). The photon spectrum is well described by a power-law dN/dE = N0(E/3 TeV)–Γ, with a differential spectral index of Γ = 2.2±0.2stat± 0.3sys, and normalization N0= (9.1±1.3stat ±1.7sys)x10–14/cm2/s.TeV–1. The integral flux, Fγ = 4.0x10–12 erg/cm2/s above 1 TeV, corresponds to 0.2% of the pulsar spin-down power at 1.4 kpc. The energetics, colocation with the SNR, and the relatively small extent of the TeV emission strongly argue for the PWN origin of the TeV photons. We consider the origin of the TeV emission in CTA 1.

Abstract Copyright: ∼

Journal keyword(s): gamma-rays: stars - pulsars: individual: PSR J0007+7303 - supernovae: individual: G119.5+10.2 - X-rays: individual: RX J0007.0+7303

Simbad objects: 12

goto Full paper

goto View the references in ADS

Number of rows : 12
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 VER J0006+729 gam 00 06 26.00 +72 59 01.0           ~ 3 0
2 SNR G119.5+10.2 SNR 00 06.6 +72 47           ~ 268 1
3 PSR J0007+7303 Psr 00 07 00.6000137 +73 03 06.849976           ~ 183 1
4 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
5 PSR J0633+1746 Psr 06 33 54.153 +17 46 12.91           ~ 1308 0
6 NAME Vela X Psr 08 33 08.880 -45 11 24.36           ~ 302 1
7 NAME Vela SNR 08 34.0 -45 50           ~ 1331 2
8 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2446 1
9 SNR G327.1-01.1 SNR 15 54 32.3 -55 03 44           ~ 112 1
10 HESS J1809-193 gam 18 10 31 -19 18.0           ~ 70 1
11 PSR B1823-13 Psr 18 26 13.06 -13 34 48.1           ~ 460 1
12 PSR J1836+5925 Psr 18 36 13.661 +59 25 29.77           ~ 153 0

To bookmark this query, right click on this link: simbad:objects in 2013ApJ...764...38A and select 'bookmark this link' or equivalent in the popup menu