2011ApJ...740...78M

Query : 2011ApJ...740...78M

2011ApJ...740...78M - Astrophys. J., 740, 78 (2011/October-3)

CANGAROO-III observation of TeV gamma rays from the unidentified gamma-ray source HESS J1614-518.

MIZUKAMI T., KUBO H., YOSHIDA T., NAKAMORI T., ENOMOTO R., TANIMORI T., AKIMOTO M., BICKNELL G.V., CLAY R.W., EDWARDS P.G., GUNJI S., HARA S., HARA T., HAYASHI S., ISHIOKA H., KABUKI S., KAJINO F., KATAGIRI H., KAWACHI A., KIFUNE T., KIUCHI R., KUNISAWA T., KUSHIDA J., MATOBA T., MATSUBARA Y., MATSUZAWA I., MIZUMURA Y., MIZUMOTO Y., MORI M., MURAISHI H., NAITO T., NAKAYAMA K., NISHIJIMA K., OHISHI M., OTAKE Y., RYOKI S., SAITO K., SAKAMOTO Y., STAMATESCU V., SUZUKI T., SWABY D.L., THORNTON G., TOKANAI F., TOYOTA Y., TSUCHIYA K., YANAGITA S., YOKOE Y., YOSHIKOSHI T. and YUKAWA Y.

Abstract (from CDS):

We report the detection, with the CANGAROO-III imaging atmospheric Cherenkov telescope array, of a very high energy gamma-ray signal from the unidentified gamma-ray source HESS J1614-518, which was discovered in the H.E.S.S. Galactic plane survey. Diffuse gamma-ray emission was detected above 760 GeV at the 8.9σ level during an effective exposure of 54 hr from 2008 May to August. The spectrum can be represented by a power law: (8.2±2.2stat± 2.5sys) x10–12x(E/1 TeV)–γ/cm2/s/TeV with a photon index γ of 2.4±0.3stat± 0.2sys, which is compatible with that of the H.E.S.S. observations. By combining our result with multiwavelength data, we discuss the possible counterparts for HESS J1614-518 and consider radiation mechanisms based on hadronic and leptonic processes for a supernova remnant (SNR), stellar winds from massive stars, and a pulsar wind nebula (PWN). Although a leptonic origin from a PWN driven by an unknown pulsar remains possible, hadronic-origin emission from an unknown SNR is preferred.

Abstract Copyright: ∼

Journal keyword(s): gamma rays: ISM - ISM: individual: HESS J1614-518

Simbad objects: 25

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Number of rows : 25
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 LS I +61 303 HXB 02 40 31.6644419688 +61 13 45.593918580 11.27 11.61 10.75 10.19 9.55 B0Ve 903 2
2 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
3 PSR J0633+1746 Psr 06 33 54.153 +17 46 12.91           ~ 1308 0
4 NAME Vela X Psr 08 33 08.880 -45 11 24.36           ~ 302 1
5 NAME Vela Jr SN SNR 08 52.0 -46 20           ~ 507 2
6 Cl Westerlund 2 OpC 10 23 58.1 -57 45 49           ~ 400 0
7 CPD-63 2495 HXB 13 02 47.6544015048 -63 50 08.626970292 10.34 10.72 9.98 10.03   O9.5Ve 852 0
8 ESO 134-11 HII 14 40 29 -62 38.7           ~ 585 1
9 PSR B1607-52 Psr 16 11 03.20 -52 09 23.6           ~ 48 0
10 PSR J1612-5136 Psr 16 12 00.6 -51 36 54           ~ 3 0
11 PSR J1613-5211 Psr 16 13 42.46 -52 11 21.0           ~ 7 0
12 Cl Pismis 22 OpC 16 14 12.5 -51 52 08           ~ 31 0
13 PSR J1614-5144 Psr 16 14 45.7 -51 44 49           ~ 3 0
14 PSR J1615-5137 Psr 16 15 12.62 -51 34 53.3           ~ 67 0
15 PSR J1616-5208 Psr 16 16 23.4 -52 08 48           ~ 4 0
16 SNR G338.3-00.0 SNR 16 40 43.2 -46 31 48           ~ 175 2
17 Cl Westerlund 1 OpC 16 47 02.4 -45 51 07           ~ 655 1
18 SNR G347.3-00.5 SNR 17 12 27 -39 41.2     12.27     ~ 761 1
19 1AGLR J1807-2103 gam 18 03 52.1 -21 10 54           ~ 79 0
20 PSR B1823-13 Psr 18 26 13.06 -13 34 48.1           ~ 460 1
21 SNR G027.3+00.0 SNR 18 41 17.8 -04 56 12           ~ 345 3
22 PSR J1841-0456 Psr 18 41 19.29 -04 56 11.4           ~ 296 1
23 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 1023 0
24 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 673 1
25 SNR G109.1-01.0 SNR 23 01 35 +58 53.0           ~ 362 0

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