2017ApJ...843...39A

Query : 2017ApJ...843...39A

2017ApJ...843...39A - Astrophys. J., 843, 39-39 (2017/July-1)

Observation of the Crab Nebula with the HAWC gamma-ray Observatory.

ABEYSEKARA A.U., ALBERT A., ALFARO R., ALVAREZ C., ALVAREZ J.D., ARCEO R., ARTEAGA-VELAZQUEZ J.C., AYALA SOLARES H.A., BARBER A.S., BAUTISTA-ELIVAR N., BECERRIL A., BELMONT-MORENO E., BENZVI S.Y., BERLEY D., BRAUN J., BRISBOIS C., CABALLERO-MORA K.S., CAPISTRAN T., CARRAMINANA A., CASANOVA S., CASTILLO M., COTTI U., COTZOMI J., COUTINO DE LEON S., DE LA FUENTE E., DE LEON C., DEYOUNG T., DINGUS B.L., DUVERNOIS M.A., DIAZ-VELEZ J.C., ELLSWORTH R.W., FIORINO D.W., FRAIJA N., GARCIA-GONZALEZ J.A., GERHARDT M., GONZALEZ MUNOZ A., GONZALEZ M.M., GOODMAN J.A., HAMPEL-ARIAS Z., HARDING J.P., HERNANDEZ S., HERNANDEZ-ALMADA A., HINTON J., HUI C.M., HUNTEMEYER P., IRIARTE A., JARDIN-BLICQ A., JOSHI V., KAUFMANN S., KIEDA D., LARA A., LAUER R.J., LEE W.H., LENNARZ D., LEON VARGAS H., LINNEMANN J.T., LONGINOTTI A.L., LUIS RAYA G., LUNA-GARCIA R., LOPEZ-COTO R., MALONE K., MARINELLI S.S., MARTINEZ O., MARTINEZ-CASTELLANOS I., MARTINEZ-CASTRO J., MARTINEZ-HUERTA H., MATTHEWS J.A., MIRANDA-ROMAGNOLI P., MORENO E., MOSTAFA M., NELLEN L., NEWBOLD M., NISA M.U., NORIEGA-PAPAQUI R., PELAYO R., PRETZ J., PEREZ-PEREZ E.G., REN Z., RHO C.D., RIVIERE C., ROSA-GONZALEZ D., ROSENBERG M., RUIZ-VELASCO E., SALAZAR H., SALESA GREUS F., SANDOVAL A., SCHNEIDER M., SCHOORLEMMER H., SINNIS G., SMITH A.J., SPRINGER R.W., SURAJBALI P., TABOADA I., TIBOLLA O., TOLLEFSON K., TORRES I., UKWATTA T.N., VILLASENOR L., WEISGARBER T., WESTERHOFF S., WISHER I.G., WOOD J., YAPICI T., YODH G.B., YOUNK P.W., ZEPEDA A. and ZHOU H.

Abstract (from CDS):

The Crab Nebula is the brightest TeV gamma-ray source in the sky and has been used for the past 25 years as a reference source in TeV astronomy, for calibration and verification of new TeV instruments. The High Altitude Water Cherenkov Observatory (HAWC), completed in early 2015, has been used to observe the Crab Nebula at high significance across nearly the full spectrum of energies to which HAWC is sensitive. HAWC is unique for its wide field of view, nearly 2 sr at any instant, and its high-energy reach, up to 100 TeV. HAWC's sensitivity improves with the gamma-ray energy. Above ∼1 TeV the sensitivity is driven by the best background rejection and angular resolution ever achieved for a wide-field ground array. We present a time-integrated analysis of the Crab using 507 live days of HAWC data from 2014 November to 2016 June. The spectrum of the Crab is fit to a function of the form φ(E)=φ0(E/E0)^-α-β⋅ln(E/E0). The data is well fitted with values of α = 2.63 ± 0.03, β = 0.15 ± 0.03, and log10(φ0 cm2 s TeV)=-12.60±0.02 when E0 is fixed at 7 TeV and the fit applies between 1 and 37 TeV. Study of the systematic errors in this HAWC measurement is discussed and estimated to be ±50% in the photon flux between 1 and 37 TeV. Confirmation of the Crab flux serves to establish the HAWC instrument's sensitivity for surveys of the sky. The HAWC all-sky survey will be the deepest survey of the northern sky ever conducted in the multi-TeV band.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): acceleration of particles - gamma rays: general - ISM: individual objects: Crab Nebula - ISM: individual objects: Crab Nebula

Simbad objects: 4

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Number of rows : 4
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 M 1 SNR 05 34 30.9 +22 00 53           ~ 6202 1
2 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5268 0
3 Mrk 421 BLL 11 04 27.3140835504 +38 12 31.798495872   13.50 12.90 8.31   ~ 2682 1
4 7C 165211.80+395026.00 BLL 16 53 52.21668403 +39 45 36.6088754 14.09 14.15 13.29 8.26   ~ 2170 2

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