Observation of TeV gamma rays from the Crab Nebula with Milagro using a new background rejection technique

被引：161

作者：

Atkins, R

Benbow, W

Berley, D

Blaufuss, E

Bussons, J

Coyne, DG

Delay, RS

DeYoung, T

Dingus, BL

Dorfan, DE

Ellsworth, RW

Falcone, A

Fleysher, L

Fleysher, R

Gisler, G

Gonzalez, MM

Goodman, JA

Haines, TJ

Hays, E

Hoffman, CM

Kelley, LA

Laird, RW

McCullough, J

McEnery, JE

Miller, RS

Mincer, AI

Morales, MF

Nemethy, P

Noyes, D

Ryan, JM

Samuelson, FW

Schneider, M

Shen, B

Shoup, A

Sinnis, G

Smith, AJ

Sullivan, GW

Tumer, OT

Wang, K

Wascko, M

Williams, DA

Westerhoff, S

Wilson, ME

Xu, X

Yodh, GB

机构：

[1] Los Alamos Natl Lab, Los Alamos, NM 87545 USA

[2] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA

[3] Univ Maryland, College Pk, MD 20742 USA

[4] Univ Calif Irvine, Irvine, CA 92717 USA

[5] George Mason Univ, Fairfax, VA 22030 USA

[6] Univ New Hampshire, Durham, NH 03824 USA

[7] NYU, New York, NY 10003 USA

[8] Univ Calif Riverside, Riverside, CA 92521 USA

[9] Univ Wisconsin, Madison, WI 53706 USA

来源：

ASTROPHYSICAL JOURNAL | 2003年 / 595卷 / 02期

关键词：

gamma rays : observations; instrumentation : detectors; ISM : individual (Crab Nebula); stars : neutron; supernova remnants;

D O I：

10.1086/377498

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The recent advances in TeV gamma-ray astronomy are largely the result of the ability to differentiate between extensive air showers generated by gamma rays and hadronic cosmic rays. Air Cerenkov telescopes have developed and perfected the "imaging '' technique over the past several decades. However, until now no background rejection method has been successfully used in an air shower array to detect a source of TeV gamma rays. We report on a method to differentiate hadronic air showers from electromagnetic air showers in the Milagro gamma-ray observatory, based on the ability to detect the energetic particles in an extensive air shower. The technique is used to detect TeV emission from the Crab Nebula. The flux from the Crab Nebula is estimated to be 2.68 (+/-0.42(stat) +/- 1.4(sys)) x 10(-7) (E/1 TeV)(-2.59) m(-2) s(-1) TeV-1, where the spectral index is assumed to be as given by the HEGRA collaboration.

引用

页码：803 / 811

页数：9

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