2025ApJ...992...22A

Query : 2025ApJ...992...22A

2025ApJ...992...22A - Astrophys. J., 992, 22 (2025/October-2)

Study of the IC 443 Region with the HAWC Observatory.

ALFARO R., ALVAREZ C., ARAYA M., ARTEAGA-VELAZQUEZ J.C., AVILA ROJAS D., AYALA SOLARES H.A., BABU R., BANGALE P., BERNAL A., CABALLERO-MORA K.S., CAPISTRAN T., CARRAMINANA A., CASANOVA S., COTTI U., COTZOMI J., COUTINO DE LEON S., DE LA FUENTE E., DEPAOLI D., DESIATI P., DI LALLA N., DIAZ HERNANDEZ R., DINGUS B.L., DUVERNOIS M.A., DIAZ-VELEZ J.C., ERGIN T., ESPINOZA C., FANG K., FRAIJA N., FRAIJA S., GARCIA-GONZALEZ J.A., GOKSU H., GONZALEZ-CERVERA J.A., GONZALEZ M.M., GOODMAN J.A., GROETSCH S., HARDING J.P., HERNANDEZ-CADENA S., HERZOG I., HINTON J., HUANG D., HUEYOTL-ZAHUANTITLA F., HUNTEMEYER P., KAUFMANN S., LARA A., LEE J., LEON VARGAS H., LINNEMANN J.T., LONGINOTTI A.L., LUIS-RAYA G., MALONE K., MARTINEZ O., MARTINEZ-CASTRO J., MATTHEWS J.A., MIRANDA-ROMAGNOLI P., MONTES J.A., MORALES-SOTO J.A., MORENO E., MOSTAFA M., NAJAFI M., NELLEN L., NISA M.U., NORIEGA-PAPAQUI R., OLIVERA-NIETO L., OMODEI N., OSORIO M., PONCE E., PEREZ ARAUJO Y., PEREZ-PEREZ E.G., RHO C.D., ROSA-GONZALEZ D., ROTH M., RUIZ-VELASCO E., SALAZAR H., SANDOVAL A., SCHNEIDER M., SCHWEFER G., SERNA-FRANCO J., SMITH A.J., SON Y., SPRINGER R.W., TIBOLLA O., TOLLEFSON K., TORRES I., TORRES-ESCOBEDO R., TURNER R., WANG X., WANG Z., WATSON I.J., WU H., YU S., YUN-CARCAMO S., ZHOU H., DE LEON C. (The HAWC Collaboration)

Abstract (from CDS):

Supernova remnants are one potential source class considered a PeVatron (i.e., capable of accelerating cosmic rays above PeV energies). The shock fronts produced after the explosion of the supernova are ideal regions for particle acceleration. IC 443 is a supernova remnant that has been studied extensively at different wavelengths. Using 2966 days of gamma-ray data from the High Altitude Water Cherenkov (HAWC) observatory, we study the emission of IC 443 with the objective of finding signatures of cosmic-ray acceleration at the PeV scale. Using a maximum likelihood method, we find a point source located at (α = 94$\mathop{.}\limits^{\unicode{x000b0}}$42, δ = 22$\mathop{.}\limits^{\unicode{x000b0}}$35) that we associate with IC 443. The measured spectrum is a simple power law with an index of -3.14 ± 0.18, which is consistent with previous TeV observations. Although we cannot confirm that IC 443 is a hadronic PeVatron, we do not find any sign that the spectrum has a cutoff at tens of TeV energies, with the spectrum extending to ∼30 TeV. Furthermore, we also find a new extended component in the region whose emission is described by a simple power law with an index of -2.49 ± 0.08 and which we call HAWC J0615+2213. While we show evidence that this new source might be a new TeV halo, we defer a detailed analysis of this new source to another publication.

Abstract Copyright: © 2025. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): High energy astrophysics - Gamma-rays - Supernova remnants

Simbad objects: 6

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Number of rows : 6
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 PSR B0611+22 Psr 06 14 17.0324288405 +22 29 57.017874999           ~ 285 0
2 HAWC J0615+221 gam 06 14.7 +22 13           ~ 1 0
3 IC 443 SNR 06 17 00.0000000 +22 34 11.998901           ~ 1314 1
4 2XMM J061705.2+222129 XB* 06 17 05.26 +22 21 29.4           ~ 55 1
5 FGES J0619.6+2229 gam 06 18 37 +22 29.0           ~ 1 0
6 SNR G189.6+03.3 SNR 06 19 +22.2           ~ 37 0

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