2025A&A...693A.255A

Query : 2025A&A...693A.255A

2025A&A...693A.255A - Astronomy and Astrophysics, volume 693A255 (2025/1-1)

Cosmic-ray acceleration and escape from supernova remnant W44 as probed by Fermi-LAT and MAGIC.

ABE S., ABHIR J., ABHISHEK A., ACCIARI V.A., AGUASCA-CABOT A., AGUDO I., ANIELLO T., ANSOLDI S., ANTONELLI L.A., ARBET ENGELS A., ARCARO C., ASANO K., BABIC A., BAQUERO A., BARRES DE ALMEIDA U., BARRIO J.A., BATKOVIC I., BAUTISTA A., BAXTER J., BECERRA GONZALEZ J., BEDNAREK W., BERNARDINI E., BERNETE J., BERTI A., BESENRIEDER J., BIGONGIARI C., BILAND A., BLANCH O., BONNOLI G., BOSNJAK Z., BRONZINI E., BURELLI I., BUSETTO G., CAMPOY-ORDAZ A., CAROSI A., CAROSI R., CARRETERO-CASTRILLO M., CASTRO-TIRADO A.J., CERASOLE D., CERIBELLA G., CHAI Y., CHILINGARIAN A., CIFUENTES A., COLOMBO E., CONTRERAS J.L., CORTINA J., COVINO S., D'AMICO G., D'ELIA V., DA VELA P., DAZZI F., DE ANGELIS A., DE LOTTO B., DE MENEZES R., DEL POPOLO A., DELFINO M., DELGADO J., DELGADO MENDEZ C., DI PIERRO F., DOMINIS PRESTER D., DONINI A., DORNER D., DORO M., ELSAESSER D., EMERY G., ESCUDERO J., FARINA L., FATTORINI A., FOFFANO L., FONT L., FROSE S., FUKAZAWA Y., GARCIA LOPEZ R.J., GARCZARCZYK M., GASPARYAN S., GAUG M., GIESBRECHT PAIVA J.G., GIGLIETTO N., GLIWNY P., GODINOVIC N., GOZZINI S.R., GRADETZKE T., GRAU R., GREEN J.G., GUNTHER P., HADASCH D., HAHN A., HASSAN T., HECKMANN L., HERRERA J., HRUPEC D., HUTTEN M., IMAZAWA R., ISHIO K., JIMENEZ MARTINEZ I., JORMANAINEN J., KAYANOKI T., KERSZBERG D., KLUGE G.W., KOBAYASHI Y., KOUCH P.M., KUBO H., KUSHIDA J., LAINEZ M., LAMASTRA A., LEONE F., LINDFORS E., LINHOFF L., LOMBARDI S., LONGO F., LOPEZ-COTO R., LOPEZ-MOYA M., LOPEZ-ORAMAS A., LOPORCHIO S., LORINI A., LYARD E., MACHADO DE OLIVEIRA FRAGA B., MAJUMDAR P., MAKARIEV M., MANEVA G., MANG N., MANGANARO M., MANGANO S., MANNHEIM K., MARIOTTI M., MARTINEZ M., MARTINEZ-CHICHARRO M., MAS-AGUILAR A., MAZIN D., MENCHIARI S., MENDER S., MICELI D., MIENER T., MIRANDA J.M., MIRZOYAN R., MOLERO GONZALEZ M., MOLINA E., MONDAL H.A., MORALEJO A., MORCUENDE D., NAKAMORI T., NANCI C., NAVA L., NEUSTROEV V., NICKEL L., NIEVAS ROSILLO M., NIGRO C., NIKOLIC L., NISHIJIMA K., NJOH EKOUME T., NODA K., NOZAKI S., OHTANI Y., OKUMURA A., OTERO-SANTOS J., PAIANO S., PALATIELLO M., PANEQUE D., PAOLETTI R., PAREDES J.M., PERESANO M., PERSIC M., PIHET M., PIROLA G., PODOBNIK F., PRADA MORONI P.G., PRANDINI E., PRINCIPE G., PRIYADARSHI C., RHODE W., RIBO M., RICO J., RIGHI C., SAHAKYAN N., SAITO T., SATALECKA K., SATURNI F.G., SCHLEICHER B., SCHMIDT K., SCHMUCKERMAIER F., SCHUBERT J.L., SCHWEIZER T., SCIACCALUGA A., SILVESTRI G., SITAREK J., SLIUSAR V., SOBCZYNSKA D., SPOLON A., STAMERRA A., STRISKOVIC J., STROM D., STRZYS M., SUDA Y., SUUTARINEN S., TAJIMA H., TAKAHASHI M., TAKEISHI R., TEMNIKOV P., TERAUCHI K., TERZIC T., TESHIMA M., TRUZZI S., TUTONE A., UBACH S., VAN SCHERPENBERG J., VAZQUEZ ACOSTA M., VENTURA S., VIALE I., VIGORITO C.F., VITALE V., VOVK I., WALTER R., WILL M., WUNDERLICH C., YAMAMOTO T., DI TRIA R., DI VENERE L., GIORDANO F., BISSALDI E., GREEN D. and MORLINO G.

Abstract (from CDS):

Context. The supernova remnant (SNR) W44 and its surroundings are a prime target for studying the acceleration of cosmic rays (CRs). Several previous studies established an extended gamma-ray emission that is set apart from the radio shell of W44. This emission is thought to originate from escaped high-energy CRs that interact with a surrounding dense molecular cloud complex.
Aims. We present a detailed analysis of Fermi-LAT data with an emphasis on the spatial and spectral properties of W44 and its surroundings. We also report the results of the observations performed with the MAGIC telescopes of the northwestern region of W44. Finally, we present an interpretation model to explain the gamma-ray emission of the SNR and its surroundings.
Methods. We first performed a detailed spatial analysis of 12 years of Fermi-LAT data at energies above 1 GeV, in order to exploit the better angular resolution, while we set a threshold of 100 MeV for the spectral analysis. We performed a likelihood analysis of 174 hours of MAGIC data above 130 GeV using the spatial information obtained with Fermi-LAT.
Results. The combined spectra of Fermi-LAT and MAGIC, extending from 100 MeV to several TeV, were used to derive constraints on the escape of CRs. Using a time-dependent model to describe the particle acceleration and escape from the SNR, we show that the maximum energy of the accelerated particles has to be ≃40 GeV. However, our gamma-ray data suggest that a small number of lower-energy particles also needs to escape. We propose a novel model, the broken-shock scenario, to account for this effect and explain the gamma-ray emission.

Abstract Copyright: © The Authors 2025

Journal keyword(s): acceleration of particles - diffusion - cosmic rays - ISM: supernova remnants - gamma rays: general

Simbad objects: 19

Full paper

View the references in ADS

Number of rows : 19

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	SNR G006.4-00.1	SNR	18 00 31.2011719	-23 25 48.001099						~	782	1
2	SNR G033.6+00.1	SNR	18 52 29.000	+00 38 42.00						~	302	2
3	4FGL J1854.7+0153	gam	18 54 46.8	+01 53 37						~	7	0
4	4FGL J1855.8+0150	gam	18 55 49.8	+01 50 36						~	9	0
5	SNR G034.6-00.5	SNR	18 56 10.650	+01 13 21.30						~	1034	2
6	4FGL J1856.7+0125c	gam	18 56 42.6	+01 25 39						~	4	0
7	4FGL J1857.7+0246e	Psr	18 57 11.0	+02 40 00						~	59	0
8	2FGL J1857.2+0055c	gam	18 57 11.7	+00 56 46						~	17	0
9	MAGIC J1857+026	Psr	18 57.2	+02 38						~	9	0
10	4FGL J1857.4+0106	gam	18 57 25.9	+01 06 46						~	6	0
11	MAGIC J1857+029	gam	18 57.6	+02 58						~	11	0
12	EGR J1856+0235	gam	18 57 37.16	+02 12 33.6						~	32	0
13	PSR J1857+0143	Psr	18 58 15.46	+01 36 55.4						~	44	0
14	4FGL J1858.3+0209	gam	18 58 18.4	+02 09 10						~	10	0
15	HESS J1858+020	gam	18 58 20.0	+02 05 24						~	45	0
16	3FGL J1859.6+0102	gam	18 59 19.8	+00 58 48						~	10	0
17	* gam Cyg	V*	20 22 13.7018357	+40 15 24.044963	3.44	2.90	2.23	1.74	1.40	F8Ib	607	0
18	NAME Cyg Loop	SNR	20 51.0	+30 40						~	964	0
19	GrW 151226	GWE	~	~						~	275	1

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