2025ApJ...979...70C

Query : 2025ApJ...979...70C

2025ApJ...979...70C - Astrophys. J., 979, 70 (2025/January-3)

An Enigmatic PeVatron in an Area around H II Region G35.6-0.5.

CAO Z., AHARONIAN F., AXIKEGU, BAI Y.X., BAO Y.W., BASTIERI D., BI X.J., BI Y.J., BIAN W., BUKEVICH A.V., CAO Q., CAO W.Y., CAO Z., CHANG J., CHANG J.F., CHEN A.M., CHEN B.Q., CHEN E.S., CHEN H.X., CHEN L., CHEN L., CHEN L., CHEN M.J., CHEN M.L., CHEN Q.H., CHEN S., CHEN S.H., CHEN S.Z., CHEN T.L., CHEN Y., CHENG N., CHENG Y.D., CHU M.C., CUI M.Y., CUI S.W., CUI X.H., CUI Y.D., DAI B.Z., DAI H.L., DAI Z.G., DANZENGLUOBU, DONG X.Q., DUAN K.K., FAN J.H., FAN Y.Z., FANG J., FANG J.H., FANG K., FENG C.F., FENG H., FENG L., FENG S.H., FENG X.T., FENG Y., FENG Y.L., GABICI S., GAO B., GAO C.D., GAO Q., GAO W., GAO W.K., GE M.M., GE T.T., GENG L.S., GIACINTI G., GONG G.H., GOU Q.B., GU M.H., GUO F.L., GUO J., GUO X.L., GUO Y.Q., GUO Y.Y., HAN Y.A., HANNUKSELA O.A., HASAN M., HE H.H., HE H.N., HE J.Y., HE Y., HOR Y.K., HOU B.W., HOU C., HOU X., HU H.B., HU Q., HU S.C., HUANG C., HUANG D.H., HUANG T.Q., HUANG W.J., HUANG X.T., HUANG X.Y., HUANG Y., HUANG Y.Y., JI X.L., JIA H.Y., JIA K., JIANG H.B., JIANG K., JIANG X.W., JIANG Z.J., JIN M., KANG M.M., KARPIKOV I., KHANGULYAN D., KULESHOV D., KURINOV K., LI B.B., LI C.M., LI C., LI C., LI D., LI F., LI H.B., LI H.C., LI J., LI J., LI K., LI S.D., LI W.L., LI W.L., LI X.R., LI X., LI Y.Z., LI Z., LI Z., LIANG E.W., LIANG Y.F., LIN S.J., LIU B., LIU C., LIU D., LIU D.B., LIU H., LIU H.D., LIU J., LIU J.L., LIU M.Y., LIU R.Y., LIU S.M., LIU W., LIU Y., LIU Y.N., LUO Q., LUO Y., LV H.K., MA B.Q., MA L.L., MA X.H., MAO J.R., MIN Z., MITTHUMSIRI W., MU H.J., NAN Y.C., NERONOV A., NG K.C.Y., OU L.J., PATTARAKIJWANICH P., PEI Z.Y., QI J.C., QI M.Y., QIAO B.Q., QIN J.J., RAZA A., RUFFOLO D., SAIZ A., SAEED M., SEMIKOZ D., SHAO L., SHCHEGOLEV O., SHENG X.D., SHU F.W., SONG H.C., STENKIN Y.V., STEPANOV V., SU Y., SUN D.X., SUN Q.N., SUN X.N., SUN Z.B., TAKATA J., TAM P.H.T., TANG Q.W., TANG R., TANG Z.B., TIAN W.W., WAN L.H., WANG C., WANG C.B., WANG G.W., WANG H.G., WANG H.H., WANG J.C., WANG K., WANG K., WANG L.P., WANG L.Y., WANG P.H., WANG R., WANG W., WANG X.G., WANG X.Y., WANG Y., WANG Y.D., WANG Y.J., WANG Z.H., WANG Z.X., WANG Z., WANG Z., WEI D.M., WEI J.J., WEI Y.J., WEN T., WU C.Y., WU H.R., WU Q.W., WU S., WU X.F., WU Y.S., XI S.Q., XIA J., XIANG G.M., XIAO D.X., XIAO G., XIN Y.L., XING Y., XIONG D.R., XIONG Z., XU D.L., XU R.F., XU R.X., XU W.L., XUE L., YAN D.H., YAN J.Z., YAN T., YANG C.W., YANG C.Y., YANG F., YANG F.F., YANG L.L., YANG M.J., YANG R.Z., YANG W.X., YAO Y.H., YAO Z.G., YIN L.Q., YIN N., YOU X.H., YOU Z.Y., YU Y.H., YUAN Q., YUE H., ZENG H.D., ZENG T.X., ZENG W., ZHA M., ZHANG B.B., ZHANG F., ZHANG H., ZHANG H.M., ZHANG H.Y., ZHANG J.L., ZHANG L., ZHANG P.F., ZHANG P.P., ZHANG R., ZHANG S.B., ZHANG S.R., ZHANG S.S., ZHANG X., ZHANG X.P., ZHANG Y.F., ZHANG Y., ZHANG Y., ZHAO B., ZHAO J., ZHAO L., ZHAO L.Z., ZHAO S.P., ZHAO X.H., ZHENG F., ZHONG W.J., ZHOU B., ZHOU H., ZHOU J.N., ZHOU M., ZHOU P., ZHOU R., ZHOU X.X., ZHOU X.X., ZHU B.Y., ZHU C.G., ZHU F.R., ZHU H., ZHU K.J., ZOU Y.C., ZUO X. (The LHAASO Collaboration)

Abstract (from CDS):

Identifying Galactic PeVatrons (PeV particle accelerators) from ultrahigh-energy (UHE, >100 TeV) γ-ray sources plays a crucial role in revealing the origin of Galactic cosmic rays. The UHE source 1LHAASO J1857+0203u is suggested to be associated with HESS J1858+020, which may be attributed to the possible PeVatron candidate supernova remnant (SNR) G35.6-0.4 or H II region G35.6-0.5. We perform detailed analysis on the very-high-energy and UHE γ-ray emissions toward this region with data from the Large High Altitude Air Shower Observatory (LHAASO). 1LHAASO J1857+0203u is detected with a significance of 11.6σ above 100 TeV, indicating the presence of a PeVatron. It has an extent of ∼0$\mathop{.}\limits^{\unicode{x000B0}}$18 with a power-law (PL) spectral index of ∼2.5 at 1-25 TeV and pointlike emission with a PL spectral index of ∼3.2 above 25 TeV. Using archival CO and H I data, we identify some molecular and atomic clouds that may be associated with the TeV γ-ray emissions. Our modeling indicates that the TeV γ-ray emissions are unlikely to arise from clouds illuminated by the protons that escaped from SNR G35.6-0.4. In the scenario in which H II region G35.6-0.5 could accelerate particles to the UHE band, the observed GeV-TeV γ-ray emission could be well explained by a hadronic model with a PL spectral index of ∼2.0 and cutoff energy of ∼450 TeV. However, an origin in an evolved pulsar wind nebula cannot be ruled out.

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

Journal keyword(s): Gamma-rays - Gamma-ray sources - H II regions - Supernova remnants

Simbad objects: 26

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Number of rows : 26
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 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7988 0
2 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 16269 0
3 1LHAASO J1850-0004u gam 18 51.6 -00 04           ~ 4 0
4 4FGL J1851.8-0007c gam 18 51 52.8 -00 07 21           ~ 6 0
5 HESS J1852-000 gam 18 52 +00.0           ~ 15 0
6 2FGL J1852.7+0047c gam 18 52 24.0 +00 37 48           ~ 13 0
7 1LHAASO J1852+0050u gam 18 52.4 +00 50           ~ 4 0
8 SNR G034.6-00.5 SNR 18 56 10.650 +01 13 21.30           ~ 1034 2
9 PSR J1856+0245 Psr 18 56 50.80 +02 45 50.2           ~ 51 0
10 2MASS J18570942+0206347 * 18 57 09.4074825374 +02 06 34.669027151           ~ 1 0
11 4FGL J1857.7+0246e Psr 18 57 11.0 +02 40 00           ~ 59 0
12 1LHAASO J1857+0203u gam 18 57.5 +02 04           ~ 3 0
13 MAGIC J1857+029 gam 18 57.6 +02 58           ~ 11 0
14 EGR J1856+0235 gam 18 57 37.16 +02 12 33.6           ~ 32 0
15 2MASS J18574979+0207101 * 18 57 49.7984113536 +02 07 10.142714048           ~ 1 0
16 SNR G035.6-00.4 SNR 18 57 55 +02 13.0           ~ 56 1
17 ZTF J185756.07+020729.3 LP* 18 57 56.0823748624 +02 07 29.250128166           ~ 4 0
18 1FGL J1857.9+0352c gam 18 58 04.5 +03 54 46           ~ 19 0
19 2MASS J18580473+0211461 * 18 58 04.7290696963 +02 11 45.976633074           ~ 1 0
20 GAL 035.6-00.5 HII 18 58 +02.1           ~ 2 0
21 2MASS J18581657+0155518 * 18 58 16.5741156717 +01 55 51.779406921           ~ 1 0
22 2MASS J18581732+0211438 * 18 58 17.3217001087 +02 11 43.809900480           ~ 1 0
23 4FGL J1858.3+0209 gam 18 58 18.4 +02 09 10           ~ 10 0
24 HESS J1858+020 gam 18 58 20.0 +02 05 24           ~ 45 0
25 1LHAASO J1858+0330 gam 18 58.4 +03 31           ~ 2 0
26 3FGL J1900.8+0337 gam 19 00 29.8 +03 39 50           ~ 10 0

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