2024ApJ...976...30A

Query : 2024ApJ...976...30A

2024ApJ...976...30A - Astrophys. J., 976, 30 (2024/November-3)

Spectral Study of Very-high-energy Gamma Rays from SS 433 with HAWC.

ALFARO R., ALVAREZ C., ARTEAGA-VELAZQUEZ J.C., AVILA ROJAS D., AYALA SOLARES H.A., BABU R., BELMONT-MORENO E., BERNAL A., CABALLERO-MORA K.S., CAPISTRAN T., CARRAMINANA A., CASANOVA S., COTZOMI J., DE LA FUENTE E., DEPAOLI D., DI LALLA N., DIAZ HERNANDEZ R., DINGUS B.L., DUVERNOIS M.A., ENGEL K., ERGIN T., ESPINOZA C., FAN K.L., FANG K., FRAIJA N., FRAIJA S., GARCIA-GONZALEZ J.A., GONZALEZ MUNOZ A., GONZALEZ M.M., GOODMAN J.A., GROETSCH S., HARDING J.P., HERNANDEZ-CADENA S., HERZOG I., HUANG D., HUEYOTL-ZAHUANTITLA F., HUNTEMEYER P., IRIARTE A., KAUFMANN S., LARA A., LEE W.H., LEE J., DE LEON C., LEON VARGAS H., LONGINOTTI A.L., LUIS-RAYA G., MALONE K., MARTINEZ-CASTRO J., MATTHEWS J.A., MIRANDA-ROMAGNOLI P., MONTES J.A., MORENO E., MOSTAFA M., NELLEN L., NISA M.U., NORIEGA-PAPAQUI R., PEREZ ARAUJO Y., PEREZ-PEREZ E.G., RHO C.D., ROSA-GONZALEZ D., RUIZ-VELASCO E., SALAZAR H., SANDOVAL A., SCHNEIDER M., SERNA-FRANCO J., SMITH A.J., SON Y., SPRINGER R.W., TIBOLLA O., TOLLEFSON K., TORRES I., TORRES-ESCOBEDO R., TURNER R., URENA-MENA F., VARELA E., VILLASENOR L., WANG X., WANG Z., WATSON I.J., YU S., YUN-CARCAMO S., ZHOU H. (The HAWC Collaboration)

Abstract (from CDS):

Very-high-energy (0.1-100 TeV) gamma-ray emissions were observed in High-Altitude Water Cherenkov (HAWC) data from the lobes of the microquasar SS 433, making them the first set of astrophysical jets that were resolved at TeV energies. In this work, we update the analysis of SS 433 using 2565 days of data from the HAWC observatory. Our analysis reports the detection of a point-like source in the east lobe at a significance of 6.6σ and in the west lobe at a significance of 8.2σ. For each jet lobe, we localize the gamma-ray emission and identify a best-fit position. The locations are close to the X-ray emission sites “e1” and “w1” for the east and west lobes, respectively. We analyze the spectral energy distributions and find that the energy spectra of the lobes are consistent with a simple power law dN/dE ∝ E^α^ with $\alpha =-{2.44}_{-0.12-0.04}^{+0.13+0.04}$ and $\alpha =-{2.35}_{-0.11-0.03}^{+0.12+0.03}$ for the east and west lobes, respectively. The maximum energy of photons from the east and west lobes reaches 56 TeV and 123 TeV, respectively. We compare our observations to various models and conclude that the very-high-energy gamma-ray emission can be produced by a population of electrons that were efficiently accelerated.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Gamma-ray sources - High mass x-ray binary stars - Jets

Simbad objects: 10

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Number of rows : 10
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 HAWC J1902+065 gam 19 02.2 +06 56           ~ 1 0
2 3FGL J1902.6+0655 gam 19 02 34.5 +06 54 36           ~ 10 0
3 HAWC J1905+071 gam 19 05.8 +07 11           ~ 1 0
4 PSR J1906+0722 Psr 19 06 31.20 +07 22 55.8           ~ 40 0
5 HAWC J1908+055 gam 19 07.6 +05 52           ~ 1 0
6 1LHAASO J1908+0621 gam 19 08.0 +06 21           ~ 1 0
7 HAWC J1908+061 gam 19 08.2 +06 18           ~ 1 0
8 ARGO J1907+0627 gam 19 08 12.24 +06 23 30.8           ~ 94 0
9 SS 433 HXB 19 11 49.5647697480 +04 58 57.827127648   16.854 14.643     A7Ib 2253 4
10 SNR G039.7-02.0 SNR 19 12 20 +04 55.0           ~ 378 1

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