2021ApJ...912L...4A

Query : 2021ApJ...912L...4A

2021ApJ...912L...4A - Astrophys. J., 912, L4-L4 (2021/May-1)

HAWC search for high-mass microquasars.

ALBERT A., ALFARO R., ALVAREZ C., ANGELES CAMACHO J.R., ARTEAGA-VELAZQUEZ J.C., ARUNBABU K.P., AVILA ROJAS D., AYALA SOLARES H.A., BAGHMANYAN V., BELMONT-MORENO E., BENZVI S.Y., BRISBOIS C., CABALLERO-MORA K.S., CAPISTRAN T., CARRAMINANA A., CASANOVA S., COTTI U., COTZOMI J., DE LA FUENTE E., DE LEON C., DIAZ HERNANDEZ R., DIAZ-VELEZ J.C., DINGUS B.L., DUROCHER M., DUVERNOIS M.A., ELLSWORTH R.W., ESPINOZA C., FAN K.L., FANG K., FRAIJA N., GALVAN-GAMEZ A., GARCIA-GONZALEZ J.A., GARFIAS F., GONZALEZ M.M., GOODMAN J.A., HARDING J.P., HERNANDEZ S., HONA B., HUANG D., HUEYOTL-ZAHUANTITLA F., HUNTEMEYER P., IRIARTE A., JARDIN-BLICQ A., JOSHI V., KIEDA D., LARA A., LEE J., LEE W.H., LEON VARGAS H., LINNEMANN J.T., LONGINOTTI A.L., LUIS-RAYA G., LUNDEEN J., MALONE K., MARTINEZ O., MARTINEZ-CASTRO J., MATTHEWS J.A., MIRANDA-ROMAGNOLI P., MORALES-SOTO J.A., MORENO E., MOSTAFA M., NAYERHODA A., NELLEN L., NEWBOLD M., NISA M.U., NORIEGA-PAPAQUI R., OLIVERA-NIETO L., OMODEI N., PEISKER A., PEREZ ARAUJO Y., RHO C.D., ROH Y.J., ROSA-GONZALEZ D., SALESA GREUS F., SANDOVAL A., SCHNEIDER M., SERNA-FRANCO J., SMITH A.J., SPRINGER R.W., TOLLEFSON K., TORRES I., TORRES-ESCOBEDO R., TURNER R., URENA-MENA F., VILLASENOR L., WATSON I.J., WEISGARBER T., WILLOX E. and ZHOU H.

Abstract (from CDS):

Microquasars with high-mass companion stars are promising very high energy (VHE; 0.1-100 TeV) gamma-ray emitters, but their behaviors above 10 TeV are poorly known. Using the High Altitude Water Cerenkov (HAWC) observatory, we search for excess gamma-ray emission coincident with the positions of known high-mass microquasars (HMMQs). No significant emission is observed for LS 5039, Cyg X-1, Cyg X-3, and SS 433 with 1523 days of HAWC data. We set the most stringent limit above 10 TeV obtained to date on each individual source. Under the assumption that HMMQs produce gamma rays via a common mechanism, we have performed source-stacking searches, considering two different scenarios: (I) gamma-ray luminosity is a fraction ε_ γ_ of the microquasar jet luminosity, and (II) VHE gamma rays are produced by relativistic electrons upscattering the radiation field of the companion star in a magnetic field B. We obtain ε_ γ_ < 5.4 x 10–6 for scenario I, which tightly constrains models that suggest observable high-energy neutrino emission by HMMQs. In the case of scenario II, the nondetection of VHE gamma rays yields a strong magnetic field, which challenges synchrotron radiation as the dominant mechanism of the microquasar emission between 10 keV and 10 MeV.

Abstract Copyright: © 2021. The American Astronomical Society. All rights reserved.

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

Simbad objects: 16

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Number of rows : 16
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 LS I +61 303 HXB 02 40 31.6644419688 +61 13 45.593918580 11.27 11.61 10.75 10.19 9.55 B0Ve 903 2
2 V* CI Cam HXB 04 19 42.1355996520 +55 59 57.706599192 12.13 12.41 11.77 10.79 9.99 B0/2I[e] 271 0
3 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
4 2HWC J1819-150 gam 18 19 09.6 -15 05 41           ~ 9 0
5 2HWC J1825-134 gam 18 25.8 -13 24           ~ 10 0
6 PSR J1826-1256 Psr 18 26 08.570 -12 56 33.53           ~ 152 1
7 PSR B1823-13 Psr 18 26 13.06 -13 34 48.1           ~ 460 1
8 V* V479 Sct HXB 18 26 15.0561548880 -14 50 54.247274304 12.02 12.23 11.27 11.04   ON6V((f))z 613 2
9 ARGO J1907+0627 gam 19 08 12.24 +06 23 30.8           ~ 94 0
10 SS 433 HXB 19 11 49.5647697480 +04 58 57.827127648   16.854 14.643     A7Ib 2253 4
11 3HWC J1913+048 gam 19 13 18.00 +04 51 18.2           ~ 2 0
12 HD 226868 HXB 19 58 21.6757355952 +35 12 05.784512688 9.38 9.72 8.91 8.42   O9.7Iabpvar 4590 0
13 2HWC J2006+341 gam 20 06.2 +34 11           ~ 15 0
14 NAME Cyg X Cld 20 30 04.7973633 +40 51 36.002197           ~ 962 1
15 TeV J2032+4130 gam 20 31.7 +41 31           ~ 148 0
16 V* V1521 Cyg HXB 20 32 25.78 +40 57 27.9           WN4/5-6/7 2035 2

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