2022ApJ...936..126A

Query : 2022ApJ...936..126A

2022ApJ...936..126A - Astrophys. J., 936, 126 (2022/September-2)

Constraints on the Very High Energy Gamma-Ray Emission from Short GRBs with HAWC.

ALBERT A., ALFARO R., ALVAREZ C., ARTEAGA-VELAZQUEZ J.C., ARUNBABU K.P., AVILA ROJAS D., AYALA SOLARES H.A., BABU R., BELMONT-MORENO E., BRISBOIS C., CABALLERO-MORA K.S., CAPISTRAN T., CARRAMINANA A., CASANOVA S., CHAPARRO-AMARO O., COTTI U., COTZOMI J., COUTINO DE LEON S., DE LEON C., DE LA FUENTE E., DIAZ HERNANDEZ R.D., DICHIARA S., DINGUS B.L., DUVERNOIS M.A., DUROCHER M., DIAZ-VELEZ J.C., ENGEL K., ESPINOZA C., FAN K.L., 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., HUMENSKY T.B., HUNTEMEYER P., IRIARTE A., JOSHI V., KAUFMANN S., LARA A., LEE W.H., LEON VARGAS H., LINNEMANN J.T., LONGINOTTI A.L., LUIS-RAYA G., MALONE K., MARINELLI S.S., 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., NORIEGA-PAPAQUI R., PEISKER A., PEREZ ARAUJO Y., PEREZ-PEREZ E.G., REN Z., RHO C.D., ROSA-GONZALEZ D., ROSENBERG M., SACAHUI J.R., SALAZAR H., SALESA GREUS F., SANDOVAL A., SERNA-FRANCO J., SMITH A.J., SPRINGER R.W., SURAJBALI P., TIBOLLA O., TOLLEFSON K., TORRES I., TORRES-ESCOBEDO R., TURNER R., VILLASENOR L., WANG X., WILLOX E., ZEPEDA A., ZHOU H. (The HAWC Collaboration)

Abstract (from CDS):

Many gamma-ray bursts (GRBs) have been observed from radio wavelengths, and a few at very high energies (VHEs, >100 GeV). The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is well suited to study transient phenomena at VHEs owing to its large field of view and duty cycle. These features allow for searches of VHE emission and can probe different model assumptions of duration and spectra. In this paper, we use data collected by HAWC between 2014 December and 2020 May to search for emission in the energy range from 80 to 800 GeV coming from a sample of 47 short GRBs that triggered the Fermi, Swift, and Konus satellites during this period. This analysis is optimized to search for delayed and extended VHE emission within the first 20 s of each burst. We find no evidence of VHE emission, either simultaneous or delayed, with respect to the prompt emission. Upper limits (90% confidence level) derived on the GRB fluence are used to constrain the synchrotron self-Compton forward-shock model. Constraints for the interstellar density as low as 10–2 cm–3 are obtained when assuming z = 0.3 for bursts with the highest keV fluences such as GRB 170206A and GRB 181222841. Such a low density makes observing VHE emission mainly from the fast-cooling regime challenging.

Abstract Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Gamma-ray bursts - Gamma-ray detectors - High energy astrophysics - Gamma-ray transient sources - Theoretical models - Extragalactic astronomy

Simbad objects: 18

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Number of rows : 18
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 GRB 180720B gB 00 02 06.99 -02 55 07.8           ~ 215 0
2 GRB 170112A gB 01 00 55.70 -17 13 57.9           ~ 24 0
3 SN 2019oyw SN* 02 58 10.510 -08 57 27.20           ~ 218 0
4 GRB 190114C gB 03 38 01.18 -26 56 47.8           ~ 343 0
5 Fermi bn141205337 gB 06 11 26.16 +37 52 33.6           ~ 27 0
6 GRB 180103A gB 10 38 24.37 -53 33 21.6           ~ 21 0
7 SN 2013cq SN* 11 32 32.84 +27 41 56.2           SNIc 613 1
8 GRB 150710A gB 12 57 52.91 +14 19 05.0           ~ 19 0
9 GrW 170817 GWE 13 09 48.0850 -23 22 53.343           ~ 2683 0
10 Fermi bn170206453 gB 14 11 09.60 +14 28 48.0           ~ 28 0
11 GRB 150423A gB 14 46 18.96 +12 17 00.6           ~ 79 0
12 Fermi bn160714097 gB 15 38 +63.8           ~ 22 0
13 Fermi bn110731465 gB 18 42 00.99 -28 32 13.8           ~ 193 0
14 GRB 970417A gB 19 21 +54.2           ~ 56 0
15 Fermi bn170709334 gB 20 40 +02.2           ~ 6 0
16 Fermi bn090510016 G 22 14 12.6230 -26 34 58.550           ~ 548 0
17 Fermi bn090926181 gB 23 33 36.18 -66 19 25.9           ~ 339 0
18 GRB 181222A gB ~ ~           ~ 8 0

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