2023ApJ...950L..16A

Query : 2023ApJ...950L..16A

2023ApJ...950L..16A - Astrophys. J., 950, L16 (2023/June-3)

Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and H.E.S.S. Blazar Observations.

AHARONIAN F., ASCHERSLEBEN J., BACKES M., BARBOSA MARTINS V., BATZOFIN R., BECHERINI Y., BERGE D., BI B., BOUYAHIAOUI M., BREUHAUS M., BROSE R., BRUN F., BRUNO B., BULIK T., BURGER-SCHEIDLIN C., BYLUND T., CAROFF S., CASANOVA S., CELIC J., CERRUTI M., CHAND T., CHANDRA S., CHEN A., CHIBUEZE J., CHIBUEZE O., COTTER G., DE BONY M., EGBERTS K., ERNENWEIN J.-P., FICHET DE CLAIRFONTAINE G., FILIPOVIC M., FONTAINE G., FUSSLING M., FUNK S., GABICI S., GHAFOURIZADEH S., GIAVITTO G., GLAWION D., GLICENSTEIN J.F., GOSWAMI P., GRONDIN M.-H., HAERER L., HOLCH T.L., HOLLER M., HORNS D., JAMROZY M., JANKOWSKY F., JOSHI V., JUNG-RICHARDT I., KASAI E., KATARZYNSKI K., KHATOON R., KHELIFI B., KLUZNIAK W., KOMIN N., KOSACK K., KOSTUNIN D., LANG R.G., LE STUM S., LEITL F., LEMIERE A., LENAIN J.-P., LEUSCHNER F., LOHSE T., LUASHVILI A., LYPOVA I., MACKEY J., MALYSHEV D., MALYSHEV D., MARANDON V., MARCHEGIANI P., MARCOWITH A., MARTI-DEVESA G., MARX R., MEYER M., MITCHELL A., MODERSKI R., MOHRMANN L., MONTANARI A., MOULIN E., MULLER J., MURACH T., NAKASHIMA K., NIEMIEC J., OHM S., OLIVERA-NIETO L., DE ONA WILHELMI E., PANNY S., PANTER M., PARSONS R.D., PERON G., PROKHOROV D.A., PROKOPH H., PUHLHOFER G., PUNCH M., QUIRRENBACH A., REICHHERZER P., REIMER A., REIMER O., REVILLE B., RIEGER F., ROWELL G., RUDAK B., RUIZ-VELASCO E., SAHAKIAN V., SANCHEZ D.A., SASAKI M., SCHUSSLER F., SCHUTTE H.M., SCHWANKE U., SHAPOPI J.N.S., SOL H., SPENCER S., STEINMASSL S., SUZUKI H., TAKAHASHI T., TANAKA T., TAYLOR A.M., TERRIER R., THORPE-MORGAN C., TSIROU M., TSUJI N., UCHIYAMA Y., VAN ELDIK C., VEH J., VENTER C., WAGNER S.J., WHITE R., WIERZCHOLSKA A., WONG Y.W., ZACHARIAS M., ZARGARYAN D., ZDZIARSKI A.A., ZOUARI S., ZYWUCKA N. (The HESS Collaboration), MEYER M. (The Fermi-LAT Collaboration)

Abstract (from CDS):

Magnetic fields in galaxies and galaxy clusters are believed to be the result of the amplification of intergalactic seed fields during the formation of large-scale structures in the universe. However, the origin, strength, and morphology of this intergalactic magnetic field (IGMF) remain unknown. Lower limits on (or indirect detection of) the IGMF can be obtained from observations of high-energy gamma rays from distant blazars. Gamma rays interact with the extragalactic background light to produce electron-positron pairs, which can subsequently initiate electromagnetic cascades. The gamma-ray signature of the cascade depends on the IGMF since it deflects the pairs. Here we report on a new search for this cascade emission using a combined data set from the Fermi Large Area Telescope and the High Energy Stereoscopic System. Using state-of-the-art Monte Carlo predictions for the cascade signal, our results place a lower limit on the IGMF of B > 7.1 × 10–16 G for a coherence length of 1 Mpc even when blazar duty cycles as short as 10 yr are assumed. This improves on previous lower limits by a factor of 2. For longer duty cycles of 104 (107) yr, IGMF strengths below 1.8 × 10–14 G (3.9 × 10–14 G) are excluded, which rules out specific models for IGMF generation in the early universe.

Abstract Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Active galaxies - High energy astrophysics - Extragalactic magnetic fields

Simbad objects: 7

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Number of rows : 7
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 RX J0232.8+2017 BLL 02 32 48.6148874688 +20 17 17.486717388     18.00 13.96   ~ 387 1
2 4FGL J0237.3+2000 Bz? 02 37 18.7 +20 00 05           ~ 9 0
3 QSO B0347-121 BLL 03 49 23.1862105584 -11 59 27.366035532   18.74 18.2 17.46   ~ 245 1
4 PMN J0416+0105 BLL 04 16 52.4945693352 +01 05 23.899102620   16.86 16.38 16   ~ 302 1
5 PKS J0550-3216 BLL 05 50 40.5705144672 -32 16 16.484718648   16.07 15.5     ~ 424 1
6 PMN J1103-2329 BLL 11 03 37.6150845072 -23 29 31.203773520   17.00 16.55 16.61   ~ 405 1
7 QSO B2356-309 BLL 23 59 07.9034996184 -30 37 40.671098544   18.414 16.44 16.795   ~ 318 2

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