Probing the Dipole of the Diffuse Gamma-Ray Background

被引：2

作者：

Kashlinsky, A. ^{[1
,2
,3
]}

Atrio-Barandela, F. ^{[4
]}

Shrader, C. S. ^{[5
,6
]}

机构：

[1] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA

[2] SSAI, Lanham, MD 20770 USA

[3] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[4] Univ Salamanca, Dept Fundamental Phys, E-37008 Salamanca, Spain

[5] NASA, Astroparticle Phys Lab, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA

[6] Catholic Univ Amer, Dept Phys, Washington, DC USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2024年 / 961卷 / 01期

关键词：

ENERGY COSMIC-RAYS; LARGE-SCALE ANISOTROPY; LARGE-AREA TELESCOPE; DARK FLOW; SPECTRUM; FLUCTUATIONS; NEUTRINOS; EMISSION; CLUSTERS; UNIVERSE;

D O I：

10.3847/2041-8213/acfedd

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We measured the dipole of the diffuse gamma-ray background (DGB), identifying a highly significant time-independent signal coincidental with that of the Pierre Auger UHECR. The DGB dipole is determined from flux maps in narrow energy bands constructed from 13 yr of observations by the Large Area Telescope (LAT) of the Fermi satellite. The gamma-ray maps were clipped iteratively of sources and foregrounds similar to that done for the cosmic infrared background. The clipped narrow energy band maps were then assembled into one broad energy map out to the given energy starting at E = 2.74 GeV, where the LAT beam falls below the sky's pixel resolution. Next we consider cuts in Galactic latitude and longitude to probe residual foreground contaminations from the Galactic plane and center. In the broad energy range 2.74 < E <= 115.5 GeV, the measured dipoles are stable with respect to the various Galactic cuts, consistent with an extragalactic origin. The gamma-ray sky's dipole/monopole ratio is much greater than that expected from the DGB clustering component and the Compton-Getting effect origin with reasonable velocities. At similar or equal to(6.5-7)% it is similar to the Pierre Auger UHECRs with E (UHECR) >= 8 EeV, pointing to a common origin of the two dipoles. However, the DGB flux associated with the found DGB dipole reaches parity with that of the UHECR around E (UHECR) <= 1 EeV, perhaps arguing for a non-cascading mechanism if the DGB dipole were to come from the higher-energy UHECRs. The signal-to-noise ratio of the DGB dipole is largest in the 5-30 GeV range, possibly suggesting the gamma-photons at these energies are the ones related to cosmic rays.

引用

页数：11

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