799 research outputs found
Anisotropies in the Diffuse Gamma-Ray Background Measured by the Fermi LAT
The contribution of unresolved sources to the diffuse gamma-ray background could induce anisotropies in this emission on small angular scales. We analyze the angular power spectrum of the diffuse emission measured by the Fermi LAT at Galactic latitudes absolute value of b > 30 deg in four energy bins spanning 1 to 50 GeV. At multipoles l >= 155, corresponding to angular scales approx 99.99% CL in the 1-2 GeV, 2- 5 GeV, and 5- 10 GeV energy bins, and at > 99% CL at 10-50 GeV. Within each energy bin the measured angular power takes approximately the same value at all multipoles l >= 155, suggesting that it originates from the contribution of one or more unclustered source populations. The amplitude of the angular power normalized to the mean intensity in each energy bin is consistent with a constant value at all energies, C(sub p) / (I)(exp 2) = 9.05 +/- 0.84 x 10(exp -6) sr, while the energy dependence of C(sub p) is consistent with the anisotropy arising from one or more source populations with power-law photon spectra with spectral index Gamma (sub s) = 2.40 +/- 0.07. We discuss the implications of the measured angular power for gamma-ray source populations that may provide a contribution to the diffuse gamma-ray background
Swift and Fermi observations of X-ray flares: the case of Late Internal Shock
Simultaneous Swift and Fermi observations of gamma-ray bursts (GRBs) offer a
unique broadband view of their afterglow emission, spanning more than ten
decades in energy. We present the sample of X-ray flares observed by both Swift
and Fermi during the first three years of Fermi operations. While bright in the
X-ray band, X-ray flares are often undetected at lower (optical), and higher
(MeV to GeV) energies. We show that this disfavors synchrotron self-Compton
processes as origin of the observed X-ray emission. We compare the broadband
properties of X-ray flares with the standard late internal shock model, and
find that, in this scenario, X-ray flares can be produced by a late-time
relativistic (Gamma>50) outflow at radii R~10^13-10^14 cm. This conclusion
holds only if the variability timescale is significantly shorter than the
observed flare duration, and implies that X-ray flares can directly probe the
activity of the GRB central engine.Comment: 13 pages, 4 figures, accepted for publication in Ap
High Energy Neutrino Emission and Neutrino Background from Gamma-Ray Bursts in the Internal Shock Model
High energy neutrino emission from GRBs is discussed. In this paper, by using
the simulation kit GEANT4, we calculate proton cooling efficiency including
pion-multiplicity and proton-inelasticity in photomeson production. First, we
estimate the maximum energy of accelerated protons in GRBs. Using the obtained
results, neutrino flux from one burst and a diffuse neutrino background are
evaluated quantitatively. We also take account of cooling processes of pion and
muon, which are crucial for resulting neutrino spectra. We confirm the validity
of analytic approximate treatments on GRB fiducial parameter sets, but also
find that the effects of multiplicity and high-inelasticity can be important on
both proton cooling and resulting spectra in some cases. Finally, assuming that
the GRB rate traces the star formation rate, we obtain a diffuse neutrino
background spectrum from GRBs for specific parameter sets. We introduce the
nonthermal baryon-loading factor, rather than assume that GRBs are main sources
of UHECRs. We find that the obtained neutrino background can be comparable with
the prediction of Waxman & Bahcall, although our ground in estimation is
different from theirs. In this paper, we study on various parameters since
there are many parameters in the model. The detection of high energy neutrinos
from GRBs will be one of the strong evidences that protons are accelerated to
very high energy in GRBs. Furthermore, the observations of a neutrino
background has a possibility not only to test the internal shock model of GRBs
but also to give us information about parameters in the model and whether GRBs
are sources of UHECRs or not.Comment: 14 pages, 17 figures, accepted for publication in PRD, with extended
descriptions. Conclusions unchange
High energy neutrino early afterglows from gamma-ray bursts revisited
The high energy neutrino emission from gamma-ray bursts (GRBs) has been
expected in various scenarios. In this paper, we study the neutrino emission
from early afterglows of GRBs, especially under the reverse-forward shock model
and late prompt emission model. In the former model, the early afterglow
emission occurs due to dissipation made by an external shock with the
circumburst medium (CBM). In the latter model, internal dissipation such as
internal shocks produces the shallow decay emission in early afterglows. We
also discuss implications of recent Swift observations for neutrino signals in
detail. Future neutrino detectors such as IceCube may detect neutrino signals
from early afterglows, especially under the late prompt emission model, while
the detection would be difficult under the reverse-forward shock model.
Contribution to the neutrino background from the early afterglow emission may
be at most comparable to that from the prompt emission unless the outflow
making the early afterglow emission loads more nonthermal protons, and it may
be important in the very high energies. Neutrino-detections are inviting
because they could provide us with not only information on baryon acceleration
but also one of the clues to the model of early afterglows. Finally, we compare
various predictions for the neutrino background from GRBs, which are testable
by future neutrino-observations.Comment: 18 pages, 12 figures, accepted for publication in PR
Periodic Emission from the Gamma-ray Binary 1FGL J1018.6-5856
Gamma-ray binaries are stellar systems containing a neutron star or black hole with gamma-ray emission produced by an interaction between the components. These systems are rare, even though binary evolution models predict dozens in our Galaxy. A search for gamma-ray binaries with the Fermi Large Area Telescope (LAT) shows that IFGL JI018.6-5856 exhibits intensity and spectral modulation with a 16.6 day period. We identified a variable X-ray counterpart, which shows a sharp maximum coinciding with maximum gamma-ray emission, as well as an 06V f) star optical counterpart and a radio counterpart that is also apparently modulated on the orbital period. IFGL J1018.6-5856 is thus a gamma-ray binary, and its detection suggests the presence of other fainter binaries in the Galaxy
On the Origin of the Highest Energy Cosmic Rays
We present the results of a new estimation of the photodisintegration and
propagation of ultrahigh energy cosmic ray (UHCR) nuclei in intergalactic
space. The critical interactions for photodisintegration and energy loss of
UHCR nuclei occur with photons of the infrared background radiation (IBR). We
have reexamined this problem making use of a new determination of the IBR based
on empirical data, primarily from IRAS galaxies, and also collateral
information from TeV gamma-ray observations of two nearby BL Lac objects. Our
results indicate that a 200 EeV Fe nucleus can propagate apx. 100 Mpc through
the IBR. We argue that it is possible that the highest energy cosmic rays
observed may be heavy nuclei.Comment: 2 pages revtex with one figure, submitted to Physical Review Letter
New Limits to the Infrared Background: Bounds on Radiative Neutrino Decay and on Contributions of Very Massive Objects to the Dark Matter Problem
From considering the effect of γ-γ interactions on recently observed TeV gamma-ray spectra, improved limits are set to the density of extragalactic infrared photons which are robust and essentially model independent. The resulting limits are more than an order of magnitude more restrictive than direct observations in the 0.025–0.3 eV regime. These limits are used to improve constraints on radiative neutrino decay in the mass range above 0.05 eV and to rule out very massive objects as providing the dark matter needed to explain galaxy rotation curves. Lower bounds on the maximum distance which TeV gamma rays may probe are also derived
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