Gamma-ray Constraints Research Articles

Radio and gamma-ray constraints on dark matter annihilation in the Galactic center

We determine upper limits on the dark matter (DM) self-annihilation cross section for scenarios in which annihilation leads to the production of electron--positron pairs. In the Galactic centre (GC), relativistic electrons and positrons produce a radio flux via synchroton emission, and a gamma ray flux via bremsstrahlung and inverse Compton scattering. On the basis of archival, interferometric and single-dish radio data, we have determined the radio spectrum of an elliptical region around the Galactic centre of extent 3 degrees semi-major axis (along the Galactic plane) and 1 degree semi-minor axis and a second, rectangular region, also centered on the GC, of extent 1.6 degrees x 0.6 degrees. The radio spectra of both regions are non-thermal over the range of frequencies for which we have data: 74 MHz -- 10 GHz. We also consider gamma-ray data covering the same region from the EGRET instrument (about GeV) and from HESS (around TeV). We show how the combination of these data can be used to place robust constraints on DM annihilation scenarios, in a way which is relatively insensitive to assumptions about the magnetic field amplitude in this region. Our results are approximately an order of magnitude more constraining than existing Galactic centre radio and gamma ray limits. For a DM mass of m_\chi =10 GeV, and an NFW profile, we find that the velocity-averaged cross-section must be less than a few times 10^-25 cm^3 s^-1.

Gamma-ray constraints on hadronic and leptonic activities of decaying dark matter

While the excess in cosmic-ray electrons and positrons reported by PAMELA and Fermi may be explained by dark matter decaying primarily into charged leptons, this does not necessarily mean that dark matter should not have any hadronic decay modes. In order to quantify the allowed hadronic activities, we derive constraints on the decay rates of dark matter into WW, ZZ, hh, qq̄ and gg using the Fermi and HESS gamma-ray data. We also derive gamma-ray constraints on the leptonic e+e−, μ+μ− and τ+τ− final states. We find that dark matter must decay primarily into μ+μ− or τ+τ− in order to simultaneously explain the reported excess and meet all gamma-ray constraints.

Soft gamma-ray constraints on a bright flare from the Galactic Center supermassive black hole

Sagittarius A ★ ( Sgr A ★ ) is the supermassive black hole residing at the center of the Milky Way. It has been the main target of an extensive multiwavelength campaign we carried out in April 2007. Herein, we report the detection of a bright flare from the vicinity of the horizon, observed simultaneously in X-rays ( XMM- Newton/EPIC) and near infrared ( VLT/NACO) on April 4 th for 1–2 h. For the first time, such an event also benefitted from a soft γ -rays ( INTEGRAL/ISGRI) and mid infrared ( VLT/VISIR) coverage, which enabled us to derive upper limits at both ends of the flare spectral energy distribution (SED). We discuss the physical implications of the contemporaneous light curves as well as the SED, in terms of synchrotron, synchrotron self-Compton and external Compton emission processes.

Anisotropy probe of galactic and extra-galactic dark matter annihilations

We study the flux and the angular power spectrum of gamma rays produced by dark matter (DM) annihilations in the Milky Way (MW) and in extra-galactic halos. The annihilation signal receives contributions from: (a) the smooth MW halo, (b) resolved and unresolved substructures in the MW, (c) external DM halos at all redshifts, including (d) their substructures. Adopting a self-consistent description of local and extra-galactic substructures, we compute the angular power spectrum of gamma-ray anisotropies and show that, quite independently from the prescription used for the concentration parameters c(M,z), an interesting signature of DM annihilations could soon be discovered by the Fermi LAT satellite at low multipoles, l{approx}100, assuming a particle physics scenario that does not violate gamma-ray constraints from the Galactic center. The DM contribution to the angular power spectrum is dominated by MW substructures (with mass M{>=}10{sup 4}M{sub {center_dot}}), while, at least for the substructures' models that we have adopted, the contribution of extra-galactic annihilations is negligible at all scales. MW subhalos also dominate the annihilation flux in the majority of the sky, with the smooth galactic halo being brighter only in the very central region.

Dark matter signals from cascade annihilations

A leading interpretation of the electron/positron excesses seen by PAMELA and ATIC is dark matter annihilation in the galactic halo. Depending on the annihilation channel, the electron/positron signal could be accompanied by a galactic gamma ray or neutrino flux, and the non-detection of such fluxes constrains the couplings and halo properties of dark matter. In this paper, we study the interplay of electron data with gamma ray and neutrino constraints in the context of cascade annihilation models, where dark matter annihilates into light degrees of freedom which in turn decay into leptons in one or more steps. Electron and muon cascades give a reasonable fit to the PAMELA and ATIC data. Compared to direct annihilation, cascade annihilations can soften gamma ray constraints from final state radiation by an order of magnitude. However, if dark matter annihilates primarily into muons, the neutrino constraints are robust regardless of the number of cascade decay steps. We also examine the electron data and gamma ray/neutrino constraints on the recently proposed ``axion portal'' scenario.

Gamma-ray constraints on dark matter annihilation into charged particles

Dark matter annihilation into charged particles is necessarily accompanied by gamma rays, produced via radiative corrections. Internal bremsstrahlung from the final state particles can produce hard gamma rays up to the dark matter mass, with an approximately model-independent spectrum. Focusing on annihilation into electrons, we compute robust upper bounds on the dark matter self-annihilation cross section $⟨{\ensuremath{\sigma}}_{A}v{⟩}_{{e}^{+}{e}^{\ensuremath{-}}}$ using gamma-ray data from the Milky Way spanning a wide range of energies $\ensuremath{\sim}{10}^{\ensuremath{-}3}--{10}^{4}\text{ }\text{ }\mathrm{GeV}$. We also compute corresponding bounds for the other charged leptons. We make conservative assumptions about the astrophysical inputs, and demonstrate how our derived bounds would be strengthened if stronger assumptions about these inputs are adopted. The fraction of hard gamma rays near the end point accompanying annihilation to ${e}^{+}{e}^{\ensuremath{-}}$ is only a factor of $\ensuremath{\lesssim}{10}^{2}$ lower than for annihilation directly to monoenergetic gamma rays. The bound on $⟨{\ensuremath{\sigma}}_{A}v{⟩}_{{e}^{+}{e}^{\ensuremath{-}}}$ is thus weaker than that for $⟨{\ensuremath{\sigma}}_{A}v{⟩}_{\ensuremath{\gamma}\ensuremath{\gamma}}$ by this same factor. The upper bounds on the annihilation cross sections to charged leptons are compared with an upper bound on the total annihilation cross section defined by neutrinos.

Gamma-ray constraints on the chemical composition of the martian surface in the Tharsis region: A signature of partial melting of the mantle?

The Gamma-Ray Spectrometer (GRS) on board Mars Odyssey is the first instrument to provide quantitative estimates of the composition of the martian surface at the global scale. At the present time published concentration maps are available across a broad equatorial swath for Ca, Cl, Fe, H, K, Si and Th. However, it remains to be determined to what extent the observed chemical signatures are the result of primary magmatic processes or secondary alteration at the surface. With this question in mind, we have considered in detail the GRS signature on the western part of the Tharsis region including Olympus Mons. This region was chosen as it is clearly of volcanic origin, has had a prolonged magmatic history, and is of spatial extent sufficiently large that potential contributions of surrounding regions to the GRS signature are limited. It also has a characteristic composition, being notably low in silica relative to the average composition of the martian mid-latitudes. The major element chemistry of the surface in this region (SiO 2, FeO, CaO, K 2O) is compared with predictions of thermodynamic calculations of liquids produced by partial melting of the martian mantle composition proposed by Dreibus and Wänke [Dreibus, G., Wänke, H., 1985. Mars, a volatile-rich planet. Meteoritics 20 (No. 2), 267–381] over a range of pressures and temperatures. For all four oxides, the Tharsis compositions are consistent with liquids produced at pressures from 15 to 20 kbar, and degrees of partial melting between 3 and 10%. This pressure of melting implies a magma source depth in the range ∼ 125–170 km, consistent with current estimates of the thickness of the lithosphere in this region. The idea that the surface chemistry in the Tharsis region is dominated by the signature of primary magmatism would therefore appear to be a reasonable working hypothesis, although as more data become available, more stringent and detailed tests of this simple model will be possible.

Gamma-ray constraints on the infrared background excess

Motivated by the idea that the recently detected near-infrared (1.2–4 μm) excess over the contribution of known galaxies is due to redshifted light from the first cosmic stars [MNRAS 339 (2003) 973], we have used the effect caused by photon–photon absorption on gamma-ray spectra of blazars to put constraints on extragalactic background light (EBL) from the optical to the far-IR bands. Our analysis is mainly based on the blazar H 1426+428, for which we assume a power-law unabsorbed spectrum. We find that an EBL model with no excess over known galaxies in the near-infrared background (NIRB) is in agreement with all the considered blazars; however, it implies a very peculiar intrinsic spectrum for H 1426+428. Additional data on the blazars 1ES1101-232, H 2356-309 and PKS 2155-304 exclude the existence of a strong NIRB excess consistent with Kelsall’s model of zodiacal light subtraction (ZL); the COBE/DIRBE measurements, after Wright’s model ZL subtraction, represent a firm NIRB upper limit. The constraints on the optical EBL are weaker, due to the fact that predictions from different optical EBL models are often comparable to the experimental errors. In the mid-infrared the SPITZER measurement of νI ν = 2.7 nW m −2 sr −1 at 24 μm gives a good fit for all the considered blazars.

Can annihilating dark matter be lighter than a few GeVs?

We estimate the gamma-ray fluxes from the residual annihilations of dark matter (DM) particles having a mass mdm ϵ [MeV, O(10) GeV] (a possible solution to the DM issue provided they have a new kind of interactions and no significant coupling to the Z) and compare them to observations. We find that particles lighter than O(100 MeV) can be viable DM candidates provided their dominant annihilation cross section is S-wave suppressed so as to satisfy the gamma-ray constraints. A similar conclusion is obtained for particles lighter than O(10) GeV from the study of radio fluxes, assuming a NFW profile and that they mainly annihilate into electrons.

Constraints on the Intergalactic Transport of Cosmic Rays

Motivated by recent experimental proposals to search for extragalactic cosmic rays (including anti-matter from distant galaxies), we study particle propagation through the intergalactic medium (IGM). We first use estimates of the magnetic field strength between galaxies to constrain the mean free path for diffusion of particles through the IGM. We then develop a simple analytic model to describe the diffusion of cosmic rays. Given the current age of galaxies, our results indicate that, in reasonable models, a completely negligible number of particles can enter our Galaxy from distances greater than $\sim 100$ Mpc for relatively low energies ($E$ $< 10^6$ GeV/n). We also find that particle destruction in galaxies along the diffusion path produces an exponential suppression of the possible flux of extragalactic cosmic rays. Finally, we use gamma ray constraints to argue that the distance to any hypothetical domains of anti-matter must be roughly comparable to the horizon scale.

Gamma-ray constraints on supernova nucleosynthesis

Gamma-ray spectroscopy holds great promise for probing nucleosynthesis in individual supernova explosions via short-lived radioactivity, and for measuring current global Galactic supernova nucleosynthesis with longer-lived radioactivity. It was somewhat surprising that the former case was realized first for a Type II supernova, when both Co-56 and Co-57 were detected in SN 1987A. These provide unprecedented constraints on models of Type II explosions and nucleosynthesis. Live Al-26 in the Galaxy might come from Type II supernovae, and if it is eventually shown to be so, can constrain massive star evolution, supernova nucleosynthesis, and the Galactic Type II supernova rate. Type Ia supernovae, thought to be thermonuclear explosions, have not yet been detected in gamma-rays. This is somewhat surprising given current models and recent Co-56 detection attempts. Ultimately, gamma-ray measurements can confirm their thermonuclear nature, probe the nuclear burning conditions, and help evaluate their contributions to Galactic nucleosynthesis. Type Ib/c supernovae are poorly understood. Whether they are core collapse or thermonuclear events might be ultimately settled by gamma-ray observations. Depending on details of the nuclear processing, any of these supernova types might contribute to a detectable diffuse glow of Fe-60 gamma-ray lines. Previous attempts at detection have come very close to expected emission levels. Remnants of any type of age less that a few centuries might be detectable as individual spots of Ti-44 gamma-ray line emission. It is in fact quite surprising that previous surveys have not discovered such spots, and the constraints on the combination of nucleosynthesis yields and supernova rates are very interesting. All of these interesting limits and possibilities mean that the next mission, International Gamma-Ray Astrophysics Laboratory (INTEGRAL), if it has sufficient sensitivity, is very likely to lead to the realization of much of the great potential of gamma-ray spectroscopy for understanding supernovae.

A ROSAT Wide Field Camera search for XUV bursts

We have searched the ROSAT Wide Field Camera all-sky survey for shorttime-scale (less than 50 s) XUV bursts down to a limiting count of 5 x 10 exp -3 count/sq arcmin, corresponding to an incident flux of about 3 x 10 exp -10 erg/sq cm. In a total observation period of 171 d covering the entire sky, we found no evidence for such events. The present results are used to place limits on the log N-log S relation for gamma-ray bursts and constraints on the spectral shape of the previously reported ultrasoft X-ray transients.

Gamma-ray constraints on the Galactic halo

Some findings from recent COS-B analyses of the diffuse Galactic γ-ray emission are briefly summarized, with emphasis on their impact for our understanding of the Galactic cosmic-ray halo.

Gamma ray constraints on dark matter reconsidered

The topic of γ ray observational constraints on dark matter candidates is reexamined here. The results of detailed calculations of γ ray source spectra from the annihilation of dark matter candidate particles as a function of mass are given. Use of these results in conjunction with γ ray observations does not generally lead to mass lower limits on ḡg's, H̃ 0's and v M′s which are as restrictive as those from the cosmological requirement that Ω⩽1. Thus, present γ ray observations do not provide new constraints on galactic dark matter.

A gamma-ray constraint on the nature of dark matter

If even a small component of the Galactic spheroid consists of the weakly interacting majorana fermions that are cold-dark-matter candidate particles for the Galactic halo, there should be a substantial flux of annihilation gamma rays from a source of about 1-deg extent at the Galactic center. COS B observations already constrain the halo cold-dark-matter (CDM) content entrained in the inner spheroid to be less than about 10 percent. A somewhat weaker constraint applies to the CDM believed to be present in the Galactic disk, but still only about 15 percent can be in such particles. Monochromatic line photons of energy 3-10 GeV are also predicted, and future experiments may be capable of improving these limits. Since both theoretical models of galaxy formation in a CDM-dominated universe and mass models for the rotation curve in the inner Galaxy suggest that a substantial fraction of the spheroid component should be nonluminous and incorporate entrained halo CDM, the hypothesis that the halo CDM consists predominantly of weakly interacting fermions such as photinos or heavy majorana mass neutrinos or higgsinos may already be subject to observational test.

Gamma ray constraints on annihilation in active galaxies

Observational constraints bearing on the possibility that active galaxies are powered by matter–antimatter annihilation are discussed. It is shown, contrary to previous work, that annihilation is not ruled out by observations.