Constraints on an annihilation signal from a core of constant dark matter density around the milky way center with H.E.S.S.

An annihilation signal of dark matter is searched for from the central region of the Milky Way. Data acquired in dedicated on-off observations of the Galactic center region with H.E.S.S. are analyzed for this purpose. No significant signal is found in a total of ∼9 h of on-off observations. Upper limits on the velocity averaged cross section, ⟨σv⟩, for the annihilation of dark matter particles with masses in the range of ∼300 GeV to ∼10 TeV are derived. In contrast to previous constraints derived from observations of the Galactic center region, the constraints that are derived here apply also under the assumption of a central core of constant dark matter density around the center of the Galaxy. Values of ⟨σv⟩ that are larger than 3×10^{-24} cm^{3}/s are excluded for dark matter particles with masses between ∼1 and ∼4 TeV at 95% C.L. if the radius of the central dark matter density core does not exceed 500 pc. This is the strongest constraint that is derived on ⟨σv⟩ for annihilating TeV mass dark matter without the assumption of a centrally cusped dark matter density distribution in the search region.

Search for photon-linelike signatures from dark matter annihilations with H.E.S.S.

Gamma-ray line signatures can be expected in the very-high-energy (E(γ)>100 GeV) domain due to self-annihilation or decay of dark matter (DM) particles in space. Such a signal would be readily distinguishable from astrophysical γ-ray sources that in most cases produce continuous spectra that span over several orders of magnitude in energy. Using data collected with the H.E.S.S. γ-ray instrument, upper limits on linelike emission are obtained in the energy range between ∼ 500 GeV and ∼ 25 TeV for the central part of the Milky Way halo and for extragalactic observations, complementing recent limits obtained with the Fermi-LAT instrument at lower energies. No statistically significant signal could be found. For monochromatic γ-ray line emission, flux limits of (2 × 10(-7) -2 × 10(-5)) m(-2) s(-1) sr(-1) and (1 × 10(-8) -2 × 10(-6)) m(-2) s(-1)sr(-1) are obtained for the central part of the Milky Way halo and extragalactic observations, respectively. For a DM particle mass of 1 TeV, limits on the velocity-averaged DM annihilation cross section ⟨σv⟩(χχ → γγ) reach ∼ 10(-27) cm(3)s(-1), based on the Einasto parametrization of the Galactic DM halo density profile.

Second positive phototropic response patterns of the oat coleoptile.

1.During second positive irradiation, bending increases steadily with time. Under optimal conditions, the lag between onset of illumination and beginning of parabolic bending behavior is about 3 min. - 2. Shortly after irradiation ceases, bending becomes linear with time. On a clinostat, bending continues for about 2.5 hr. Auxanometric measurements show that the ultimate cessation of bending is not due to failing growth rate. - 3. The second positive response shows a striking dependence on intensity of irradiation. Inactivation occurs when irradiation approaches the intensity of full daylight. - 4. Induction is linear with duration of illumination, both at purely activating intensities and at partially inactivating intensities. - 5. Induction at 2°, while somewhat slower than at 25°, retains linear dependence on exposure duration. This suggests that the reactions immediately following light reception are slowed but not stopped at low temperature. - 6. Growth, which drops to about 0.5 µ/min at 2°, resumes at about 18 µ min(-1) as soon as plants are warmed to 25°. Curvature does not seem to begin for about 10 min. Combined with information about lag time for primary auxin action, this suggests that lateral auxin transport, as well as growth, is strongly inhibited at near-freezing temperatures. - 7. The induced transport system is highly stable at 2°. - 8. Under optimal conditions, the lag between onset of irradiation and induction of capacity to produce measurable curvature is only a few seconds. The length of the lag is dependent on the rate of induction. The lag is thought to be due to the requirement that enough induction be accumulated to overcome resistance of the coleoptile. - 9. Induction is dependent on the gradient of light across the coleoptile, whether measured for purely activating or partially inactivating intensities. The light received is probably integrated either across individual cells or across the entire width of the coleoptile.