We present deep radio observations of four nearby dwarf spheroidal (dSph) galaxies, designed to detect extended synchrotron emission resulting from weakly interacting massive particle (WIMP) dark matter annihilations in their halos. Models by Colafrancesco et al. (CPU07) predict the existence of angularly large, smoothly distributed radio halos in such systems, that stem from electron and positron annihilation products spiraling in a turbulent magnetic field. We map a total of 40.5 deg 2 around the Draco, Ursa Major II, Coma Berenices, and Willman 1 dSphs with the GBT at 1.4 GHz to detect this annihilation signature, greatly reducing discrete-source confusion using the NVSS catalog. We achieve a sensitivity of σ sub 7 mJy/beam in our discrete source-subtracted maps, implying that the NVSS is highly effective at removing background sources from GBT maps. For Draco we obtained approximately concurrent VLA observations to quantify the variability of the discrete source background, and find it to have a negligible effect on our results. We construct radial surface brightness profiles from each of the subtracted maps, and jackknife the data to quantify the significance of the features therein. At the ∼ 10 ′ resolution of our observations, foregrounds contribute a standard deviation of 1.8 mJy/beam ≤ σ ast ≤ 5.7 mJy/beam to our high-latitude maps, with the emission in the Draco and Coma dominated by foregrounds. On the other hand, we find no significant emission in the Ursa Major II and Willman 1 fields, and explore the implications of non-detections in these fields for particle dark matter using the fiducial models of CPU07. For a WIMP mass M χ = 100 GeV annihilating into bb final states and B = 1 µG, upper limits on the annihilation cross-section for Ursa Major II and Willman I are log( σv χ , cm 3 s −1 ) −25 for the prefereed set of charged particle propagation parameters adopted by CPU07; this is comparable to that inferred at γ-ray energies from the two-year Fermi-LAT data. We discuss three avenues for improving the constraints on σv χ presented here, and conclude that deep radio observations of dSphs are highly complementary to indirect WIMP searches at higher energies.

Although cytokine therapy is an attractive strategy to build a more robust immune response in tumors, cytokines have faced clinical failures due to toxicity. In particular, interleukin-12 has shown great clinical promise but was limited in translation because of systemic toxicity. In this study, we demonstrate an enhanced ability to reduce toxicity without affecting the efficacy of IL-12 therapy. We engineer the material properties of a NP to meet the enhanced demands for optimal cytokine delivery by using the layer-by-layer (LbL) approach. Importantly, using LbL, we demonstrate cell-level trafficking of NPs to preferentially localize to the cell’s outer surface and act as a drug depot, which is required for optimal payload activity on neighboring cytokine membrane receptors. LbL-NPs showed efficacy against a tumor challenge in both colorectal and ovarian tumors at doses that were not tolerated when administered carrier-free.

The redshifted 21 cm monopole is expected to be a powerful probe of the epoch of the first stars and galaxies ( < < z 10 35). The global 21 cm signal is sensitive to the thermal and ionization state of hydrogen gas and thus provides a tracer of sources of energetic photons-primarily hot stars and accreting black holes-which ionize and heat the high redshift intergalactic medium (IGM). This paper presents a strategy for observations of the global spectrum with a realizable instrument placed in a low-altitude lunar orbit, performing night-time 40-120 MHz spectral observations, while on the farside to avoid terrestrial radio frequency interference, ionospheric corruption, and solar radio emissions. The frequency structure, uniformity over large scales, and unpolarized state of the redshifted 21 cm spectrum are distinct from the spectrally featureless, spatially varying, and polarized emission from the bright foregrounds. This allows a clean separation between the primordial signal and foregrounds. For signal extraction, we model the foreground, instrument, and 21 cm spectrum with eigenmodes calculated via Singular Value Decomposition analyses. Using a Markov Chain Monte Carlo algorithm to explore the parameter space defined by the coefficients associated with these modes, we illustrate how the spectrum can be measured and how astrophysical parameters (e.g., IGM properties, first star characteristics) can be constrained in the presence of foregrounds using the Dark Ages Radio Explorer (DARE).