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We present ALMA 230 GHz continuum and CO(2-1) observations of the nearby Compton-thick Seyfert galaxy ESO428-G14, with angular resolution 0.'' 7 (78 pc). CO(2-1) is distributed in clumpy spiral arms, a lopsided circumnuclear ring (CNR) with similar to 200 pc radius, and a transverse gas lane with size

It is proposed that the coincidence of higher brightness and upward electric current observed by Janvier et al. during a flare indicates electron acceleration by field-parallel potential drops sustained by extremely strong field-aligned currents of order 104 A m−2. A few consequences are discussed here.

Polarized foreground emission is a potential contaminant of attempts to measure the fluctuation power spectrum of highly redshifted 21 cm H i emission from the epoch of reionization. Using the Donald C. Backer Precision Array for Probing the Epoch of Reionization, we present limits on the observed power spectra of all four Stokes parameters in two frequency bands, centered at 126 MHz (z = 10.3) and 164 MHz (z = 7.66), for a three-month observing campaign of a deployment involving 32 antennas, for which results on the unpolarized power spectrum have been reported at z = 7.7 (by Parsons et al.) and at (by Jacobs et al.). The power spectra in this paper are processed in the same way as by those authors, and show no definitive detection of polarized power. This nondetection is consistent with what is known about polarized sources, combined with the suppression of polarized power by fluctuations in the ionospheric rotation measure, which can strongly affect Stokes Q and U. We are able to show that the net effect of polarized leakage is a negligible contribution at the levels of the limits reported by Parsons et al. and Jacobs et al.

The epoch of reionization power spectrum is expected to evolve strongly with redshift, and it is this variation with cosmic history that will allow us to begin to place constraints on the physics of reionization. The primary obstacle to the measurement of the EoR power spectrum is bright foreground emission. We present an analysis of observations from the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER) telescope which place new limits on the HI power spectrum over the redshift range of $7.5, Comment: 9 pages, submitted to apj, fixed author list and abstract typo

We present new observations with the Precision Array for Probing the Epoch of Reionization with the aim of measuring the properties of foreground emission for 21 cm epoch of reionization (EoR) experiments at 150 MHz. We focus on the footprint of the foregrounds in cosmological Fourier space to understand which modes of the 21 cm power spectrum will most likely be compromised by foreground emission. These observations confirm predictions that foregrounds can be isolated to a "wedge"-like region of two-dimensional (k ⊥, k ∥)-space, creating a window for cosmological studies at higher k ∥ values. We also find that the emission extends past the nominal edge of this wedge due to spectral structure in the foregrounds, with this feature most prominent on the shortest baselines. Finally, we filter the data to retain only this "unsmooth" emission and image its specific k ∥ modes. The resultant images show an excess of power at the lowest modes, but no emission can be clearly localized to any one region of the sky. This image is highly suggestive that the most problematic foregrounds for 21 cm EoR studies will not be easily identifiable bright sources, but rather an aggregate of fainter emission.

The preceding paper by Lee and Fisk discusses many of the topics considered in an earlier paper of ours. We reiterate our previous results in the context of their paper and point out several misinterpretations and inaccurate statements which they make.

Hawkins and Stewart's interpretation of the results of the V/V/sub max/ test for QSO samples is shown to be invalid. Their suggestion that the high values of V/V/sub max/ at small redshifts result from the exclusion of nearby QSOs from the samples is examined quantitatively for the well-studied 3CR sample, and shown to have a negligible effect on the results. Their claim that the values of V/V/sub max/ at larger redshifts indicate a uniform space density of QSOs is not true after an error in their calculations is corrected. Although the V/V/sub max/ test is less sensitive to space density evolution at large redshifts, current results are in good agreement with the hypothesis that a single density evolution law describes the observations out to a redshift of at least 2.5.