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We have mapped faint 1667 OH line emission (TA approx 20 - 40 mK in our approx 30 beam) along many lines of sight in the Galaxy covering an area of approx 4circ times 4circ in the general direction of l approx 108circ, b approx 5circ. The OH emission is widespread, similar in extent to the local HI (r </= 2 kpc) both in space and in velocity. The OH profile amplitudes show a good general correlation with those of HI in spectral channels of approx 1 km/s; this relation is described by TA(OH) approx 1.50 times 10^{-4} TB(HI) for values of TB(HI) </approx 60 - 70 K. Beyond this the HI line appears to saturate, and few values are recorded above approx 90 K. However, the OH brightness continues to rise, by a further factor approx 3. The OH velocity profiles show multiple features with widths typically 2 - 3 km/s, but less than 10% of these features are associated with CO(1-0) emission in existing surveys of the area smoothed to comparable resolution.
We report the first results from a survey for 1665, 1667, and 1720 MHz OH emission over a small region of the Outer Galaxy centered at $l approx 105.0deg , b approx +1.0deg$ . This sparse, high-sensitivity survey ($Delta Ta approx Delta Tmb approx 3.
Recent work reported the discovery of a gamma-ray burst (GRB) associated with the galaxy GN-z11 at $zsim 11$. The extreme improbability of the transient source being a GRB in the very early Universe requires robust elimination of all plausible altern
Do molecular clouds collapse to form stars at the same rate in all environments? In large spiral galaxies, the rate of transformation of H2 into stars (hereafter SFE) varies little. However, the SFE in distant objects (z~1) is much higher than in the
The statistical characterization of the diffuse magnetized ISM and Galactic foregrounds to the CMB poses a major challenge. To account for their non-Gaussian statistics, we need a data analysis approach capable of efficiently quantifying statistical
Context: The interstellar medium (ISM) on all scales is full of structures that can be used as tracers of processes that feed turbulence. Aims: We used HI survey data to derive global properties of the angular power distribution of the local ISM. Met