The WSRT wide - field H survey II . Local Group features ⋆

We have used the Westerbork array to carry out an unbiased wide-field survey of H  emission features, achieving an  sensitivity of about 18 mJy/Beam at a velocity resolution of 17 km s−1 over 1800 deg2 and between −1000 < VHel < + 6500 km s−1. The primary data consists of auto-correlation spectra with an effective angular resolution of 49 FWHM. The survey region is centered approximately on the position of Messier 31 and is Nyquist-sampled over 60×30 in R.A.×Dec. In this paper we present our H  detections at negative velocities which could be distinguished from the Galactic foreground. Fully 29% of the entire survey area has high velocity H  emission at a column density exceeding our 3σ limit of about 1.5 × 1017cm−2 over 30 km s−1. We tabulate the properties of 95 discrete HVC components in the field, corresponding to more than an order of magnitude increase in number over that known previously. The distribution of discrete object number with flux density has an inflection point near 12 Jy-km s−1 which may correspond to a characteristic mass and distance for this population. A faint population of discrete HVCs is detected in the immediate vicinity of M31 which spans a large fraction of the M31 rotation velocity. This class of features is confined to about 12 (160 kpc) projected radius of M31 and appears to be physically associated. Independent confirmation of the features within 3. 5 (47 kpc) of M31 has been obtained in our Green Bank Telescope survey (Thilker et al. 2003). We detect a diffuse northern extension of the Magellanic Stream (MS) from at least δ = +20 → 40, which subsequently loops back toward the south. Recent numerical simulations had predicted just such an MS extension corresponding to the apo-galacticon portion of the LMC/SMC orbit at a distance of 125 kpc. A faint bridge of H  emission appears to join the systemic velocities of M31 with that of M33 and continues beyond M31 to the north-west. This may be the first detection of H  associated with the warm-hot intergalactic medium (WHIM). The distribution of peculiar velocity H  associated with M31 can be described by a projected exponential of 25 kpc scale-length and 5 × 1017cm−2 peak column density. We present the distribution function of NHI in the extended M31 environment, which agrees well with the low red-shift QSO absorption line data over the range log(NHI) = 17.2 to log(NHI) = 21.9. Our data extend this comparison about two orders of magnitude lower than previously possible and provide the first image of the Lyman limit absorption system associated with an L∗ galaxy.