We report optical spectroscopy of the putative optical counterpart to the Swift source J052522.48+241331.8 (Page, Tueller & Beardmore 2007, ATEL #1279). We note that the XRT position (ATEL #1279) is consistent with that of the ROSAT source 1RXS J052523.2+241331. Using the X-ray flux and power-law model reported in ATEL #1279, we computed with

The Spitzer Wide-area InfraRed Extragalactic survey (SWIRE; Lonsdale et al., 2003PASP..115..897L) Version 1.0 data products release includes an image atlas and a source catalogs from the first of the 6 SWIRE fields to be observed by Spitzer, the ELAIS-N1 field. The release includes both Spitzer IRAC and MIPS mid/far-infrared data products and also

The SWIRE Photometric Redshift Catalogue consists of 1025119 sources, split between the SWIRE fields as follows: EN1 (218117), EN2 (125364), Lockman (229238), SWIRE-VVDS (34630), SWIRE-SXDS (55432), XMM-LSS (excluding VVDS and SXDS) (212572), Chandra DFS (149766). It is available via IRSA and also at http://astro.ic.ac.uk/~mrr/swirephotzcat . The

We present the SWIRE Photometric Redshift Catalogue 1 025 119 redshifts of unprecedented reliability and of accuracy comparable with or better than previous work. Our methodology is based on fixed galaxy and quasi-stellar object templates applied to data at 0.36-4.5um, and on a set of four infrared emission templates fitted to infrared excess data

Intermediate-resolution (0.5-1 Å) optical spectroscopy of the cataclysmic variable (CV) SY Cnc reveals the spectrum of the donor star. Our data enable us to resolve the orbital motion of the donor and provide a new orbital solution, binary mass ratio and spectral classification. We find that the donor star has spectral-type G8 +/- 2 V and orbits

Aims:The detection and measurement of acoustic modes on the giant planets of the solar system is of great interest for the study of the internal structure and evolution of the giant planets, as well as the study of the solar system formation. Such observations require a dedicated instrument and observing procedure. Methods: We describe the