HAWK-I is a cryogenic wide-field imager installed at the Nasmyth A focus of UT4. The on-sky field of view is 7.5'x7.5', with a cross-shaped gap of 15" between the four HAWAII 2RG 2048x2048 pixels detectors. The pixel scale is of 0.106". The instrument is offered with 10 observing filters placed in two filter wheels: 4 broad band filters (Y(Z), J, H & K) and 6 narrow band filters (Bracket gamma, CH4, H2, 1.061 μm, 1.187 μm & 2.090 μm).

The Science Verification observations of the APEX Swedish Heterodyne Facility Instrument (SHFI) were observed in March 2008. ESO requested input from the community by issuing a call for SV projects in February 2008, with 39 proposals received. A selection of the APEX-1 proposals listed below have been observed during the week of joint SV observations in March 2008. The APEX-3 and APEX-T2 SV projects will be observed later in dynamical scheduling. ESO will also continue observing APEX-1 proposals during period 81.

This new query form provides the users with a unified access to the ESO collection of both imaging and spectroscopic Advanced Data Products (ADP).

The Commissioning of the VLTI RMN recorder took place in January 2008 using a configuration involving two ATs and Finito in Fringe tracking mode. The raw data now are available in the ESO archive. Data can be downloaded in one package or file-by-file.

Within the framework of AIDA (Astronomical Infrastructure for Data Access), the European Virtual Observatory (EURO-VO) project is seeking proposals from teams carrying out archival research or projects that could benefit from the Virtual Observatory concept. The Virtual Observatory tools and applications allow seamless access to most of the world's large data archives such as ESO, ESA or HST. They also allow users to access a huge variety of reduced multiwavelength data and catalogues and to perform high-level analysis of images, spectra and large tabular datasets. Successful applicants will receive support from EURO-VO astronomers in using the VO facilities and software to complete their projects.

As of 1st April 2008, PIs can access their own raw proprietary data at any time through the ESO archive.

As part of the ESO Deep Public Survey (DPS), optical imaging observations were carried out in U, B, V, R, I bands, using the Wide Field Imager (WFI) instrument mounted at the 2.2m telescope at La Silla, Chile. This survey consisted of three square degrees in three well-separated regions (Deep1, Deep2 and Deep3) split into 4 adjacent WFI pointings (named a, b, c, d). The Garching-Bonn Deep Survey (GaBoDS) combines the data from this survey with data from most other ESO programmes that coincide with the original DPS regions, up until December 2006.

ESO/MVM (or "alambic") is an end-to-end, high-throughput image reduction system, originally developed by Benoit Vandame at the Nice Observatory for a project based on Multi-resolution Vision Model (MVM), then as part of the ESO Imaging Survey (EIS) project, and finally it was taken over by the Virtual Observatory Systems department for the processing of targeted archival data, with the aim of enhancing the legacy value of the ESO archive. ESO/MVM allows seamless processing of optical and near-IR data (e.g. WFI, VIMOS, FORS2, ISAAC, SOFI, HAWKI). It was developed over 10 years, it incudes 171,000 lines of code and was the engine at the core of the EIS data processing and other ESO public surveys, such as GOODS/ISAAC. The software package released here replaces a previous and now obsolete public version of MVM (v1.0.1). The latest stable version (v1.3.5) includes significant algorithmic improvements, bug fixes, new configuration files extending its application to more ESO instruments. The software is maintained only on a best-effort basis.

As part of the Great Observatories Origins Deep Survey (GOODS), multi-object spectroscopy of faint galaxies in the Chandra Deep Field South (CDF-S) has been carried out, using the VIMOS instrument mounted at the Melipal Unit Telescope of the VLT at ESO's Cerro Paranal Observatory, Chile.

The Science Demonstration (SD) of MAD is carried out largely following the philosophy applied to the Science Verification of the VLT instruments (see the VLT Science Verification Policy and Procedures document as reference). MAD SD runs took place in November 2007 and January 2008.