The ESO Archive Science Portal allows browsing and exploration of archive content using an intuitive interactive user interface that supports iterative queries or by direct database and Virtual Observatory (VO) access using user scripts and VO-aware tools. The latest version, released on 23 April 2020, provides the features and improvements listed below.

During the commissioning runs of MATISSE at VLTI in the second half of 2018 several astronomical targets were observed, in order to assess the scientific capabilities of the instrument and to optimise the observing strategies. This page provides links to selected data obtained during those runs, for both science and calibration targets.

The MUSE Analysis of Gas around Galaxies project (MAGG, ESO programme ID: 197.A-0384, PI: M. Fumagalli) provides the community with high quality VLT/MUSE cubes centered on bright redshift z~3.5 quasars (Lofthouse et al. 2019). These absorbers were discovered in archival high-to-medium resolution spectra of the quasars collected, among others, with UVES and XSHOOTER.

The VISTA Hemisphere Survey (VHS, ESO Programme ID: 79.A-2010, PI R. McMahon) is a wide area - multi band - near infrared survey, which when combined with other VISTA public surveys, will result in the coverage of the whole southern celestial hemisphere (Declination < 0; 20,000 deg²), to a depth 30 times fainter than 2MASS/DENIS in at least two filters (J and Ks), with a minimum exposure time of 60 seconds per filter and a median 5*sigma point source depth of AB = 20.8 and 20.0 in J and Ks filters respectively.

The VISTA Kilo-degree Infrared Galaxy Public Survey (VIKING) is a wide area (covering a final area of 1350 sq. deg.), intermediate-depth (5-sigma detection limit J~21 on Vega system) near-infrared imaging survey, in the five broadband filters Z, Y, J, H, Ks. The sky coverage has maximum overlap with the Kilo-Degree Survey KiDS in the optical bands.

The VISTA EXtension to Auxiliary Surveys (VEXAS, 'Spiniello & Agnello, 2019, A&A, 630') project aims at providing photometric catalogues with the most uniform spatial coverage, in the multi-wavelength sky for various scientific uses, for example object classification (e.g. quasars, galaxies, and stars; high-z galaxies, white dwarfs), photometric redshifts of large galaxy samples and identification of exotic objects (e.g. extremely red objects and lensed quasars).

The ADHOC programme (096.C-0730(A) and 097.C-0749(A), PI G. Beccari) is equivalent to an OmegaCAM mini-survey targeting circumstellar discs in nearby Galactic star-forming regions. The scientific goal of this mini-survey is the study of the star formation history of several star-forming regions using deep, wide field, multi-band observations in the optical filters u, g, r, i and Hα, with depth reaching 21 AB mag in r. A total of eight star-forming regions in the Galaxy were observed.

VANDELS  is a deep Public Spectroscopic Survey targeting high-redshift galaxies in the UKIDSS Ultra Deep Survey (UDS) and Chandra Deep Field South (CDFS) survey fields using the VIMOS spectrograph. The goal is to obtain spectra with sufficient signal-to-noise ratio to derive stellar population ages, metallicities and outflows velocities from absorption line studies, allowing a detailed investigation of the physics of galaxies in the early Universe. Within an area of 0.2 deg²,  the survey aims at delivering ~2100 high signal-to-noise spectra of star-forming galaxies in the redshift range 1 < z < 7, with 85% of its targets selected to be at z >= 3, and passive galaxies in the redshift range 1 < z < 2.5.

The primary goal of the VST Photometric Hα Survey of the Southern Galactic Plane and Bulge (VPHAS+, PI J. E. Drew) is to collect single-epoch ugri broad-band and Hα narrow-band photometry across the southern Galactic Plane within the latitude range -5 < b < +5 with typical 5-sigma sensitivities for point sources down to 21 mag in Vega or fainter.

Archive users are informed that the generation of the in-house processed science data products for FEROS is currently suspended since February 2019. ESO is working on an improved version of the pipeline and the newly generated products will become available via the ESO archive interfaces in the incoming months. A new announcement will be posted once the publication of the reprocessed FEROS products is resumed.