Oxford University Museum of Natural History, Oxford, United Kingdom, 29 June òÀÓ 3 July 2015

This workshop will explore some of the first science that will emerge from the European Extremely Large Telescope (EòÀÐELT) in the next decade. The primary spectroscopic capability of E-ELT at first light will be provided by the HARMONI instrument, a visible and near-infrared integral field spectrograph that will be capable of working close to the diffraction limit of the telescope or in natural seeing mode.

ESO Headquarters, Garching, Germany, 13òÀÓ15 April 2015

The ESO ALMA Regional Centre (ARC) will organise another Community Days workshop at ESO Headquarters in order to optimally prepare the European astronomical community for ALMA Cycle 3. The call for Cycle 3 observing proposals will be released in March 2015 and the main new scientific capability will be significantly longer baselines than in previous cycles.

The ALMA Long Baseline Campaign, taking place from 1 September to 30 November 2014, has been proceeding well. As a result, the observatory has decided to expand the scope of the capabilities to be demonstrated with two Science Verification (SV) targets with Band 7: the pre-main sequence star HL Tau and the gravitational lens SDP 81. Information on ALMA SV can be found here.

An ALMA status report for November 2014 is available. The report ( PDF) summarizes the status and recent progress of Cycle 2 Early Science observations as of October 2014, including "Cycle 1 Transfer" projects. It includes the 12-m array configuration schedule for the rest of Cycle 2 and a summary of the number of unfinished òÀÜhigh priorityòÀÝ observations. The report also contains plans and references to ongoing work as part of the òÀÜExtension and Optimization of Capabilities (EOC)òÀÝ and preparations for Cycle 3.

ESO Headquarters, Garching, Germany, 15òÀÓ17 April 2015

All Herschel science data, and some user-provided data products, are publicly available through the Herschel Science Archive. Meanwhile, the ALMA Science Archive is being populated with observations from the first three Cycles, with more data released daily. The higher frequency ALMA bands overlap with the lower frequency Herschel bands, and, despite the huge difference in spatial resolution, Herschel sources provide ideal targets for ALMA follow-up. In order to explore the full potential of both archives, archival users need to be aware of the contents and differences.

ESO Workshop, ESO Headquarters, Garching, Germany, 6òÀÓ10 July, 2015
Mass loss from cool Asymptotic Giant Branch and Red Supergiant stars inputs large amounts of material to the ISM and is therefore an important process for understanding stellar lifecycles and galactic ecology. Significant advances in observations (e.g. VLTI, ALMA and other facilities), and theory, now provide an opportunity to revisit outstanding questions of late stellar evolution, such as the role of mass loss, magnetic fields and binarity. The aim of the meeting is to bring together observers and theorists from the low and high mass stellar communities with the goals of exploring the commonalities of evolved star mass loss.

The most recently installed instrument at Paranal, the ESO Planet-finder instrument SPHERE, underwent its last commissioning run during 05 òÀÓ 15 October 2014. SPHERE saw first light on 04 May 2014 (see the Release) and was followed by three periods of commissioning in May, July and August 2014.

After a year at UT3, X-shooter was re-installed at UT2 earlier this month to make room for the re-commissioning and integration of VISIR on UT3, which will start next month. In spite of poor weather conditions, which delayed the precise measurement of the telescope focus for X-shooter, the long list of recommissioning tasks, were completed as planned, thanks to the efficient work of the science and engineering teams. Routine science operations with X-shooter have re-commenced.

Pipeline processed HARPS echelle data are now available as Science Data Products via the Phase 3 spectral query form. The data consist of 1D spectra in the ESO/SDP format and the tar files containing unaltered output of the HARPS pipeline (DRS v. 3.5), as previously available.

ESO Workshop, Vitacura, Santiago, Chile, 23òÀÓ27 March 2015

Angular and spectral resolutions are fundamental limitations to our understanding of the properties of galaxies in the nearby and distant Universe. The advent of state-of-the-art facilities with high angular and spectral resolution capabilities coupled with high sensitivity, such as ALMA, allows the interstellar medium and star formation properties of galaxies at intermediate redshift to be probed in unprecedented detail, along with their counterparts in the local Universe.