SPHERE Science Verification
SPHERE Science Verification
SPHERE Science Verification Observations has been carried out between December 1 and December 12, 2014, and, in a service-mode like fashion, between Dec. 30 and Feb. 13, 2015. The observations have been performed in "service mode style" by a dedicated team and the collected data are made available to the whole ESO user community. See VLT Science Verification Policy and Procedures for more details.
WARNING: all (raw) data and calibrations are public immediately after the observations. There is no proprietary period nor earlier data release to the PIs.
Clicking on the programme ID for each programme provides a link to the raw data in the ESO archive.
A pre-release version of the SPERE data reduction pipeline can be found here.
Selected observing programmes
|Programme ID||PI Name||Title||Status|
|60.A-9352(A)||Daniel Apai||A SPHERE Discovery of Exoplanet Variability||Completed|
|60.A-9353(A)||Claes Fransson||SN1987A at the right resolution.||Completed|
|60.A-9354(A)||Melissa McClure||Distribution and abundance of water ice in a young extrasolar system||Partly Completed|
|60.A-9355(A)||Matthias Schreiber||The First Ever Detection of a Circumbinary Companion in a Post-Common Envelope Binary||Completed|
|60.A-9356(A)||Stefan Kraus||Searching for the accretion signatures of young protoplanets||Completed|
|60.A-9357(A)||John Carter||Mapping Io's volcanism with SPHERE-IFS: where did the silica go?||Partly Completed|
|60.A-9358(A)||Christian Thalmann||Revealing the true face of the LkCa 15 disk with ZIMPOL||Completed
|60.A-9359(A)||Wouter Vlemmings||The mass loss of supergiant VY CMa||Completed|
|60.A-9360(A)||Nuria Huelamo||The Young Proto-Planet in the Transitional system LkCa 15||Completed|
|60.A-9361(A)||Damien Gratadour||The NGC1068 core||Partly Completed|
|60.A-9362(A)||Bin Yang||Origin of Multiple Asteroid Systems by Component-Resolved Spectroscopy||Completed|
|60.A-9363(A)||Markus Kasper||Resolving the Mysteries of the T Tau System with SPHERE-IRDIS||Completed|
|60.A-9364(A)||Gergely Csepany||Examining disks in young multiple T Tauri systems||Completed|
|60.A-9365(A)||Cecile Gry||Search for close companions around Sirius||Completed|
|60.A-9366(A)||Theo Khouri||Unveiling the wind-driving mechanism of RDoradus||Completed|
|60.A-9367(A)||Pierre Kervella||The dust disk of the nearest AGB star L2 Pup in polarized light||Completed|
|60.A-9368(A)||Ralf Siebenmorgen||The structure in the ejecta of the extreme red supergiant VY CMa||Completed|
|60.A-9369(A)||H. Sana||Hunting for sub-solar companions around massive stars||Completed|
|60.A-9370(A)||E. Buenzli||Search for signs of disk-planet interactions around GG Tau A||Partly Completed
|60.A-9371(A)||Mario van den Ancker||Seeing Through the Dust: High-Resolution Infrared Polarimetry of R Mon||Completed
|60.A-9372(A)||Leigh Fletcher||Revealing the Thermochemical Properties of Jupiter's Satellites||Partly Completed|
|60.A-9373(A)||Siyi Xu||Are There Jupiter Analogs around White Dwarfs?||Partly Complted|
|60.A-9374(A)||Justine Lannier||Astrometry of suspected extremely tight young low-mass binaries with SPHERE: uncovering the best dynamical calibrators||Completed|
|60.A-9375(A)||Jos de Boer||Direct imaging of the Proto Planetary Disk around the CTTS or G giant BP PSC||Completed|
|60.A-9376(A)||Olivier Absil||The first image of an exozodiacal disk||Completed
|60.A-9377(A)||M. Bonnefoy||Optical images of a gas giant exoplanet||Partly Completed|
|60.A-9378(A)||Jun Hashimoto||Is the Spiral Structure in Transitional Disks Excited by Planet(s)?||Not Started
|60.A-9379(A)||Christophe Dumas||3-D shape of main-belt asteroids: Probing their internal structure||Completed|
|60.A-9380(A)||Anne-Marie Lagrange||Unveiling the inner part of the beta Pic disk||Completed
|60.A-9381(A)||Sasha Hinkley||Spectroscopy of a "Bridge" Companion to a Nearby Young M dwarf||Completed|
|60.A-9382(A)||Anne-Marie Lagrange||Searching for new planets around beta Pictoris and testing the photometric and astrometric precisions achievable on close giant planets
|60.A-9383(A)||Catherine Dougados||Resolving protostellar jet launching regions with SPHERE||Not Started|
|60.A-9384(A)||Toshiya Ueta||Enabling Polarimetric Angular Differential Imaging with SPHERE||Not Started|
|60.A-9385(A)||Blake Pantoja||Search for Companions to Radial Velocity Search Stars||Completed
|60.A-9386(A)||Markus Janson||Resolving the orbit of the AB Dor Ba/Bb pair||Completed|
|60.A-9387(A)||Amelia Bayo||Testing IRDIS limits: resolving the debris disk around the M dwarf TWA7||Completed
|60.A-9388(A)||Veselin Kostov||Is a circumbinary brown dwarf to blame for the irregular eclipse clock of V471 Tau?||Not Started|
|60.A-9389(A)||Myriam Benisty||Understanding disk evolution through the distribution of small dust particles in MWC758||Partly Completed|
|60.A-9390(A)||Matthias Maercker||The binary companion of R Sculptoris||Completed|
|60.A-9391(A)||M. Kuerster||The dynamical mass of a brown dwarf candidate||Completed
Further information on the observations can be found in the VLT/Melipal night-log for the night in which the observations were obtained:
- Melipal Telescope Report for Dec. 1/2, 2014 (pdf)
- Melipal Telescope Report for Dec. 2/3, 2014 (pdf)
- Melipal Telescope Report for Dec. 3/4, 2014 (pdf)
- Melipal Telescope Report for Dec. 4/5, 2014 (pdf)
- Melipal Telescope Report for Dec. 5/6, 2014 (pdf)
- Melipal Telescope Report for Dec. 6/7, 2014 (pdf)
- Melipal Telescope Report for Dec. 7/8, 2014 (pdf)
- Melipal Telescope Report for Dec. 8/9, 2014 (pdf)
- Melipal Telescope Report for Dec. 9/10, 2014 (pdf)
- Melipal Telescope Report for Dec. 10/11, 2014 (pdf)
- Melipal Telescope Report for Dec. 11/12, 2014 (pdf)
- Melipal Telescope Report for Feb. 09/10, 2015 (pdf)
- Melipal Telescope Report for Feb. 10/11, 2015 (pdf)
- Melipal Telescope Report for Feb. 11/12, 2015 (pdf)
- Melipal Telescope Report for Feb. 12/13, 2015 (pdf)
An integral part of the commissioning of a new instrument at the VLT is the Science Verification phase. SV programmes include a set of typical scientific observations that should verify and demonstrate to the community the capabilities of the new instrument in the operational framework of the VLT Observatory. In accordance with its SV Policy and Procedures (http://www.eso.org/sci/activities/vltsv/svdoc.pdf) ESO encourages the community to submit also highly challenging or risky science observations that will push SPHERE and the VLT to its limits in order to better understand the performance parameter space and its envelope. Such observations should focus on the instruments core modes in order to benefit a wide community.
SPHERE, the Spectro-Polarimetric High-contrast Exoplanet Research instrument is the extreme adaptive optics system and coronagraphic facility at the VLT. Its primary science goal is imaging, low-resolution spectroscopic, and polarimetric characterization of extra-solar planetary systems at optical and near-infrared wavelengths. SPHERE is fully described at:
Eleven nights from 3 to 11 December 2014 and from 9 to 12 February 2015 (all half-nights) were allocated to the SPHERE science verification. A call for proposals has been issued and the community was invited to submit proposals for the SPHERE science verification using the simplified proposal template.
In addition to the observing modes offered in P95. The restriction of some P95 SPHERE modes to visitor observing only will not apply to science verification, which is done entirely in service mode. SV will also consider proposals for the coronagraphic modes and IRDIS DPI will be offered on a best effort basis, depending on the remaining commissioning runs.
The limiting magnitudes will be relaxed relative to the P95 call for proposals. Please refer to the figure below for the expected performance.
Deadline for SPHERE SV proposals was 18:00 Central European Summer Time on 15 October 2014. Proposals need to be submitted to email@example.com. This is the only submission channel.
The list of protected targets for SPHERE Guaranteed Time Observations is given at http://www.eso.org/sci/observing/teles-alloc/gto/95.html.
Observations of targets protected by SPHERE GTO will not be accepted for SV.
The observations will be conducted in Service Mode by a dedicated team of ESO astronomers. The SPHERE SV team will be able to assist the successful PI¹s in the preparation and optimisation of the OBs on a best effort basis only.