Instruments

• HARPS:
  
  • A commissioning of the Laser Frequency Comb took place during April 2015. Additional commissioning activities will take place during Period 96 to make the system ready for operations. Interested users are invited to consult the HARPS News page before the start of their run.
  • The upgrade of the optical fibers successfully took place in May and early June 2015. See the HARPS News page. A detailed report will be published in the Messenger. In particular:
    
    • radial velocity systematics due to slight de-centering and de-focussing have been eliminated;
      
    • the broken sky fiber of EGGS has been repaired;
    • HARPS has gained in throughput by at least 10%;
      
    • however, a constant offset is expected to be introduced in the radial velocity measurements taken after the fiber exchange (May 28th). Although the instrument and its pipeline are fully operational, the data-reduction is being optimized, in particular, to determine this offset as accurately as possible with the goal to assure best precision and long-term continuity to all programmes, especially to the ones spanning pre- and post-upgrade observing time.
      

Large Programmes

• Large Programmes are not offered on the NTT in Period 96.
• Large Programmes on the 3.6-m telescope may span up to Period 100. See the Call for Proposals for Period 97 for details.

UT instruments and facilities

Telescopes: all UTs

• The concept of "Virtual Image Slicer" has been developed and implemented on the UTs. The Virtual Image Slicer consists in elongating the stars in a given direction by the introduction of a small amount of astigmatism thanks to the Active Optics of the telescope. Alignment of the major axis of the elongated star along the entrance slit of a spectrograph allows to increase the total signal collected in a single spectrum by a factor of up to 100 relative to a perfectly shaped image for bright sources in comparable execution time,  as overheads would otherwise be much longer than the actual observing (shutter) time. The use of the "Virtual Image Slicer" is only allowed in Visitor Mode. It must be explicitly mentioned in box 8b 'Observing Mode Justification'. Details can be found in Guisard, Sterzik & Munoz Proc. SPIE 9145, Ground-based and Airborne Telescopes V, 914544 (July 22, 2014).
• The installation and commissioning of the Coudé train for ESPRESSO will take place during Period 97.

UT1 - Antu

• CRIRES was taken out of operations as of July 17th, 2014 to undergo a major upgrade to transform it into a cross-dispersed echelle spectrograph. It is therefore not offered in Period 97. Operations will likely not start before the end of 2017.
  
• Instead, NACO has been offered on the Nasmyth A focus since Period 94, with a limited list of offered modes.
  • During Period 97, only the following modes are offered:
    
    • NAOS:
      • VIS & IR wavefront sensing;
      • Pupil tracking;
    • CONICA:
      • Imaging without chopping, in NoAO; usage of the Mp filter is only possible in VM;
        
      • Cube mode;
      • Focal plane AGPM coronography, with the  Lp, NB_3.74 or NB_4.05 filters;
        
      • Wollaston/HWP polarimetry;
        
      • SAM/SAMPOL, only in VM.
  • The following modes are not offered: LGS, SDI+, 4QPM/Lyot coronography, APP imaging and spectroscopy, prism spectroscopy, and, starting with Period 97, grism spectroscopy, and coronagraphy other than the AGPM coronagraphy.
    
  • As for February 2015, the Aladdin2 detector (installed in CONICA at the end of 2014) features a spurious background noise that limits the sensitivity of NACO when long individual exposure times (DIT) are used. This extra noise is caused  by an imperfect thermal shielding of the detector electronics.
    Nearly wavelength-independent, the contribution of the background noise can be modeled as a brighter sky: about -0.6 mag/arcsec through the Ks-band filter and -0.7 mag/arcsec through the H-band filter. There is no significant degradation at long wavelengths (L’, M’) as observations anyway require short DITs due to the nigh ambient background (sky + optics).
    Following problems with the camera wheel, NACO was fixed with the S13 objective on June 8th, 2015.  In addition, following a power cut on June 14, 2015, the upper right quadrant is not suitable for science. The 3 problems are expected to be solved during a 2-month long intervention starting early in October 2015. Please check the News page for updates.
    In particular, the current NACO ETC over-predicts the flux in JHK by up to 50 percent. An improved version will be delivered for Phase 2, after the intervention in October/November; this new version will take into account the  reduced background and also measurements in bands red-wards of K.
  • Large and Monitoring Programmes with NACO will not be accepted as the availability of several modes cannot be guaranteed in the coming periods.
    

UT2 - Kueyen

• XSHOOTER:
  
  • A project to fix the Atmospheric Dispersion Correction (ADC) systems started in 2015. XSHOOTER will likely be taken out of operations - possibly for several months - to modify the ADC system or install re-designed ones in the future. As a consequence, Large and Monitoring Programmes using XSHOOTER will not be accepted in Period 97. Updates on the status of the ADCs can be found on the XSHOOTER news webpage.
    
  • Starting from Period 96, two additional templates in slit and IFU modes are available for mapping of an extended object with a sequence of offsets and with or without any sky position. In parallel, the behavior for the FixedSky and GenericOffset  is slightly changed. The FixedSky offset template allows one to observe the object and a defined, allways identical, sky position. The GenericOffset template allows one to observe an object or a sequence of objects and a sequence of sky positions, which can be different, but the number of sky observations must be equal to the number of object observations. These changes allow a better support by the data reduction pipeline.
    
• FLAMES:
  
  • Improved measures of the instrument efficiency at all settings have been acquired and are used to feed the ETC. As a result, the current ETC outputs a signal-to-noise ratio that can be significantly different from the output obtained using previous versions under the same conditions. The current ETC is expected to provide more accurate predictions of the signal-to-noise ratio. Compared to the previous ETC version, the predicted signal-to-noise ratios are generally lower in blue settings and higher in red settings. Significant differences (less than a factor 2) are expected in the most blue and most red settings.
  • A redetermination of the focus of GIRAFFE has been carried out. As a result, the spectral resolution has significantly improved, as summarized in the FLAMES News page.
  • An alternative, low noise read-out mode for GIRAFFE is offered for Period 97, in Visitor Mode only.

UT3 - Melipal

• SPHERE
  
  • (Spectro-Polarimetric High-contrast Exoplanet REsearch) is an extreme adaptive optics system and coronagraphic facility. The primary science goal of this second generation VLT instrument is imaging, low-resolution spectroscopic, and polarimetric characterization of extra-solar planetary systems. The instrument design is optimized to provide the highest image quality and contrast performance in a narrow field of view around bright targets in the visible or near infrared bands. SPHERE is installed at the Nasmyth focus of UT3 and includes:
    • the Common Path and Infrastructure (CPI), which receives direct light from the telescope, and provides highly stabilized, AO-corrected, and coronagraphic beams to the three science instruments;
    • the Infrared Dual-Band Imager and Spectrograph (IRDIS), which provides Classical Imaging (CI), Dual-Band Imaging (DBI), Dual-Polarization Imaging (DPI), and Long Slit Spectroscopy (LSS) in low-resolution covering the range 0.95 to 2.32 μm with resolving power of R ~ 50 (LRS) or medium-resolution 0.95 to 1.65 μm with R ~ 400 (MRS);
    • the Integral Field Spectrograph (IFS), which provides a data cube of 38 monochromatic images either covering the range 0.95 to 1.35 μm (Y-J) at spectral resolution of R ~ 50 or 0.95 to 1.65 μm (Y-H) at R ~ 30, and
    • the Zurich IMaging POLarimeter (ZIMPOL), which provides diffraction limited classical imaging and differential polarimetric imaging (DPI) at 15 milli-arcsec resolution in the visible.
  • SPHERE has been offered since Period 95.
  • Starting from Period 96, the IRDIS DPI mode is offered in Visitor Mode only.
  • Starting from Period 97, the broadband H filter for IRDIS is offered in IRDIFS mode, while the broadband Ks filter is offered in the IRDIFS_EXT mode.
  • As described in the CPI section of the SPHERE Overview, the quality of the correction strongly depends on the seeing: in particular,  seeing conditions for SPHERE proposals must be better than 1.4"
• VISIR is offered again since Period 95.
  
  • The offered modes include imaging, low-resolution specctroscopy, and long slit and cross-dispersed high-resolution spectroscopy in both Service and Visitor Modes. Coronagraphy using the Annular Grooves Phase Mask (AGPM)  is offered in Visitor Mode only. Details on the offered modes and configurations are provided in the User Manual.
    
  • Only Large and Monitoring programmes involving imaging, low-resolution specctroscopy, and long slit and cross-dispersed high-resolution spectroscopy will be accepted.
    
  • The PWV must be provided as an observing constraint during their Phase 1 and Phase 2 preparation.
• VIMOS:
  • Since Period 95, rules regarding attached calibrations for the MOS mode have updated.  For the more accurate grisms LR_blue, LR_red and HR_red (<1 pixel) the previously implemented waivable error has been converted to a warning. That is, users can create their MOS OBs without attached calibrations, but need to check that their science case can accept wavelength accuracies of 0.5-1.0 pixels. For the less accurate grisms HR_Blue, MR, and HR_orange the waivable error remains in place.
    
  • Starting from Period 95 onwards, pre-imaging OBs are not allowed to be in concatenation containers. The execution time for pre-imaging runs has to be calculated for single OBs.
  • Large and Monitoring Programmes are not offered in Period 97 for operational reasons compounded by the ongoing Public Spectroscopic Surveys.
    
  • Public Spectroscopic Surveys started in Period 94 and substantially use all the dark and grey time in good conditions (PHO/CLR, seeing < 1.000) in RA ranges 00-05:30h and dark time in RA ranges 08-12h (also see the Public Survey webpages). Please note that even though the best observing conditions in the RA ranges above are substantially committed to the ongoing Public Spectroscopic Surveys, some time may be allocated to a very strong, scientifically compelling Normal or DDT programme.

UT4 - Yepun

• Adaptive Optics Facility
  • Installation of the first Laser Guide Star Unit (LGSU) took place in March 2015. It was commissioned during Period 95;
  • GRAAL was installed on the telescope in August 2015.
    
  • During Periods 96 ad 97 the following installation and commissioning activities affect operation on UT4. Although the dates provided are the best estimates at the time of writing, they can be affected by significant shifts. Large and monitoring programmes must be compatible with these activities.
    
    • installation of the first Laser Guide Star Unit (LGSU) took place in March 2015 and was commissioned during Period 95;
    • installation of GRAAL on the telescope and re-commissioning of HAWK-I took place in August 2015;
      
    • commissioning of GRAAL with the first LGSU takes place early in Period 96;
    • installation of the 3 other LGSUs and commissioning of common features with all LGSUs and GRAAL takes place during the second half of Period 96
    • commissioning of the 4 LGSus will continue early in Period 97 during which the telescope is not available for about 10 nights.
• HAWK-I :
  
  • Starting from Period 96, users of Fast Photometry may control the adapter focus from the acquisition template therefore allowing out-of-focus observations.
    
• SINFONI:
  
  • An upgrade of the SPIFFI  optics is planned for January 2016: its main goal is to improve transmission in the J band. Changes are expected to include:
    • Replacement of pre-optics including the pre-optics wheel.
    • New J and K filters with improved transmission. The filter wheel will also be changed.
    • Replacement of mirrors to improve the line spread function (LSF).
    • Enlarged sky baffle to cure vignetting of slits #1 and #32.
• MUSE:
  • Starting from Period 96, MUSE has been available for observations in Rapid Response Mode.

Visitor focus

• No focus for Visitor Instrument is available on the VLT since Period 95.

VLTI instruments and facilities

• During Period 95 the laboratory underwent major modifications in view of the arrival of the 2nd generation instruments GRAVITY and MATISSE as well as ESPRESSO, which will go in the nearby combined-Coudé laboratory.
• AMBER is  offered again since Period 96.
  
• PIONIER is offered again, as an ESO instrument, since Period 96: therefore, it is no longer mandatory to contact the instrument team or to include them as co-I before submitting the proposal. It is available in both service and visitor modes.  Follow late breaking news from technical time results in March, 2015:
  
  • The instrument can track fringes on visibilities higher than 5%  (V=0.05)
  • The LOW detector gain has been commissioned. The brightest  targets that can be observed in service mode are H=-1mag. Since no suitable calibrators might be available for the LOW gain within the recommended area around the target,  cross-calibration with other gain values has been tested and is  within the typical precision of the instrument. In that case, calibrators well fainter than the target can be used.
    
  • Tests on the UTs have shown no improvement of sensitivity or precision over the ATs. UTs can only be requested if use of ATs is excluded (e.g. no guide star available).

• VLTI-UTs and ATs: By early Period 97, all UTs Coudé and all ATs will be exclusively equipped with Star Separator Systems (STS) in view of operations with
  GRAVITY.
• Starting from Period 96 the AT configurations have slightly changed, but the overall characteristics remain. Three different AT quadruplets are offered for Period 97 (check the VLTI configuration page for more information):
  
  • small (baselines from 10 to 40m): A0-B2-C1-D0 to replace A1-B2-C1-D0
    
  • medium (baselines from 40 to 100m): K0-D0-G2-J3 to replace H0-D0-G1-I1
    
  • large (baselines from 60 to 140m): A0-J2-G1-J3 to replace A1-K0-G1-J3
    
• The installation of GRAVITY, the second generation VLTI instrument for precision narrow-angle astrometry and interferometric imaging, starts in 2015 during the VLTI laboratory refurbishment. Commissioning of the instrument starts during the first half of Period 96 and will continue during Period 97: during this time the VLTI will not be available for regular operations for approximately 2 weeks every 2 months. The number of baseline configurations for the ATs may also be restricted during the second half of the period due to these commissioning activities.
• The installation of the 4 units of the GRAVITY Coudé Infrared Adaptive Optics (CIAO) system for the VLT Interferometer is expected to take place during Period 96 and 97, during which the corresponding UT will not be available for VLTI operation. The commissioning of each of these units is expected to require approximately 10 half-nights.
• No VLTI Visitor focus is available in Period 97.

Survey Telescopes and Instruments

VISTA

• A Call for Letters of Intent to propose new public surveys has been released with a deadline of 15 October 2015. Further details can be found via the
  Applying for Observing Time webpage.

VST

• Normal programme proposals are accepted on the VST in Period 97. However, in order to ensure the timely progress of the ongoing Public Surveys these are restricted to filler programmes that request poor weather conditions (i.e., no moon constraints, and/or seeing>1.4", and/or thin/thick clouds). Target of Opportunity proposals requesting  a short amount of time with OmegaCAM will also be considered.
  
• The installation of an improved baffling mechanism including specially designed system of ribs was completed in April 2015. Measurements show that most of the stray-light component has been reduced. Also, the brightness of the background is at least 10% fainter than before the installation of the ribs and baffles.
  
  

General

• During Period 97, the ESO time slots are expected to be scheduled in April, June and August.
  
• The exact distribution of the observing time between the APEX partners can be found on the APEX web pages. Time-critical observations should only be requested during the ESO runs.
• Large Programmes with APEX using Poor PWV conditions: In order to make the best use of the time where the PWV is high (PWV>2 mm) ESO invites Large Programmes for those conditions. Poor PWV large programmes must be clearly identied as such in Box 5 and 8 of the large programme proposal form. Ideally a "Poor PWV LP Programme" therefore consists of a large sample of targets covering a wide RA range. The proposal must demonstrate that the scientic goals can be reached with only a signicant subset of the observations completed. Poor PWV-LPs may cover up to 4 consecutive semesters.

Instruments

• The new 350 μm camera ARTEMIS is offered conditional to its successful commissioning in November 2015. ARTEMIS will cover a field of view of 4'x2' at 350µm. Parallel observations at 450 μm may be available, but cannot be guaranteed. Sensitivity estimations for 450 μm will not be available before the deadline, and the science case should not depend on this band. If the commissioning is delayed, ESO may execute ARTEMIS programmes with SABOCA instead. A new observing time calculator is available
  
• SABOCA  is not offered in Period 97 as the same capabilities are offered by ARTEMIS.
• SHFI:
  • APEX-1: Large proposals for PWV>2mm conditions are encouraged.
  • APEX-T2:  this 1.3 THz receiver has been de-commissioned
    
• FLASH:
  
  • This PI instruments is offered to the ESO community on a collaborative basis with MPIfR. Large programmes or time critical observations with PI instruments will not be accepted. Users who would like to use FLASH must contact the instrument PI, Dr. Rolf Guesten (rguesten[AT]mpifr-bonn.mpg.de), at least two weeks prior to submitting their proposal. Members of the PI team should be included as CoIs on the proposal. The operation of these PI instruments requires the presence of the instrument team so all ESO FLASH and observations will be scheduled on fixed dates; the exact dates have not been determined yet.
  • Observations will be done by the PI team during a maximum of 3 days. Preference will be given to proposals using the dual-beam, wide-bandwidth capabilities of FLASH due to limited ESO observing time.
• CHAMP+: this MPIfR PI instrument is not offered in Period 97 because of a planned technical intervention. It may be offered again in Period 98.
• SUPERCAM: this PI instrument is no longer offered. There are currently no plans to offer it again.
• SEPIA: this new instrument is offered conditional to a successful commissioning in September 2015. It can house up to 3 ALMA-type receiver cartridges. In Period 97, only the band 5 receiver is offered, covering 159 to 211 GHz with dual polarization, sideband-separating mixers. The XFFTS backends will cover the full 4 GHz IF bandwidth simultaneously in both sidebands and in both polarizations (i.e. two bandpasses of 4 GHz width each, with an 8 GHz gap in between). An observing time calculato is available.
  The Late Breaking News page should be checked for updates on the commissioning as it take place after the release of the call for proposals.