The preparation of the long-term telescope schedule follows the submission and scientific review of new proposals. At the European Southern Observatory (ESO) this process entails scheduling the scientific proposals according to their scientific merit and available observing resources, as well as scheduling technical, maintenance, and commissioning activities for all operational telescopes of the La Silla Paranal Observatory. After the recent overhaul of the phase one proposal submission software, ESO started the development of a new telescopes time allocation and scheduling tool. The new tool makes the scheduling process more efficient while optimizing the use of observing facilities. Besides scheduling activities and allocating time according to scientific merit, available resources, operational and programmatic needs, the tool will enable simultaneous scheduling of multiple telescopes to appropriately account for dependencies between them. The implementation of this new Time Allocation tool opens the possibility for dynamic re-scheduling of the telescopes, which is a pre-requisite to implementing a yearly “Call for Proposals” along with the “Fast Track Channel” at ESO.
ESO’s VLT interferometer (VLTI) is a general-user optical/infrared interferometric facility. Its operations scheme is fully integrated into the well-established scheme of all VLT instruments and profits enormously from this experience and the implemented infrastructure to offer a unique service to the community. Based on the greatly improved capabilities of the 2nd generation VLTI instruments and taking advantage of a further development of ESO’s Observation Handling Tools, we have evolved the VLTI operations scheme as well. We have offered to VLTI investigators the possibility to indicate baseline configurations in a more flexible way and have introduced nested scheduling containers to better formalize the observational strategy. We have prepared for dedicated support of different types of interferometric observations. For imaging observations specifically, we have introduced an improved workflow to fill the uv plane and to handle time-critical imaging.
During the last years, ESO has undertaken the re-definition of all its front-end interfaces, from the preparation and submission of observing proposals up to their final scientific review by the ESO Observing Programmes Committee (OPC). Because of its overall complexity, ESO decided to go for a staged approach, which on one hand allowed us to offer the new proposals interface as soon as it was available, but on the other hand it has been challenging us in the operational handling of two simultaneous systems, the old and the new one. In 2019, we successfully deployed the new, web-based, Phase1 user interface for proposals preparation and submission (p1ui) and in 2021 we were able to offer for the first time a web-based, proposals grading system, that supported the proposals review and Expert Panel discussions, albeit online due to the COVID19 pandemic. In this presentation, we describe the overall project, focusing on the successful deployments of the new Phase 1 User Interface (for proposals submission), of the Proposal Evaluation Interface (for the proposals review process) and their subsequent improvements, made possible by closing the loop very effectively with our users’ community. We will then conclude by presenting ESO future plans in the Phase1 area, including new proposal submission channels and new review schemes.
ESO’s La Silla Paranal Observatory uses a set of integrated tools for preparation and execution of Service and Visitor Mode (SM and VM, respectively) observations. The web interface for the observation preparation (p2) provides a versatile and robust environment for users to efficiently design their observations. The software architecture of p2 enabled implementation of new services, modeled according to the instruments’ specifications and operational standards. The automatic creation of Finding Charts is integrated within p2 and the Observation Preparation (ObsPrep) tool enables interactive observing strategy configuration including for example fine-tuning of the science field pointings, selection of blind offset and guide stars as well as selection of auxiliary stars for instruments using Adaptive Optics. Through the Visitor Execution Sequence, observers can plan and monitor in real-time their (on-site or remote) observations. For Service Mode runs the use of scheduling containers, recently extended to include nesting of containers, enables design of complex observing strategies that are machine readable, which allows programmatic preparation of short term scheduling for execution and planning of the night at the observatory.
Observatory end-to-end science operations is the overall process starting with a scientific question, represented by a proposal requesting observing time; ending with the analysis of observation data addressing that question; and including all of the intermediate steps needed to plan, schedule, obtain, and process these observations. Increasingly complex observing facilities demand a highly efficient science operations approach and at the same time must be user friendly to the astronomical user community and enable the highest possible scientific return. Therefore, this process is supported by a collection of tools. We describe the overall end-to-end process and its implementation for the three upcoming Extremely Large Telescopes (ELTs): European Southern Observatory’s ELT, the Thirty Meter Telescope, and the Giant Magellan Telescope.
Until recently, users of ESO’s Very Large Telescope had to prepare Observing Blocks (OBs) with a standalone desktop tool. Tool support for automated OB mass production was mostly limited to imaging public surveys. Furthermore, there was no connection between the OB preparation software and other ancillary tools, such as Exposure Time Calculators, finding chart preparation software, and observatory schedule, meaning that users had to re-type the same information in several tools, and could design observations that would be incompatible with the Service Mode schedule. To address these shortcomings, we have implemented a new programming interface (API) and a state-of-the-art web application which provide observers with unprecedented flexibility and promote the usage of instrument and science-case specific tools, from small scripts to full-blown user interfaces. In this paper, we describe the software architecture of our solution, important design concepts and the technology stack adopted. We report on first user experience in both Visitor and Service Mode. We discuss tailored API programming examples, solving specific user requirements, and explain API usage scenarios for the next generation of ESO instruments. Finally, we describe the future evolution of our new approach.
Monitoring and prediction of astronomical observing conditions are essential for planning and optimizing observations. For this purpose, ESO, in the 90s, developed the concept of an Astronomical Site Monitor (ASM), as a facility fully integrated in the operations of the VLT observatory[1]. Identical systems were installed at Paranal and La Silla, providing comprehensive local weather information. By now, we had very good reasons for a major upgrade:
• The need of introducing new features to satisfy the requirements of observing with the Adaptive Optics Facility and to benefit other Adaptive Optics systems.
• Managing hardware and software obsolescence.
• Making the system more maintainable and expandable by integrating off-the-shelf hardware solutions.
The new ASM integrates:
• A new Differential Image Motion Monitor (DIMM) paired with a Multi Aperture Scintillation Sensor (MASS) to measure the vertical distribution of turbulence in the high atmosphere and its characteristic velocity.
• A new SLOpe Detection And Ranging (SLODAR) telescope, for measuring the altitude and intensity of turbulent layers in the low atmosphere.
• A water vapour radiometer to monitor the water vapour content of the atmosphere.
• The old weather tower, which is being refurbished with new sensors. The telescopes and the devices integrated are commercial products and we have used as much as possible the control system from the vendors. The existing external interfaces, based on the VLT standards, have been maintained for full backward compatibility. All data produced by the system are directly fed in real time into a relational database. A completely new web-based display replaces the obsolete plots based on HP-UX RTAP. We analyse here the architectural and technological choices and discuss the motivations and trade-offs.
KEYWORDS: Observatories, Telescopes, Data archive systems, Atmospheric Cherenkov telescopes, Data storage, Prototyping, Databases, Data modeling, Data acquisition, Space telescopes
The Laser Traffic Control System (LTCS) of the Paranal Observatory is the first component of the Adaptive Optics Facility (AOF, [8]) entering routine operations: a laser beam avoidance tool to support operations of an observatory equipped with five lasers and several laser-sensitive instruments, providing real-time information about ongoing and future collisions. LTCS-Paranal interfaces with ESO’s observing tools, OT and vOT. Altogether, this system allows the night operators to plan and execute their observations without worrying about possible collisions between the laser beam(s) and other lasersensitive equipment, aiming at a more efficient planning of the night, preventing time losses and laser-contaminated observations.
We present the data model utilised in maintaining the lifecycle of astronomical frames in the ESO Archive
activities. The principal concept is that complete file metadata are managed separately from the data and
merged only upon delivery of the data to the end user. This concept is now applied to all ESO Archive assets:
raw observation frames originated in ESO telescopes in all Chilean sites, reduced frames generated intra-ESO
using pipeline processing, as well as the processed data generated by the PIs and delivered to the ESO Archive
through "Phase 3" infrastructure. We present the implementation details of the model and discuss future
applications.
Throughout the course of many years of observations at the VLT, the phase 2 software applications supporting the
specification, execution and reporting of observations have been continuously improved and refined. Specifically the
introduction of astronomical surveys propelled the creation of new tools to express more sophisticated, longer-term
observing strategies often consisting of several hundreds of observations. During the execution phase, such survey
programs compete with other service and visitor mode observations and a number of constraints have to be considered.
In order to maximize telescope utilization and execute all programs in a fair way, new algorithms have been developed to
prioritize observable OBs taking into account both current and future constraints (e.g. OB time constraints, technical
telescope time) and suggest the next OB to be executed. As a side effect, a higher degree of observation automation
enables operators to run telescopes mostly autonomously with little supervision by a support astronomer. We describe
the new tools that have been deployed and the iterative and incremental software development process applied to
develop them. We present our key software technologies used so far and discuss potential future evolution both in terms
of features as well as software technologies.
The start of operations of the VISTA survey telescope will not only offer a new facility to the ESO community, but also
a new way of observing. Survey observation programs typically observe large areas of the sky and might span several
years, corresponding to the execution of hundreds of observations blocks (OBs) in service mode. However, the execution
time of an individual survey OB will often be rather short. We expect that up to twelve OBs may be executed per hour,
as opposed to about one OB per hour on ESO's Very Large Telescope (VLT). OBs of different programs are competing
for observation time and must be executed with adequate priority. For these reasons, the scheduling of survey OBs is
required to be almost fully automated. Two new key concepts are introduced to address these challenges: ESO's phase 2
proposal preparation tool P2PP allows PIs of survey programs to express advanced mid-term observing strategies using
scheduling containers of OBs (groups, timelinks, concatenations). Telescope operators are provided with effective short-term
decision support based on ranking observable OBs. The ranking takes into account both empirical probability
distributions of various constraints and the observing strategy described by the scheduling containers. We introduce the
three scheduling container types and describe how survey OBs are ranked. We demonstrate how the new concepts are
implemented in the preparation and observing tools and give an overview of the end-to-end workflow.
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