Service Mode Rules and Recommendations for Observation Blocks
Preparing Observation Blocks
Observations at all ESO telescopes are carried out by executing Observation Blocks (OBs) provided by the users. OBs for Service Mode runs with Paranal Instruments must be made with p2. For (designated) Visitor Mode observation preparation, please follow dedicated Visitor Mode Guidelines.
Please refer to the P2PP3 User Manual and to the User Manuals of the different instruments for more specific information on the structure and content of OBs, and how to build OBs for different instruments. A number of tutorials describing step-by-step the construction of OBs for different instruments is available.
Service Mode OBs: rules and advices
It is important to keep in mind the Service Mode policies and the following rules and guidelines when designing a Service Mode programme or when preparing a Phase 2 package:
- Some observing strategies cannot be supported in Service Mode; in particular, real-time decisions about the sequencing of OBs, complex OB sequencing, or decisions based on the outcome of previously executed OBs (like adjustment of integration times or execution of some OBs instead of others).
- OBs are only executed once. If you want to repeat an identical observation multiple times, you must submit multiple OBs. This requirement applies to standard stars as well.
- OBs are normally executed non-contiguously. Since efficient Service Mode operations require continuous flexibility to best match the OB constraints with actual observing conditions, OBs for a given programme may be scheduled non-contiguously. Therefore, users should not expect their OBs to be executed in a specific sequence or in a linked way, unless a sound scientific justification (indicated in the README file and approved with a Phase 2 Waiver in case of a contiguous execution lasting longer than 1 hr) exists. Approved OB sequences should then be prepared as concatenations. Exceptions to this rule are cases in which one OB observing a calibration source needs to be executed contiguously to a science OB. In such a case place both OBs into a concatenation scheduling container to enforce their contiguous execution.
- Multi-mode, multi-configuration OBs are normally not permitted in Service Mode. Although multiple configurations within one OB may sometimes reduce overheads, scheduling and calibrating such OBs is extremely inefficient and can increase the calibration load to an unsustainable level. Examples of such multi-configuration OBs are those combining imaging and spectroscopy in a single OB, spectroscopy with multiple grisms or multiple central wavelength settings, or imaging with a large number of filters (although most imagers allow multiple broadband filters in one OB). Multi-configuration OBs are accepted only if duly justified and authorized by means of a Phase 2 Waiver Request.
- OB execution times must be below 1 hour. Long OBs are more difficult to schedule and execute within the specified constraints because of the unpredictable evolution of the observing conditions. For this reason, OBs taking more than one hour to execute are accepted by ESO only in exceptional cases and provided that a Phase 2 Waiver Request is submitted and approved. In such cases, ESO will consider the OB successfully executed if the constraints were fulfilled during the first hour of execution, even if conditions degrade after that time.
- Concatenation scheduling container execution time must be below 1 hour and exceptionally for CRIRES instrument science+telluric standard concatenation must be below 1.5h. Only in exceptional cases, and provided that a Phase 2 Waiver Request is submitted and approved, longer concatenations may be submitted. In such cases, ESO will consider the concatenated OBs successfully executed if the constraints were fulfilled during the first hour of execution, even if conditions degrade after that time.
- User-provided calibration OBs that need to be executed contiguously with science OBs need to be specified via concatenation scheduling containers.
- Time constraints must be indicated in the OBs. If you intend to observe time-critical events or monitor a target at specific time windows, you need to indicate this under the Time Intervals tab of the OBs. Please note that absolute (UT) time constraints refer to the interval in which the OB can be started, whereas for Local Sidereal Time (LST) time intervals, the time interval refers to the entire duration of the OB. For monitoring observations it is often more appropriate to put OBs in a time-link container. Specifying time windows as broad as possible will reduce the possibilities that your OBs are not executed because of higher priority programmes or because the observing conditions did not allow the observations during the interval that you specified. Usage of absolute time intervals must be scientifically justified in the README file. Please read carefully the time-critial OB execution policy.
- Specify the weakest possible Constraint Set values. OBs that can be executed under a broad range of conditions are easier to schedule. In particular, if photometry is needed of a field, it is normally sufficient to obtain a short integration under photometric conditions (transparency = PHO) and carry out the rest of the integration with OBs having a transparency = CLR constraint.
Some OBs must be executed within precise time windows, rather than any time when the external conditions (moon, seeing, transparency...) would allow the execution. The following types of time-dependencies can be recognized:
- Absolute time constraints, meaning that an OB must be executed at specific dates that can be predetermined. An example is the observation of a binary star at a precise phase of its period.
- Relative time links, implying that an OB must be executed within a time interval after the execution of a previous OB, but not necessarily at a fixed date. Examples of this are monitoring observations of a variable source at roughly constant intervals.
Both types of time-dependency are implemented within p2. Whereas absolute time constraints are available at the level of single OBs, the relative time links are implemented within the new "Time Link" container.
Within a Time Link container, the user can define a series of OBs, having the earliest and latest time when a given OB in the series must be executed with respect to the preceding OB. The time-related information is stored in a database, from where it is retrieved by scheduling tools available to the operator on the mountain in order to build up a short-term schedule that properly takes these constraints into account.
In some cases it may be desired to execute the OBs consecutively, with no other observations in between. This has been implemented in p2 within the "Concatenation" container. The Concatenation container consists of two or more OBs that must be executed "back-to-back" without breaks. The sequence of the execution of OBs in a Concatenation follows the sequence as they are listed in the p2 window. However, please notice that this sequence is not strictly enforced during execution.
In P2PP v2 it was possible to assign an execution priority to each OB, so that the operator is aware of the ones that have a higher scientific importance at the time of deciding on observations to execute for a given programme.
It has been recognized nevertheless that such simple priority scheme is sometimes insufficient to deal with programmes containing large number of OBs, and especially for surveys containing large numbers of target fields observed in a number of instrumental setups. In such cases the need for a prioritization scheme above the individual OB level, which can take into account the past execution history of the programme, becomes clear. One can consider for instance the case of a survey of several target fields to be observed through several different filters, with each field and filter specified in a single OBs. Depending on the science goals of the programme it may be desirable to complete the observations of a given field in all filters before proceeding to the next field, or conversely to observe all the fields in a given filter before proceeding to the next filter, or even ensure that contiguous coverage among the fields takes priority.
The approach adopted to deal with such cases is the definition of Groups of OBs, in which internal priorities within each group are reflected in the form of a contribution of each OB to the total group score. The short-term scheduling tools available on the mountain will take into account the current scores of each group of OBs, and will then apply a number of rules in order to prioritize the possible OBs to be executed according to them. Such rules will for instance give the highest execution priority to those OBs that set a new maximum of the score among the existing groups; and among those, the highest priority will be given in turn to those that produce the largest increase in group score. By assigning to the OBs the appropriate contributions to the scores of their respective groups, the users can make sure that the progress in the execution of the programme will take place in a way that is consistent with the scientific priorities of the observations. In addition, it will be possible to assign different priorities to each group.
The Survey Area Definition Tool (SADT) is a utility developed by the VISTA consortium that allows users to define areas to be covered by surveys executed with either VIRCAM at VISTA or OmegaCam at the VST according to a number of criteria. The SADT determines the central coordinates of the different pointings required to cover the field according to the specifications, as well as ancillary guide star information to allow acquisition and guiding. The output produced is a file to be ingested into P2PP version 3 containing all the target information needed for the preparation of the OBs with which the survey will be executed.
The latest distribution of the tool can be downloaded from the SADT web page, where also the SADT Cookbook with step-by-step instructions and examples can be found.
Additional Service Mode Requirements for SINFONI
These observing modes are not offered:
- observations with the sky spider
- observations with spectral dithering
Selected DIT Values
In order to prevent daytime calibrations (dark frames) to run for a large fraction of the morning, it is recommended to limit the use of different DIT values to a minimum set (0.83, 1, 2, 5, 10, 15, 20, 30,60, 100, 150, 300, 600, 900 seconds). It is mandatory to select one of these values for DIT longer than 150 seconds. The choice of the DIT should also take into account the possible detector persistence effects (please check Table 2 )
Magnitude limits for natural guide stars and targets
Note (a): Stars brighter than R-band ~ 2mag cannot be used as AO reference because they would exceed the 10^6 ADU saturation limit for the APDs.
Note (B): Observations using an AO reference star fainter than R-band ~ 14mag (down to R~17) are possible only under tight weather condition (Clear/seeing < 0.6").
Note (c): Observations using a Tip-Tilt star as faint as R~18 are possible under very tight weather constraints but the correction will be very poor.
The SPIFFI detector has a persistence effect, even after being illuminated below the saturation level (typically ~ 10 000 ADUs), that can last for many hours if the observed sources are too bright. In Service Mode, this problem can affect subsequent observations of other programs. To exclude any risk of artifacts produced by wavelength-dependent detector persistence, given the magnitude of your target and the requested seeing conditions, the DIT must be selected checking that the predicted fluxes do not exceed the values (ADUs/DIT/pixel) listed in the table below.
Observations of point-source targets brighter than J/H/K/-band = 5mag or (H+K)-band = 6 mag are therefore not allowed in Service Mode, except if acquisition is performed via SINFONI_IFS_acq_NGSfast, and if the 25mas scale is used for the science template. Observation of such bright targets requires the submission of a Phase 2 Waiver Request.
Angular Size of the AO Reference Object
The WFS FOV is 3.6" on the sky. Therefore, the angular extent of the AO reference source should be much smaller than this. If you use an extended object as AO reference source (i.e. galaxy nucleus) then make sure that at visible wavelength it has a very contrasty core (i.e. nearly point-like).
Telescope guide star
For any NGS fainter than 11 magnitudes it is mandatory that the telescope guide star coordinates are given by the Users (in the acquisition template: Telescope Guide Star Selection == SETUPFILE). The reason for this is that inaccuracies (~1") in the telescope and/or NGS coordinates cause the target to fall off the small field of view of SINFONI.