README web version of /home/usg/OPS/MTS/readme_xml/readme_79058700
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
This program is devoted to the study of the variable star population
of the newly discovered dwarf spheroidal (dSph) galaxy Hercules,
through acquisition of BVI time series photometry covering the entire
body of the galaxy. In particular we aim at discovering RR Lyrae
variables which are expected to be present in Hercules based on the
morfology of the galaxy CMD. The FOV of the WFI@2.2m allows to fully
image the Hercules dSph in just one exposure. For this reason the same
finding chart holds for all OBs. We have attached this same finding
chart to each individual OB without reporting on it the name of
the specific OB which is related to. Exposures of the time-series are to
be taken at fixed pointing with NO dither, since dithering disturbs
the image subtraction that we will to use to identify the variable
stars. The program consists of a total of 42 OBs distributed as
follows: 5 VIBV OBs, 37 BV OBs.
Waiver Requests
Critical Observing Condition Constraints
The program does not require photometric conditions. We can tolerate a
moon illumination up to 0.5, seeing of 1.5 arcsec, airmass up to 1.8
and CLEAR conditions. However, in order to perform the photometric
calibration we require that the 4 OBs named: her_vibv_1; her_vibv_2;
her_bv_1; her_bv_2 are executed in photometric conditions. These OBs
should possibly be executed in DIFFERENT photometric nights to make
sure that we catch at least 1-2 truly photometric nights.
Time-Critical Aspects
In order to better determine the periods of the variables, it would be
important to observe at least 4-5 OBs during the April "window". If in
April photometric conditions will be present, it would be desiderable
that the aforementioned "photometric" OBs were observed during that
"window". However, we do not put any firm constrain on this point,
since we do not want to wait for the first photometric night to start
the observations!
In general, in order to better sample the variable star light curves,
it would be desiderable to have the OBs spread over a number of nights
as large as possible. In particular, the best observing strategy for
us would be the execution of 2-3 OBs during the same night and spaced
in time by at least 1 hr. Should this cause too many complications in
the scheduling, OBs can also be executed consecutively.
Special Execution Requirements
Special Calibration Information
ToO Information
ToO Activators List
Is this a Pre-imaging run ?
Pre-imaging Requirements
Source(s) of Pre-imaging
Pre-imaging sources not listed above
Do all your OBs comply with the instrument-specific requirements listed
on the instrument-specific Phase 2 web page ?
If this is a pre-imaging run, did you select PRE-IMAGING for the Observing
Category for each Observing Template ?
Do all your finding charts comply with both the general and instrument-specific
Phase 2 Web Pages ?
If you submitted OBs for standard stars, did you specify the magnitude
and spectral type of all standard stars in the OBs ?
Have you included OBs for any calibrations that you need but which are
not part of the Calibration Plan ?
If you are observing Moving Targets, have you attached suitable ephemeris
files to your OBs?
If you have preferences which OBs should be executed first, did you make
use of the User Priority field in the OBs ?
If this is a run that requires coordinated observations with other facilities,
did you give proper instructions in the Time-Critical Aspects Section ?
Did you set 'New Preset' flag in all acquisition templates to 'True'?
Have all your submitted OBs the same filter for the acquisition template
and for the first science template?
Did you combine calibration templates with science templates for any
OB?
Did you combine imaging and spectroscopic templates for any OB?
Did you submit any Focus template?
Last creation of page: Tue Oct 6 15:40:19 2009
If you have comments, please contact usd-help@eso.org