README web version of /home/usg/OPS/MTS/readme_xml/readme_83063801
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
In this run we take high-res spectra of common proper motion pairs composed
of G-K dwarf primaries and M dwarf secondaries. In addition we also take the solar
spectrum reflected from the asteroid 3 Juno and the spectrum of a solar twin (HIP79672).
All observations are done with the UVES red arm centred at 860 nm, and the highest
resolution achievable (image slicer-3, slit 0.3 arcsec).
With the exception of the asteroid 3 Juno, for all our science targets we link each
OB to the OB of a telluric standard with similar coordinates, to ensure both science
and telluric stars will be observed at similar airmasses and close in time.
The S/N reported in the Instrument Comments is that expected from one exposure,
computed with the UVES Exposure Time Calculator for the requested configuration,
adopting a spectral template representative of our target and assuming a typical
seeing of 1 arcsec. For the brightest targets (i.e. the tellurics) we have checked
that there is no saturation even with considerable better seeing (0.5 arcsec). We
expect the exposure times computed with the Exposure Time Calculator to be rather
reliable, however if weather/seeing conditions should considerably differ from those
we have assumed in our computation, please optimize the exposure time.
In particular, for the telluric standards we usually ask for two or more exposures
to ensure we reach a good S/N in the extreme red and to avoid saturation at shorter
wavelength where these stars emit most of their flux. Please avoid saturation or
the opposite, underexposure of the red part.
For the asteroid 3 Juno we have attached the ephemeris file, in time-steps of 1
day for the entire period 83A. We can provide ephemeris with smaller time-steps
when a likely period for observing the asteroid with UVES will be scheduled. The
coordinates given in the observing block (MOV_JUNO) refers to the middle of period
83A, i.e. July 1st 2009. Also, the V magnitude of the asteroid during the entire
period 83A will vary from approximately 10.5 to 8. It is obviously very difficult
to tailor the exposure time and the number of exposures, but we have reserved a
rather long OB for such object, so if needed, please optimize/change the exposure
time we have indicated so as to achieve the best S/N.
Waiver Requests
A waiver request (submitted at 13:53:52 27 January 2009) has been approved
to change the central wavelength of the UVES red arm from 600nm (standard setting,
with image slicer-3) to 860nm (standard setting, with image slicer-3) for all our
observations.
A waiver request (submitted at 14:45:37 27 January 2009) has been approved to replace
the targets NLTT49961 and NLTT49963 with NLTT43097 and G17-27.
A waiver request (submitted at 18:56:05 29 January 2009) has been approved to add
the two following targets: asteroid 3 Juno and HIP79672.
Critical Observing Condition Constraints
Time-Critical Aspects
Ideally the observation of the telluric standards should be done at the
same (or as close as possible) airmass of the science targets. Since it is not know
the exact date and time when observations will be carried, it is impossible to decide
beforehand which order, i.e. science--telluric target or telluric--science target,
would be better.
If possible, when the observations will be executed, please optimize the order in
which observe the two targets so as to ensure that both science and telluric stars
will be observed at very similar airmasses.
Special Execution Requirements
We request to observe common proper motion pairs composed of G-K dwarf
primaries and M dwarf secondaries. The metallicity measured in the primaries will
be used to calibrate that measured in the M dwarf secondaries. Therefore it is important
that if an M dwarf is observed, also its primary is.
Whereas the primaries are rather bright and one OB is enough, all the M dwarfs are
rather faints and the observations are split in various nights. Before completing
all the nights for a given M dwarfs, please complete also the OB of the corresponding
primary. Namely:
1) before the OB G17-27 Night2 is done, please do the OB NLTT43097
2) before all the OBs for NLTT51082 are done, please do the OB for NLTT51085
2) before all the OBs for NLTT54930 are done, please do the OB for NLTT54927
Special Calibration Information
Each OB containing a science target must be linked to the corresponding
OB containing a telluric standard star. In all cases, we have verified that the
two observing blocks linked together (science target + telluric) never exceed 1
hour, including overheads. The only target for which we do not request a telluric
calibration is the asteroid 3 Juno (MOV_Juno).
We have specified in User Comments and Calibration Requirements of each OB which
is the name of the corresponding OB containing the telluric star. We have adopted
the following convention to indicate that two OBs must be linked together: e.g.
NLTT54930 Night 3 is the name of the OB containing the science target NLTT54930
and it must be linked to the OB named
CAL_NLTT54930 Night3 which contains the telluric star.
In the User Comments of each CAL_ observing block we give the V magnitude and the
spectral type of the telluric. For tellurics we usually ask two or more exposures
to ensure we reach a good S/N in the extreme red and to avoid saturation at shorter
wavelength where these stars emit most of their flux. Some of the tellurics are
very bright and we have computed the exposure time using the UVES Exposure Time
Calculator, assuming a typical seeing of 1 arcsec. We have checked that even with
better seeing (0.5 arcsec) there should be no risk of saturation, but please, depending
on the seeing and/or weather conditions avoid saturation or the opposite, under-exposure
of the red part.
ToO Information
ToO Activators List
Do all your OBs comply with the instrument-specific requirements listed
on the instrument-specific Phase 2 web page ?
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 specified the S/N ratio at given wavelength in the User Comments
field of each OB?
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 ?
If you need secondary guiding, are there suitable objects within 30 arcsec
from your target ?
Last creation of page: Tue Oct 6 15:40:30 2009
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