README web version of /home/usg/OPS/MTS/readme_xml/readme_75024600
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
The pre-main sequence Herbig Ae/Be stars (HAeBes) exhibit conspicuous
signs of intense winds and activity. We will observe HAeBes in the young open clusters
NGC 6383 and NGC 6530 spaning a range in age of a few Myr. This allows to measure
accurately their activity level and mass-loss rates, along with their fundamental
stellar parameters (age, mass, rotation, etc...).
To undertake this program efficiently, high S/N ratio (S/N~100 at 5200 AA) is mandatory
for the determination of the photospheric parameters, due to the weakness of the
lines that must be used. Similarly, S/N~100 are needed for lines tracing the winds
and activity, because some important features, e.g. small absorption or emission
components bearing valuable information about the stellar structure, are not stronger
than a few percents of the continuum.
The magnitude of the VLT Guide Star of NGC 6383 is V= 12.60
The magnitudes of the Fiducial Stars of NGC 6383 are V= 11.26, 12,80, 11.10, 12.53
The magnitude of the VLT Guide Star of NGC 6530 is V= 12.41
The magnitudes of the Fiducial Stars of NGC 6530 are V= 11.59, 11.93, 12.49, 12.96
Waiver Requests
Critical Observing Condition Constraints
Time-Critical Aspects
Most Herbig Ae/Be stars are spectroscopic and photometric variables, with
periods of a few days. For this reason, the OBs corresponding to each cluster (3
OBs each, for NGC 6530 and NGC 6383) should be performed one after the other (i.e.
in a sequence), the same night. Nevertheless, in case of changing weather conditions
over a night, spreading the 3 OBs over 2 (or 3 nights at most) is acceptable.
Special Execution Requirements
Most Herbig Ae/Be stars are spectroscopic and photometric variables, with
periods of a few days. For this reason, the OBs corresponding to each cluster (3
OBs each for NGC 6530 and NGC 6383) should be performed in a raw the same night.
Nevertheless, in case of changing weather conditions over a night, spreading the
3 OBs over 2 or 3 nights (at most) is acceptable.
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 specify in your OBs the hour angle range for which your Target
Setup files are valid ?
Did you specify in your OBs the magnitudes of FACBs and Guide Star for
all your fields ?
Are the FACBs and Guide Star in the brightness ranges specified in the
FLAMES manual ?
Did you enter the expected signal to noise in your OBs ?
Last creation of page: Tue Oct 6 15:40:07 2009
If you have comments, please contact usd-help@eso.org