The data products will be defined by a "Product
level" designation. The lower the number, the more basic the data
product
will be. The G refers to GIRAFFE data. All of these were reduced using
the GIRAFFE data reduction pipleine girBLDRS.
The star ID numbers will be detailed in a preliminary version of the
second
data paper to be released soon.
The GIRAFFE observations of the SMC clusters had exposure times of 6x2275s per wavelength order, although in
some cases
there are more than 6 observations due to deterioration of sky
conditions and
hence repeat observations to match our constraints (6 central
wavelengths).
Details
of stars and IDs from Evans et al. (2006) ; but note erratum Evans
et
al. (2007)
Finding chart available (fchart_346.eps).
Product level |
Details |
Format |
Download |
No. Spectra |
Released |
|
G0 |
Individual orders, single exposures, no sky subtraction (tarballs are 16-25MB) |
ASCII |
NGC346.3958.G0.V1.ascii.tar.gz |
678 per tarfile |
20041104 |
|
G1 |
Individual orders, single exposures, sky subtracted (tarballs are 16-25MB) . Note that these are the 2nd version release of the sky subtracted spectra. The sky subtraction is more robust, and these spectra should be used in preference to the previous vesion, V1. |
NGC346.3958.G1.V2.ascii.tar.gz |
678 per tarfile |
20060624 |
|
|
G2 |
Co-added spectra merged together (20MB) IMPORTANT - SEE NOTE BELOW |
ASCII |
113 |
20041104 |
|
|
G3 |
Normalised orders, merged together (20MB) IMPORTANT - SEE NOTE BELOW |
ASCII |
113 |
20041104 |
Details
of stars and IDs from Evans et al. (2006) ; but note erratum Evans
et
al. (2007)
Finding chart available (fchart_330.eps).
Product level |
Details |
Format |
Download |
No. Spectra |
Released |
|
G0 |
Individual orders, single exposures, no sky subtraction (tarballs are 16-33MB) |
ASCII |
NGC330.3958.G0.V1.ascii.tar.gz |
regions where observed between 6-9 times, hence between 690-1035 spectra in each tarball |
20051124 |
|
G1 |
Individual orders, single exposures, sky subtracted (tarballs are 16-25MB). Note that these are the 2nd version release of the sky subtracted spectra. The sky subtraction is more robust, and these spectra should be used in preference to the previous vesion, V1. |
NGC330.3958.G1.V2.ascii.tar.gz |
regions where observed between 6-9 times, hence between 690-1035 spectra in each tarball |
20060624 |
|
|
G2 |
Co-added spectra merged together (20MB) IMPORTANT - SEE NOTE BELOW |
ASCII |
115 |
20050212 |
|
|
G3 |
Normalised orders, merged together (20MB) IMPORTANT - SEE NOTE BELOW |
ASCII |
|
|
|
|
UVES |
UVES spectra of an extra 5 stars â observed with UVES during a different observing campaign by Danny Lennon (contact I. Hunter for more details of the particular stars) |
ASCII |
5 stars |
20060726 |
Notes
The NGC330 wavelength region centred on
4124 was
re-observed in July 2005 due to quality problems with the first
attempt. Both
sets of
spectra are available in the above table, best to use the JUL05
versions. In
these spectra there was light contamination from
an
unknown sources at the red end of a small portion of the CCD.
Thus bright
patch filters through to some of the spectra as a sharp rise at the redward end but it's not a major problem and
rectifies out
fairly easily for most of the stars. In NGC330 star
#105
is deliberately missing in the July 2005 spectra. The fibre
has hot pixel problems which destroyed extraction and sky subtraction
etc.
ALL of the ascii spectra have been correcrted to the heliocentric velocity frame
When the tar files are unpacked, the individual spectra files will be
labeled
cluster_wavelength_exposure_level_date_version.idnumber.fits : where exposure=exposure
number
(1-6), date=date of reduction, version=incremental
number to
allow re-release of corrected data, idnumber=running
ID number in each field.
Example: NGC346_3958_01_G0_20040101_v01.099.fits is NGC346
lambda_central=3958, exposure 01
(of 6),
Level=G0, date reduced= 20040101, version=v01,
Star ID
number=99
If there are any corrections in the reductions, then a full release of
these
files will be done, with a note as to what has changed, and the version
number
will increment.
The co-added spectra are simple sums of the sky-subtracted orders,
which have
not been checked for binarity. They are
meant to be
used as a first-look data product but should not be used for science
purposes
before the individual exposures have been checked for radial velocity
variability. They are also based on the V1 sky subtraction which� has been improved
and released as V2.
When consortia members do produce Vrad
checked and
corrected spectra, email me and I will make them available in the
archive as a
Level 4 product.