LEGEND OF TABLE 1 TO 4

INDEX

Miscellaneous information on IC2391

The raw data can be downloaded from the UVES ESO archive using program ID 266.D-5655(A).

Cluster members were selected with the help of WEBDA, a web database for open clusters developed and maintained by Jean-Claude Mermillod, at the Institute of Astronomy of the University of Lausanne, Switzerland. In addition, the selection of pre-main sequence objects (called SHJM in the table) usedStauffer, Hartmann, Jones, McNamara, 1989, ApJ, 342, 285(paper in pdf)

The observations were performed in the period February 7-12 2001, and few hoursin March 2001.

In the table, the HD and SHJM stars are linked up withSIMBAD (when available), they are listed with increasing right ascension.SHJM stars finding charts can be found inStauffer, Hartmann, Jones, McNamara, 1989, ApJ, 342, 285(paper in pdf)

The stars called IC2391_# are not confirmed members of the cluster, very little is known about them, they were randomly chosen from the field of IC2391.

The numbering system of column ## is from Perry, C.L. & Hill, G., 1969, AJ, 74, 899.

Miscellaneous information on NGC6475

The raw data can be downloaded from theUVES ESO archive using program ID 266.D-5655(A).

Cluster members were selected with the help of WEBDA, a web database for open clusters developed and maintained by Jean-Claude Mermillod, at the Institute of Astronomy of the University of Lausanne, Switzerland. In addition, the stars called JJ were selected fromJames & Jeffries, 1997, MNRAS, 292, 252. (paper in pdf), they are linked to the paper where some physical properties can be found. Other papers may also be consulted.Gieseking, F., 1985, A&AS, 61, 75 andProsser, C.F., Stauffer, J.R., Caillaut,J.P., et al., 1995, AJ, 110, 1229.

The observations were performed in the second half of August 2001.

In the table, the HD stars have a direct link with SIMBAD, they are listed with increasing right ascension.The stars which do not have cl in column peculiarities are not confirmed members of the cluster.

The numbering system of column ## is from Koelbloed, D., 1959, Bul Astr. Inst. Netherl., 14, 265

Miscellaneous information on bright stars

The raw data can be downloaded from theUVES ESO archive using program ID 266.D-5655(A).

The bright stars are the brightest stars of the southern sky.

Miscellaneous information on field stars

The raw data can be downloaded from theUVES ESO archive using program ID 266.D-5655(A).

The stars have been selected with the help of SIMBAD, of HIPPARCOS catalogue,and various catalogues such as the 13th General Catalog of MK Spectral Classification (Buscombe 1998, originally published in: Northwestern Univ., Evanston, Illinois, ISBN 0-939160-11-3 1998).

In the table, the stars are ordered from O to M, within a spectral type in increasing value of temperature index from 0 to 9, within a temperature index in increasing value of the luminosity index from I to V.

HD Name

The name of the star is linked to SIMBAD database where it applies. Peculiar names are described at the beginning of the corresponding table.

##

For IC2391 numbering system from Perry, C.L. & Hill, G., 1969, AJ, 74, 899.
For NGC6475 numbering system from Koelbloed, D., 1959, Bul Astr. Inst. Netherl., 14, 265.

Sp. Type

Spectral Type as given by SIMBAD.When SIMBAD does not specify a complete spectral type (letter + temperature index 0-9 + luminosity index I-V), we use the spectral type given by the HD catalogue. If the spectral type given by the HD catalog is not complete, we use the spectral type given by the HR catalog. If none of these catalogs provide a complete spectral type, a putative spectral type is given followed by (?). SIMBAD gives direct links to the two catalogs.

For O stars, we used the revised classification of Maíz-Apellániz, J., Walborn N. R., Galué, H. Á., & Wei, L. H. (2003), also available online at www-int.stsci.edu/~jmaiz/GOScatalog.html.

The star HD 211998 is classified as A3V in SIMBAD, but it appears to bea G3V in Evans, Menzies & Stoy, 1957, MNRAS, 117, 534 (Thanks to Chris Evans for pointing us at this one). It might be a binary star as well according to Lambert & McWilliam, 1986, ApJ, 304, 436.

Peculiarities

Peculiarities as given by SIMBAD.In order to save space in the tables, our abbreviated notations do not follow the international nomenclature.Our abbreviations and the corresponding peculiarities are listed below in alphabetical order.

agb asymptotic giant branch star
c carbon star
ceph cepheid
cl member of a cluster
d double/multiple
el shows emission lines
ebAgl eclipsing binary of Algol type
ev ellipsoidal variable
f O star with He and NIII emission
G-CN G and CN-Band
He-s helium strong
He-w helium weak
hpm high proper motion
m magnetic
MetA metallic A Star
mp metal poor
n diffuse line
pagb post-asympotic giant branch star
pv pulsating variable
S S star
sb Spectroscopic binary
Si Eu Sr Cr Fe (or any element) Si, Eu, Sr, Cr, Fe (or any element) strong star
she shell
v used when SIMBAD defines a star as variable without specifying the variability type, otherwise we use the variability type instead of v.
list of abbreviated variability types used in the tables:
- aCVn alpha2 Canes Venatici variable
- bCep Beta Cephi variable
- BYDra BY Draconis variable
- dSct delta Scuti variable
- MirCet Mira Ceti variable
- nova nova
- rsCVn RS Canes Venatici variable
- srp Semi-Regular Pulsating variable
wr Wolf-Rayet star

V mag.

Magnitude in V Band, as given by SIMBAD. If the V magnitude is not given, the B-(B-V) magnitude is derived fromthe spectral type information. The magnitude of variable stars is indicative only.

Merged Spectrum

Final product of the reduction : this 1D-spectrum ranges from 300 nm to 1000 nm with a step of 0.015 A/pix. All individual exposures have been combined, the extinction correction and a relative flux calibration applied, and the wavelength rebinned to the heliocentric rest frame. More details on the reduction can be found in the data reduction section of the UVES POP home page.

Merged spectra are inserted into the table only after a Quality Check has been performed.

This final file is a tfits table with 3 columns : (1) the wavelengths rebinned to the heliocentric rest frame, (2) the flux of the combined spectra (on an arbitrary scale) and (3) the associated standard deviation. NB: the associate standard deviation as given by the UVES pipeline v1.2 products is not correct. The standard deviation given in (3)is the corrected value.

tfits files can be read with IRAF tables->fitsio->strfits routine.All tfits files are also provided as ascii files (text)

NB: Known IRAF problems : Header Interpretation Problem. ESO FITS files use the ESO HIERARCH FITS keyword extensions standard to all ESO telescopes. Note that IRAF treats all ESO HIERARCH header lines as COMMENT lines, i.e. IRAF and IDL cannot automatically interpret the information provided in ESO HIERARCH header lines. The problem may be solved using the tool hierarch28. Find information about this tool here

The tfits tables include a different binning for each instrumental setting.Unfortunately IRAF noao>onedspec>splot does not support multiple binning.In order to plot the merged spectra with splot, you must first transform the tfits tables into standard iraf spectra. The following procedure is one way of doing it:

Rebin the tfits table with iraf>tables>ttools>trebin(you should choose a step corresponding to the smallest binning of your spectrum, i.e. 0.0125 for the independent variable step)
Dump the binned table as a text file with iraf>tables>ttools>tdump(tdump spectrum_binned.tab > spectrum_binned.txt). The file will be large (ca. 40Mb for a complete spectrum). Edit the file by commenting out the header lines (type # at the beginning of each header line).
Read the binned spectrum with iraf>noao>onedspec>rspectext. Specify the starting wavelength value (CRVAL) and step (CDELT=0.0125).You have now a rebinned spectrum fully compliant with splot.

NB: the rebinning step is not absolutely necessary, if you wish to read your multi-binned spectrum with rspectext, use the dispersion type (dtype) interp (the program will select the binning for you), or non-linear(the program will keep the wavelength info in the header, requires more disk space).

The FITS tables available for download have a FITS header with one extension which can easily be read using the dfits command of the ESO eclipse package. (dfits -x 1 Menkar.tfits | more)

Warning: we do not check for binarity. Hence, for a given star, the merged spectrum obtained from observations taken a long time apart may have a degraded resolution or complex velocity blending between different settings.

SPI: Spectrum Preview Interface

The UVES POP Spectrum Preview Interface (SPI) allows you to plot individual stars or overplot star spectra in your favorite wavelength range.
Some regions of the spectra are affected by bad column artifacts (flag.txt), you can visualize these regions by selecting the option, Plot Bad Column Regions.Clicking on the Plot sign in table column SPIautomatically calls the UVES POP SPI and displays the full-ranges pectrum of the selected star.
If you want to plot more than one stars of IC 2391, NGC 6475, or from any other table at the same time (max. 5),click on the SPI link and type IC2391, NGC6475, bright,or field in the POP star name search box.The POP star name search box also allows you to type a list of known star names (e.g. Castor, hd 12345, ...).

304 - 388 nm (DIC1 346B)

Gzipped tar file with all individual reduced spectra (not flux calibrated) obtained with this setting. For this special setup we provide also the spectra flat fielded with deuterium lamp, obtained with the average extraction (D) and also with the optimal extraction (Do). Flat field with the deuterium lamp provides better results at shorter wavelengths. Error files are also included. Wavelength range is 303 - 388 nm. An example of the UVES Exposure Time Calculator (ETC) is given for a V=6mag A0V star. It provides a detailed description the wavelength intervals and overlaps per order.