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INDEX

• Miscellaneous information on IC2391
• Miscellaneous information on NGC6475
• Miscellaneous information on bright stars
• Miscellaneous information on field stars
• HD Name
• ##
• Sp. Type
• Peculiarities
• V mag.
• Merged Spectrum
• SPI
• DIC1 346B
• DIC2 437B
• DIC1 580L
• DIC1 580U
• DIC2 860L
• DIC2 860U
• Unmerged 2D
• dd/mm/yy
• QC

Miscellaneous information on IC2391

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) used Stauffer, Hartmann, Jones, McNamara, 1989, ApJ, 342, 285 (paper in pdf)

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

In the table, the HD and SHJM stars are linked up with SIMBAD (when available), they are listed with increasing right ascension. SHJM stars finding charts can be found in Stauffer, 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

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 from James & 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 and Prosser, 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 bright stars are the brightest stars of the southern sky.

Miscellaneous information on field stars

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

##

Sp. Type

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 be a 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

• 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.

Merged Spectrum

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.

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

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 flatfielded 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.

If all files of the setting are rejected after a quality control, the gzipped tar file is replaced by QC Reject.

If the files are of less-than-average quality they are not included in the merged final spectrum. They are still released and the link appears in red.

373 - 499 nm (DIC2 437B)

Gzipped tar file with all individual reduced spectra (not flux calibrated) obtained with this setting. Error files are also included. 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.

If all files of the setting are rejected after a quality control, the gzipped tar file is replaced by QC Reject.

If the files are of less-than-average quality they are not included in the merged final spectrum. They are still released and the link appears in red.

476 - 577 nm (DIC1 580L)

Gzipped tar file with all individual reduced spectra (not flux calibrated) obtained with this setting (lower chip). Error files are also included. 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.

If all files of the setting are rejected after a quality control, the gzipped tar file is replaced by QC Reject.

If the files are of less-than-average quality they are not included in the merged final spectrum. They are still released and the link appears in red.

584 - 684 nm (DIC1 580U)

Gzipped tar file with all individual reduced spectra (not flux calibrated) obtained with this setting (upper chip). Error files are also included. 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.

If all files of the setting are rejected after a quality control, the gzipped tar file is replaced by QC Reject.

If the files are of less-than-average quality they are not included in the merged final spectrum. They are still released and the link appears in red.

660 - 854 nm (DIC2 860L)

Gzipped tar file with all individual reduced spectra (not flux calibrated) obtained with this setting (lower chip). Error files are also included. 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.

If all files of the setting are rejected after a quality control, the gzipped tar file is replaced by QC Reject.

If the files are of less-than-average quality they are not included in the merged final spectrum. They are still released and the link appears in red.

866 - 1040 nm (DIC2 860U)

Gzipped tar file with all individual reduced spectra (not flux calibrated) obtained with this setting in the upper chip. Error files are also included. 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.

If all files of the setting are rejected after a quality control, the gzipped tar file is replaced by QC Reject.

If the files are of less-than-average quality they are not included in the merged final spectrum. They are still released and the link appears in red.

Unmerged 2D

Each order can be extracted separately from these files using the following sequence of MIDAS commands:

mer/ech    2D_unmerged.bdf    1D_unmerged.bdf    1 , { 2D_unmerged.bdf , npix(2) }    noappend

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dd/mm/yy

Date of observation. Sometimes, the two settings (DIC1 and DIC2) have been observed on different dates. The date of the observation of the setting observed first is always given unless the observations of the most recent dates represent the largest part of the data.

The date given in the column is the UT date of the beginning of the night. The precise date and time of observations for each individual spectrum can be obtained in the QC log file.

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QC

Quality Check (QC): Pipeline products are checked and the final products are briefly described in the log file. The log file is self explanatory. The Tutorial on pipeline problem describes the possible problems of UVES pipeline leading to QC rejection.

Note that even if the worst cases are rejected, the released spectra may still be affected by problems such as ripple effects (due to bad blaze function correction) and bad order merging.

For any given star, the merged spectrum is inserted into the table only after a Quality Check has been performed on the reduction products.

If all files of the setting are rejected after the quality control, the gzipped tar file is replaced by QC Reject.

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Send comments to <cabanac@cfht.hawaii.edu> Last modified: 10 December 2003, 18:00 CLST