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III/251             ELODIE library V3.1         (Prugniel+ 2007)

New release of the ELODIE library: Version 3.1 Prugniel P., Soubiran C, Koleva M., Le Borgne D. <astro-ph/0703658 (2007)> =astro-ph/0703658
ADC_Keywords: Spectrophotometry ; Atlases ; Spectroscopy ; Populations, stellar Keywords: atlases - stars: abundances - stars: atmospheres - stars: fundamental parameters - galaxies: stellar content Description: ELODIE.3.1 is an updated release of the library published in Prugniel & Soubiran (2001A&A...369.1048P, Cat. III/218; and 2004 version, in astro-ph/0409214). The library includes 1959 spectra of 1388 stars obtained with the ELODIE spectrograph at the Observatoire de Haute-Provence 193cm telescope in the wavelength range 390 to 680 nm. It provides a wide coverage of atmospheric parameters: Teff from 3100K to 50000K, logg from -0.25 to 4.9 and [Fe/H] from -3 to +1. The library is given at two resolutions: R around 42000, with the flux normalized to the pseudo-continuum. A lower resolution version of the spectra (R around 10000), is calibrated in physical flux (reduced above earth atmosphere) with a broad-band photometric precision of 2.5% and narrow-band precision of 0.5%. In this new release the data-reduction (flux calibration, reconnection of the echelle orders) has been improved, and in particular the blue region, between 390 and 400nm has been added. The FITS files for each spectra, and the measured atmospheric parameters are publicly available. See the ELODIE.3.1 page for more details: http://www.obs.u-bordeaux1.fr/m2a/soubiran/elodie library.html File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 264 1959 List of spectra (several lines exist for stars observed several times) lh/* 0 1959 *High-resolution FITS spectra ll/* 0 1959 *Low-resolution calibrated FITS spectra ll99/* 0 12 *Pipeline processing files
Note on lh/*: see the "Description of the lh/0*.fits files" section below. Note on ll/*: see the "Description of the ll/0*.fits files" section below. Note on ll99/*: see the "Description of the ll99 files" section below.
See also: http://www.obs.u-bordeaux1.fr/m2a/soubiran/elodie_library.html : ELODIE home page. Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 5 I05 --- Num Running number in the archive 7- 16 A10 --- Name *Object identifier 17 A1 --- u_Name *[?] when name is uncertain 19- 28 A10 --- SpType MK Spectral type 30- 36 F7.2 km/s Vr Heliocentric radial velocity 38 I1 --- qF [0,3] Quality of flux calibration (3=good) 40- 43 F4.2 --- Airm Airmass at mid-time of observation 44- 50 F7.0 K Teff Effective temperature 52- 53 I2 --- q_Teff *[-1,4] Quality flag on Teff 55- 60 F6.2 [cm/s+2] logg decimal log of surface gravity 62- 63 I2 --- q_logg *[-1,1] Quality flag on logg 65- 70 F6.2 [Sun] [Fe/H] Iron abundance relative to solar 72- 73 I2 --- q_[Fe/H] *[-1,4] Quality flag on [Fe/H] 74- 80 F7.0 K TeffM Estimated effective temperature 82- 87 F6.2 [cm/s+2] loggM Estimated log of surface gravity 89- 94 F6.2 [Sun] [Fe/H]M Estimated [Fe/H] 96 I1 --- Int *[0,3] Interpolator flag 97-104 F8.4 0.1nm Ca4227 Ca4227 index 105-112 F8.4 0.1nm G4300 G4300 index 113-120 F8.4 0.1nm HgamA H gamma A index 121-128 F8.4 0.1nm HgamF H gamma F index 129-136 F8.4 0.1nm Fe4383 Fe4383 index 137-144 F8.4 0.1nm Ca4455 Ca4455 index 145-152 F8.4 0.1nm Fe4531 Fe4531 index 153-160 F8.4 0.1nm Fe4668 Fe4668 index 161-168 F8.4 0.1nm Hbeta Hbeta index 169-176 F8.4 0.1nm Fe5015 Fe5015 index 177-184 F8.4 mag Mg1 Mg1 index 185-192 F8.4 mag Mg2 Mg2 index 193-200 F8.4 0.1nm Mgb Mgb index 201-208 F8.4 0.1nm Fe5270 Fe5270 index 209-216 F8.4 0.1nm Fe5335 Fe5335 index 217-224 F8.4 0.1nm Fe5406 Fe5406 index 225-232 F8.4 0.1nm Fe5709 Fe5709 index 233-240 F8.4 0.1nm Fe5782 Fe5782 index 241-248 F8.4 0.1nm NaD NaD index 249-256 F8.4 mag TiO1 TiO1 index 257-264 F8.4 mag TiO2 TiO2 index
Note on Name, u_Name: The names are generally from the HD catalogue (III/135), BD numbers (I/122) are also used. Uncertain identification are noted with a "?" in column u_Name. Note on q_Teff: The quality varies from 1 (poor determination) to 4 (excellent). The special value q_Teff=0 means that we have estimated Teff from the B-V colour (Tycho2 I/259 catalogue), assuming the empirical colour-temperature relation for a main sequence star and neglecting the interstellar extinction; and q_Teff=-1 means an internal determination of the effective temperature. Note on q_logg: (see section 2 of paper) -- q_logg=1 means that the determination of log.g is taken from the literature -- q_logg=0 means that log.g was converted from the V absolute magnitude from Hiparcos and Teff, using a bolometric correction valid for a main sequence start and an empirical mass-to-light relation. -- q_logg=-1 means an internal determination of the surface gravity Note on q_[Fe/H]: (see section 2 of paper) -- values from 1 (poor determination to 4 (excellent) -- q_[Fe/H]=-1 means an internal determination of [Fe/H] Note on Int: Interpolator flags are numbered as follows: flag = 0 - Normal spectrum used for computing interpolator flag = 1 - Spectrum ignored in the model fit (Absolute and Internal) flag = 2 - Spectrum has half weight in A model flag = 3 - Input T G Z ignored (spectrum only used for I model)
Description of the ll/0*.fits files: -------------------------------------------------------------------------------- Low-resolution archive (R=10000) The FITS files have one axis which is the wavelength (CTYPE1='WAVE-WAV'), scaled in units of 0.1nm (CUNIT='10**(-10)m'), with a step of 0.02nm. They contain 2 image-type extensions. The primary extension gives the fluxes (BTYPE='FLUX-PHY') above the atmosphere and normalized to continuum. The other image-type extension contains the corresponding detector noise, its EXTAME is 'NOISE'. Two other extensions contain the flux calibration relations (FCR) needed to convert the instrumental flux (BTYPE='FLUX-INS') into physical flux (ie. above atmosphere) (BTYPE='FLUX-PHY') and into continuum- normalized flux (BTYPE='FLUX-NOR'). The EXTNAME of these FCR are respectively 'FCANOR' and 'FCAPHY'. Explanations about the content of the FCR can be found in the documentation of Pleinpot available from Hypercat. The processing pipeline in the FITS archive of Hypercat allows the different conversions. Description of some particular keywords: TEFF [K] Teff from literature Q_TEFF Quality flag for Teff: 4=excellent LOGG [log cm/s**2)] log g from literature Q_LOGG Quality flag for LOGG [Fe/H] [Sun] [Fe/H] from literature Q_[Fe/H] Quality flag for [Fe/H]: 4=excellent MV [mag] Mv from Hipparcos Q_MV Quality flag for Mv: 4=excellent S/N S/N-per-pixel of original spectrum at 555 nm VR [km/s] heliocentric radial velocity FWHM [km/s] FWHM line broadening Q_VR comment on Vr determination SPTYPE spectral type from INCA VMAG [mag] V-magnitude E_VMAG [mag] error on V-magnitude B-V [mag] B-V Johnson R_PHOT Source of photometry: TYCHO2, INCA H_WRESOL [0.1nm] FWHM wavelength resolution at 550 nm Description of the lh/0*.fits files: -------------------------------------------------------------------------------- High-resolution archive (R=42000) The structure of the files is similar to ll/0*.fits (see the "Description of the ll/0* fits files"(?) section above). The main differences are that the sampling is 0.005nm and that the fluxes are normalized to the pseudo-continuum (BTYPE='FLUX-NOR') Description of the ll99 files: -------------------------------------------------------------------------------- These files are primarily intended to be used by the specialized reduction programs and by the pipeline processing. Their description may not be accurate enough for a standalone usage, and for such applications the users are invited to contact the authors for additional help. ll99/99001 Blaze function used as reference This is a "s2d" file produced by the ELODIE reduction program (TACOS). "s2d" means: spectra extracted by TACOS, each line is one order. The Blaze function is obtained from a Tungsten lamp spectrum. Each order is smoothed using a degree 17 polynomial and is normalized to its maximum value. ll99/99002 Correction to the TACOS blaze (ll99/99001) Dividing a spectrum by a TACOS blaze produces a stair case result (consecutive orders do not connect because of the independent normalizations). In order to connect the orders and to reduce the instrumental response to a "typical" stellar SED, we computed this correction using 3 metal-deficient stars observed during the same observing run. The original "s2d" spectra are divided by ll99/99001 and the continuum of each order is modelled with a degree 2 polynomial. ll99/99003 Pseudo-continuum mask It is computed after the whole archive has been reduced. In each continuum-normalized spectrum, a simple threshold is used to diagnostic if a given wavelength point belong to the pseudo-continuum. We chose 0.97 as threshold. The corresponding wavelength point is given the value 1 or 0 if it belongs respectively to the continuum or not. ll99/99003 is the average of this mask over the whole archive. In some sense it indicates the probability for each wavelength point to be a continuum point. It is used as a weight for iterating the computation of ll99/99002 and of the whole archive. (determining the continuum is required to fit and correct variations of the blaze, see the text of the article). ll99/99004 Primary flux calibration. The first axis is the wavelength direction The first line is the instrumental response, The second the airmass dependence and the third the "haze" dependence (see text). ll99/99004 is obtained after a comparison between the instrumental fluxes and templates from the datasets L1985BURN L1998GLUS and L1997ALEK ll99/99005 Smoothed flux calibration file Each line of ll99/99004 is modeled by a degree 17 polynomial in order to discard the wavy residuals due to an approximate modeling of the spectral resolution of the templates ll99/99006 Secondary flux calibration. ll99/99005 with correction after pairwise comparisons ll99/99007 Corrected flux calibration file The spectra calibrated in physical flux with ll99/99005 are compared with spectra from L1984JACO L1996SERO L96111KP1. The details of these comparison are given in ll99/99007. The mean comparison is smoothed and used to compute a correction to the instrumental response. ll99/99006 serves to compute the final flux calibration relations associated to each spectrum in the archive. ll99/99008 Comparison with other templates. The first axis is the wavelength direction. The 9 first lines contains respectively the comparisons with (1) L96111KP1 (Jone's library, red band), (2) L96111KP2 (Jone's library, blue band), (3) L1996SERO (OHP observations), (4) L1996SERO (CFH observations), (5) L1984JACO (Jacoby's library) (6) L1987KIEH (Kiehling, 1987, Cat. III/124) (7) L1994DANK (Danks & Dennefeld, 1994PASP..106..382D) (8) L1983GUNN (Gunn & Stryker, 1983, Cat. III/88 ) and (9) L1984NSOA (Solar flux atlas). The 10th line combines the first 9 lines. And the 11th is the final correction obtained by smoothing the 10th. ll99/99010 Absolute TGM model The first axis is the wavelength direction. The second axis contains the 20 parameters of the TGM model fitted to the spectra for which the atmospheric parameters are known. The functions of the models are: 1 Cst 2 T 3 Z 4 G 5 T**2 6 T**3 7 T**4 8 T*Z 9 T*G 10 G**2 11 Z**2 12 T**2*G 13 T**2*Z 14 G**3 15 Z**3 16 T*G**2 17 T*Z**2 18 10**T 19 10**(T*2) 20 G*Z If Teff is the effective temperature, log(G) the decimal logarithm of the surface gravity, T and G are defined as: T=log(Teff)-3.7 and G=log(G)-4.44. Z is [Fe/H]. Each wavelength point is fitted to the 20 functions above and each line in 99010 are the coefficients of these functions. This is a preliminary model and the final version will be described in the paper presenting TGMET. ll99/99011 Internal TGM model Same format as ll99/99009 but the coefficient are fitted on the whole archive using the atmospheric parameters obtained from a fit to ll99/99010. Contact: Philippe Prugniel, obs.univ-lyon1.fr
(End) Philippe Prugniel, Francois Ochsenbein [CDS] 12-Apr-2007
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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