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III/218             ELODIE archive                        (Prugniel+, 2001)

A database of high and medium-resolution stellar spectra Prugniel P., Soubiran, C. <Astron. Astrophys. 369, 1048 (2001)> =2001A&A...369.1048P
ADC_Keywords: Spectrophotometry ; Atlases ; Spectroscopy ; Populations, stellar Keywords: atlases - stars: abundances - stars: atmospheres - stars: fundamental parameters - galaxies: stellar content Abstract: We present a database of 908 stellar spectra of 709 stars in the wavelength range 410 to 680 nm obtained with the ELODIE spectrograph. The archive provides a large coverage of the space of stellar parameters: Spectral types O to M, luminosity classes V to I and metallicities [Fe/H] from -3.0 to +0.8. At the nominal resolution, R=42000, the mean signal-to-noise ratio is 150 per pixel. The spectra given at this resolution are normalized to their pseudo-continuum and are intended to serve for abundance studies, spectral classification and tests of stellar atmosphere models. A lower resolution version of the archive, R=10000, is calibrated in physical flux with a broad-band photometric precision of 2.5% and narrow-band precision of 0.5%. It is scoped for stellar population synthesis of galaxies and clusters, and for kinematical investigations of stellar systems. The archive is also distributed in FITS format through the HYPERCAT database . File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 284 908 *Spectrophotometry and atmospheric parameters table2.dat 52 21 Comparison of Lick indices ll/* 0 919 Sub-directory: low-resolution archive (R=10000) lh/* 0 908 Sub-directory: high-resolution archive (R=42000)
Note on table1.dat: For the definition of the Lick indices see Tragger et al. (1998ApJS..116....1T) and Worthey & Ottaviani (1997ApJS..111..377W)
See also: : the HYPERCAT database : the ELODIE Archive Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 5 I5 --- Num Running number in the archive 7- 16 A10 --- Name *Object identifier 17 A1 --- u_Name *[?] Uncertain name 19- 20 I2 h RAh *? Right Ascension J2000 (hours) 22- 23 I2 min RAm *? Right Ascension J2000 (minutes) 25- 28 F4.1 s RAs *? Right Ascension J2000 (seconds) 30 A1 --- DE- *? Declination J2000 (sign) 31- 32 I2 deg DEd *? Declination J2000 (degrees) 34- 35 I2 arcmin DEm *? Declination J2000 (minutes) 37- 38 I2 arcsec DEs *? Declination J2000 (seconds) 41- 50 A10 --- SpType Spectral type (from INCA) 52- 58 F7.2 km/s HRV Heliocentric radial velocity 60 I1 --- q_Flux [0,3] Quality of the flux calibration 62- 65 F4.2 --- Airm Airmass at mid-time of observation 66- 72 F7.0 K Teff Effective temperature 74- 75 I2 --- q_Teff *[-1,4] Quality flag on Teff 78- 82 F5.2 [cm/s+2] logg decimal log of surface gravity 84- 85 I2 --- q_logg *[-1,1] Quality flag on logg 86- 92 F7.2 [Sun] [Fe/H] Iron abundance relative to solar 94- 95 I2 --- q_[Fe/H] *[-1,4] Quality flag on [Fe/H] 96-102 F7.0 K TeffM Estimated effective temperature 105-109 F5.2 [cm/s+2] loggM Estimated log of surface gravity 110-116 F7.2 [Sun] [Fe/H]M Estimated [Fe/H] 117-124 F8.4 0.1nm Ca4227 Ca4227 index 125-132 F8.4 0.1nm G4300 G4300 index 133-140 F8.4 0.1nm HgamA H gamma A index 141-148 F8.4 0.1nm HgamF H gamma F index 149-156 F8.4 0.1nm Fe4383 Fe4383 index 157-164 F8.4 0.1nm Ca4455 Ca4455 index 165-172 F8.4 0.1nm Fe4531 Fe4531 index 173-180 F8.4 0.1nm Fe4668 Fe4668 index 181-188 F8.4 0.1nm Hbeta Hbeta index 189-196 F8.4 0.1nm Fe5015 Fe5015 index 197-204 F8.4 mag Mg1 Mg1 index 205-212 F8.4 mag Mg2 Mg2 index 213-220 F8.4 0.1nm Mgb Mgb index 221-228 F8.4 0.1nm Fe5270 Fe5270 index 229-236 F8.4 0.1nm Fe5335 Fe5335 index 237-244 F8.4 0.1nm Fe5406 Fe5406 index 245-252 F8.4 0.1nm Fe5709 Fe5709 index 253-260 F8.4 0.1nm Fe5782 Fe5782 index 261-268 F8.4 0.1nm NaD NaD index 269-276 F8.4 mag TiO1 TiO1 index 277-284 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 RAh, RAm, RAs, DE-, DEd, DEm, DEs: The position was extracted from SIMBAD (when the Name is accurately known), or from the FITS headers. Note on q_Teff: q_Teff=1: Poor determination -> Q_Teff=4: Excellent (see Sect. 2) 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 q_Teff=-1: Internal determination of the effective temperature Note on q_logg: q_logg=1 means that the determination of LOGG is taken from the literature (see Sect. 2). q_logg=0 means that LOGG 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 Internal determination of the surface gravity Note on q_[Fe/H]: See the definition in Sect. 2. q_[Fe/H]=1: Poor determination -> q_[Fe/H]=4: Excellent q_[Fe/H]=-1: Internal determination of [Fe/H]
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Band *Designation of the spectrophotometric band 10- 12 I3 --- Nco *Number of comparisons 17- 22 F6.3 --- Ave *Average value of the index 27- 32 F6.3 --- Diff *Mean difference 37- 42 F6.3 --- rms rms of the difference after 3σ clipping 46- 52 F7.4 --- error *Majorant of relative error
Note on Band: The designation is as in table1.dat Note on Ave: Average value of the measurements used for the comparison. Note on Nco: A (non-iterated) 3-sigma clipping was done. Nco is the number of comparisons left afterward. Note on Diff: The units are in the "natural" units of the corresponding index, 0.1nm or mag. "Molecular" indices: Mg1, Mg2, TiO1, TiO2 and in mag, the others in 0.1nm. Note on error: The mean difference Diff is converted into relative error by assuming that the error is concentrated on the central band of the index
Description of files: ll/0*.fits -------------------------------------------------------------------------------- The 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 files: lh/0*.fits -------------------------------------------------------------------------------- High-resolution archive (R=42000) The structure of the files is similar to ll/0*.fits. 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 files: ll/99*.fits -------------------------------------------------------------------------------- These files are primarly 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 additional help. ll/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. ll/99002 Correction to the TACOS blaze (ll/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 ll/99001 and the continuum of each order is modelled with a degree 2 polynomial. ll/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. ll/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 ll/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). ll/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). ll/99004 is obtained after a comparison between the instrumental fluxes and templates from the datasets L1985BURN L1998GLUS and L1997ALEK ll/99005 Smoothed flux calibration file Each line of ll/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 ll/99006 Secondary flux calibration. ll/99005 with correction after pairwyse comparisons ll/99007 Corrected flux calibration file The spectra calibrated in physical flux with ll/99005 are compared with spectra from L1984JACO L1996SERO L96111KP1. The details of these comparison are given in ll/99007. The mean comparison is smoothed and used to compute a correction to the instrumental response. ll/99006 serves to compute the final flux calibration relations associated to each spectrum in the archive. ll/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. ll/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. ll/99011 Internal TGM model Same format as ll/99009 but the coefficient are fitted on the whole archive using the atmospheric parameters obtained from a fit to ll/99010. Acknowledgements: Philippe Prugniel
(End) Philippe Prugniel, Patricia Bauer [CDS] 19-Jan-2001
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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