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.
<0703658 (2007)>
=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 2001A&A...369.1048P, Cat. III/218; and 2004 version, in
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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 264 1959 List of spectra (several lines exist for
stars observed several times)
lh/* . 1959 *High-resolution FITS spectra
ll/* . 1959 *Low-resolution calibrated FITS spectra
ll99/* . 12 *Pipeline processing files
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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.
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See also:
http://www.obs.u-bordeaux1.fr/m2a/soubiran/elodie_library.html :
ELODIE home page.
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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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
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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)
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Description of the ll/0*.fits files:
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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:
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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:
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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 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