J/A+A/442/1127 Library of 2500-10500Å synthetic spectra (Munari+, 2005)
An extensive library of 2500-10500 A synthetic spectra.
Munari U., Sordo R., Castelli F., Zwitter T.
<Astron. Astrophys., 442, 1127-1134 (2005)>
=2005A&A...442.1127M 2005A&A...442.1127M (SIMBAD/NED BibCode)
ADC_Keywords: Atlases ; Spectroscopy
Keywords: astronomical data bases: miscellaneous - stars: atmospheres -
stars: fundamental parameters - surveys
Abstract:
We present a complete library of synthetic spectra based on Kurucz's
codes that covers the 2500-10500Å wavelength range at resolving
powers RP=20000, 11500 (=GAIA), 8500 (=RAVE), 2000 (=SLOAN) and
uniform dispersions of 1 and 10 Å/pix. The library maps the whole
HR diagram, exploring 51288 combinations of atmospheric parameters
spanning the ranges: 3500≤Teff≤47500K, 0.0≤logg≤5.0,
-2.5≤[M/H]≤0.5, [α/Fe]=0.0,+0.4, ξ=1, 2, 4km/s,
0≤Vrot≤500km/s. The spectra are available both as absolute fluxes
as well as continuum normalized. Performance tests and spectroscopic
applications of the library are discussed, including automatic
classification of data from spectroscopic surveys like RAVE, SLOAN,
GAIA. The entire library of synthetic spectra is accessible via the
web.
Description:
The spectra in our library covers from 2500 to 10 500Å and were
calculated at a resolving power RP=λ/Δλ=500000
and then degraded by Gaussian convolution to lower resolving powers
and properly re-sampled to the Nyquist criterion (the FWHM of the PSF
being 2 pixels), to limit the data volume and therefore facilitate the
distribution.
The highest resolving power for our library is RP=20000, which is
typical of moderately high resolution Echelle observations, such as
the spectral database of real stars of Munari & Tomasella (1999, Cat.
J/A+AS/137/521) and Marrese et al. (2003, Cat. J/A+A/406/995). The
library is also provided at the resolving powers of the SLOAN survey
RP=2000 (York et al., 2000AJ....120.1579Y 2000AJ....120.1579Y), of the RAVE survey
RP=8500 (Steinmetz, 2003, ASP Conf. Ser. 298, 381, Munari et al.,
2005, ESA SP-576, 529 ) and of the Gaia space mission RP=11500 (Katz
et al., 2004MNRAS.354.1223K 2004MNRAS.354.1223K, Wilkinson et al., 2005MNRAS.359.1306W 2005MNRAS.359.1306W).
The present library is also made available at the uniform dispersions
of 1 and 10Å/pix (again with the FWHM of the PSF being 2 pixels).
The latter two are intended to be of assistance in classification of
medium and low resolution grating spectra obtained in single
dispersion mode (as with conventional B&C spectrographs or EFOSC-like
imager/spectrographs).
Each spectrum is provided for a range of rotational velocities, as
detailed in Table 1, spanning 14 values between 0 and 500km/s for
stars hotter than 6000K and 11 values between 0 and 100km/s for
cooler ones.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 64 6 List of resolving power/dispersion directories
disp1A/* . 3 Uniform dispersion: 1Å/pix
disp10A/* . 3 Uniform dispersion: 10Å/pix
sloan2000/* . 3 Resolving power 2000 SLOAN
rp8500/* . 3 Resolving power 8500
rp11500/* . 3 Resolving power 11500
rp20000/* . 3 Resolving power 20000
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See also:
http://archives.pd.astro.it/2500-10500 : the spectral 2500-10500Å library
Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Mod Name of the resolving power/dispersion directory (1)
12- 15 A4 --- Size Size of the directory
17- 30 A14 --- Wave Name of the file with wavelengths (2)
32- 45 A14 --- FS [fluxed_spectra] Name of the subdirectory with
fluxed spectrum files (3)
47- 64 A18 --- NS [normalized_spectra] Name of the subdirectory
with normalized spectrum files (3)
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Note (1): Each directory contains the wavelength file, and the 59 Teff
subdirectories, T_03500 to T_47500.
Note (2): To have the classic double-column spectrum file (wavelengths, flux),
use "paste wavelengths_file flux_file > spectrum.txt"
Note (3): Naming scheme for the spectra contained in the library.
TtttttGggMmmVvvvK2AnnNVRRRF.ASC (example: T04000G45M05V015K2ANWNVR20F.ASC)
characters meaning
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1- 6 Tttttt Effective temperature (K)
(03500 03750 04000 04250 04500 04750 05000 05250 05500
05750 06000 06250 06500 06750 07000 07250 07500 07750
08000 08250 08500 08750 09000 09250 09500 09750 10000
10500 11000 11500 12000 13000 14000 15000 16000 17000
18000 19000 20000 21000 22000 23000 24000 25000 26000
27000 28000 29000 30000 31000 32000 33000 34000 35000
37500 40000 42500 45000 47500)
7- 9 Ggg 10xlogg (cgs units)
(logg = 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.5, 4.0, 4.5, 5.0)
10 M [-+] sign for metallicity: M = "-" P = "+"
11-12 mm 10x[M/H] ([M/H] = -2.5, -2.0, -1.5, -1.0, -0.5, +0.0, +0.5)
13-16 Vvvv rotational velocity (km/s)
(Vrot = 0, 10, 20, 30, 40, 50, 60, 75, 100, 150, 200,
250, 300, 400, 500)
17-18 K2 Microturbulent velocity (km/s), always 2km/s
19 A [α/Fe] enhancement: S=0.0, A=+0.4
20-21 nn NW = new ODF models, OD = old ODF models
22-23 NV no overshooting (always NV)
24-26 RRR Resolving power or dispersion
R20 = resolving power 20000;
RVS = resolving power 11500 (GAIA);
RAV = resolving power 8500 (RAVE);
SLN = resolving power 2000 (SLOAN);
D01 = 1Å/pix dispersion;
D10 = 10Å/pix dispersion
27 F [F/N] F = fluxed spectrum (erg/cm2/s/Å)
in subdirectory fluxed_spectra
or N = normalized spectrum
in subdirectory normalized_spectra
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Acknowledgements:
Ulisee Munari, munari(at)pd.astro.it
(End) Patricia Vannier [CDS] 30-Aug-2016