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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 (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), 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, Wilkinson et al., 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:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 64 6 List of resolving power/dispersion directories disp1A/* 0 3 Uniform dispersion: 1Å/pix disp10A/* 0 3 Uniform dispersion: 10Å/pix sloan2000/* 0 3 Resolving power 2000 SLOAN rp8500/* 0 3 Resolving power 8500 rp11500/* 0 3 Resolving power 11500 rp20000/* 0 3 Resolving power 20000
See also: http://archives.pd.astro.it/2500-10500 : the spectral 2500-10500Å library Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
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)
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. Note (3): Naming scheme for the spectra contained in the library. TtttttGggMmmVvvvK2AnnNVRRRF.ASC (example: T04000G45M05V015K2ANWNVR20F.ASC) characters meaning ------------------------------------------------ 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
Acknowledgements: Ulisee Munari, munari(at)pd.astro.it
(End) Patricia Vannier [CDS] 30-Aug-2016
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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