J/A+A/618/A25 Model stellar spectra for B to early-M (Allende Prieto+, 2018)
A Collection of model stellar spectra for spectral types B to early-M.
Allende Prieto C., Koesterke L., Hubeny I., Bautista M., Barklem P.S.,
Nahar S.N.
<Astron. Astrophys. 618, A25 (2018)>
=2018A&A...618A..25A 2018A&A...618A..25A (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Spectroscopy
Keywords: radiative transfer - atlases - stars: atmospheres
Abstract:
Models of stellar spectra are necessary for interpreting light from
individual stars, planets, integrated stellar populations, nebulae,
and the interstellar medium.
We provide a comprehensive and homogeneous collection of synthetic
spectra for a wide range of atmospheric parameters and chemical
compositions.
We compile atomic and molecular data from the literature. We adopt the
largest and most recent set of ATLAS9 model atmospheres, and use the
radiative code ASSεT.
The resulting collection of spectra is made publicly available at
medium and high-resolution (R≡λ/δλ=10000,
100000 and 300000) spectral grids, which include variations in
effective temperature between 3500K and 30000K, surface gravity
(0≤log g≤5), and metallicity (-5≤[Fe/H]≤+0:5), spanning the
wavelength interval 120-6500nm. A second set of denser grids with
additional dimensions, [alpha/Fe] and micro-turbulence, are also
provided (covering 200-2500nm). We compare models with observations
for a few representative cases.
Description:
The following text describes the data files available from
ftp://carlos:allende@ftp.ll.iac.es/collection
These are in ASCII (but bzip2 compressed), and ready to be used with
the FERRE code (github.com/callendeprieto/ferre). The format includes
a header and as many rows as model spectra. See the FERRE manual for
more details (github.com/callendeprieto/ferre/docs/ferre.pdf).
There are two main families of files. The 'coarse' (nsc) grids
consider three atmospheric parameters ([Fe/H], Teff and logg) and
typically include hundreds of models on a very coarse network, while
the 'large' (ns) grids consider five (the previous three plus [alpha/Fe]
and microturbulence), and include tens to hundreds of thousands of models.
The files are numbered 1-5 depending on the
Teff range they span. There are files (ns and nsc) smoothed with
a Gaussian kernal to R=10,000, while nsc files are provided for
R=100,000 and 200,000 as well. The spectral range is 0.12-6.6um
for the nsc files and 0.2-2.5um for the ns files.
for the nsc files and 0.2-2.5um for the ns files.
nsc ('coarse' grids): [Fe/H], Teff, logg
size filename Teff range R
158004765 f_nsc1.dat.bz2 3500≤ Teff≤6000 10000
128868874 f_nsc2.dat.bz2 5750≤ Teff≤8000
102539424 f_nsc3.dat.bz2 7000≤ Teff≤12000
77786534 f_nsc4.dat.bz2 10000≤Teff≤20000
26089034 f_nsc5.dat.bz2 20000≤Teff≤30000
1430284037 f_hnsc1.dat.bz2 3500≤ Teff≤6000 100000
1159906320 f_hnsc2.dat.bz2 5750≤ Teff≤8000
913976329 f_hnsc3.dat.bz2 7000≤ Teff≤12000
695827559 f_hnsc4.dat.bz2 10000≤Teff≤20000
234598400 f_hnsc5.dat.bz2 20000≤Teff≤30000
2596690648 f_uhnsc1.dat.bz2 3500≤ Teff≤6000 300000
2067630039 f_uhnsc2.dat.bz2 5750≤ Teff≤8000
1605227763 f_uhnsc3.dat.bz2 7000≤ Teff≤12000
1221970143 f_uhnsc4.dat.bz2 10000≤Teff≤20000
411096450 f_uhnsc5.dat.bz2 20000≤Teff≤30000
ns ('large' grids): [Fe/H], [alpha/Fe], log(micro), Teff, logg
30936708717 f_ns1.dat.bz2 3500≤ Teff≤6000 10000
22957349531 f_ns2.dat.bz2 5750≤ Teff≤8000
19640724566 f_ns3.dat.bz2 7000≤ Teff≤12000
14267448478 f_ns4.dat.bz2 10000≤Teff≤20000
8622793847 f_ns5.dat.bz2 20000≤Teff≤30000
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
ns/* . 5 *Individual 'large' (ns) grids
nsc/* . 15 *Individual 'coarse' (nsc) grids
--------------------------------------------------------------------------------
Note on ns/* : ns ('large' grids): [Fe/H], [alpha/Fe], log(micro), Teff, logg
size filename Teff range R
30936708717 f_ns1.dat.bz2 3500≤Teff≤ 6000 10000
22957349531 f_ns2.dat.bz2 5750≤Teff≤ 8000
19640724566 f_ns3.dat.bz2 7000≤Teff≤12000
14267448478 f_ns4.dat.bz2 10000≤Teff≤20000
8622793847 f_ns5.dat.bz2 20000≤Teff≤30000
Note on nsc/* : nsc ('coarse' grids): [Fe/H], Teff, logg
size filename Teff range R
158004765 f_nsc1.dat.bz2 3500≤Teff≤ 6000 10000
128868874 f_nsc2.dat.bz2 5750≤Teff≤ 8000
102539424 f_nsc3.dat.bz2 7000≤Teff≤12000
77786534 f_nsc4.dat.bz2 10000≤Teff≤20000
26089034 f_nsc5.dat.bz2 20000≤Teff≤30000
1430284037 f_hnsc1.dat.bz2 3500≤Teff≤ 6000 100000
1159906320 f_hnsc2.dat.bz2 5750≤Teff≤ 8000
913976329 f_hnsc3.dat.bz2 7000≤Teff≤12000
695827559 f_hnsc4.dat.bz2 10000≤Teff≤20000
234598400 f_hnsc5.dat.bz2 20000≤Teff≤30000
2596690648 f_uhnsc1.dat.bz2 3500≤Teff≤ 6000 300000
2067630039 f_uhnsc2.dat.bz2 5750≤Teff≤ 8000
1605227763 f_uhnsc3.dat.bz2 7000≤Teff≤12000
1221970143 f_uhnsc4.dat.bz2 10000≤Teff≤20000
411096450 f_uhnsc5.dat.bz2 20000≤Teff≤30000
--------------------------------------------------------------------------------
See also:
J/A+A/605/A40 : Example of FERRE code spectra (Aguado+, 2017)
Acknowledgements:
Carlos Allende Prieto, callende(at)iac.es
(End) Patricia Vannier [CDS] 27-Jul-2018