J/A+A/690/A318 MC OB stars CMFGEN grids of atmosphere models (Marcolino+, 2024)
CMFGEN grids of atmosphere models for massive stars.
OB-type stars at the Magellanic Clouds.
Marcolino W., Bouret J.-C., Martins F., Hillier D.J.
<Astron. Astrophys. 690, A318 (2024)>
=2024A&A...690A.318M 2024A&A...690A.318M (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Magnitudes ; Magellanic Clouds ; Stars, OB
Keywords: stars: atmospheres - stars: fundamental parameters - stars: massive -
stars: winds, outflows
Abstract:
Large spectroscopic surveys of individual massive stars, such as
ULLYSES and XSHOOTU, provide observational data for hundreds of
massive stars. Their analysis requires large numbers of synthetic
spectra so that stellar parameters can be determined. In addition,
libraries of massive stars' spectra are needed to produce population
synthesis models able to reproduce the observed spectra of unresolved
young stellar populations, such as those revealed by the James Webb
Space Telescope (JWST) in the early Universe. Our main goal is to
provide an extensive library of synthetic spectra and spectral energy
distributions of OB stars at metallicities of the Magellanic Clouds.
This library will offer a wealth of spectrophotometric information,
making it readily applicable to a variety of astrophysical problems.
We used the CMFGEN code to calculate 606 NLTE, line-blanketed,
expanding atmosphere models using a comprehensive set of atomic data.
An overall metallicity of 1/2 Z☉ and 1/5 Z☉ was adopted
for the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC),
respectively. We produced high-resolution spectra from 30 angstroms to
3 microns for stars on the Main Sequence and slightly beyond. We
provide spectral energy distributions, normalized synthetic spectra,
ionizing fluxes, and photometry in various bands: Johnson UBV, Cousins
RI, Bessel JHK, selected wide JWST filters, Gaia, and LSST ugrizy
filters. For each of these filters, we compute bolometric corrections
for all synthetic spectra and calibrations as a function of effective
temperature. All of our synthetic spectra are publicly available
through the POLLUX database, aiming to expedite multiwavelength
analyses of massive stars in low metallicity environments.
Description:
We provide a table with synthetic absolute magnitudes and bolometric
corrections for OB stars at the Magellanic Clouds in various
photometric bands: Johnson UBV, Cousins RI, Bessel JHK, JWST (F070W,
F090W, F115W, F150W, F200W), Gaia (G, Gbp, Grp), and LSST (u, g, r, i,
z, y). The corresponding spectra are publicly available through the
POLLUX database, aiming to expedite multiwavelength analyses of
massive stars in low metallicity environments.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table.dat 279 606 Absolute magnitudes and bolometric corrections
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See also:
B/pollux : POLLUX database of synthetic stellar spectra (Palacios+ 2010-2024)
https://pollux.oreme.org/collections/ : POLLUX Home Page
Byte-by-byte Description of file: table.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- Galaxy LMC (1/2 Zsun) or SMC (1/5 Zsun) model
5- 11 F7.1 K Teff Effective temperature of the model
13- 15 F3.1 [cm/s2] logg Surface gravity of the model
17- 21 F5.2 mag U Absolute magnitude in the U band
23- 27 F5.2 mag B Absolute magnitude in the B band
29- 33 F5.2 mag V Absolute magnitude in the V band
35- 39 F5.2 mag J Absolute magnitude in the J band
41- 45 F5.2 mag H Absolute magnitude in the H band
47- 51 F5.2 mag K Absolute magnitude in the K band
53- 57 F5.2 mag R Absolute magnitude in the R band
59- 63 F5.2 mag I Absolute magnitude in the I band
65- 69 F5.2 mag F070W Absolute magnitude in the F070W band
71- 75 F5.2 mag F090W Absolute magnitude in the F090W band
77- 81 F5.2 mag F115W Absolute magnitude in the F115W band
83- 87 F5.2 mag F150W Absolute magnitude in the F150W band
89- 93 F5.2 mag F200W Absolute magnitude in the F200W band
95- 99 F5.2 mag LSST-u Absolute magnitude in the LSST u band
101-105 F5.2 mag LSST-g Absolute magnitude in the LSST g band
107-111 F5.2 mag LSST-r Absolute magnitude in the LSST r band
113-117 F5.2 mag LSST-i Absolute magnitude in the LSST i band
119-123 F5.2 mag LSST-z Absolute magnitude in the LSST z band
125-129 F5.2 mag LSST-y Absolute magnitude in the LSST y band
131-135 F5.2 mag GAIA-G Absolute magnitude in the GAIA G band
137-141 F5.2 mag GAIA-Bp Absolute magnitude in the GAIA bp band
143-147 F5.2 mag GAIA-Rp Absolute magnitude in the GAIA rp band
149-153 F5.2 mag BC(U) Bolometric correction in the U band
155-159 F5.2 mag BC(B) Bolometric correction in the B band
161-165 F5.2 mag BC(V) Bolometric correction in the V band
167-171 F5.2 mag BC(J) Bolometric correction in the J band
173-177 F5.2 mag BC(H) Bolometric correction in the H band
179-183 F5.2 mag BC(K) Bolometric correction in the K band
185-189 F5.2 mag BC(R) Bolometric correction in the R band
191-195 F5.2 mag BC(I) Bolometric correction in the I band
197-201 F5.2 mag BC(F070W) Bolometric correction in the F070W band
203-207 F5.2 mag BC(F090W) Bolometric correction in the F090W band
209-213 F5.2 mag BC(F115W) Bolometric correction in the F115W band
215-219 F5.2 mag BC(F150W) Bolometric correction in the F150W band
221-225 F5.2 mag BC(F200W) Bolometric correction in the F200W band
227-231 F5.2 mag BC(LSST-u) Bolometric correction in the LSST u band
233-237 F5.2 mag BC(LSST-g) Bolometric correction in the LSST g band
239-243 F5.2 mag BC(LSST-r) Bolometric correction in the LSST r band
245-249 F5.2 mag BC(LSST-i) Bolometric correction in the LSST i band
251-255 F5.2 mag BC(LSST-z) Bolometric correction in the LSST z band
257-261 F5.2 mag BC(LSST-y) Bolometric correction in the LSST y band
263-267 F5.2 mag BC(GAIA-G) Bolometric correction in the GAIA G band
269-273 F5.2 mag BC(GAIA-Bp) Bolometric correction in the GAIA bp band
275-279 F5.2 mag BC(GAIA-Rp) Bolometric correction in the GAIA rp band
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History:
From Wagner Marcolino, wagner(at)ov.ufrj.br
Acknowledgements:
This research has made use of the Spanish Virtual Observatory
(https://svo.cab.inta-csic.es) project funded by
CIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00.
(End) Patricia Vannier [CDS] 30-Sep-2024