J/MNRAS/506/4781 HR-PYPOPSTAR model (Millan-irigoyen+, 2021)
HR-PYPOPSTAR: high-wavelength-resolution stellar populations evolutionary
synthesis model.
Millan-irigoyen I., Molla M., Cervino M., Ascasibar Y., Garcia-vargas M.L.,
Coelho P.R.T.
<Mon. Not. R. Astron. Soc., 506, 4781-4799 (2021)>
=2021MNRAS.506.4781M 2021MNRAS.506.4781M (SIMBAD/NED BibCode)
ADC_Keywords: Models, atmosphere ; Energy distributions ; Associations, stellar
Keywords: galaxies: stellar content - galaxies: stars clusters: general -
galaxies: evolution - stars: atmospheres - stars: evolution
Abstract:
We present the HR-PYPOPSTAR model, which provides a complete set (in
ages) of high-resolution (HR) spectral energy distributions of Single
Stellar Populations. The model uses the most recent
high-wavelength-resolution theoretical atmosphere libraries for
main-sequence, post-AGB/planetary nebulae and Wolf-Rayet stars. The
spectral energy distributions are given for more than a hundred ages
ranging from 0.1Myr to 13.8Gyr, at four different values of the
metallicity (Z = 0.004, 0.008, 0.019, and 0.05), considering four
different IMFs. The wavelength range goes from 91 to 24000Å in
linear steps δλ=0.1Å, giving a theoretical
resolving power Rth,5000∼50000 at 5000Å. This is the main
novelty of these spectra, unique for their age and wavelength ranges.
The models include the ionizing stellar populations that are relevant
at both young (massive hot stars) and old (planetary nebulae) ages. We
have tested the results with some examples of HR spectra recently
observed with MEGARA at GTC. We highlight the importance of wavelength
resolution in reproducing and interpreting the observational data from
the last and forthcoming generations of astronomical instruments
operating at 8-10m class telescopes, with higher spectral resolution
than their predecessors.
Description:
We give the electronic tables corresponding to Table 5 and Table 6 of
the publication. We also present the Stellar Energy Distributions
(SEDs) for the Simple Stellar Populations (SSPs) computed in the work,
for 4 different IMFs: Salpeter (1955ApJ...121..161S 1955ApJ...121..161S, SAL), Ferrini,
Penco & Palla (1990A&A...231..391F 1990A&A...231..391F, FER), Kroupa (2002Sci...295...82K 2002Sci...295...82K,
with exponent -2.7 for the massive star range, KRO), and Chabrier
(2003ApJ...586L.133C 2003ApJ...586L.133C, CHA), 4 metallicities (Z=0.004, 0.008, 0.02 and
0.05) for each one, and 106 ages from logage=5.00 until logage=10.18
(a shorter range in age for SAL) for wavelengths in the range 91Å
until 24000Å.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 165 3322 Magnitudes in broad band Systems for
stellar and total spectra
table6.dat 54 1662 Number of ionizing photons
spectra.dat 49 1662 List of spectra
sp/* . 1662 Individual spectra
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- IMF IMF: CHA, KRO, FER or SAL (G1)
6- 10 F5.3 --- Z Metallicity:0.004,0.008,0.02,0.05
13 A1 --- Type [ST] Type of spectra: S(stellar) or T(total)
17- 21 F5.2 [yr] logtau Logarithm of the age in yr
25- 30 F6.3 mag UV1mag Magnitude in Johnson-Cousins band UV1
34- 39 F6.3 mag UV2mag Magnitude in Johnson-Cousins band UV2
43- 48 F6.3 mag Umag Magnitude in Johnson-Cousins band U
52- 57 F6.3 mag B1mag Magnitude in Johnson-Cousins band B1
61- 66 F6.3 mag B2mag Magnitude in Johnson-Cousins band B2
70- 75 F6.3 mag Vmag Magnitude in Johnson-Cousins band V
79- 84 F6.3 mag Rmag Magnitude in Johnson-Cousins band R
88- 93 F6.3 mag Imag Magnitude in Johnson-Cousins band I
97-102 F6.3 mag Jmag Magnitude in Johnson-Cousins band J
106-111 F6.3 mag Hmag Magnitude in Johnson-Cousins band H
115-120 F6.3 mag Kmag Magnitude in Johnson-Cousins band K
124-129 F6.3 mag umag Magnitude in SDSS-SLOAN band u
133-138 F6.3 mag gmag Magnitude in SDSS-SLOAN band g
142-147 F6.3 mag rmag Magnitude in SDSS-SLOAN band r
151-156 F6.3 mag imag Magnitude in SDSS-SLOAN band i
160-165 F6.3 mag zmag Magnitude in SDSS-SLOAN band z
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- IMF IMF: CHA, KRO, FER or SAL (G1)
6- 10 F5.3 --- Z Metallicity:0.004,0.008,0.02,0.05
14- 18 F5.2 [yr] logtau Logarithm of the age in yr
23- 27 F5.2 s-1 QHI Number of ionizing photons by s for H
32- 36 F5.2 s-1 QHeI Number of ionizing photons by s for He I
41- 45 F5.2 s-1 QOI Number of ionizing photons by s for OI
50- 54 F5.2 s-1 QHeII Number of ionizing photons by s for HeII
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Byte-by-byte Description of file: spectra.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- IMF IMF: CHA, KRO, FER or SAL (G1)
5- 9 F5.3 --- Z Metallicity:0.004,0.008,0.02,0.05
11- 15 F5.2 [yr] logtau Logarithm of the age in yr
17- 49 A33 --- FileName Name of the spectrum file in subdirectory sp
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Byte-by-byte Description of file: sp/*
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Bytes Format Units Label Explanations
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2- 9 F8.2 0.1nm lambda Wavelength in Anstrong
12- 23 E12.6 10Lsun/nm FluxS Stellar flux in solar luminosity by Angstroms
for each solar mass of created star
26- 37 E12.6 10Lsun/nm FluxT Total flux (stellar+nebular) in solar
luminosity by Angstroms for each solar mass
of created star
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Global notes:
Note (G1): IMF as follows:
SAL = Salpeter (1955ApJ...121..161S 1955ApJ...121..161S)
FER = Ferrini, Penco & Palla (1990A&A...231..391F 1990A&A...231..391F)
KRO = Kroupa (2002Sci...295...82K 2002Sci...295...82K) with exponent -2.7 for the massive
star range
CHA = Chabrier (2003ApJ...586L.133C 2003ApJ...586L.133C)
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Acknowledgements:
Mercedes Molla, mercedes.molla(at)hotmail.es
(End) Patricia Vannier [CDS] 02-Nov-2021