“Observations” of simulated dwarf galaxies - Star-formation histories from color-magnitude diagrams

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Volume 642 (October 2020)

A&A, 642 (2020) A40

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Table 2.

Parameters used for creating a synthetic CMD.

Parameter	Value
Stellar evolution library	BaSTI stellar evolution library (Pietrinferni et al. 2004)
Bolometric correction library	Castelli & Kurucz (2003)
Number of synthetic stars	1 million ^(a)
RGB and AGB mass loss parameters, respectively	0.35, 0.4
Star-formation rate (SFR(t))	Constant star formation between 0 and 14 Gyr.
Metallicity law Z(t)	Upper and lower metallicity laws ^(b)
Initial mass function	Chabrier IMF ^(c)
Binary fraction	0

Notes.

^(a)

Due to long run-times, IAC-star allows for the calculation of a maximum of 1 million synthetic stars at a time. So we generated 50 different 1-million synthetic CMDs and combined them to obtain a synthetic CMD with 50 million stars.

^(b)

This gives a uniform dispersion in metallicity between 0.0001 and 0.03.

^(c)

We computed stars with masses between 0.1 M_⊙ and 70 M_⊙. IAC-star only allows for a power-law form of the IMF, so we approximated the low-mass end of the Chabrier IMF (0.1 M_⊙ ≤ m ≤ 1 M_⊙) with a power law of the form ϕ(m) dm = m^−1.6.

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