Table 1
Free Chempy parameters, θ, and their priors with assumed Gaussian error model.
| θ | Description |
|
Limits | Approximated prior based upon |
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| stellar (SSP) evolution parameters | ||||
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| α IMF | high-mass slope of the Chabrier (2001) IMF (Eq. (1)) | − 2.29 ± 0.2 | [ − 4, − 1 ] | Côté et al. (2016a, Table 7) |
|
number of SN Ia exploding per M⊙ over 15 Gyr | − 2.75 ± 0.3 | [ − ∞,0 ] | Maoz & Mannucci (2012, Table 1) |
|
SN Ia delay time in Gyr for Maoz et al. (2010) distribution | − 0.8 ± 0.3 | [− ∞,1] | estimate from Maoz et al. (2012) |
|
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| ISM evolution parameters | ||||
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|
star formation efficiency governing the infall and ISM gas mass | − 0.3 ± 0.3 | [ − ∞,∞ ] | Bigiel et al. (2008) |
| SFR peak | peak of SFR in Gyr (scale of γ-distribution with k = 2, Eq. (2)) | 3.5 ± 1.5 | [ 0,∞ ] | inspired by van Dokkum et al. (2013, Fig. 4b) |
| x out | fraction of stellar feedback outflowing to the corona | 0.5 ± 0.2 | [ 0,1 ] | estimate because uncommon parametrization |
| log 10(fcorona) | corona mass factor times total SFR gives initial corona mass | 0.3 ± 0.3 | [ − ∞,∞ ] | Stern et al. (2016), Werk et al. (2014) |
Notes. Theoretical work by Côté et al. (2017) derives values in a range of 2−0.03 per Gyr. The work of Chiappini et al. (2001) and Andrews et al. (2017) uses 1 per Gyr. Côté et al. (2017) and Andrews et al. (2017) both assume a linear Schmidt law nSchmidt = 1 (same as this work), whereas Chiappini et al. (2001) use nSchmidt = 1.5 together with a gas density threshold. See Vincenzo et al. (2017) for a detailed comparison between linear and non-linear Schmidt law.
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