SandersBinney2015

class cogsworth.sfh.SandersBinney2015(potential, time_bins=5, include_bar=False, bar_params={}, tau_m=<Quantity 12. Gyr>, tau_S=<Quantity 0.43 Gyr>, tau_T=<Quantity 10. Gyr>, tau_F=<Quantity 8. Gyr>, tau_1=<Quantity 0.11 Gyr>, **kwargs)

Bases: CompositeStarFormationHistory

Star formation history model based on a Quasi-Isothermal Disc distribution function from Sanders & Binney 2015.

This class doesn’t account for the extended distribution function described in SB15, instead following the quasi-isothermal DF described in Section 2.2 of that paper. We follow their prescription for the time evolution of the velocity dispersions and the metallicity distribution, but do not include radial migration.

Parameters are inherited from DistributionFunctionBasedSFH and StarFormationHistory but additionally with the following:

Parameters:

time_binsint, optional

Number of time bins to use when computing different radial and vertical velocity dispersions, which accounts for how these parameters evolve with time. More bins means a more accurate representation of the SFH but takes longer to compute. By default 5.

include_barbool, optional

Whether to include the bar component in the model, by default False

bar_paramsdict, optional

If include_bar is True, the keyword arguments to pass to the bar component, which is an instance of MilkyWayBarSormani2022. By default an empty dict, which will use the default parameters for that class.

tau_mQuantity [time], optional

Maximum lookback time, by default 12*u.Gyr

tau_SQuantity [time], optional

Star formation timescale, by default 0.43*u.Gyr

tau_TQuantity [time], optional

Lookback time separating thin and thick disc components, by default 10*u.Gyr

tau_FQuantity [time], optional

Timescale for the exponential decline of the star formation rate, by default 8*u.Gyr

tau_1Quantity [time], optional

Timescale for the initial rise of the star formation rate, by default 0.11*u.Gyr