Cosmology package
Submodules
simple_pe.cosmology.cosmology module
- simple_pe.cosmology.cosmology.luminosity_distance(distance)[source]
return luminosity distance for a given comoving distance
- simple_pe.cosmology.cosmology.redshift_at_comoving_dist(distance)[source]
return redshift at a given comoving distance
simple_pe.cosmology.merger_rate_evolution module
- simple_pe.cosmology.merger_rate_evolution.P(t_D, t_D_max=array(13.7976159), t_D_min=0.02)[source]
1/t delay time distribution
- simple_pe.cosmology.merger_rate_evolution.integrand(z, R0=<Quantity 1500. 1 / (yr Gpc3)>, z_max=20, sfr=<function sfrMD>)[source]
- simple_pe.cosmology.merger_rate_evolution.rate_density(z, z_max=20, sfr=<function sfrMD>)[source]
computes the rate density at z by integrating over the contributions from all possible delay times from binary birth to merger and the attending SFR at the at the time of formation
z_max: define a maximum redshift beyond which we assume there is no star formation
sfr: specify a cosmic sfr function
- simple_pe.cosmology.merger_rate_evolution.rate_density_integrand(tb, t, sfr=<function sfrMD>)[source]
eq 37 of Nakar (2007) http://www.sciencedirect.com/science/article/pii/S0370157307000476?via%3Dihub
equivalent to eq 3 of LIGO GW150914 stochastic paper (2016) https://journals.aps.org/prl/pdf/10.1103/PhysRevLett.116.131102
also eq 1 from Anand (2017) https://arxiv.org/pdf/1710.04996.pdf
also eq 3 of Ghirlanda (2016) https://www.aanda.org/articles/aa/full_html/2016/10/aa28993-16/aa28993-16.html
also eq 1 of LIGO kilanova paper (2017) http://iopscience.iop.org/article/10.3847/2041-8213/aa9478/pdf
also eq 18 in Taylor and Gair (2012) https://arxiv.org/abs/1204.6739
- simple_pe.cosmology.merger_rate_evolution.sfr2_porciani_madau(z)[source]
SFR2 from porciani madau 2001 http://stacks.iop.org/0004-637X/548/i=2/a=522
- simple_pe.cosmology.merger_rate_evolution.sfrHB(z)[source]
SFR of Hopkins and Beacom (2006) http://iopscience.iop.org/article/10.1086/506610/pdf
- simple_pe.cosmology.merger_rate_evolution.sfrMD(z)[source]
equation 15 on p. 48 of Madau and Dickenson (2014) http://www.annualreviews.org/doi/pdf/10.1146/annurev-astro-081811-125615 uses (O_M, O_de, h) = (0.3, 0.7, 0.7) params
- simple_pe.cosmology.merger_rate_evolution.t_D_max = 13.7
We are using Planck15 cosmological parameters:
simple_pe.cosmology.star_formation_rate_injection module
- simple_pe.cosmology.star_formation_rate_injection.age_at_redshift(z)[source]
t in billions of years
- simple_pe.cosmology.star_formation_rate_injection.delay_distribution(t, t_D_min=0.02, t_D_max=13.7)[source]
- simple_pe.cosmology.star_formation_rate_injection.integrand(z, R0=<Quantity 1500. 1 / (yr Gpc3)>)[source]
- simple_pe.cosmology.star_formation_rate_injection.rate_density_coalescence(z, t_D_min=0.02, t_D_max=13.7)[source]
- simple_pe.cosmology.star_formation_rate_injection.rate_density_coalescence_integrand(t_D, z)[source]
- simple_pe.cosmology.star_formation_rate_injection.redshift_at_age(t)[source]
t in billions of years
- simple_pe.cosmology.star_formation_rate_injection.sfr(z)[source]
equation 15 on p. 48 of Madau and Dickenson (2014) http://www.annualreviews.org/doi/pdf/10.1146/annurev-astro-081811-125615
- simple_pe.cosmology.star_formation_rate_injection.t_D_max = 13.7
We are using Planck15 cosmological parameters: