Code used in arXiv:1707.00007 ("Clarifying the Hubble constant tension with a Bayesian hierarchical model of the local distance ladder"); arXiv:1802.03404 ("Prospects for resolving the Hubble constant tension with standard sirens"); and arXiv:1811.11723 ("Unbiased Hubble constant estimation from binary neutron star mergers").
- Stephen Feeney, Daniel Mortlock and Niccolò Dalmasso (arXiv:1707.00007)
- Stephen Feeney, Hiranya Peiris, Andrew Williamson, Samaya Nissanke, Daniel Mortlock, Justin Alsing and Dan Scolnic (arXiv:1802.03404)
- Daniel Mortlock, Stephen Feeney, Hiranya Peiris, Andrew Williamson and Samaya Nissanke (arXiv:1811.11723)
Clarifying the Hubble constant tension with a Bayesian hierarchical model of the local distance ladder
A more complete README is incoming, as is a more user-friendly interface. For now, note the following dependencies
and that the Planck chains can be downloaded from the Planck Legacy Archive for comparison. Why not try the following?
python stan_cpl.py python stan_cpl_sample_plots.py
The following variables can be changed in
stan_cpl.py to set up different runs. Any changes should also be made to
stan_cpl_sample_plots.py to process the resulting outputs.
n_chains = 4 # number of independent parallel chains n_samples = 10000 # 100000 will take 10-20 hours (linear scaling) recompile = True # True recompiles Stan model: set to False after first run use_riess_rejection = False # sigma clip Cepheids before passing to BHM sne_sum = False # replace full SN dataset with intercept of mag-log(z) relation gauss_mu_like = False # sample from anchor distance moduli, not distances model_outliers = None # Gauss (None) or heavy-tailed ('ht') intrinsic scatter ng_maser_pdf = False # replace Gauss MASER distance likelihood with (approx) non-Gauss form nir_sne = False # use near infra-red SNe from Dhawan et al. (1707.00715) fit_cosmo_delta = None # fit H_0 (None) or perform model selection ('hq') v_pla = 2015 # use Planck 2015 or 2016 inputs in model selection constrain = True # if using simulated data, fix random seed to test stability stan_constrain = True # fix random seed in sampling run setup = 'r16' # dataset: try 'r16' (1604.01424) or 'd17' (1707.00715) sim = True # fit existing data or simulation
Prospects for resolving the Hubble constant tension with standard sirens
Note the following dependencies:
python h_of_z.py to produce inverse distance ladder constraints, and
python gw_grb_h_0_ppd.py (or
mpirun -np X python gw_grb_h_0_ppd.py if you have mpi4py installed and want to use it) to generate binary neutron star merger constraints.
Unbiased Hubble constant estimation from binary neutron star mergers
Note the following dependencies:
The main code is contained in
bias_test_stan.py. This generates simple simulations of catalogues of binary neutron star mergers, selected by their gravitational-wave signal to noise, and then samples either their distances and inclinations (conditioned on the measured strains only) or the cosmological parameters (Hubble constant and deceleration parameter, if selected) conditioned on both gravitational-wave and electromagnetic observations. It can be run using
mpirun -np X python bias_test_stan.py if you have MPI4PY installed and want to use it, which you should unless you have a lot of time. By default, Stan uses 4 OpenMP threads to sample, so use 4 CPUs per MPI process and set
OMP_NUM_THREADS=4. Additional plots for the paper were produced using
A lot of variables can be changed in
bias_test_stan.py to set up different runs, the most useful of which are explained below. Any changes should also be made to
bias_test_stan_plots.py to process the resulting outputs.
n_event = 100 # Catalogue size n_rpt = 1 # Number of catalogues to simulate use_mpi = True # Use MPI? Yes! constrain = True # Use a standard initial seed to generate simulations? sample = True # Sample or not? Turn off to save time plotting n_samples = 1000 # Number of samples to take per chain: half will be discarded as warmup by Stan n_chains = 4 # Number of Stan chains recompile = True # Recompile Stan code: do this once then turn off to save time fixed_n_bns = False # Fix the catalogue size when sampling ntlo = True # Adopt a quadratic Hubble law with variable q_0 vary_m_c = True # Draw chirp masses from a Gaussian rather than fixing them all to one value inc_rate_redshift = True # Include rate redshifting in inference plot_dist_cos_i_posts = False # Plot gravitational-wave-only distance and inclination posteriors sample_dist_cos_i_posts = False # Sample gravitational-wave-only distance and inclination posteriors find_n_bar = True # Find parameter-dependent fit to number of detectable merger events: do once then turn off