def test_get_values_from_distribution():
center, std = 1, 0.2
np.random.seed(12345)
n_distr = unc.normal(center * u.kpc, std=std * u.kpc, n_samples=100)
result = _get_values_from_distribution(n_distr)
assert center == pytest.approx(result['value'], abs=1e-2)
assert std == pytest.approx(result['error'], abs=1e-2)
assert 'kpc' == result['unit']
np.random.seed(12345)
n_distr = unc.normal(center, std=std, n_samples=100)
result = _get_values_from_distribution(n_distr)
assert center == pytest.approx(result['value'], abs=1e-2)
assert std == pytest.approx(result['error'], abs=1e-2)
assert result.get('unit', None) is None
result = _get_values_from_distribution(n_distr, unit='kpc')
assert 'kpc' == result['unit']
distr = [
1.20881063, 0.93766121, 1.20136033, 1.11122468, 0.88140548, 0.98529047,
0.83750181, 0.95603778, 0.90262727, 0.76719971, 0.96954131, 0.83957612,
1.05208742, 0.9203976, 0.5388856, 0.82028187, 0.99002746, 0.99821842,
1.08264829, 0.88236597, 1.07393172, 0.68800062, 0.95087714, 0.95349601,
1.20331926, 1.1427941, 1.13346843, 1.12862014, 1.32770298
]
result = _get_values_from_distribution(distr)
assert center == pytest.approx(result['value'], abs=5e-2)
assert std == pytest.approx(result['error'], abs=5e-2)
nsteps, nwalkers = reader.get_log_prob().shape
samples = reader.get_chain(discard=int(mcmc_burnfrac * nsteps),
flat=True)
avs_dist = unc.Distribution(samples[:, -1])
av_per = avs_dist.pdf_percentiles([16.0, 50.0, 84.0])
avs[k] = av_per[1]
avs_unc[1, k] = av_per[2] - av_per[1]
avs_unc[0, k] = av_per[1] - av_per[0]
# print(avs_dist.pdf_percentiles([33., 50., 87.]))
(indxs, ) = np.where((cext.waves["BAND"] > 0.4 * u.micron)
& (cext.waves["BAND"] < 0.5 * u.micron))
ebvs_dist = unc.normal(
cext.exts["BAND"][indxs[0]],
std=cext.uncs["BAND"][indxs[0]],
n_samples=avs_dist.n_samples,
)
ebvs[k] = ebvs_dist.pdf_mean()
ebvs_unc[k] = ebvs_dist.pdf_std()
rvs_dist = avs_dist / ebvs_dist
rv_per = rvs_dist.pdf_percentiles([16.0, 50.0, 84.0])
rvs[k] = rv_per[1]
rvs_unc[1, k] = rv_per[2] - rv_per[1]
rvs_unc[0, k] = rv_per[1] - rv_per[0]
(indxs, ) = np.where((cext.waves["BAND"] > 2.1 * u.micron)
& (cext.waves["BAND"] < 2.3 * u.micron))
# print(cext.waves["BAND"][indxs[0]])
ekvs_dist = unc.normal(
def fit_spex_ext(
starpair,
path,
functype="pow",
dense=False,
profile="drude_asym",
exclude=None,
bootstrap=False,
fixed=False,
):
"""
Fit the observed SpeX NIR extinction curve
Parameters
----------
starpair : string
Name of the star pair for which to fit the extinction curve, in the format "reddenedstarname_comparisonstarname" (no spaces), or "average" to fit the average extinction curve
path : string
Path to the data files
functype : string [default="pow"]
Fitting function type ("pow" for powerlaw or "pol" for polynomial)
dense : boolean [default=False]
Whether or not to fit the features around 3 and 3.4 micron
profile : string [default="drude_asym"]
Profile to use for the features if dense = True (options are "gauss", "drude", "lorentz", "gauss_asym", "drude_asym", "lorentz_asym")
exclude : list of tuples [default=None]
list of tuples (min,max) with wavelength regions (in micron) that need to be excluded from the fitting, e.g. [(0.8,1.2),(2.2,5)]
bootstrap : boolean [default=False]
Whether or not to do a quick bootstrap fitting to get more realistic uncertainties on the fitting results
fixed : boolean [default=False]
Whether or not to add a fixed feature around 3 micron (for diffuse sightlines)
Returns
-------
Updates extdata.model["type", "waves", "exts", "residuals", "chi2", "params"] and extdata.columns["AV"] with the fitting results:
- type: string with the type of model (e.g. "pow_elx_Drude")
- waves: np.ndarray with the SpeX wavelengths
- exts: np.ndarray with the fitted model to the extinction curve at "waves" wavelengths
- residuals: np.ndarray with the residuals, i.e. data-fit, at "waves" wavelengths
- chi2 : float with the chi square of the fitting
- params: list with output Parameter objects
"""
# retrieve the SpeX data to be fitted, and sort the curve from short to long wavelengths
filename = "%s%s_ext.fits" % (path, starpair.lower())
if fixed:
filename = filename.replace(".", "_ice.")
extdata = ExtData(filename)
(waves, exts, exts_unc) = extdata.get_fitdata(["SpeX_SXD", "SpeX_LXD"])
indx = np.argsort(waves)
waves = waves[indx].value
exts = exts[indx]
exts_unc = exts_unc[indx]
# exclude wavelength regions if requested
if exclude:
mask = np.full_like(waves, False, dtype=bool)
for region in exclude:
mask += (waves > region[0]) & (waves < region[1])
waves = waves[~mask]
exts = exts[~mask]
exts_unc = exts_unc[~mask]
# get a quick estimate of A(V)
if extdata.type == "elx":
extdata.calc_AV()
AV_guess = extdata.columns["AV"]
else:
AV_guess = None
# convert to A(lambda)/A(1 micron)
# ind1 = np.abs(waves - 1).argmin()
# exts = exts / exts[ind1]
# exts_unc = exts_unc / exts[ind1]
# obtain the function to fit
if "SpeX_LXD" not in extdata.waves.keys():
dense = False
fixed = False
func = fit_function(
dattype=extdata.type,
functype=functype,
dense=dense,
profile=profile,
AV_guess=AV_guess,
fixed=fixed,
)
# for dense sightlines, add more weight to the feature region
weights = 1 / exts_unc
if dense:
mask_ice = (waves > 2.88) & (waves < 3.19)
mask_tail = (waves > 3.4) & (waves < 4)
weights[mask_ice + mask_tail] *= 2
# use the Levenberg-Marquardt algorithm to fit the data with the model
fit = LevMarLSQFitter()
fit_result_lev = fit(func, waves, exts, weights=weights, maxiter=10000)
# set up the backend to save the samples for the emcee runs
emcee_samples_file = path + "Fitting_results/" + starpair + "_emcee_samples.h5"
# do the fitting again, with MCMC, using the results from the first fitting as input
fit2 = EmceeFitter(nsteps=10000, burnfrac=0.1, save_samples=emcee_samples_file)
# add parameter bounds
for param in fit_result_lev.param_names:
if "amplitude" in param:
getattr(fit_result_lev, param).bounds = (0, 2)
elif "alpha" in param:
getattr(fit_result_lev, param).bounds = (0, 4)
elif "Av" in param:
getattr(fit_result_lev, param).bounds = (0, 10)
fit_result_mcmc = fit2(fit_result_lev, waves, exts, weights=weights)
# create standard MCMC plots
fit2.plot_emcee_results(
fit_result_mcmc, filebase=path + "Fitting_results/" + starpair
)
# choose the fit result to save
fit_result = fit_result_mcmc
# fit_result = fit_result_lev
print(fit_result)
# determine the wavelengths at which to evaluate and save the fitted model curve: all SpeX wavelengths, sorted from short to long (to avoid problems with overlap between SXD and LXD), and shortest and longest wavelength should have data
if "SpeX_LXD" not in extdata.waves.keys():
full_waves = extdata.waves["SpeX_SXD"].value
full_npts = extdata.npts["SpeX_SXD"]
else:
full_waves = np.concatenate(
(extdata.waves["SpeX_SXD"].value, extdata.waves["SpeX_LXD"].value)
)
full_npts = np.concatenate((extdata.npts["SpeX_SXD"], extdata.npts["SpeX_LXD"]))
# sort the wavelengths
indxs_sort = np.argsort(full_waves)
full_waves = full_waves[indxs_sort]
full_npts = full_npts[indxs_sort]
# cut the wavelength region
indxs = np.logical_and(full_waves >= np.min(waves), full_waves <= np.max(waves))
full_waves = full_waves[indxs]
full_npts = full_npts[indxs]
# calculate the residuals and put them in an array of the same length as "full_waves" for plotting
residuals = exts - fit_result(waves)
full_res = np.full_like(full_npts, np.nan)
if exclude:
mask = np.full_like(full_waves, False, dtype=bool)
for region in exclude:
mask += (full_waves > region[0]) & (full_waves < region[1])
full_res[(full_npts > 0) * ~mask] = residuals
else:
full_res[(full_npts > 0)] = residuals
# bootstrap to get more realistic uncertainties on the parameter results
if bootstrap:
red_star = StarData(extdata.red_file, path=path, use_corfac=True)
comp_star = StarData(extdata.comp_file, path=path, use_corfac=True)
red_V_unc = red_star.data["BAND"].get_band_mag("V")[1]
comp_V_unc = comp_star.data["BAND"].get_band_mag("V")[1]
unc_V = np.sqrt(red_V_unc ** 2 + comp_V_unc ** 2)
fit_result_mcmc_low = fit2(fit_result_lev, waves, exts - unc_V, weights=weights)
fit_result_mcmc_high = fit2(
fit_result_lev, waves, exts + unc_V, weights=weights
)
# save the fitting results to the fits file
if dense:
functype += "_" + profile
extdata.model["type"] = functype + "_" + extdata.type
extdata.model["waves"] = full_waves
extdata.model["exts"] = fit_result(full_waves)
extdata.model["residuals"] = full_res
extdata.model["chi2"] = np.sum((residuals / exts_unc) ** 2)
print("Chi2", extdata.model["chi2"])
extdata.model["params"] = []
for param in fit_result.param_names:
# update the uncertainties when bootstrapping
if bootstrap:
min_val = min(
getattr(fit_result_mcmc, param).value,
getattr(fit_result_mcmc_low, param).value,
getattr(fit_result_mcmc_high, param).value,
)
max_val = max(
getattr(fit_result_mcmc, param).value,
getattr(fit_result_mcmc_low, param).value,
getattr(fit_result_mcmc_high, param).value,
)
sys_unc = (max_val - min_val) / 2
getattr(fit_result, param).unc_minus = np.sqrt(
getattr(fit_result, param).unc_minus ** 2 + sys_unc ** 2
)
getattr(fit_result, param).unc_plus = np.sqrt(
getattr(fit_result, param).unc_plus ** 2 + sys_unc ** 2
)
extdata.model["params"].append(getattr(fit_result, param))
# save the column information (A(V), E(B-V) and R(V))
if "Av" in param:
extdata.columns["AV"] = (
getattr(fit_result, param).value,
getattr(fit_result, param).unc_minus,
getattr(fit_result, param).unc_plus,
)
# calculate the distrubtion of R(V) and 1/R(V) from the distributions of A(V) and E(B-V)
nsamples = getattr(fit_result, param).posterior.n_samples
av_dist = unc.normal(
extdata.columns["AV"][0],
std=(extdata.columns["AV"][1] + extdata.columns["AV"][2]) / 2,
n_samples=nsamples,
)
b_indx = np.abs(extdata.waves["BAND"] - 0.438 * u.micron).argmin()
ebv_dist = unc.normal(
extdata.exts["BAND"][b_indx],
std=extdata.uncs["BAND"][b_indx],
n_samples=nsamples,
)
ebv_per = ebv_dist.pdf_percentiles([16.0, 50.0, 84.0])
extdata.columns["EBV"] = (
ebv_per[1],
ebv_per[1] - ebv_per[0],
ebv_per[2] - ebv_per[1],
)
rv_dist = av_dist / ebv_dist
rv_per = rv_dist.pdf_percentiles([16.0, 50.0, 84.0])
extdata.columns["RV"] = (
rv_per[1],
rv_per[1] - rv_per[0],
rv_per[2] - rv_per[1],
)
inv_rv_dist = ebv_dist / av_dist
inv_rv_per = inv_rv_dist.pdf_percentiles([16.0, 50.0, 84.0])
extdata.columns["IRV"] = (
inv_rv_per[1],
inv_rv_per[1] - inv_rv_per[0],
inv_rv_per[2] - inv_rv_per[1],
)
print(extdata.columns)
# save the fits file
extdata.save(filename)
# print information about the ice feature
if fixed:
print(
"Ice feature strength: ",
extdata.model["params"][3].value,
extdata.model["params"][3].unc_minus,
extdata.model["params"][3].unc_plus,
)
from astropy.cosmology import FlatLambdaCDM, Planck15
from astropy.coordinates import SkyCoord
import astropy.units as u
import astropy.uncertainty as aun
import astropy.constants as ac
from uncertainties import ufloat
coords = SkyCoord('09h47m40.156s -30d56m55.44s', frame='fk5')
# from page 64 of
# https://ui.adsabs.harvard.edu/abs/2003AJ....126.2268W/abstract
z = ((2544 * u.km / u.s) / ac.c).to('')
deltaz = ((12 * u.km / u.s) / ac.c).to('')
# from
# http://simbad.u-strasbg.fr/simbad/sim-id?Ident=MCG-5-23-16
z2 = ((2466.09 * u.km / u.s) / ac.c).to('')
deltaz2 = ((47.97 * u.km / u.s) / ac.c).to('')
compat = ufloat(z, deltaz) - ufloat(z, deltaz2)
# cosmo = FlatLambdaCDM(H0=67.8, Om0=.308)
cosmo = Planck15
z_pdf = aun.normal(z.value, std=deltaz.value, n_samples=10_000)
dist = aun.Distribution(cosmo.comoving_distance(z_pdf.distribution))
def ESO280_params(PRINT=True):
params_dict = {
"eso_280_m_M_V": 17.011,
"eso_280_e_m_M_V": 0.045,
"eso_280_ebv": 0.141,
"eso_280_e_ebv": 0.006,
"rv": 94.644,
"e_rv": 0.476,
"std_rv": 2.305,
"e_std_rv": 0.363,
"r_t": [0.14693 * u.deg, 0.04126 * u.deg],
"r_c": [0.00410 * u.deg, 0.00009 * u.deg]
}
n_samples = 10000
eso_280_m_M_V_dist = unc.normal(params_dict['eso_280_m_M_V'],
std=params_dict['eso_280_e_m_M_V'],
n_samples=n_samples)
eso_280_ebv_dist = unc.normal(params_dict['eso_280_ebv'],
std=params_dict['eso_280_e_ebv'],
n_samples=n_samples)
eso_280_m_M_0_dist = eso_280_m_M_V_dist - 3.1 * eso_280_ebv_dist
eso_280_dist_dist = unc.Distribution(
10**(1 + eso_280_m_M_0_dist / 5).distribution * u.pc)
# Hardcoded values. Calculated using velocity_estimate.py
rv_dist = unc.normal(params_dict['rv'] * u.km / u.s,
std=params_dict['e_rv'] * u.km / u.s,
n_samples=n_samples)
rv_std_dist = unc.normal(params_dict['std_rv'] * u.km / u.s,
std=params_dict['e_std_rv'] * u.km / u.s,
n_samples=10000)
# Size values from ASteCA
r_0_dist = unc.normal(params_dict['r_c'][0],
std=params_dict['r_c'][1],
n_samples=10000)
r_t_dist = unc.normal(params_dict['r_t'][0],
std=params_dict['r_t'][1],
n_samples=10000)
size_dist = (np.tan(r_0_dist) * eso_280_dist_dist)
tidal_dist = (np.tan(r_t_dist) * eso_280_dist_dist)
cluster_mass = ((7.5 * rv_std_dist**2 * 4 / 3 * size_dist) / const.G)
sc_best = SkyCoord(ra=cluster_centre.ra,
dec=cluster_centre.dec,
radial_velocity=rv_dist.pdf_mean(),
distance=eso_280_dist_dist.pdf_mean(),
pm_ra_cosdec=-0.548 * u.mas / u.yr,
pm_dec=-2.688 * u.mas / u.yr)
eso_280_pmra_dist = unc.normal(sc_best.pm_ra_cosdec,
std=0.073 * u.mas / u.yr,
n_samples=n_samples)
eso_280_pmdec_dist = unc.normal(sc_best.pm_dec,
std=0.052 * u.mas / u.yr,
n_samples=n_samples)
sc_dist = SkyCoord(
ra=np.ones(eso_280_dist_dist.n_samples) * cluster_centre.ra,
dec=np.ones(eso_280_dist_dist.n_samples) * cluster_centre.dec,
radial_velocity=rv_dist.distribution,
distance=eso_280_dist_dist.distribution,
pm_ra_cosdec=eso_280_pmra_dist.distribution,
pm_dec=eso_280_pmdec_dist.distribution)
if PRINT:
print(
rf"$r_c$ & ${params_dict['r_c'][0].to(u.arcsec).value:0.2f}\pm{params_dict['r_c'][1].to(u.arcsec).value:0.2f}$~arcsec\\"
)
print(
rf"$r_t$ & ${params_dict['r_t'][0].to(u.arcmin).value:0.2f}\pm{params_dict['r_t'][1].to(u.arcmin).value:0.2f}$~arcmin\\"
)
print(
rf"$(m-M)_V$ & ${params_dict['eso_280_m_M_V']:0.2f}\pm{params_dict['eso_280_e_m_M_V']:0.2f}$\\"
)
print(
rf"$\ebv$ & ${params_dict['eso_280_ebv']:0.2f}\pm{params_dict['eso_280_e_ebv']:0.2f}$\\"
)
print(
rf"$(m-M)_0$ & ${eso_280_m_M_0_dist.pdf_mean:0.2f}\pm{eso_280_m_M_0_dist.pdf_std:0.2f}$\\"
)
print(
rf"$d_\odot$ & ${eso_280_dist_dist.pdf_mean.to(u.kpc).value:0.1f}\pm{eso_280_dist_dist.pdf_std.to(u.kpc).value:0.1f}$~kpc\\"
)
print(
rf"$r_c$ & ${size_dist.pdf_mean.to(u.pc).value:0.2f}\pm{size_dist.pdf_std.to(u.pc).value:0.2f}$~pc\\"
)
print(
rf"$r_t$ & ${tidal_dist.pdf_mean.to(u.pc).value:0.1f}\pm{tidal_dist.pdf_std.to(u.pc).value:0.1f}$~pc\\"
)
print(
rf"Mass & $({cluster_mass.pdf_mean.to(u.solMass).value/1000:0.1f}\pm{cluster_mass.pdf_std.to(u.solMass).value/1000:0.1f})\times10^3$~M$_\odot$\\"
)
print(
rf"$v_r$ & ${params_dict['rv']:0.2f}\pm{params_dict['e_rv']:0.2f}$\kms\\"
)
print(
rf"$\sigma_r$ & ${params_dict['std_rv']:0.2f}\pm{params_dict['e_std_rv']:0.2f}$\kms\\"
)
return params_dict, sc_best, sc_dist
# ## 常量 [constants](https://docs.astropy.org/en/stable/constants/)
from astropy import constants as const
const.c
const.hbar
print(const.c)
print(const.hbar)
from astropy import uncertainty as unc
a = unc.normal([1, 2] * u.kpc, std=[30, 50] * u.pc, n_samples=100000)
a
a.pdf_mean()
a.pdf_std()
# # 表格 [Table](https://docs.astropy.org/en/stable/table/)
from astropy.table import Table
t = Table.read('../data/AF.csv')
t
t[0]
if sname != "DIFFUS":
mcmcfile = bfile.replace(".fits", ".h5")
reader = emcee.backends.HDFBackend(mcmcfile)
nsteps, nwalkers = reader.get_log_prob().shape
samples = reader.get_chain(discard=int(mcmc_burnfrac *
nsteps),
flat=True)
# R(V) calc
avs_dist = unc.Distribution(samples[:, -1])
(indxs,
) = np.where((edata.waves["BAND"] > 0.4 * u.micron)
& (edata.waves["BAND"] < 0.5 * u.micron))
ebvs_dist = unc.normal(
edata.exts["BAND"][indxs[0]],
std=edata.uncs["BAND"][indxs[0]],
n_samples=avs_dist.n_samples,
)
rvs_dist = avs_dist / ebvs_dist
rv_per = rvs_dist.pdf_percentiles([16.0, 50.0, 84.0])
val = rv_per[1]
punc = rv_per[2] - rv_per[1]
munc = rv_per[1] - rv_per[0]
else:
(indxs,
) = np.where((edata.waves["BAND"] > 0.4 * u.micron)
& (edata.waves["BAND"] < 0.5 * u.micron))
val, punc, munc = (1.0 /
(edata.exts["BAND"][indxs[0]] - 1), 0.0,
0.0)
