def process_mock_densdata(options):
print("Using mock Pal 5 data from %s" % options.mockfilename)
# Read and prep data for mocks
xvid= numpy.loadtxt(options.mockfilename)
xv= xvid[:,:6]
xv= xv[numpy.argsort(xvid[:,6])]
XYZ= bovy_coords.galcenrect_to_XYZ(xv[:,0],xv[:,1],xv[:,2],
Xsun=R0,Zsun=0.025)
lbd= bovy_coords.XYZ_to_lbd(XYZ[0],XYZ[1],XYZ[2],degree=True)
radec= bovy_coords.lb_to_radec(lbd[:,0],lbd[:,1],degree=True)
xieta= pal5_util.radec_to_pal5xieta(radec[:,0],radec[:,1],degree=True)
# make sure the progenitor is at (0,0)
xieta[:,0]-= numpy.median(xieta[:,0])
xieta[:,1]-= numpy.median(xieta[:,1])
h,e= numpy.histogram(xieta[:,0],range=[0.2,14.3],bins=141)
xdata= numpy.arange(0.25,14.35,0.1)
# Compute power spectrum
tdata= h-0.
pp= Polynomial.fit(xdata,tdata,deg=options.polydeg,w=1./numpy.sqrt(h+1.))
tdata/= pp(xdata)
ll= xdata
py= signal.csd(tdata,tdata,fs=1./(ll[1]-ll[0]),scaling='spectrum',
nperseg=len(ll))[1]
py= py.real
# Also compute the bispectrum
Bspec, Bpx= bispectrum.bispectrum(numpy.vstack((tdata,tdata)).T,
nfft=len(tdata),wind=7,nsamp=1,overlap=0)
ppyr= numpy.fabs(Bspec[len(Bspec)//2+_BISPECIND,len(Bspec)//2:].real)
ppyi= numpy.fabs(Bspec[len(Bspec)//2+_BISPECIND,len(Bspec)//2:].imag)
return (numpy.sqrt(py*(ll[-1]-ll[0])),numpy.sqrt(h+1.)/pp(xdata),
ppyr,ppyi)
def sky_coords(cluster):
"""Get the sky coordinates of every star in the cluster
Parameters
----------
cluster : class
StarCluster
Returns
-------
ra,dec,d0,pmra,pmdec,vr0 : float
on-sky positions and velocities of cluster stars
History
-------
2018 - Written - Webb (UofT)
"""
origin0 = cluster.origin
if origin0 != "galaxy":
cluster.to_galaxy()
x0, y0, z0 = bovy_coords.galcenrect_to_XYZ(cluster.x,
cluster.y,
cluster.z,
Xsun=8.0,
Zsun=0.025).T
vx0, vy0, vz0 = bovy_coords.galcenrect_to_vxvyvz(
cluster.vx,
cluster.vy,
cluster.vz,
Xsun=8.0,
Zsun=0.025,
vsun=[-11.1, 244.0, 7.25],
).T
l0, b0, d0 = bovy_coords.XYZ_to_lbd(x0, y0, z0, degree=True).T
ra, dec = bovy_coords.lb_to_radec(l0, b0, degree=True).T
vr0, pmll0, pmbb0 = bovy_coords.vxvyvz_to_vrpmllpmbb(vx0,
vy0,
vz0,
l0,
b0,
d0,
degree=True).T
pmra, pmdec = bovy_coords.pmllpmbb_to_pmrapmdec(pmll0,
pmbb0,
l0,
b0,
degree=True).T
if origin0 == "centre":
cluster.to_centre()
elif origin0 == "cluster":
cluster.to_cluster()
return ra, dec, d0, pmra, pmdec, vr0
def sky_coords(cluster):
"""
NAME:
sky_coords
PURPOSE:
Get the sky coordinates of every star in the cluster
INPUT:
cluster - a StarCluster-class object
OUTPUT:
ra,dec,d0,pmra,pmdec,vr0
HISTORY:
2018 - Written - Webb (UofT)
"""
origin0 = cluster.origin
if origin0 != "galaxy":
cluster.to_galaxy()
x0, y0, z0 = bovy_coords.galcenrect_to_XYZ(
cluster.x, cluster.y, cluster.z, Xsun=8.0, Zsun=0.025
).T
vx0, vy0, vz0 = bovy_coords.galcenrect_to_vxvyvz(
cluster.vx,
cluster.vy,
cluster.vz,
Xsun=8.0,
Zsun=0.025,
vsun=[-11.1, 244.0, 7.25],
).T
l0, b0, d0 = bovy_coords.XYZ_to_lbd(x0, y0, z0, degree=True).T
ra, dec = bovy_coords.lb_to_radec(l0, b0, degree=True).T
vr0, pmll0, pmbb0 = bovy_coords.vxvyvz_to_vrpmllpmbb(
vx0, vy0, vz0, l0, b0, d0, degree=True
).T
pmra, pmdec = bovy_coords.pmllpmbb_to_pmrapmdec(pmll0, pmbb0, l0, b0, degree=True).T
if origin0 == "centre":
cluster.to_centre()
elif origin0 == "cluster":
cluster.to_cluster()
return ra, dec, d0, pmra, pmdec, vr0
def get_star_dx(pepperdf, n=1000, returnapar=False, returnxi=False):
(Omega, angle, dt) = pepperdf.sample(n=n, returnaAdt=True)
RvR = pepperdf._approxaAInv(Omega[0], Omega[1], Omega[2], angle[0],
angle[1], angle[2])
vo = pepperdf._vo
ro = pepperdf._ro
R0 = pepperdf._R0
Zsun = pepperdf._Zsun
vsun = pepperdf._vsun
XYZ = bovy_coords.galcencyl_to_XYZ(RvR[0] * ro,
RvR[5],
RvR[3] * ro,
Xsun=R0,
Zsun=Zsun).T
slbd = bovy_coords.XYZ_to_lbd(XYZ[0], XYZ[1], XYZ[2], degree=True)
sradec = bovy_coords.lb_to_radec(slbd[:, 0], slbd[:, 1], degree=True)
xieta = pal5_util.radec_to_pal5xieta(sradec[:, 0],
sradec[:, 1],
degree=True)
l = slbd[:, 0]
b = slbd[:, 1]
r = slbd[:, 2]
if returnapar:
closesttrackindexes = np.zeros(len(r))
for i in np.arange(len(r)):
closesttrackindexes[i] = pepperdf.find_closest_trackpoint(
RvR[0][i],
RvR[1][i],
RvR[2][i],
RvR[3][i],
RvR[4][i],
RvR[5][i],
interp=True)
starapar = pepperdf._interpolatedThetasTrack[(
closesttrackindexes).astype(int)]
return starapar
if returnxi: return xieta[:, 0]
else: return None
def galcencyl_to_lbd(R, phi, Z, degree=True):
xyz = bovy_coords.galcencyl_to_XYZ(R, phi, Z)
lbd = bovy_coords.XYZ_to_lbd(xyz[0], xyz[1], xyz[2], degree=degree)
return lbd[0], lbd[1], lbd[2]
def xyzuvw_to_skycoord(xyzuvw_in,
solarmotion='schoenrich',
reverse_x_sign=True):
"""Converts XYZUVW with respect to the LSR or the sun
to RAdeg, DEdeg, plx, pmra, pmdec, RV
Parameters
----------
xyzuvw_in:
XYZUVW with respect to the LSR.
solarmotion: string
The reference of assumed solar motion. "schoenrich" or None if inputs are already
relative to the sun.
reverse_x_sign: bool
Do we reverse the sign of the X co-ordinate? This is needed for dealing with
galpy sign conventions.
TODO: not working at all... fix this
"""
if solarmotion == None:
xyzuvw_sun = np.zeros(6)
elif solarmotion == 'schoenrich':
xyzuvw_sun = [0, 0, 25, 11.1, 12.24, 7.25]
else:
raise UserWarning
#Make coordinates relative to sun
xyzuvw = xyzuvw_in - xyzuvw_sun
#Special for the sun itself...
#FIXME: This seems like a hack.
#if (np.sum(xyzuvw**2) < 1) and solarmotion != None:
# return [0,0,1e5, 0,0,0]
#Find l, b and distance.
#!!! WARNING: the X-coordinate may have to be reversed here, just like everywhere else,
#because of the convention in Orbit.x(), which doesn't seem to match X.
if reverse_x_sign:
lbd = bovy_coords.XYZ_to_lbd(-xyzuvw[0] / 1e3,
xyzuvw[1] / 1e3,
xyzuvw[2] / 1e3,
degree=True)
else:
lbd = bovy_coords.XYZ_to_lbd(xyzuvw[0] / 1e3,
xyzuvw[1] / 1e3,
xyzuvw[2] / 1e3,
degree=True)
radec = bovy_coords.lb_to_radec(lbd[0], lbd[1], degree=True)
vrpmllpmbb = bovy_coords.vxvyvz_to_vrpmllpmbb(xyzuvw[3],xyzuvw[4], xyzuvw[5],\
lbd[0],lbd[1],lbd[2], degree=True)
pmrapmdec = bovy_coords.pmllpmbb_to_pmrapmdec(vrpmllpmbb[1],
vrpmllpmbb[2],
lbd[0],
lbd[1],
degree=True)
return [
radec[0], radec[1], 1.0 / lbd[2], pmrapmdec[0], pmrapmdec[1],
vrpmllpmbb[0]
]
def to_radec(cluster, do_order=False, do_key_params=False, ro=8.0, vo=220.0):
"""Convert to on-sky position, proper motion, and radial velocity of cluster
Parameters
----------
cluster : class
StarCluster
do_order : bool
sort star by radius after coordinate change (default: False)
do_key_params : bool
call key_params to calculate key parameters after unit change (default: False)
ro : float
galpy radius scaling parameter
vo : float
galpy velocity scaling parameter
Returns
-------
None
History:
-------
2018 - Written - Webb (UofT)
"""
if len(cluster.ra) == len(cluster.x):
cluster.x = copy(cluster.ra)
cluster.y = copy(cluster.dec)
cluster.z = copy(cluster.dist)
cluster.vx = copy(cluster.pmra)
cluster.vy = copy(cluster.pmdec)
cluster.vz = copy(cluster.vlos)
cluster.units = "radec"
cluster.origin = "sky"
else:
units0, origin0 = cluster.units, cluster.origin
cluster.to_galaxy()
cluster.to_kpckms()
x0, y0, z0 = bovy_coords.galcenrect_to_XYZ(cluster.x,
cluster.y,
cluster.z,
Xsun=8.0,
Zsun=0.025).T
cluster.dist = np.sqrt(x0**2.0 + y0**2.0 + z0**2.0)
vx0, vy0, vz0 = bovy_coords.galcenrect_to_vxvyvz(
cluster.vx,
cluster.vy,
cluster.vz,
Xsun=8.0,
Zsun=0.025,
vsun=[-11.1, 244.0, 7.25],
).T
cluster.vlos = (vx0 * x0 + vy0 * y0 +
vz0 * z0) / np.sqrt(x0**2.0 + y0**2.0 + z0**2.0)
l0, b0, cluster.dist = bovy_coords.XYZ_to_lbd(x0, y0, z0,
degree=True).T
cluster.ra, cluster.dec = bovy_coords.lb_to_radec(l0, b0,
degree=True).T
vr0, pmll0, pmbb0 = bovy_coords.vxvyvz_to_vrpmllpmbb(vx0,
vy0,
vz0,
l0,
b0,
cluster.dist,
degree=True).T
cluster.pmra, cluster.pmdec = bovy_coords.pmllpmbb_to_pmrapmdec(
pmll0, pmbb0, l0, b0, degree=True).T
x0, y0, z0 = bovy_coords.galcenrect_to_XYZ(cluster.xgc,
cluster.ygc,
cluster.zgc,
Xsun=8.0,
Zsun=0.025)
vx0, vy0, vz0 = bovy_coords.galcenrect_to_vxvyvz(
cluster.vxgc,
cluster.vygc,
cluster.vzgc,
Xsun=8.0,
Zsun=0.025,
vsun=[-11.1, 244.0, 7.25],
)
cluster.vlos_gc = (vx0 * x0 + vy0 * y0 +
vz0 * z0) / np.sqrt(x0**2.0 + y0**2.0 + z0**2.0)
l0, b0, cluster.dist_gc = bovy_coords.XYZ_to_lbd(x0,
y0,
z0,
degree=True)
cluster.ra_gc, cluster.dec_gc = bovy_coords.lb_to_radec(l0,
b0,
degree=True)
vr0, pmll0, pmbb0 = bovy_coords.vxvyvz_to_vrpmllpmbb(vx0,
vy0,
vz0,
l0,
b0,
cluster.dist_gc,
degree=True)
cluster.pmra_gc, cluster.pmdec_gc = bovy_coords.pmllpmbb_to_pmrapmdec(
pmll0, pmbb0, l0, b0, degree=True)
cluster.x = copy(cluster.ra)
cluster.y = copy(cluster.dec)
cluster.z = copy(cluster.dist)
cluster.vx = copy(cluster.pmra)
cluster.vy = copy(cluster.pmdec)
cluster.vz = copy(cluster.vlos)
cluster.xgc = copy(cluster.ra_gc)
cluster.ygc = copy(cluster.dec_gc)
cluster.zgc = copy(cluster.dist_gc)
cluster.vxgc = copy(cluster.pmra_gc)
cluster.vygc = copy(cluster.pmdec_gc)
cluster.vzgc = copy(cluster.vlos_gc)
cluster.units = "radec"
cluster.origin = "sky"
cluster.rv3d()
if do_key_params:
cluster.key_params(do_order=do_order)
def sample_and_hist_apars(pepperdf, apar, survey, nsample):
(Omega, angle, dt) = pepperdf.sample(n=nsample, returnaAdt=True)
RvR = pepperdf._approxaAInv(Omega[0], Omega[1], Omega[2], angle[0],
angle[1], angle[2])
vo = pepperdf._vo
ro = pepperdf._ro
R0 = pepperdf._R0
Zsun = pepperdf._Zsun
vsun = pepperdf._vsun
XYZ = bovy_coords.galcencyl_to_XYZ(RvR[0] * ro,
RvR[5],
RvR[3] * ro,
Xsun=R0,
Zsun=Zsun).T
slbd = bovy_coords.XYZ_to_lbd(XYZ[0], XYZ[1], XYZ[2], degree=True)
l = slbd[:, 0]
b = slbd[:, 1]
r = slbd[:, 2]
closesttrackindexes = np.zeros(len(r))
for i in np.arange(len(r)):
closesttrackindexes[i] = pepperdf.find_closest_trackpoint(RvR[0][i],
RvR[1][i],
RvR[2][i],
RvR[3][i],
RvR[4][i],
RvR[5][i],
interp=True)
starapar = pepperdf._interpolatedThetasTrack[(
closesttrackindexes).astype(int)]
masses = assign_masses(nsample)
if 'LSST' in survey:
mag1 = isodict['lsst_g-10.00-0.0001'](masses) + (
5 * np.log10(r * 1e3) - 5)
magerror1 = errormodels[survey]['g'](mag1)
mag2 = isodict['lsst_r-10.00-0.0001'](masses) + (
5 * np.log10(r * 1e3) - 5)
magerror2 = errormodels[survey]['r'](mag2)
elif survey == 'CASTOR':
mag1 = isodict['castor_u-10.00-0.0001'](masses) + (
5 * np.log10(r * 1e3) - 5)
magerror1 = errormodels[survey]['u'](mag1)
mag2 = isodict['castor_g-10.00-0.0001'](masses) + (
5 * np.log10(r * 1e3) - 5)
magerror2 = errormodels[survey]['g'](mag2)
elif survey == 'WFIRST':
mag1 = isodict['Z087-10.00-0.0001'](masses) + (5 * np.log10(r * 1e3) -
5)
magerror1 = errormodels[survey]['z'](mag1)
mag2 = isodict['H158-10.00-0.0001'](masses) + (5 * np.log10(r * 1e3) -
5)
magerror2 = errormodels[survey]['h'](mag2)
else:
mag1 = isodict['sdss_g-10.00-0.0001'](masses) + (
5 * np.log10(r * 1e3) - 5)
magerror1 = errormodels[survey]['g'](mag1)
mag2 = isodict['sdss_r-10.00-0.0001'](masses) + (
5 * np.log10(r * 1e3) - 5)
magerror2 = errormodels[survey]['r'](mag2)
omag1 = (mag1 +
np.random.normal(size=len(mag1)) * magerror1)[((magerror1 < .1) &
(magerror2 < .1))]
omag2 = (mag2 +
np.random.normal(size=len(mag2)) * magerror2)[((magerror1 < .1) &
(magerror2 < .1))]
magsel = ((magerror1 < .1) & (magerror2 < .1))
lrange = [340, 360]
brange = [37.5, 47.5]
skysel = ((l < lrange[1]) & (l > lrange[0]) & (b < brange[1]) &
(b > brange[0]))
aparbins = np.linspace(apar[0] - (apar[1] - apar[0]) / 2.,
apar[-1] + 3 * (apar[1] - apar[0]) / 2.,
len(apar) + 1,
endpoint=False)
#centroids = bins[1:]-(bins[1]-bins[0])/2.
counts, bins = np.histogram(starapar[magsel & skysel], bins=aparbins)
