def plot_edd_rate_line(MBH1d, eddrate=1, **kwargs):
L_AGN_edd = compute_eddington_luminosity(MBH1d)
x, y = log_lum(L_AGN_edd * eddrate), log_bhm(MBH1d)
plt.plot(x, y, "--", label='$\lambda=%s$' % eddrate, **kwargs)
plt.text(x[4],
y[4],
'$\lambda=%s$' % eddrate,
va='center',
ha='center',
rotation=60,
bbox=dict(color='white', pad=0),
size=8)
ms=8,
mew=3)
plt.xlabel("Luminosity $L_{46}$ [erg/s]")
plt.ylabel("BLR size [lightdays]")
plt.savefig("windyblr_2d_BLRsize.pdf", bbox_inches="tight")
plt.close()
plt.imshow(
CFgrid,
origin="lower",
aspect="auto",
extent=[L_AGN_lo, L_AGN_hi, MBH_lo, MBH_hi],
cmap="Oranges", #cmap="gray_r"
)
cb = plt.colorbar()
CS = plt.contour(log_lum(L_AGN1d), log_bhm(MBH1d), numpy.transpose(CFgrid),
[0.02, 0.05, 0.1, 0.2, 0.3])
plt.clabel(CS, inline=True)
plt.xlim(L_AGN_lo, L_AGN_hi)
plt.ylim(MBH_lo, MBH_hi)
#from labellines import labelLine, labelLines
# compute eddington rate:
def plot_edd_rate_line(MBH1d, eddrate=1, **kwargs):
L_AGN_edd = compute_eddington_luminosity(MBH1d)
x, y = log_lum(L_AGN_edd * eddrate), log_bhm(MBH1d)
plt.plot(x, y, "--", label='$\lambda=%s$' % eddrate, **kwargs)
plt.text(x[4],
y[4],
def plot_log_agn_postcard(MBH, eddrate,
# from Baskin & Laor (2017)
rad_efficiency = 0.1,
Z = 5, # metallicity
# Radiative Fountain system assumptions
dust_to_gas_ratio = 1/20.,
kappa = 1e3 * u.cm**2/u.g,
rho_g = 300 * u.Msun / u.pc**3,
show_BH = True,
show_corona = True,
show_disk = True,
show_BLR = True,
show_NLR = True,
show_jet = True,
show_TOR = True,
show_SOI = True,
show_viewing = True,
colored_disk = True,
show_flows = True,
):
L_AGN_edd = compute_eddington_luminosity(MBH)
L_AGN = eddrate * L_AGN_edd
L_AGN_46 = (L_AGN / (1e46 * u.erg/u.s)).to(1)
L_AGN_edd = compute_eddington_luminosity(MBH)
r_grav = compute_grav_radius(MBH).to(u.pc)
M_dot = (L_AGN / c.c**2 / rad_efficiency).to(u.Msun / u.yr)
R_in = compute_sublimation_radius(MBH, M_dot)
# from Kormendy & Ho+13, compute sigma from BH mass
sigma = 200 * u.km / u.s * 10**((log10((MBH / (1e9 * u.Msun)).to(1)) + 0.510) / 4.377)
r_infl = compute_sphere_of_influence(MBH, sigma).to(u.pc)
R = numpy.logspace(log10(r_grav/R_in), 3, 1000) * R_in
R = numpy.logspace(log10(r_grav/R_in), max(3, log10(r_infl/R_in)), 1000) * R_in
title = "$M_\mathrm{BH}=%s$ $\lambda=%.3f$ $L_\mathrm{AGN}=%.1f$ $\dot{M}=%.1f M_\odot/yr$" % (log_bhm(MBH), eddrate, log_lum(L_AGN), M_dot.to(u.Msun / u.yr).value)
#plt.title(title)
colors = plt.rcParams['axes.prop_cycle'].by_key()['color']
textsize = 10
xlo, xhi = 8e-8 * u.pc, 50*100 * u.pc
ylo, yhi = xlo / 100, 200*100 * u.pc
# Sphere of influence:
theta = numpy.linspace(0, pi/2, 400)
y, x = pol2cart(r_infl, theta)
if show_SOI:
plt.plot(x, y, ls='--', lw=0.5, color=colors[8], label='Sphere of influence')
#plt.text(x.max().value*1.1, r_infl.value / 1000, 'Sphere of influence',
# va='bottom', ha='left', rotation=90)
plt.text(x.max().value * 1.2, ylo.value * 2, 'Sphere of influence',
va='bottom', ha='left', rotation=90)
#plt.fill_between(x.value, y.value, y.value*0 + yhi.value,
# color=colors[8], alpha=0.1)
#plt.fill_between([x.max().value, xhi.value], [ylo.value]*2, [yhi.value]*2,
# color=colors[8], alpha=0.1)
#plt.fill_between(x.value, y.value, y.value*0 + ylo.value,
# color=colors[8], alpha=0.06)
# Accretion disk:
R_disk = R
z_disk = compute_alphadisk_height(MBH, M_dot, R_disk, alpha=1).to(u.pc)
T_disk = compute_alphadisk_temperature(MBH, M_dot, R_disk, alpha=1).to(u.K)
if show_disk:
mask = R < r_infl
if colored_disk:
for color, R_part, z_disk_part in find_color_chunks(color_data_T, T_disk[mask], color_data_rgb, R_disk[mask], z_disk[mask]):
plt.fill_between(R_part, z_disk_part, z_disk_part * 0 + ylo, color=color)
else:
plt.fill_between(R_disk[mask], z_disk[mask], z_disk[mask] * 0 + ylo, color='k', label="Accretion disk (SS)")
# 'Accretion disk\n$\log \dot{M}=%.1f$' % rround(log10(M_dot.value)),
plt.text(7 * r_grav.value, ylo.value * 2,
'Accretion disk\n$\log L_\mathrm{bol}=%.1f$' % log_lum(L_AGN),
va='bottom', ha='left', color='k', size=textsize, bbox=dict(color='white'))
#idx = numpy.where(R>20*r_grav)[0][0]
#plt.text(R_disk[idx].value, z_disk[idx].value, 'Accretion disk',
# va='top', ha='left', color='k', size=textsize)
if show_flows:
outflow = compute_outflow_rate(L_AGN, Mstar = 1e11 * u.Msun, SFR = 0*u.Msun/u.yr)
inflow = M_dot # at accretion disk at least, or when considering steady-state
# y = z_disk[mask][-1].value/10
plt.text(r_infl.value*2, 1e-3, '$\\uparrow$ Outflow\n$%s M_\odot/\mathrm{yr} \cdot M_{\star,11}^{-0.4}$\n$\leftarrow$ BH Inflow\n$%s M_\odot/\mathrm{yr}$' % (rround(outflow.to(u.Msun/u.yr).value), rround(inflow.to(u.Msun/u.yr).value)),
va='top', ha='left', color='k', size=textsize)
# Jet:
R_fullrange = numpy.logspace(log10(r_grav.value), log10(R.value.max()*5), 400) * u.pc
R_fullrange = numpy.logspace(log10(r_grav.value), log10(max(yhi, 1e8*r_grav).value), 400) * u.pc
R_j = compute_jet_edge(MBH, R_fullrange)
if show_jet:
jetcolor = colors[4]
plt.plot(R_j, R_fullrange, '--', color=jetcolor, label='Jet')
plt.fill_betweenx(R_fullrange, R_j, color=jetcolor, label='Jet', alpha=0.05)
plt.text(R_j.value[-1] / 5, R_fullrange.value[-1] / 2, 'Jet', color=jetcolor,
va='top', ha='right', size=textsize)
# BH:
theta = numpy.linspace(0, pi/2, 4000)
y, x = pol2cart(r_grav, theta[::-1])
if show_BH:
plt.fill_between(x, 1e-10 + 0*y.value, y, color='k', label='Black hole')
#plt.plot(x, y / 10, '-', color='k', label='Black hole 1')
plt.text(r_grav.value * 0.8, r_grav.value / 3,
'Black Hole\n\n$\log M=%.1f$' % (log_bhm(MBH)) if MBH > 10**7.5 * u.Msun else 'BH\n\n$\log M=%.1f$' % (log_bhm(MBH)),
va='top', ha='right', color='white', fontweight='bold', size=textsize)
# Corona:
y, x = pol2cart(6*r_grav, theta)
if show_corona:
plt.plot(x, y, ls=':', color=colors[1], label='X-ray Corona')
plt.text(xlo.value*1.2, 6*r_grav.value, 'Corona',
va='bottom', ha='left', color=colors[1])
# BLR:
z1, z2, zmax = compute_blr_shape(MBH, M_dot, L_AGN, R, Z, variant='static')
z1, z2, zmax_dyn = compute_blr_shape(MBH, M_dot, L_AGN, R, Z, variant='dynamic', dyn_factor=2)
CF = get_blr_covering_factor(z1, z2, R)
Rpeak, Hpeak = get_peak(z2, z1, R)
z1, z2, zmax_dyn_nodust = compute_blr_shape(MBH, M_dot, L_AGN, R, Z, variant='dustfree', dyn_factor=2)
idx, = numpy.where(numpy.logical_or(zmax_dyn_nodust > z_disk, zmax_dyn > z_disk))
if idx.any():
lo, hi = idx.min() - 1, idx.max() + 1
zmax_dyn_disk = numpy.where(zmax_dyn > z_disk, zmax_dyn, z_disk)
zmax_dyn_nodust_disk = numpy.where(zmax_dyn_nodust > z_disk, zmax_dyn_nodust, z_disk)
else:
lo, hi = 0, -1
zmax_dyn_disk = zmax_dyn
zmax_dyn_nodust_disk = zmax_dyn_nodust
if show_BLR:
color = colors[0]
l, = plt.plot(R[lo:hi], zmax_dyn_nodust_disk[lo:hi], '--',
label="Broad Line Region (BLCH, CF=%.0f%%)" % (CF*100),
color=color,
)
plt.plot(R[lo:hi], zmax_dyn_disk[lo:hi], '-', color=color, label='Dusty BLR')
plt.fill_between(R[lo:hi], z_disk[lo:hi], zmax_dyn_disk[lo:hi], color=color)
#plt.plot(Rpeak, Hpeak, 'o', color=color)
plt.text(Rpeak.value, Hpeak.value, 'BLCH BLR\nCF=%.2f' % (CF),
va='bottom', ha='center', color=color)
#plt.fill_between(R.flatten(), 0, zmax_dyn, color=color, hatch='//')
#plt.vlines(R_in.to(u.pc).value, 0, Hpeak.to(u.pc).value, linestyles=[':'], colors=[color])
# Radiative fountain
r_d = compute_dust_sublimation_radius(L_AGN)
r_0 = compute_heating_radius(L_AGN, rho_g = 300 * u.Msun / u.pc**3)
r_max = compute_rmax(MBH, L_AGN, theta, r_0, r_d,
dust_to_gas_ratio = dust_to_gas_ratio,
kappa = kappa).to(u.pc)
theta_crit = compute_critical_angle(MBH, L_AGN, r_0, r_d,
dust_to_gas_ratio, kappa = kappa)
CF = cos(theta_crit)
color = colors[3]
r_max[r_max > 1000 * u.pc] = numpy.nan
z_min = numpy.interp(r_d.value, R.value, z_disk.value)
theta_min = arctan2(z_min, r_d.value)
y, x = pol2cart(r_max, theta)
if show_TOR:
#plt.plot(x, y, ls='-.', color=color, label="Radiative Fountain TOR")
## structure:
rng = numpy.random.RandomState(1)
Nrad = 100
# 100 pixels in radial direction
rho = 10**rng.normal(size=(Nrad, Nrad))
rho[rho > 1000] = 1000
from scipy.signal import sepfir2d, convolve2d
# we need 5 degree smoothing in theta according to Wada+ sims
# but this could be partly due to resolution issues,
# so I take twice that here
correlation_degrees = 5 / 2
# same scale in radial direction as in vertical direction
sigma_rad_pixels = len(rho) * sin(correlation_degrees * pi / 180)
H_r = numpy.exp(-0.5 * numpy.linspace(-5, 5, int(sigma_rad_pixels)*10)**2)
H_r /= H_r.sum()
H_c = H_r
kernel = H_r.reshape((-1, 1)) * H_c.reshape((1, -1))
kernel /= kernel.sum()
rad = numpy.linspace(0, r_infl.to(u.pc).value, Nrad)
X, Y = numpy.meshgrid(rad, rad)
R, THETA = cart2pol(X, Y)
low_density = 0
# use high values close to disk
rho[THETA <= theta_min] = 10
# now erase disallowed regions:
# empty jet
X_jet = compute_jet_edge(MBH, Y * u.pc).to(u.pc).value
rho[X < X_jet] = low_density
RMAX = numpy.interp(pi/2 - THETA, xp=theta, fp=r_max.value)
RMAX[~numpy.isfinite(RMAX)] = numpy.inf
# only fill below r_max
rho[R <= RMAX] = low_density
# only fill within SOI
rho[R > r_infl.to(u.pc).value] = low_density
# do convolution
convolved = sepfir2d(rho, H_r, H_c)
#convolved = convolve2d(rho, kernel, mode='same', fillvalue=low_density)
convolved[R <= RMAX] = low_density
convolved[R > r_infl.to(u.pc).value] = low_density
convolved[X < X_jet] = low_density
#convolved[THETA <= theta_min] = 3
#plt.contourf(rad, rad, convolved/convolved[convolved>low_density].std(),
# levels=numpy.linspace(-3, 3, 10), cmap='Reds', zorder=-10)
#convolved[convolved > 3] = 3
#convolved[convolved < -3] = numpy.nan
C = plt.contourf(rad, rad, convolved,
levels=10, cmap='Reds', zorder=-10)
C.collections[0].set_facecolor('white')
## end structure
mask = theta > 89.7/180*pi
if show_TOR and mask.any() and numpy.isfinite(x[mask][0].value):
plt.text(x[mask][0].value, y[mask][0].value, 'RF TOR \nCF=%.2f ' % CF,
va='bottom', ha='right', color=color)
# NLR
R_NLR_hi = get_nlr_size().to(u.pc)
# these are chosen arbitrarily: the inner edge of the NLR and the maximum angle
# in practice they are observationally and host galaxy limited, respectively
R_NLR_lo = r_infl
R_NLR = numpy.array([R_NLR_lo.value, R_NLR_hi.value]) * u.pc
thetai = numpy.linspace(pi/400, pi/4, 10)
for i, (thetalo, thetahi) in enumerate(zip(thetai[:-1], thetai[1:])):
if not show_NLR: break
ylo1, ylo2 = R_NLR.value
xlo1, xlo2 = compute_jet_edge(MBH, R_NLR).value
(yhi1, yhi2), (xhi1, xhi2) = pol2cart(R_NLR.value, thetahi)
#(ylo1, ylo2), (xlo1, xlo2) = pol2cart(R_NLR_lo.value, numpy.array([thetalo, thetahi]))
#(yhi1, yhi2), (xhi1, xhi2) = pol2cart(R_NLR_hi.value, numpy.array([thetalo, thetahi]))
label = 'NLR' if i == 0 else None
alpha = (1. - (i*1./len(thetai))**0.8)*0.5
plt.fill([xlo1, xhi1, xhi2, xlo2], [ylo1, yhi1, yhi2, ylo2],
color=colors[2],
alpha=alpha, lw=0,
label=label)
plt.text(xlo2, ylo2*0.9, 'NLR',
color='white', va='top', ha='left', size=textsize)
# sight-lines
theta = numpy.array([1, 5, 15, 30, 60, 85])
theta[theta == 0] = 5
theta[theta == 90] = 85
for thetai in theta:
if not show_viewing: break
Rline = numpy.array([5 * r_grav.to(u.pc).value, 4])
#Rline = numpy.linspace(5 * r_grav.to(u.pc).value, 10, 1000)
y, x = pol2cart(Rline, thetai / 180 * pi)
#x = R_fullrange.value
#y = x * sin(thetai / 180 * pi)
#mask = y > 1
#y, x = y[mask], x[mask]
plt.plot(x, y, ':', color='k', alpha=0.1)
plt.text(x[-1], y[-1], '$%d^\circ$' % (thetai))
plt.xlabel("R [pc]")
plt.ylabel("z [pc]")
plt.xticks()
#plt.legend(loc="lower right", prop=dict(size=12))
#plt.ylim(r_grav.value / 100, 200*100)
#plt.xlim(r_grav.value / 2, 50*100)
plt.ylim(8e-8 / 100, 200*100)
plt.xlim(8e-8, 50*100)
plt.xscale('log')
plt.yscale('log')
kappa=kappa) / pi * 180
plt.imshow(
theta_crit,
origin="lower",
aspect="auto",
extent=[L_AGN_lo, L_AGN_hi, MBH_lo, MBH_hi],
cmap="Oranges", #cmap="gray_r"
)
cb = plt.colorbar()
plt.xlim(L_AGN_lo, L_AGN_hi)
plt.ylim(MBH_lo, MBH_hi)
# compute eddington rate:
L_AGN_edd = compute_eddington_luminosity(MBH1d)
plt.plot(log_lum(L_AGN_edd), log_bhm(MBH1d), "--", color="k")
plt.plot(log_lum(L_AGN_edd * 0.1), log_bhm(MBH1d), "--", color="k", alpha=0.5)
plt.plot(log_lum(L_AGN_edd * 0.01),
log_bhm(MBH1d),
"--",
color="k",
alpha=0.25)
plt.xlabel("Bolometric Luminosity $L_\mathrm{AGN}$ [erg/s]")
plt.ylabel("Black Hole Mass $M_\mathrm{BH}$ [$M_\odot$]")
cb.set_label(r'$\theta_\mathrm{crit}$')
plt.savefig("radfountain_2d_LAGN.pdf", bbox_inches="tight")
plt.close()
L_X_lo, L_X_hi = 41, 45
L_X1d = bolcorr_hardX(L_AGN1d)
for logLAGN in numpy.arange(42, 47.4, 0.2):
L_AGN = 10**logLAGN * (u.erg/u.s)
L_AGN_edd = compute_eddington_luminosity(MBH)
eddrate = L_AGN / L_AGN_edd
plt.figure(figsize=(10,7))
MBH = 10**logMBH * u.Msun
#print(logMBH, eddrate)
prefix = "img/combinedstructure_2d_MBH%s_LAGN%.1f" % (logMBH, logLAGN)
plot_log_agn_postcard(MBH, eddrate)
plt.savefig(prefix + '_log.pdf', bbox_inches="tight")
plt.savefig(prefix + '_log.png', bbox_inches="tight")
plt.close()
Ls = dict(
L_X = round(log_lum(bolcorr_hardX(L_AGN)), 3),
L_B = round(log_lum(bolcorr_B(L_AGN)), 3),
L_R = round(log_lum(compute_radiocore_luminosity(MBH, L_AGN)), 3),
lambda_edd = rround(eddrate.to(1).value),
M_in = round(log10((L_AGN / c.c**2 / 0.1).to(u.Msun / u.yr).value), 3),
M_out = round(log10(compute_outflow_rate(L_AGN, Mstar = 1e11 * u.Msun, SFR = 0*u.Msun/u.yr).value), 3),
)
fL.write("\t\t[" + ",".join(["%s" % Ls[k] for k in lumlist]) + "],\n")
fL.flush();
plt.figure(figsize=(10,7))
plot_log_agn_postcard(MBH, eddrate,
show_BH = True,
show_corona = True,
show_disk = True,
show_BLR = True,