aboutsummaryrefslogtreecommitdiffstats
path: root/fg21sim/extragalactic/clusters/halo.py
diff options
context:
space:
mode:
Diffstat (limited to 'fg21sim/extragalactic/clusters/halo.py')
-rw-r--r--fg21sim/extragalactic/clusters/halo.py174
1 files changed, 0 insertions, 174 deletions
diff --git a/fg21sim/extragalactic/clusters/halo.py b/fg21sim/extragalactic/clusters/halo.py
index 4e5f30f..29262b8 100644
--- a/fg21sim/extragalactic/clusters/halo.py
+++ b/fg21sim/extragalactic/clusters/halo.py
@@ -62,12 +62,10 @@ import numpy as np
from . import helper
from .solver import FokkerPlanckSolver
-from .emission import SynchrotronEmission
from ...share import CONFIGS, COSMO
from ...utils.units import (Units as AU,
UnitConversions as AUC,
Constants as AC)
-from ...utils.convert import Fnu_to_Tb
logger = logging.getLogger(__name__)
@@ -494,178 +492,6 @@ class RadioHalo:
else:
raise ValueError("given electron spectrum has wrong shape!")
- def calc_emissivity(self, frequencies, n_e=None, gamma=None, B=None):
- """
- Calculate the synchrotron emissivity for the derived electron
- spectrum.
-
- Parameters
- ----------
- frequencies : float, or 1D `~numpy.ndarray`
- The frequencies where to calculate the synchrotron emissivity.
- Unit: [MHz]
- n_e : 1D `~numpy.ndarray`, optional
- The electron spectrum (w.r.t. Lorentz factors γ).
- If not provided, then use the cached ``self.electron_spec``
- that was solved at above.
- Unit: [cm^-3]
- gamma : 1D `~numpy.ndarray`, optional
- The Lorentz factors γ of the electron spectrum.
- If not provided, then use ``self.gamma``.
- B : float, optional
- The magnetic field strength.
- If not provided, then use ``self.B_obs``.
- Unit: [uG]
-
- Returns
- -------
- emissivity : float, or 1D `~numpy.ndarray`
- The calculated synchrotron emissivity at each specified
- frequency.
- Unit: [erg/s/cm^3/Hz]
- """
- if n_e is None:
- n_e = self.electron_spec
- if gamma is None:
- gamma = self.gamma
- if B is None:
- B = self.B_obs
- syncem = SynchrotronEmission(gamma=gamma, n_e=n_e, B=B)
- emissivity = syncem.emissivity(frequencies)
- return emissivity
-
- def calc_power(self, frequencies, emissivity=None, **kwargs):
- """
- Calculate the halo synchrotron power (i.e., power *emitted* per
- unit frequency) by assuming the emissivity is uniform throughout
- the halo volume.
-
- NOTE
- ----
- The calculated power (a.k.a. spectral luminosity) is in units of
- [W/Hz] which is common in radio astronomy, instead of [erg/s/Hz].
- 1 [W] = 1e7 [erg/s]
-
- Parameters
- ----------
- frequencies : float, or 1D `~numpy.ndarray`
- The frequencies where to calculate the synchrotron power.
- Unit: [MHz]
- emissivity : float, or 1D `~numpy.ndarray`, optional
- The synchrotron emissivity at the input frequencies.
- If not provided, then invoke above ``calc_emissivity()``
- method to calculate them.
- Unit: [erg/s/cm^3/Hz]
- **kwargs : optional arguments, i.e., ``n_e``, ``gamma``, and ``B``.
-
- Returns
- -------
- power : float, or 1D `~numpy.ndarray`
- The calculated synchrotron power at each input frequency.
- Unit: [W/Hz]
- """
- frequencies = np.asarray(frequencies)
- if emissivity is None:
- emissivity = self.calc_emissivity(frequencies=frequencies,
- **kwargs)
- else:
- emissivity = np.asarray(emissivity)
- if emissivity.shape != frequencies.shape:
- raise ValueError("input 'frequencies' and 'emissivity' "
- "do not match")
- power = emissivity * (self.volume * AUC.kpc2cm**3) # [erg/s/Hz]
- power *= 1e-7 # [erg/s/Hz] -> [W/Hz]
- return power
-
- def calc_flux(self, frequencies, **kwargs):
- """
- Calculate the synchrotron flux density (i.e., power *observed*
- per unit frequency) of the halo, with k-correction considered.
-
- NOTE
- ----
- The *k-correction* must be applied to the flux density (Sν) or
- specific luminosity (Lν) because the redshifted object is emitting
- flux in a different band than that in which you are observing.
- And the k-correction depends on the spectrum of the object in
- question. For any other spectrum (i.e., vLv != const.), the flux
- density Sv is related to the specific luminosity Lv by:
- Sv = (1+z) L_v(1+z) / (4π DL^2),
- where
- * L_v(1+z) is the specific luminosity emitting at frequency v(1+z),
- * DL is the luminosity distance to the object at redshift z.
-
- Reference: Ref.[hogg1999],Eq.(22)
-
- Parameters
- ----------
- frequencies : float, or 1D `~numpy.ndarray`
- The frequencies where to calculate the flux density.
- Unit: [MHz]
- **kwargs : optional arguments, i.e., ``n_e``, ``gamma``, and ``B``.
-
- Returns
- -------
- flux : float, or 1D `~numpy.ndarray`
- The calculated flux density w.r.t. each input frequency.
- Unit: [Jy] = 1e-23 [erg/s/cm^2/Hz] = 1e-26 [W/m^2/Hz]
- """
- z = self.z_obs
- freqz = np.asarray(frequencies) * (1+z)
- power = self.calc_power(freqz, **kwargs) # [W/Hz]
- DL = COSMO.DL(self.z_obs) * AUC.Mpc2m # [m]
- flux = 1e26 * (1+z) * power / (4*np.pi * DL*DL) # [Jy]
- return flux
-
- def calc_brightness_mean(self, frequencies, flux=None, pixelsize=None,
- **kwargs):
- """
- Calculate the mean surface brightness (power observed per unit
- frequency and per unit solid angle) expressed in *brightness
- temperature* at the specified frequencies.
-
- NOTE
- ----
- If the solid angle that the object extends is smaller than the
- specified pixel area, then is is assumed to have size of 1 pixel.
-
- Parameters
- ----------
- frequencies : float, or 1D `~numpy.ndarray`
- The frequencies where to calculate the mean brightness temperature
- Unit: [MHz]
- flux : float, or 1D `~numpy.ndarray`, optional
- The flux density w.r.t. each input frequency.
- Unit: [Jy]
- pixelsize : float, optional
- The pixel size of the output simulated sky image.
- If not provided, then invoke above ``calc_flux()`` method to
- calculate them.
- Unit: [arcsec]
- **kwargs : optional arguments, i.e., ``n_e``, ``gamma``, and ``B``.
-
- Returns
- -------
- Tb : float, or 1D `~numpy.ndarray`
- The mean brightness temperature at each frequency.
- Unit: [K] <-> [Jy/pixel]
- """
- frequencies = np.asarray(frequencies)
- if flux is None:
- flux = self.calc_flux(frequencies=frequencies, **kwargs) # [Jy]
- else:
- flux = np.asarray(flux)
- if flux.shape != frequencies.shape:
- raise ValueError("input 'frequencies' and 'flux' do not match")
-
- omega = np.pi * self.angular_radius**2 # [arcsec^2]
- if pixelsize and (omega < pixelsize**2):
- omega = pixelsize ** 2 # [arcsec^2]
- logger.warning("Halo size < 1 pixel; force to be 1 pixel!")
-
- Tb = Fnu_to_Tb(flux, omega, frequencies) # [K]
- return Tb
-
def fp_injection(self, gamma, t=None):
"""
Electron injection (rate) term for the Fokker-Planck equation.