diff options
Diffstat (limited to 'fg21sim')
| -rw-r--r-- | fg21sim/extragalactic/clusters/emission.py | 80 |
1 files changed, 2 insertions, 78 deletions
diff --git a/fg21sim/extragalactic/clusters/emission.py b/fg21sim/extragalactic/clusters/emission.py index 38ad919..99f8a22 100644 --- a/fg21sim/extragalactic/clusters/emission.py +++ b/fg21sim/extragalactic/clusters/emission.py @@ -26,11 +26,7 @@ import scipy.special from scipy import integrate from scipy import interpolate -from ...utils import COSMO -from ...utils.units import (Units as AU, - UnitConversions as AUC, - Constants as AC) -from ...utils.convert import Fnu_to_Tb_fast +from ...utils.units import (Units as AU, Constants as AC) logger = logging.getLogger(__name__) @@ -48,22 +44,14 @@ class SynchrotronEmission: n_e : `~numpy.ndarray` Electron number density spectrum. Unit: [cm^-3] - z : float - Redshift of the cluster/halo been observed/simulated. B : float The assumed uniform magnetic field within the cluster ICM. Unit: [uG] - radius : float - The radius of the halo, within which the uniform magnetic field - and electron distribution are assumed. - Unit: [kpc] """ - def __init__(self, gamma, n_e, z, B, radius): + def __init__(self, gamma, n_e, B): self.gamma = np.asarray(gamma) self.n_e = np.asarray(n_e) - self.z = z self.B = B # [uG] - self.radius = radius # [kpc] @property def B_gauss(self): @@ -203,67 +191,3 @@ class SynchrotronEmission: return syncem[0] else: return syncem - - def power(self, nu): - """ - Calculate the synchrotron power (power emitted per frequency) - at the requested frequency. - - Returns - ------- - P_nu : float - Synchrotron power at frequency ``nu``. - Unit: [erg/s/Hz] - """ - r_cm = self.radius * AUC.kpc2cm - volume = (4.0/3.0) * np.pi * r_cm**3 - P_nu = self.emissivity(nu) * volume - return P_nu - - def flux(self, nu): - """ - Calculate the synchrotron flux (power observed per frequency) - at the requested frequency. - - Returns - ------- - F_nu : float - Synchrotron flux at frequency ``nu``. - Unit: [Jy] = 1e-23 [erg/s/cm^2/Hz] - """ - DL = COSMO.DL(self.z) * AUC.Mpc2cm # [cm] - P_nu = self.power(nu) - F_nu = 1e23 * P_nu / (4*np.pi * DL*DL) # [Jy] - return F_nu - - def brightness(self, nu, pixelsize): - """ - Calculate the synchrotron surface brightness (power observed - per frequency and per solid angle) at the specified frequency. - - NOTE - ---- - If the radio halo has solid angle less than the pixel area, then - it is assumed to have solid angle of 1 pixel. - - Parameters - ---------- - pixelsize : float - The pixel size of the output simulated sky image - Unit: [arcsec] - - Returns - ------- - Tb : float - Synchrotron surface brightness at frequency ``nu``. - Unit: [K] <-> [Jy/pixel] - """ - DA = COSMO.DL(self.z) * AUC.Mpc2cm # [cm] - radius = self.radius * AUC.kpc2cm # [cm] - omega = (np.pi * radius**2 / DA**2) * AUC.rad2deg**2 # [deg^2] - pixelarea = (pixelsize * AUC.arcsec2deg) ** 2 # [deg^2] - if omega < pixelarea: - omega = pixelarea - F_nu = self.flux(nu) - Tb = Fnu_to_Tb_fast(F_nu, omega, nu) - return Tb |