diff options
Diffstat (limited to 'fg21sim/extragalactic/clusters')
| -rw-r--r-- | fg21sim/extragalactic/clusters/halo.py | 50 | ||||
| -rw-r--r-- | fg21sim/extragalactic/clusters/helper.py | 106 |
2 files changed, 116 insertions, 40 deletions
diff --git a/fg21sim/extragalactic/clusters/halo.py b/fg21sim/extragalactic/clusters/halo.py index d11004f..f056735 100644 --- a/fg21sim/extragalactic/clusters/halo.py +++ b/fg21sim/extragalactic/clusters/halo.py @@ -48,7 +48,6 @@ from .emission import SynchrotronEmission from ...share import CONFIGS, COSMO from ...utils.units import (Units as AU, UnitConversions as AUC) -from ...utils.convert import Fnu_to_Tb_fast logger = logging.getLogger(__name__) @@ -285,15 +284,9 @@ class RadioHalo: def calc_power(self, emissivity): """ - Calculate the synchrotron power (i.e., power *emitted* per + Calculate the halo synchrotron power (i.e., power *emitted* per unit frequency) from emissivity. - 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 ---------- emissivity : float, or 1D `~numpy.ndarray` @@ -306,10 +299,7 @@ class RadioHalo: The calculated synchrotron power w.r.t. each input emissivity. Unit: [W/Hz] """ - emissivity = np.asarray(emissivity) - power = emissivity * self.volume # [erg/s/Hz] - power *= 1e-7 # [erg/s/Hz] -> [W/Hz] - return power + return helper.calc_power(emissivity, volume=self.volume) def calc_flux(self, emissivity): """ @@ -329,29 +319,21 @@ class RadioHalo: Unit: [Jy] = 1e-23 [erg/s/cm^2/Hz] = 1e-26 [W/m^2/Hz] """ power = self.calc_power(emissivity) # [W/Hz] - DL = COSMO.DL(self.z_obs) * AUC.Mpc2m # [m] - flux = 1e26 * power / (4*np.pi * DL*DL) # [Jy] - return flux + return helper.calc_flux(power, z=self.z_obs) - def calc_brightness_mean(self, emissivity, frequencies, pixelsize=None): + def calc_brightness_mean(self, emissivity, frequency, pixelsize=None): """ Calculate the mean surface brightness (power observed per unit - frequency and per unit solid angle) at the specified frequencies - from emissivity. - - NOTE - ---- - If the solid angle that the radio halo extends is smaller than - the specified pixel area, then the halo is assumed to cover a - solid angle of 1 pixel. + frequency and per unit solid angle) expressed in *brightness + temperature* at the specified frequencies from emissivity. Parameters ---------- emissivity : float, or 1D `~numpy.ndarray` The synchrotron emissivity at multiple frequencies. Unit: [erg/s/cm^3/Hz] - frequencies : float, or 1D `~numpy.ndarray` - The frequencies where to calculate the synchrotron emissivity. + frequency : float, or 1D `~numpy.ndarray` + The frequencies where the synchrotron emissivity is calculated. Unit: [MHz] pixelsize : float, optional The pixel size of the output simulated sky image. @@ -364,21 +346,9 @@ class RadioHalo: Unit: [K] <-> [Jy/pixel] """ omega = np.pi * self.angular_radius**2 # [arcsec^2] - if pixelsize: - pixelarea = pixelsize ** 2 # [arcsec^2] - if omega < pixelarea: - omega = pixelarea - logger.warning("Halo sky coverage (%.2f [arcsec^2])" % omega + - " < pixel area (%.2f [arcsec^2])" % pixelarea) - flux = self.calc_flux(emissivity) - Tb = [Fnu_to_Tb_fast(Fnu, omega, freq) - for Fnu, freq in zip(np.array(flux, ndmin=1), - np.array(frequencies, ndmin=1))] - if len(Tb) == 1: - return Tb[0] - else: - return np.array(Tb) + return helper.calc_brightness_mean(flux, frequency=frequency, + omega=omega, pixelsize=pixelsize) def fp_injection(self, gamma, t=None): """ diff --git a/fg21sim/extragalactic/clusters/helper.py b/fg21sim/extragalactic/clusters/helper.py index 0d66dee..4b7185f 100644 --- a/fg21sim/extragalactic/clusters/helper.py +++ b/fg21sim/extragalactic/clusters/helper.py @@ -27,6 +27,7 @@ References http://adsabs.harvard.edu/abs/2014MNRAS.438..124Z """ +import logging import numpy as np from scipy import integrate @@ -35,6 +36,10 @@ from ...share import CONFIGS, COSMO from ...utils.units import (Units as AU, Constants as AC, UnitConversions as AUC) +from ...utils.convert import Fnu_to_Tb_fast + + +logger = logging.getLogger(__name__) def radius_virial(mass, z=0.0): @@ -293,3 +298,104 @@ def magnetic_field(mass): M_mean = 1.6e15 # [Msun] B = b_mean * (mass/M_mean) ** b_index return B + + +def calc_power(emissivity, volume): + """ + Calculate the synchrotron power (i.e., power *emitted* per unit + frequency) from emissivity, which assumed to be uniform within + the 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 + ---------- + emissivity : float, or 1D `~numpy.ndarray` + The synchrotron emissivity at multiple frequencies. + Unit: [erg/s/cm^3/Hz] + volume : float + The volume of the radio halo + Unit: [kpc^3] + + Returns + ------- + power : float, or 1D `~numpy.ndarray` + The calculated synchrotron power w.r.t. each input emissivity. + Unit: [W/Hz] + """ + emissivity = np.asarray(emissivity) + power = emissivity * (volume * AUC.kpc2cm**3) # [erg/s/Hz] + power *= 1e-7 # [erg/s/Hz] -> [W/Hz] + return power + + +def calc_flux(power, z): + """ + Calculate the synchrotron flux density (i.e., power *observed* + per unit frequency) from radio power at a certain redshift (i.e., + distance). + + Parameters + ---------- + power : float, or 1D `~numpy.ndarray` + The synchrotron power at multiple frequencies. + Unit: [W/Hz] + + Returns + ------- + flux : float, or 1D `~numpy.ndarray` + The calculated synchrotron flux w.r.t. each input power. + Unit: [Jy] = 1e-23 [erg/s/cm^2/Hz] = 1e-26 [W/m^2/Hz] + """ + DL = COSMO.DL(z) * AUC.Mpc2m # [m] + flux = 1e26 * power / (4*np.pi * DL*DL) # [Jy] + return flux + + +def calc_brightness_mean(flux, frequency, omega, pixelsize=None): + """ + Calculate the mean surface brightness (power observed per unit + frequency and per unit solid angle) expressed in *brightness + temperature* at the specified frequencies from flux. + + 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 + ---------- + flux : float, or 1D `~numpy.ndarray` + The synchrotron flux densities at multiple frequencies. + Unit: [Jy] + frequency : float, or 1D `~numpy.ndarray` + The frequencies where the above flux calculated. + Unit: [MHz] + omega : float + The sky coverage (angular size) of the object. + Unit: [arcsec^2] + pixelsize : float, optional + The pixel size of the output simulated sky image. + Unit: [arcsec] + + Returns + ------- + Tb : float, or 1D `~numpy.ndarray` + The mean surface brightness at each frequency. + Unit: [K] <-> [Jy/pixel] + """ + if pixelsize and (omega < pixelsize**2): + omega = pixelsize ** 2 # [arcsec^2] + logger.warning("Object sky coverage < 1 pixel; force to be 1 pixel") + + Tb = [Fnu_to_Tb_fast(Fnu, omega, freq) + for Fnu, freq in zip(np.array(flux, ndmin=1), + np.array(frequency, ndmin=1))] + if len(Tb) == 1: + return Tb[0] + else: + return np.array(Tb) |