diff options
Diffstat (limited to 'fg21sim/extragalactic/clusters/halo.py')
| -rw-r--r-- | fg21sim/extragalactic/clusters/halo.py | 50 |
1 files changed, 10 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): """ |