From 915bb22299a9927fcd3bce8456e4ae0dc99dac90 Mon Sep 17 00:00:00 2001
From: Aaron LI <aly@aaronly.me>
Date: Sun, 30 Jul 2017 10:19:43 +0800
Subject: cluster/halo.py: Add method "calc_brightness_mean()"

Signed-off-by: Aaron LI <aly@aaronly.me>
---
 fg21sim/extragalactic/clusters/halo.py | 48 ++++++++++++++++++++++++++++++++++
 1 file changed, 48 insertions(+)

(limited to 'fg21sim/extragalactic/clusters/halo.py')

diff --git a/fg21sim/extragalactic/clusters/halo.py b/fg21sim/extragalactic/clusters/halo.py
index adc2bc5..9c030a5 100644
--- a/fg21sim/extragalactic/clusters/halo.py
+++ b/fg21sim/extragalactic/clusters/halo.py
@@ -49,6 +49,7 @@ from ...configs import CONFIGS
 from ...utils import COSMO
 from ...utils.units import (Units as AU,
                             UnitConversions as AUC)
+from ...utils.convert import Fnu_to_Tb_fast
 
 
 logger = logging.getLogger(__name__)
@@ -314,6 +315,53 @@ class RadioHalo:
         flux = 1e26 * power / (4*np.pi * DL*DL)  # [Jy]
         return flux
 
+    def calc_brightness_mean(self, emissivity, frequencies, 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.
+
+        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.
+            Unit: [MHz]
+        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]
+        """
+        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)
+
     def fp_injection(self, gamma, t=None):
         """
         Electron injection (rate) term for the Fokker-Planck equation.
-- 
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