diff options
Diffstat (limited to 'fg21sim/extragalactic/clusters.py')
| -rw-r--r-- | fg21sim/extragalactic/clusters.py | 55 |
1 files changed, 45 insertions, 10 deletions
diff --git a/fg21sim/extragalactic/clusters.py b/fg21sim/extragalactic/clusters.py index b20d261..8249e3a 100644 --- a/fg21sim/extragalactic/clusters.py +++ b/fg21sim/extragalactic/clusters.py @@ -175,7 +175,7 @@ class GalaxyClusters: logger.info("Adopted dimensionless Hubble parameter: {0}".format(h)) # Cluster masses, unit: solMass (NOTE: h dependence) self.catalog["mass"] = (self.catalog["m"] * - self.catalog_prop["m_particles"].value / h) + self.catalog_prop["m_particle"].value / h) self.units["mass"] = au.solMass logger.info("Catalog: calculated cluster masses") # Cluster distances from the observer, unit: Mpc @@ -199,7 +199,8 @@ class GalaxyClusters: fullsky = 4*np.pi * au.sr factor = float(fullsky / self.catalog_prop["coverage"]) n0_cluster = len(self.catalog) - logger.info("Halo fraction in clusters: %f" % self.halo_fraction) + logger.info("Radio halo fraction in clusters: {0}".format( + self.halo_fraction)) # Total number of clusters on the full sky N_cluster = int(n0_cluster * factor * self.halo_fraction) logger.info("Total number of clusters on the full sky: {0:,}".format( @@ -281,10 +282,10 @@ class GalaxyClusters: Attributes ---------- catalog["r_vir"] : 1D `~numpy.ndarray` - The virial radii (unit: Mpc) calculated from the cluster masses + The virial radii (unit: Mpc) calculated from the cluster masses catalog["size_major"], catalog["size_minor] : 1D `~numpy.ndarray` - The major and minor axes (unit: degree) of the clusters calculated - from the above virial radii and the random eccentricities. + The major and minor axes (unit: degree) of the clusters calculated + from the above virial radii and the random eccentricities. NOTE ---- @@ -308,7 +309,7 @@ class GalaxyClusters: # Calculate (elliptical) angular sizes, i.e., major and minor axes logger.info("Calculating the elliptical angular sizes ...") distance = self.catalog["distance"].data * self.units["distance"] - theta2 = float(2 * r_vir / distance) # [ rad ] + theta2 = (r_vir / distance).decompose().value # [ rad ] size_major = theta2 / (1 - self.catalog["eccentricity"]**2) ** 0.25 size_minor = theta2 * (1 - self.catalog["eccentricity"]**2) ** 0.25 self.catalog["size_major"] = size_major * au.rad.to(au.deg) @@ -325,6 +326,16 @@ class GalaxyClusters: Then, derive the radio luminosity by employing the scaling relation between X-ray and radio luminosity. + Attributes + ---------- + catalog["luminosity"] : 1D `~numpy.ndarray` + The luminosity density (at 1.4 GHz) of each cluster. + catalog_prop["luminosity_freq"] : `~astropy.units.Quantity` + The frequency (as an ``astropy`` quantity) where the above + luminosity derived. + units["luminosity"] : `~astropy.units.Unit` + The unit used by the above luminosity. + XXX/TODO -------- The scaling relations used here may be outdated, and some of the @@ -367,7 +378,9 @@ class GalaxyClusters: # Hubble parameter conversion factor h_conv1 = (h_our / h_others) ** (b_X-2) # X-ray luminosity (0.1-2.4 keV) [ erg/s ] - L_X = (a_X * 1e45 * float(mass_RB / (1e15*au.solMass))**b_X) * h_conv1 + L_X = ((a_X * 1e45 * + (mass_RB / (1e15*au.solMass)).decompose().value ** b_X) * + h_conv1) # Calculate the radio luminosity from X-ray luminosity a_r = 2.78 b_r = 1.94 @@ -380,6 +393,24 @@ class GalaxyClusters: self.units["luminosity"] = au.W / au.Hz logger.info("Done Calculate the radio luminosity") + def _calc_specindex(self): + """Calculate the radio spectral indexes for each cluster. + + Attributes + ---------- + catalog["specindex"] : 1D `~numpy.ndarray` + The radio spectral index of each cluster. + + XXX/TODO + -------- + Currently, a common/uniform spectral index (1.2) is assumed for all + clusters, which may be improved by investigating more recent results. + """ + specindex = 1.2 + logger.info("Use common spectral index for all clusters: " + "{0}".format(specindex)) + self.catalog["specindex"] = specindex + def _calc_Tb(self, luminosity, distance, specindex, frequency, size): """Calculate the brightness temperature at requested frequency by assuming a power-law spectral shape. @@ -453,6 +484,9 @@ class GalaxyClusters: logger.info("Simulating HEALPix templates for each cluster ...") templates = [] resolution = self.resolution.to(au.deg).value + # Make sure the index is reset, therefore, the *row indexes* can be + # simply used to identify the corresponding template image. + self.catalog.reset_index(inplace=True) # XXX/TODO: be parallel for row in self.catalog.itertuples(): # TODO: progress bar @@ -492,8 +526,8 @@ class GalaxyClusters: -------- `self._simulate_template()` for more detailed description. """ - name = data.name - hpidx, hpval = self.templates[name] + index = data.Index + hpidx, hpval = self.templates[index] # Calculate the brightness temperature luminosity = data.luminosity distance = data.distance @@ -525,7 +559,7 @@ class GalaxyClusters: history) for the simulated products. """ header = fits.Header() - header["COMP"] = ("extragalactic clusters of galaxies (radio halos)", + header["COMP"] = ("Extragalactic clusters of galaxies", "Emission component") header["UNIT"] = ("Kelvin", "Map unit") header["CREATOR"] = (__name__, "File creator") @@ -586,6 +620,7 @@ class GalaxyClusters: # self._calc_sizes() self._calc_luminosity() + self._calc_specindex() # self._simulate_templates() # |