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* clusters/psformalism: Use functools.lru_cache()Aaron LI2017-10-231-0/+3
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* clusters/halo: merge halo_rprofile() & draw_halo(); Fix halo radius errorAaron LI2017-10-232-40/+28
| | | | | | | * Fix the error that misses to divide the halo radius by 3 for the e-folding radius, which causes the generated halo image has a 3x size! * Merge function "halo_rprofile()" into "draw_halo()" * Skip transform circular halo into elliptical one if "felong" is None
* clusters/halo: Use "lru_cache()", also improves some performanceAaron LI2017-10-233-13/+26
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* clusters/formation: Fix problem that no mergers occurredAaron LI2017-10-222-2/+9
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* clusters/halo: Add "use_max_merger" option to allow use max merger eventsAaron LI2017-10-221-20/+30
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* clusters/formation: Add method to found the maximum merger eventAaron LI2017-10-221-1/+51
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* clusters/halo: Add option "kT_out" to tune cluster temperatureAaron LI2017-10-222-5/+7
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* clusters/halo: Rewrite turbulence acceleration & diffusion coefficient!Aaron LI2017-10-212-58/+92
| | | | | | | | | | | | The previous calculation of the turbulence acceleration efficiency has significant problems, which is too low, i.e., the acceleration timescale is too large (~10 Gyr). However, it is reported that turbulent acceleration has a timescale ~100 Myr (0.1 Gyr). I believe this problem is due to the over-simplification to the formula proposed by [cassano2005]. Rewrite the turbulence acceleration and diffusion coefficient calculations, adopting the method proposed by [brunetti2016]. To this end, two new options "f_lturb" and "f_acc" are introduced to tune the results.
* clusters/halos: Add more cluster and halo propertiesAaron LI2017-10-212-12/+39
| | | | | | * Rvir0, Rvir_main, Rvir_sub * kT_main, kT_sub (replace kT_merger) * radius -> Rhalo, angular_radius -> Rhalo_angular, B -> B0
* clusters: Fix a comment about "felong"Aaron LI2017-10-211-2/+1
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* clusters/halo: Add function "speed_sound()"Aaron LI2017-10-211-0/+28
| | | | Also add "gamma" the adiabatic index of ideal gas to utils/units.py
* clusters/halo: Determine magnetic field by fraction of its energy densityAaron LI2017-10-202-32/+26
| | | | | | | | | | * Rewrite "magnetic_field()" function to calculate the mean magnetic field strength within ICM according its energy density fraction w.r.t. the ICM thermal energy density. * Remove config options "b_mean" and "b_index", which are replaced with the option "eta_b", the assumed magnetic energy density fraction w.r.t. the ICM thermal energy density.
* clusters/halo: Remove "mass_to_kT()", replaced by "kT_cluster()"Aaron LI2017-10-201-39/+0
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* clusters/halo: Add "kT_obs" and "tback_merger" propertiesAaron LI2017-10-192-2/+19
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* clusters/halo: Use "kT_cluster()" instead of "mass_to_kT()"Aaron LI2017-10-192-4/+4
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* clusters/halo: Add kT_cluster() to calculate the cluster ICM temperatureAaron LI2017-10-191-0/+25
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* clusters/helper: Add kT_virial() to calculate the virial temperatureAaron LI2017-10-191-0/+36
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* clusters/halo: rewrite power/flux/Tb calc with k-correction consideredAaron LI2017-10-193-130/+98
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* clusters/halo: Fix load halos data; fix save halos catalogAaron LI2017-10-191-27/+28
| | | | | The "template" item should be removed before convert the halos data into a Pandas DataFrame to be saved.
* clusters/halo: Force to use cluster catalog if use_dump_halos_data=TrueAaron LI2017-10-191-0/+5
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* clusters/halo: Support use the previously dumped halos raw dataAaron LI2017-10-191-1/+11
| | | | | | Add option "use_dump_halos_data" to control whether to just use the previously dumped halos data, therefore, the radio emissions at additional frequencies can be simply calculated.
* cluster/halos: Split out "_calc_halos_emission()" methodAaron LI2017-10-191-11/+32
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* clusters/halo: Add set_electron_spectrum() method; update doc a bitAaron LI2017-10-191-1/+26
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* clusters/halo: Add and use attribute "self.halos_data_dumpfile"Aaron LI2017-10-191-2/+4
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* clusters/halo: Rewrite halos catalog and raw data saveAaron LI2017-10-191-15/+39
| | | | | Replace option "halos_dumpfile" with "halos_catalog_outfile", and use option "dump_halos_data" to control whether to dump the raw data.
* clusters: "catalog_outfile" is requiredAaron LI2017-10-191-3/+1
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* clusters/halo: Improve time step determination a bitAaron LI2017-10-192-3/+6
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* clusters/halo: Increase the time step, but require a minimum of 20 stepsAaron LI2017-10-181-0/+7
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* clusters: Update radio halo radius estimationAaron LI2017-10-182-23/+25
| | | | | | | | | The simulated radio halo is assumed to have a radius of the falling sub-cluster; while previously it is assumed to be 1/4 of the virial radius of the merged cluster. The new estimation can agree better with the currently observed radio halos, which generally have a angular diameter size of ~2-7 [arcmin].
* clusters: More regular shape for radio halosAaron LI2017-10-161-6/+5
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* clusters: Update the documents/comments a b itAaron LI2017-10-142-11/+6
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* clusters/solver.py: Add FokkerPlanckTests with 3 casesAaron LI2017-10-121-9/+158
| | | | | | | | The FokkerPlanckSolver is validated with all the 3 test cases! References: * Park & Petrosian 1996, ApJS, 103, 255 * Donnert & Brunetti 2014, MNRAS, 443, 3564
* clusters/solver.py: significantly improve fix_boundary()Aaron LI2017-10-121-10/+30
| | | | Also suggest that ``buffer_np`` be specified to 5%-10% of ``x_np``.
* clusters/solver.py: Small tweaksAaron LI2017-10-071-8/+6
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* clusters/solver.py: Adjust parameter tc,uc ordersAaron LI2017-10-061-10/+7
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* clusters/solver.py: Stop calc. at "tstop" by adding "tstep" parameterAaron LI2017-10-061-12/+19
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* clusters/solver.py: Update comments/references/descriptions etc.Aaron LI2017-10-061-25/+31
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* clusters/psformalism.py: Rewrite sample_z_m() methodAaron LI2017-10-042-38/+54
| | | | | Also update clusters/main.py to calculate the halo mass distributions before sampling the mass and redshifts for clusters.
* clusters: Use "hmf" to calculate halo mass functions/distributionsAaron LI2017-10-041-69/+136
| | | | | | | | | | | | * New dependency "hmf" (halo mass functions) module * Calculate halo mass distributions/functions (dndlnm) with respect to masses and redshifts, instead of use the previous data file ("ps_data") * New section "[extragalactic][psformalism]" in configurations * New functions to write and read the dndlnm data TODO: * update the method to sample (mass, redshift) for clusters from the dndlnm data
* clusters/psformalism.py: Improve catalog commentsAaron LI2017-10-021-4/+7
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* clusters/emission: Assume electron pitch angle be pi/2Aaron LI2017-09-201-23/+17
| | | | And some cleanup and small changes
* clusters/emission: Rewrite synchrotron kernel functionAaron LI2017-09-201-9/+38
| | | | | | | | | | | Add asymptotic functions to calculate the values beyond the interpolation bounds (e.g., <1e-3 and >10), otherwise, the calculated synchrotron emissivity is overestimated at the higher frequencies. By rewrite this synchrotron kernel function, the calculated results is consistent with the theoretical/analytical results, e.g., the synchrotron radiation of a population of electrons of power-law index n is also a power-law with index (n-1)/2.
* clusters: Add option "use_output_catalog" to continue halo simulationAaron LI2017-09-031-4/+19
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* clusters: Add config option "boost"Aaron LI2017-09-011-2/+5
| | | | | | | NOTE: The cluster number (especially the bright ones) may be rather small within a sky patch. This ``boost`` config option increase the expected cluster number by a specified times, for better testing purpose.
* Update "Fnu_to_Tb_fast()" to "Fnu_to_Tb()"Aaron LI2017-09-016-9/+9
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* clusters/psformalism: Remove config "f_darkmatter"Aaron LI2017-08-291-3/+2
| | | | Use "1 - baryon_fraction = 1 - Ob0/Om0" to replace "f_darkmatter".
* clusters/halo.py: Update injection rate calculationAaron LI2017-08-261-10/+5
| | | | | The electrons are assumed to be injected throughout the whole cluster ICM/volume.
* Return the list of filepath to the written sky filesAaron LI2017-08-261-0/+8
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* clusters/main.py: Update sky header; update comments etc.Aaron LI2017-08-261-5/+7
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* configs: Remove option "save"; all enabled components will be savedAaron LI2017-08-261-1/+0
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