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* | clusters/halo: Add function "speed_sound()" | Aaron LI | 2017-10-21 | 2 | -0/+31 | |
| | | | | Also add "gamma" the adiabatic index of ideal gas to utils/units.py | |||||
* | clusters/halo: Determine magnetic field by fraction of its energy density | Aaron LI | 2017-10-20 | 3 | -40/+30 | |
| | | | | | | | | | | * 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 LI | 2017-10-20 | 1 | -39/+0 | |
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* | clusters/halo: Add "kT_obs" and "tback_merger" properties | Aaron LI | 2017-10-19 | 2 | -2/+19 | |
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* | clusters/halo: Use "kT_cluster()" instead of "mass_to_kT()" | Aaron LI | 2017-10-19 | 2 | -4/+4 | |
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* | clusters/halo: Add kT_cluster() to calculate the cluster ICM temperature | Aaron LI | 2017-10-19 | 1 | -0/+25 | |
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* | clusters/helper: Add kT_virial() to calculate the virial temperature | Aaron LI | 2017-10-19 | 1 | -0/+36 | |
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* | clusters/halo: rewrite power/flux/Tb calc with k-correction considered | Aaron LI | 2017-10-19 | 3 | -130/+98 | |
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* | Bump version to v0.6.2v0.6.2 | Aaron LI | 2017-10-19 | 1 | -1/+1 | |
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* | clusters/halo: Fix load halos data; fix save halos catalog | Aaron LI | 2017-10-19 | 1 | -27/+28 | |
| | | | | | The "template" item should be removed before convert the halos data into a Pandas DataFrame to be saved. | |||||
* | clusters: Update configuration defaults and description | Aaron LI | 2017-10-19 | 1 | -12/+12 | |
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* | clusters/halo: Force to use cluster catalog if use_dump_halos_data=True | Aaron LI | 2017-10-19 | 1 | -0/+5 | |
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* | clusters/halo: Support use the previously dumped halos raw data | Aaron LI | 2017-10-19 | 3 | -1/+26 | |
| | | | | | | 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()" method | Aaron LI | 2017-10-19 | 1 | -11/+32 | |
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* | clusters/halo: Add set_electron_spectrum() method; update doc a bit | Aaron LI | 2017-10-19 | 1 | -1/+26 | |
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* | clusters/halo: Add and use attribute "self.halos_data_dumpfile" | Aaron LI | 2017-10-19 | 1 | -2/+4 | |
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* | clusters/halo: Rewrite halos catalog and raw data save | Aaron LI | 2017-10-19 | 2 | -18/+50 | |
| | | | | | 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 required | Aaron LI | 2017-10-19 | 2 | -3/+3 | |
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* | clusters/halo: Improve time step determination a bit | Aaron LI | 2017-10-19 | 2 | -3/+6 | |
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* | clusters/halo: Increase the time step, but require a minimum of 20 steps | Aaron LI | 2017-10-18 | 2 | -1/+8 | |
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* | clusters: Update radio halo radius estimation | Aaron LI | 2017-10-18 | 2 | -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]. | |||||
* | utils/units.py: add "rad2arcmin" and some cleanup/simplifications | Aaron LI | 2017-10-18 | 1 | -16/+20 | |
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* | utils/analyze.py: countdist_integrated(): Add xmin and xmax param. | Aaron LI | 2017-10-18 | 1 | -2/+15 | |
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* | clusters: More regular shape for radio halos | Aaron LI | 2017-10-16 | 1 | -6/+5 | |
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* | configs: remove "filemode" option | Aaron LI | 2017-10-16 | 2 | -6/+2 | |
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* | clusters: Update the documents/comments a b it | Aaron LI | 2017-10-14 | 2 | -11/+6 | |
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* | clusters/solver.py: Add FokkerPlanckTests with 3 cases | Aaron LI | 2017-10-12 | 1 | -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 LI | 2017-10-12 | 1 | -10/+30 | |
| | | | | Also suggest that ``buffer_np`` be specified to 5%-10% of ``x_np``. | |||||
* | clusters/solver.py: Small tweaks | Aaron LI | 2017-10-07 | 1 | -8/+6 | |
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* | clusters/solver.py: Adjust parameter tc,uc orders | Aaron LI | 2017-10-06 | 1 | -10/+7 | |
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* | clusters/solver.py: Stop calc. at "tstop" by adding "tstep" parameter | Aaron LI | 2017-10-06 | 1 | -12/+19 | |
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* | clusters/solver.py: Update comments/references/descriptions etc. | Aaron LI | 2017-10-06 | 1 | -25/+31 | |
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* | clusters/psformalism.py: Rewrite sample_z_m() method | Aaron LI | 2017-10-04 | 2 | -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/distributions | Aaron LI | 2017-10-04 | 6 | -82/+230 | |
| | | | | | | | | | | | | * 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 | |||||
* | configs/manager.py: Add missing cosmology parameters | Aaron LI | 2017-10-04 | 1 | -0/+2 | |
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* | utils/cosmology.py: Add parameter Tcmb0 [K] | Aaron LI | 2017-10-04 | 2 | -6/+13 | |
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* | utils/units.py: Add "K2eV" and "K2keV" | Aaron LI | 2017-10-04 | 1 | -0/+2 | |
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* | configs: Use lower case for logging levels | Aaron LI | 2017-10-04 | 7 | -24/+18 | |
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* | bin/fg21sim-download-data: Update description | Aaron LI | 2017-10-04 | 1 | -2/+3 | |
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* | utils/cosmology: Add scalar spectral index "ns" | Aaron LI | 2017-10-04 | 2 | -4/+8 | |
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* | configs: Clean up some comments | Aaron LI | 2017-10-03 | 2 | -14/+0 | |
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* | utils/cosmology.py: Add methods Dc() and Dc_to_redshift() | Aaron LI | 2017-10-02 | 1 | -0/+48 | |
| | | | | | | * Dc(): simple wrapper on astropy cosmology's comoving_distance() * Dc_to_redshift(): determine the redshift w.r.t. the input comoving distances using interpolation. | |||||
* | clusters/psformalism.py: Improve catalog comments | Aaron LI | 2017-10-02 | 1 | -4/+7 | |
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* | Bump version to 0.6.1v0.6.1 | Aaron LI | 2017-09-26 | 1 | -1/+1 | |
| | | | | | | Component "extragalactic/clusters" is tuned and tested to work. Start working on radio relics from galaxy clusters. | |||||
* | utils/units.py: Add eV and keV to temperature conversions | Aaron LI | 2017-09-26 | 1 | -0/+3 | |
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* | clusters/emission: Assume electron pitch angle be pi/2 | Aaron LI | 2017-09-20 | 1 | -23/+17 | |
| | | | | And some cleanup and small changes | |||||
* | clusters/emission: Rewrite synchrotron kernel function | Aaron LI | 2017-09-20 | 1 | -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 simulation | Aaron LI | 2017-09-03 | 3 | -4/+36 | |
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* | configs: Update option descriptions; also tweak checkers a bit | Aaron LI | 2017-09-03 | 2 | -7/+12 | |
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* | utils/io.py: Add function "csv_to_dataframe()" to support CSV comments | Aaron LI | 2017-09-03 | 1 | -2/+35 | |
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