aboutsummaryrefslogtreecommitdiffstats
Commit message (Collapse)AuthorAgeFilesLines
* utils/transform/circle2ellipse: skip rotation if it's NoneAaron LI2017-10-231-4/+5
|
* clusters/halo: Use "lru_cache()", also improves some performanceAaron LI2017-10-233-13/+26
|
* clusters/formation: Fix problem that no mergers occurredAaron LI2017-10-222-2/+9
|
* clusters/halo: Add "use_max_merger" option to allow use max merger eventsAaron LI2017-10-222-24/+40
|
* clusters/formation: Add method to found the maximum merger eventAaron LI2017-10-221-1/+51
|
* clusters/halo: Add option "kT_out" to tune cluster temperatureAaron LI2017-10-223-5/+16
|
* configs: Update option descriptionAaron LI2017-10-211-4/+5
|
* clusters/halo: Rewrite turbulence acceleration & diffusion coefficient!Aaron LI2017-10-213-60/+104
| | | | | | | | | | | | 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
|
* clusters/halo: Add function "speed_sound()"Aaron LI2017-10-212-0/+31
| | | | Also add "gamma" the adiabatic index of ideal gas to utils/units.py
* clusters/halo: Determine magnetic field by fraction of its energy densityAaron LI2017-10-203-40/+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 LI2017-10-201-39/+0
|
* clusters/halo: Add "kT_obs" and "tback_merger" propertiesAaron LI2017-10-192-2/+19
|
* clusters/halo: Use "kT_cluster()" instead of "mass_to_kT()"Aaron LI2017-10-192-4/+4
|
* clusters/halo: Add kT_cluster() to calculate the cluster ICM temperatureAaron LI2017-10-191-0/+25
|
* clusters/helper: Add kT_virial() to calculate the virial temperatureAaron LI2017-10-191-0/+36
|
* clusters/halo: rewrite power/flux/Tb calc with k-correction consideredAaron LI2017-10-193-130/+98
|
* Bump version to v0.6.2v0.6.2Aaron LI2017-10-191-1/+1
|
* 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: Update configuration defaults and descriptionAaron LI2017-10-191-12/+12
|
* clusters/halo: Force to use cluster catalog if use_dump_halos_data=TrueAaron LI2017-10-191-0/+5
|
* clusters/halo: Support use the previously dumped halos raw dataAaron LI2017-10-193-1/+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()" methodAaron LI2017-10-191-11/+32
|
* clusters/halo: Add set_electron_spectrum() method; update doc a bitAaron LI2017-10-191-1/+26
|
* clusters/halo: Add and use attribute "self.halos_data_dumpfile"Aaron LI2017-10-191-2/+4
|
* clusters/halo: Rewrite halos catalog and raw data saveAaron LI2017-10-192-18/+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 requiredAaron LI2017-10-192-3/+3
|
* clusters/halo: Improve time step determination a bitAaron LI2017-10-192-3/+6
|
* clusters/halo: Increase the time step, but require a minimum of 20 stepsAaron LI2017-10-182-1/+8
|
* 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].
* utils/units.py: add "rad2arcmin" and some cleanup/simplificationsAaron LI2017-10-181-16/+20
|
* utils/analyze.py: countdist_integrated(): Add xmin and xmax param.Aaron LI2017-10-181-2/+15
|
* clusters: More regular shape for radio halosAaron LI2017-10-161-6/+5
|
* configs: remove "filemode" optionAaron LI2017-10-162-6/+2
|
* clusters: Update the documents/comments a b itAaron LI2017-10-142-11/+6
|
* 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
|
* clusters/solver.py: Adjust parameter tc,uc ordersAaron LI2017-10-061-10/+7
|
* clusters/solver.py: Stop calc. at "tstop" by adding "tstep" parameterAaron LI2017-10-061-12/+19
|
* clusters/solver.py: Update comments/references/descriptions etc.Aaron LI2017-10-061-25/+31
|
* 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 LI2017-10-046-82/+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 parametersAaron LI2017-10-041-0/+2
|
* utils/cosmology.py: Add parameter Tcmb0 [K]Aaron LI2017-10-042-6/+13
|
* utils/units.py: Add "K2eV" and "K2keV"Aaron LI2017-10-041-0/+2
|
* configs: Use lower case for logging levelsAaron LI2017-10-047-24/+18
|
* bin/fg21sim-download-data: Update descriptionAaron LI2017-10-041-2/+3
|
* utils/cosmology: Add scalar spectral index "ns"Aaron LI2017-10-042-4/+8
|
Copyright © 2017-2018 Aaron LI. All Rights Reserved.