B d@sdZddlZddlmZy ddlZWnek r@edYnXddZ ddZ dd Z d d Z d d Z GdddZGdddZdVddZddZddZddZddZddZdd ZdWd"d#ZdXd$d%Zd&d'ZdYd(d)Zd*d+ZdZd,d-Zejfd.d/Zejfd0d1Zd2d3Z d4d5Z!d6d7Z"d[d9d:Z#d\d;d<Z$d=d>Z%d?d@Z&d]dBdCZ'd^dDdEZ(GdFdGdGZ)dHdIZ*dJdKZ+dLdMZ,dNdOZ-dPdQZ.dRdSZ/dTdUZ0dS)_z~ Various fitting formulas provided by numerical relativity Archisman Ghosh, Nathan K. Johnson-McDaniel, P. Ajith, 2015-04-09 NzCannot import lal SWIG bindingscCs0t|dkrtdt|dkr,tddS)Nrzm1 has to be positivezm2 has to be positive)npany ValueError)m1m2rh/work/yifan.wang/ringdown/master-ringdown-env/lib/python3.7/site-packages/lalinference/imrtgr/nrutils.py_check_msr cCs\t|dkrtdt|dkr,tdt|dkrBtdt|dkrXtddS)Nzchi1 has to be <= 1zchi2 has to be <= 1rzchi1 has to be nonnegativezchi2 has to be nonnegative)rrr)chi1chi2rrr _check_chisr cCs8tt|dkrtdtt|dkr4tddS)Nr zchi1 has to be <= 1zchi2 has to be <= 1)rrabsr)r r rrr_check_chi_aligned srcCst||t||dS)N)r r )rrr r rrr _check_mchi&s rcCst||t||dS)N)r r)rrr r rrr_check_mchi_aligned*s rc@s(eZdZdZdZdZdZdZdZdZ dS) bbh_final_state_fitsZPan2011HLZ2014ZPhenomDZ UIB2016v1UIB2016ZHBR2016HL2016N) __name__ __module__ __qualname__pan2011hlz2014phenD uib2016v1uib2016hbr2016hl2016rrrrr3src@s eZdZdZdZdZdZdZdS)bbh_Kerr_trunc_optsZTRUNCATEZTRUNCATESILENTZKEEPZIGNOREERRORN)rrrtrunc trunc_silentkeepignerrrrrrr =s r thiscCs||ttjkrtd||tjkrxtt|dkrxt |ttj frt t|dk}|tj kst|tj krt||d}|tj krtdt||f|||<nB|tjkrtd|t|fn |tjkrtd|t|fn|tj ks |tj kr>t|d}|tj kr8td|||f|}n:|tjkr\td||fn|tjkrxtd||f|S) Nz6Unknown user option '%s' for Kerr truncation behavior.g?zFTruncating %d excessive chif values from %s fit to Kerr limit of +-1.0zANote: %s fit predicts %d chif values in excess of the Kerr limit.z;%s fit predicts %d chif values in excess of the Kerr limit.z?Truncating excessive chif of %f from %s fit to Kerr limit of %fz=Note: %s fit predicts chif of %f in excess of the Kerr limit.z7%s fit predicts chif of %f in excess of the Kerr limit.)listr __dict__valuesrr%rrr isinstanceZndarraywherer"r#signprintsizer$r&)chifZbehaviorfitnameZidx_overZ chif_truncrrr_truncate_at_Kerr_limitFs0         r2cCsvttt|}ttt|}||}||||d}|dtdd|d|dd|dS)a Calculate the mass of the final BH resulting from the merger of two non-spinning black holes using eqn. 29a of from Pan et al, Phys Rev D 84, 124052 (2011). Parameters ---------- m1, m2 : component masses Returns ------ final mass, mf g@g?gqq?gV/?gQ?)r vectorizefloatarraysqrt)rrmetarrr#bbh_final_mass_non_spinning_Panetalcs r:cCsbttt|}ttt|}||||d}td|d|dd|dS)a Calculate the spin of the final BH resulting from the merger of two non-spinning black holes using eqn. 29b of Pan et al, Phys Rev D 84, 124052 (2011). Parameters ---------- m1, m2 : component masses Returns ------ final dimensionless spin, chif g@g(@g+@g&1@r3)rr4r5r6r7)rrr9rrr#bbh_final_spin_non_spinning_Panetalvs r;cCstt|d}dd|ddd|dd|d}td|d|d}t|}d|td|d|d||S)z Calculate the ISCO radius of a Kerr BH as a function of the Kerr parameter using eqns. 2.5 and 2.8 from Ori and Thorne, Phys Rev D 62, 24022 (2000) Parameters ---------- a : Kerr parameter Returns ------- ISCO radius g?g@gUUUUUU?g@r3)rminimumr6r7r-)aZz1Zz2Za_signrrrcalc_isco_radiuss , r?c Csrt||||||}||||}|||}|||||||d}|||||}||||fS)za Internal function to compute the combinations of masses and spins that are used in the RIT fits r<)r) rrr r r8r9delta_mSDeltarrr _RIT_setups  rCc Cs@||}||}||}||}d|||d|d||d||d||d||d||d|||d |||d |||d |||d |||d |||d|||d|||d|||d|||d|||d|||d||S)a8 Internal function to return the basic even-in-interchange-of-particles expression used in the RIT fits for the final mass, final spin, and peak luminosity The coefficients in the expression are passed as a vector as [0 1 2a 2b 2c 2d 3a 3b 3c 3d 4a 4b 4c 4d 4e 4f 4g 4h 4i] (giving the subscripts). g0@rr r<r3 r) r9r@rArBcoeffsS2dm2ZDeltadmZDelta2rrr_RIT_symm_expresss  rVcCs^t|}dt|d|dtd|}|dkrd}d} d} d} d } d } d }d }d }d}d}d}d}d}d}d}d}d}d}n^|dkrd}d} d} d} d} d} d}d }d!}d"}d#}d$}d%}d&}d'}d(}d)}d*}d+}ntd,||}||}||}t|||||| | | | | |||||||||||||g|d-d.|||||}t||S)/zh Internal function: the final spin with the Healy et al. fits is determined by minimizing this function r3r<g@2014g??g+,?gIJzZ¿gǁW˝g\7ugV*?g!Z+粿g1`U,~s?g3ۃgK= By_?gHPhgDXPhgyTq?g{h+g?/gZ?g01"Qhg'jinZ?gC2016g?gga?gxLÿg;#g<jg+O?g2[FgV+&U?gxoRgpIX?g2zcwg<[?x?gu[g%g-go]w2Wwgg^gBhg?gzILqt?gL|?낿gLֿ#޾ggHaϐ?g"1gsuv]gsgqE?gp O Ŀg?g|o@gxrrcCsttt|}ttt|}ttt|}ttt|}tt|dkrjtdtt|dkrtd||}||}|||}||}||}||} ||d|} ||d|} | | } | dd|} | | }|| }|| }d|d|d |d | dd |d || d |d||d|d||d|d||}|S)a} Calculate the spin of the final BH resulting from the merger of two black holes with non-precessing spins using the fits used by IMRPhenomD, given in Eqs. (3.6) and (3.8) of Husa et al. arXiv:1508.07250. Note that Eq. (3.8) gives the radiated energy, not the final mass directly m1, m2: component masses chi1, chi2: dimensionless spins of two BHs r zchi1 has to be in [-1, 1]zchi2 has to be in [-1, 1]r<g?g@gLXz @gVHԘ@gy.i"@g9+w\*@g,u5ȵ?gYf6Y@g&~˵?gQ1@g2.Ŭgo޽o@gb\,gOO*@)rr4r5r6rrr)rrr r r8r|r9r}r~rrrTrArZSsqZScuZSqur0rrrrvds.  trvcCsttt|}ttt|}ttt|}ttt|}t|dkrftdt|dkr|tdtt|dkrtdtt|dkrtd||}t|dkrtd||}||}||}|||}t|dkrtd t|d}t|d kr:td t |d }||} | |} | | } |||} |||} | | }||||||}||}||}||}||}t||krt |||}||}d }d }dd|d}||| | | ||||||||||fS)zP common setup function for UIB final-state and luminosity fit functions rzm1 must not be negativezm2 must not be negativer zchi1 has to be in [-1, 1]zchi2 has to be in [-1, 1]zm1+m2 must be positiveg?zTruncating eta from above to 0.25. This should only be necessary in some rounding corner cases, but better check your m1 and m2 inputs...gzTruncating negative eta to 0.0. This should only be necessary in some rounding corner cases, but better check your m1 and m2 inputs...g;f?gLXz?g?g@g?) rr4r5r6rrrr.r=maximumr-)rrr r r8r|Zm1sqZm2sqr9r}r~rrrTStotShatShat2Shat3Shat4chidiffchidiff2sqrt2sqrt3 sqrt1m4etarrrbbh_UIBfits_setupsV     rroc.CsRt||||\}}}}} } } } } }}}}}}|dkrd}d}d}d}d}d}d}d }d }d }d }d }d} d}!d}"d}#d}$d}%d}&d}'d}(d})d}*d}+nt|dkrd}d}d}d}d}d }d!}d"}d#}d$}d%}d&}d'} d(}!d)}"d}#d*}$d+}%d,}&d-}'d.}(d/})d0}*d1}+ntd2d3d4|||||||| d3||| |"|)|d5d5|"d6|)|||| ||#|d5d5|d6|#|||| | |*|d5d5| d6|*|d3||| |!|+|d5d5|!d6|+||$||d3|%|||'| ||d3|(|||&||},|d3|,}-|-S)7a Calculate the final mass with the aligned-spin NR fit by Xisco Jimenez Forteza, David Keitel, Sascha Husa et al. [LIGO-P1600270] [https://arxiv.org/abs/1611.00332] versions v1 and v2 use the same ansatz, with v2 calibrated to additional SXS and RIT data m1, m2: component masses chi1, chi2: dimensionless spins of two BHs Results are symmetric under simultaneous exchange of m1<->m2 and chi1<->chi2. rpg^I +?gzG?g(\?g cZgfa?g#{gfӌ˝t @gkG^9ĿgvH=>ĿgdM¿g J!@gΉt@g9@gTSn?gy<5?ggMe(qgx  g?gsw/g%wg2V,@gB3=mg|$5rog/$?g5^I ?gMb?gA`"˿gO*?gg-;A) @gqhʿg'0J:ɿgV*TĿgM@gq'@gAA?@gWl?gA?gppgYYZ g!R?gKetAg~g{#y/@gUSZ(tngq /vz1Unknown version -- should be either "v1" or "v2".g?gUUUUUUg0@g@)rr).rrr r rYr8r9r}r~rrrrrrrrrrrb10b20b30b50a2a3a4b1b2b3b5f20f30f50f10f21d10d11d20d30d31f11f31f51ZEradrrrrrssp , 9 rsc2Cst||||\}}}}} } } } } }}}}}}|dkrd}d}d}d}d}d}d}d }d }d }d }d }d} d}!d}"d}#d}$d}%d}&d}'d}(d})d}*d}+d},d}-d}.d}/n|dkr"d}d }d!}d}d"}d#}d$}d%}d&}d'}d(}d)}d*} d+}!d,}"d-}#d.}$d/}%d}&d0}'d1}(d2})d3}*d4}+d5},d6}-d7}.d8}/ntd9d:||||||||d;|||||| |%||,|d|,|||| |"||-|d|-||| | |#||.|d|.|d;||!| |$|/||&|d|&||'||d;|(|||*| ||d;|+|||)||}0|0| }1|1S)?a Calculate the final spin with the aligned-spin NR fit by Xisco Jimenez Forteza, David Keitel, Sascha Husa et al. [LIGO-P1600270] [https://arxiv.org/abs/1611.00332] versions v1 and v2 use the same ansatz, with v2 calibrated to additional SXS and RIT data m1, m2: component masses chi1, chi2: dimensionless spins of two BHs Results are symmetric under simultaneous exchange of m1<->m2 and chi1<->chi2. rpgQ@gRQ?gQ@gEȿg333333?g ?gw/gd-@gFpA#g #5@g++?gU)?gE 5+!@g;V7@ga^?gL3@ggy1D?guCu'@g& gg@gJI?5 g[YO?gB-Dg3.Yfg S:rog(\@g?g ףp= @gӼɵ?gD ?gI +gB$v<@gTkˇ"gW@g?gntA5?g o?gXon?g!@gIg!}6@g`i?gz|@gC=?gcPeG"@gJ2g #L@gLP> gz2`?gR@g&ˠ:cgz1Unknown version -- should be either "v1" or "v2".g@g?gP@g0@g@)rr)2rrr r rYr8r9r}r~rrrrrrrrrrrZa20Za30Za50rrrrrra5rrrrrrrrZf52rrrrrZf12Zf22Zf32rZLorbr0rrrrw*s , ]rwcCsbttt|}ttt|}ttt|}ttt|}||||||fS)z Setup function for the Hofmann, Barausse, and Rezzolla final spin fits to vectorize the masses and spins and calculate the mass ratio. )rr4r5r6)rrr r rrr_bbh_HBR2016_setups rc*Cs|dkr.d}d}d}d}d} d} d} d } d } n|d krd }d }d }d}d} d}d} d} d} d}d}d}d}d}d}d}d}d}d} nn|dkrd }d}d }d!}d"} d#}d$}d%} d&} d'} d(}d)}d*}d+}d,}d-}d.}d/}d0}d1}d2}d3}d4} ntd5||}||}||||}||||d6|d6|}|| |||} t| }!d6d7|!d8}"d9d6d:d;|!d:d8}#|dkr| | }$||| | |$|| | | | |$}%|d kr.||}&|&|}'|$| }(|%||||(|&||| ||$||(|'||| ||$||(}%|dkr`|%||||&||'||(| }%t|#d:||"d6||%})|)S)# @gd`@gL;gm4*g6[A@g6;Rg~:Uglxz,oW@g33333i@gMZbgm2x@g/${@g㥛 6}gʡEgx&k@gtDg#~jɅgCl獇@g(\;@g,V?zm2) chi1: the component of the dimensionless spin of m1 along the angular momentum (z) chi2: the component of the dimensionless spin of m2 along the angular momentum (z) gzq has to be > 0.g?zq has to be <= 1.)rr4r5r6rr+bbh_peak_luminosity_non_precessing_T1600018)rr r rrrrrbbh_aligned_Lpeak_6mode_SHXJDK^s   rcCsTttt|}ttt|}ttt|}ttt|}t||||\}}}}}} } } } } }}}}}dd|}|||||}||}||}||}||}dd|d|d|d|d||d d |d |d |d |d||d|d|d|d|d|d|}t|S)a5 Calculate the peak luminosity (using modes 22, 21, 33, 32, 44, and 43) of a binary black hole with aligned spins using the fit made by Sascha Husa, Xisco Jimenez Forteza, David Keitel [LIGO-T1500598] using 5th order in chieff and return results in units of 10^56 ergs/s m1, m2: component masses chi1: the component of the dimensionless spin of m1 along the angular momentum (z) chi2: the component of the dimensionless spin of m2 along the angular momentum (z) Results are symmetric under simultaneous exchange of m1<->m2 and chi1<->chi2. g?g@gtQ?g"t?gQ3V2?g;)ES/?glk#R?g4J5?guȩ7;?g\?g]?g?gn5w?gQjg?g*Uʚ?g&qV?g,üM @gvovI?gh?g{?)rr4r5r6rr)rrr r r8r9r}r~rrrrrrrrrrrrUZchi_effZchi_eff2Zchi_eff3Zchi_eff4Zchi_eff5rrrrrws , rc.Cst||||\}}}}}} } } } } }}}}}||}d}d}d}d}d}d}d}d}d }d }d }d }d } d}!d}"d}#d}$d}%d}&d}'d}(d})d}*d}+|||||||||||d|| | |!|dd| d|!|d|| |"|#|dd|"d|#|| |$|%|d|$d|%|| |&|'|d|&d|'|dd|| |(|)|dd|(d|)|| |*|+|d|*d|+||||| ||||},d }-|,||-},t|,S)!a Calculate the peak luminosity with the aligned-spin NR fit by David Keitel, Xisco Jimenez Forteza, Sascha Husa, Lionel London et al. [LIGO-P1600279-v5] [https://arxiv.org/abs/1612.09566v1] using modes up to lmax=6, and return results in units of 10^56 ergs/s m1, m2: component masses chi1, chi2: dimensionless spins of two BHs Results are symmetric under simultaneous exchange of m1<->m2 and chi1<->chi2. gڐו?ghgBImgA@g`ngۻyh@g3Rg"4aS\?g?N1ƿgi!?g 1P@g&Z?g*D @gp} ?g䛈* g$?@gSHqgᱥ οg?Aʰ@g }?gh?g0@g&0gD|gd3?gg(\?g0@g@g1Zd?g0g?gˡE?g=IQŐ?)rr).rrr r r8r9r}r~rrrrrrrrrrrZeta5Za0Za1rrrrrrZb4rrrrrrrrrZf40Zf41Zf60Zf61Zf70Zf71rr[rrr*bbh_peak_luminosity_non_precessing_UIB2016s> ,M rc Csttt|}ttt|}ttt|}ttt|}t||||\}}}}ddddddddd d d d d ddddddg}t|||||} t| S)a Calculate the peak luminosity of an aligned-spin binary black hole coalescence using the fit from Healy and Lousto arXiv:1610.09713 (henceforth HL) Parameters ---------- m1, m2 : component masses chi1z, chi2z : components of the dimensionless spins of the two BHs along their orbital angular momentum Returns ------- peak luminosity in units of 10^56 ergs/s g7{ uP?gl-hM?gثgX,N?g[G>g(59g ĚDog[‹|i#?gV?gmK-@g5-L?gY!d>gg`cX>g&X?g7qbu#g!?g8%?g\p6gDgP)rr4r5r6rCrVr) rrrrr9r@rArBrSrrrr,bbh_peak_luminosity_non_precessing_Healyetals*rc Csttt|}ttt|}ttt|}ttt|}ttt|}ttt|}t|||||t|}|t|}|tjkrt||||} n<|tj krt ||||} n"|tj krt ||||} nt d| S)a Calculate the peak luminosity of the merger of two black holes, only using the projected spins along the total angular momentum and some aligned-spin fit from the literature Parameters ---------- m1, m2 : component masses chi1, chi2 : dimensionless spins of two BHs tilt1, tilt2 : tilts (in radians) in the new spin convention fitname: fit selection currently supports T1600018, UIB2016, HL2016 Returns ------- peak luminosity, Lpeak, in units of 10^56 ergs/s zUnrecognized fit name.)rr4r5r6rrqrrrrrrrr) rrr r rgrhr1rtrurrrr#bbh_peak_luminosity_projected_spinss"   rc  sdkr&ttt|dkr&tddkr:tdfdd} dd } t|}|jsftd t|} t| || || || || || || |} t| | g} t |d r|j }nd }x8t |D],\}}| ||||||||}| d | |<qWtj | dd }| |S)aD Calculate the average of the predictions of various fits, currently just for the final mass, final spin, or peak luminosity of a quasicircular binary black hole coalescence. The final spin calculation returns the magnitude of the final spin, including the contribution from in-plane spins; the other two cases just apply aligned-spin fits to the components of the spins along the orbital angular momentum. Parameters ---------- m1, m2 : component masses chi1, chi2 : dimensionless spins of two BHs tilt1, tilt2 : tilts (in radians) in the new spin convention phi12: angle (in radians) between in-plane spin components (only used for the final spin) quantity: "Mf", "af", "afz", or "Lpeak" fits: An array of fit names to be used. The possible fit names are those known by bbh_final_mass_projected_spins, bbh_final_spin_precessing, and bbh_peak_luminosity_projected_spins The shape of m1 is used to determine the shape of the output. Returns ------- Average of the results for the given fits for the chosen quantity afrz=Note: phi12 is only used for the full final spin calculation.)rrafzrzUnknown quantity: %sc svdkrt|||||||Sdkr:t||||||||SdkrVt|||||||Sdkrrt|||||||SdS)Nrrrr)rjrlrfr)rrr r rgrhrmr1)quantityrr_return_quantity:sz5bbh_average_fits_precessing.._return_quantitycSst|drt|SdSdS)Nr_r )rblen)rcrrr _len_smartEs z/bbh_average_fits_precessing.._len_smartz1The list of fits passed cannot be an empty array.shape)Zaxis)maxrrZ atleast_1dr.rr/rZzerosrbr enumerateZreshapeZmean)rrr r rgrhrmrZfitsrrZnum_fitsZnum_datadataZ data_shapekfitZ data_portionZdata_avgr)rrbbh_average_fits_precessings(   0 r)r')rW)rWN)N)N)ro)ro)r)r)1__doc__numpyrZscipy.optimizeoptimizerar ImportErrorr.r r rrrrr r2r:r;r?rCrVr]r`rerirkrnrjr"rfrlrrrvrrsrwrrrxrzrrrrrrrrrrrrsZ      > & Y  <59*.A W _ h  ;!8-