-
xpipeline.waveform.xwaveform.
xmakewaveform
(family, parameters, T, T0, fs, **kwargs)[source]¶ Create timeseries data containing a simulated GW.
Parameters:
family (str):
- A char or cell array containing one of (not case sensitive):
- adi-a,…,-e accretion disk
instability waveforms as used in STAMP searches
- AORDDMJ10 Abdikamalov et al. accretion-induced collapse waveforms
[PRD81 044012 2010],
- BLDOM07 Burrows et al. acoustic mechanism supernova waveforms
[ApJ655 416 2007],
CG cosine-Gaussians (special case of ‘chirplet’), chirplet chirping sine/cosine-Gaussian, cusp waveform from a cosmic string cusp (see cuspgw.m), DFM NOT FUNCTIONAL. Dimmelmeier-Font-Mueller 2002 supernova waveforms,
relativistic simulations only [A&A393 523 2002], WARNING: Normalization may be incorrect.
- DFMc NOT FUNCTIONAL. Conditioned Dimmelmeier-Font-Mueller supernova
waveforms. Same as DFM except detrended. WARNING: Normalization may be incorrect.
- DFM02 Dimmelmeier-Font-Mueller 2002 supernova waveforms,
relativistic & Newtonian simulations, conditioned and detrended [A&A393 523 2002]. WARNING: Normalization may be incorrect.
- DOJMM07 Dimmelmeier et al. 2007 supernova waveforms [PRL98
251101 2007],
- DOMJ08 Dimmelmeier et al. 2008 supernova waveforms [PRD78
064056 2008]
DS damped sinusoids, DS2P 2-polarization damped sinusoids with smooth turn-on, ebbh-a,…,-e eccentric binary black-hole waveforms as used in STAMP
searches
G Gaussians (special case of ‘chirplet’), inspiral post-Newtonian inspiral, inspiralgated As inspiralsmooth, with a gate applied centered 1 sec
before coalescence time. Gate is 0.5 sec hann roll-off, 0.3 sec zeros, 0.5 sec hann roll-on.
inspiralsmooth post-Newtonian inspiral, tapered at the end iscochirp* Broadband chirps from ISCO waves around rotating black holes,
from https://arxiv.org/abs/1602.03634 (Van Putten)
kotake09 Kotake et al. supernova waveform – NEED INFO, lalinspiral post-Newtonian inspiral, generated using LALsuite Lazarus Lazarus project black-hole merger waveforms (analytic
approximation) [PRD65 124012 2002],
longbar long-lived bar mode, magnetar GW emission by magnetar undergoing spin down caused by EM
and/or EM emission,
marek09 Marek et al. 2009 supernova waveforms – NEED INFO, methodspaper One of four numerical supernova waveforms from
- mono Monochromatic waveforms used by STAMP-AS (including mono-*,
line-, quad-) see https://wiki.ligo.org/Main/O1analysisInjections,
- mob09 Murphy-Ott-Burrows 2009 supernova waveforms
[arXiv:0907.4762],
murphy09 Murphy+09 waveforms mvp van Putten based waveform model – NEED INFO, NCSA-CAM eccentric binary neutron star mergers, generated with the
NCSA-CAM waveform model. The waveforms start at 15Hz and continue through merger and ringdown. See https://dcc.ligo.org/DocDB/0140/G1700265/001/ecc_presentation.pdf
- OBDL06 Ott, Burrows, Dessart, & Livne supernova waveforms
[PRL 96 201102 2006]
- OBLW04 Ott-Burrows-Livne-Walder 2004 supernova waveforms
[ApJ600 834 2004],
onecyclesine single cycle (phase -pi->0->pi) of a sine wave, osnsearch test waveform used in S5/S6 optical supernova search, o1snews Waveforms for O1 X SNEWS Search. O09 Ott SASI supernova waveforms [CQG26 063001 2009], O10 Ott 2010 supernova waveforms – NEED INFO, PCA Principle Component Analysis Wave Forms piro NOT FUNCTIONAL. Piro-based waveform model – NEED INFO, scalarchirplet scalar-mode chirping cosine-Gaussian, pmns_pca A large number of precalculated Post-Merger Remnant Signals for a
variety of EOS mass configurations. some include ‘nl3_1515’ ‘tma_1215’ ‘tma_1212’ ‘dd2_1314’ ‘ls375_1215’ ‘dd2_1215’ ‘dd2_165165’ ‘tma_1515’ ‘ls375_1212’ ‘ls220_1414’
- scalarsn Model A follows solution number 4 from Table 1 for a 1.5
solar mass star undergoing spontaneous scalarization. See http://journals.aps.org/prd/abstract/10.1103/PhysRevD.58.064019 Model B follows the collpase of aspherical NS star to blackhole following solution B in table 1. http://journals.aps.org/prd/abstract/10.1103/PhysRevD.57.4789 Models C, D, E are Novak and Ibanez scalar supernovae waveforms.
scheide Scheidegger et al. 2010 equatorial waveforms – NEED INFO, scheidp Scheidegger et al. 2010 for polar waveforms – NEED INFO,
SG sine-Gaussians (special case of ‘chirplet’),
- snmp Waveforms used for SN Methods Paper that are not included in
osnsearch.
- SNN94 Shibata, Nakao, and Nakamura scalar-mode GWs from
gravitational collapse [PRD 50 7304 1994],
- stamp_* STAMP-AS waveforms for O1 long-duration search see
- WNB windowed, band-limited white-noise burst (2 independent
polarizations).
Yakunin2010 Yakunin et al. http://arxiv.org/abs/1005.0779 zero null signal (hp=0=hc), ZM Zwerger-Mueller supernova waveforms [A&A320 209 1997].
WARNING: Normalization may be incorrect see eqn (21) of the reference.
params (Array, or tilde-delimited string):
containing parameters for the specified waveform type. The format and definition of the parameters depend on the waveform type. For details on a specific waveform, e.g. WNB, do xmakewaveform(‘WNB’).
- T (int):
Duration of the waveform. Must have T*fs = integer. Recommend T>=1 for astrophysical waveforms.
- T0 (int):
Desired peak time of the waveform, as measured in hrss for (hp.^+hc.^2).^(0.5). Must have 0<T0<T. See “Notes” below for caveats.
- fs (int):
Sampling rate of the time series. T*fs must be an
integer.
- Returns:
- t:
Times at which the waveform is sampled, starting from zero.
- hp:
Plus polarization waveform [strain].
- hc:
Cross polarization waveform [strain].
- hb:
Breathing (scalar) polarization waveform [strain]. Identically zero for all waveform types unless explicitly stated otherwise.
Notes:
The waveform is interpolated so that the RSS-weighted center time, [int dt t (hp.^+hc.^2+hb.^2)].^(0.5), is at T0. Note that for 2-polarization waveforms that include an inclination angle (eg, DS2P) different inclination angles will cause hp, hc to be weighted differently and therefore will produce different shifts.
The cusp waveform (generated by P. Shawhan’s cuspgw function) and most astrophysical waveforms that are loaded from files are always 1 sec long with sampling rate 16384 Hz when created/loaded. These are resampled linearly and truncated or zero-padded to the desired length. One should be cautious in using T<1 for these waveforms.