DOI: 10.5281/zenodo.17735649
title: Data release for paper "Constraints on gravitational waves from the 2024 Vela pulsar glitch"

description: This posting contains data for the scientific article "Constraints on gravitational waves from the 2024 Vela pulsar glitch" by the LIGO-Virgo-KAGRA collaboration, available from https://dcc.ligo.org/P2500086/public

In detail, the included data are:

* Radio pulsar timing ephemeris file J0835-4510_long_F3.par as used for calculating the post-fit residuals in Fig. 1, the parameters in Table 1, and as input to the GW searches. This is derived from observations by the Argentine Institute of Radio Astronomy (IAR, for details of the observations and data processing see section 2.1 of this paper and also Zubieta et al. A&A, 698, A72 (2025)) and the Mount Pleasant Radio Observatory (MPRO) of the University of Tasmania (see section 2.2 of this paper). 

* o4_vela_glitch_data_release_psds.tar.gz including GW detector power spectral density (PSD) files:  * individual H1, L1 and V1 PSDs for Tglitch +-20 s, computed with the Welch method in gwpy, as shown in Fig. 2    (can be plotted with the script o4_vela_glitch_plot_fig_02_asd.py)  * a combined H1+L1 PSD for 4 months of data as used for computing the sensitivity depths for the CW-like searches

* o4_vela_glitch_data_release_segments.tar.gz including segment files corresponding to the analyzable GW detector data stretches:  * the three "plusminus12h" files correspond to the bottom left panel of Fig. 2  * the other three files correspond to the bottom right panel of Fig. 2  Both panels can be plotted with the script o4_vela_glitch_plot_fig_02_segments.py

* o4_vela_glitch_bursts_search_sensitivity_all_pipelines.txt including the sensitivity results of the burst search pipelines shown in Fig. 4,  which can be reproduced with the script o4_vela_glitch_plot_fig_04.py

* o4_vela_glitch_data_release_cw_upper_limits.tar.gz including upper limits on GW strain from the four CW-like searches.  Results are included for all search configurations discussed in the paper.  The representative curves shown in Fig. 5 correspond to the following files:  * uls_cwinpy/1stHarmonic_fixed_freq_fixed_angles_exp_H1L1_ULs.txt  * uls_fstat/uls_glitch1_tau_exp_lnBtSG_thresh9.160627.txt  * uls_peakmap/vela_glitch_ul_h0_uniform.txt  * uls_viterbi/o4_vela_glitch_HMM_Tcoh32400_2f_uls.txt  This figure can be reproduced with the script o4_vela_glitch_plot_fig_05.py  Additional upper limits plots in the appendix are produced by the following scripts:  * CWInPy: o4_vela_glitch_plot_fig_08.py and o4_vela_glitch_plot_fig_09.py  * F-stat: o4_vela_glitch_plot_fig_10.py  * WPM: o4_vela_glitch_plot_fig_12.py  * HMM-Viterbi: o4_vela_glitch_plot_fig_14.py

* o4_vela_glitch_data_release_cw_sensitivity_depths.tar.gz including more detailed values of the sensitivity depths quoted for the CW-like searches in Sec. 5.6, given here as functions of signal duration parameter tau and for the same representative configuration of each search as plotted in Fig. 5.

* o4_vela_glitch_data_release_inference.tar.gz including prior samples, posterior samples and equation-of-state data for figures 6 and 7, which can be reproduced by the scripts o4_vela_glitch_plot_fig_06.py and o4_vela_glitch_plot_fig_07.py

* o4_vela_glitch_data_release_appendix_wpm.tar.gz including additional data for the follow-up of outliers from the WPM search discussed in appendix C.2:  * ps_cand2_param.h5  * ps_cand2_param_shift1.h5  * ps_cand2_param_shift2.h5  * topt_preliminary_3decaytimes.h5The .h5 files are read by the plotting scripts o4_vela_glitch_plot_fig_11.py and o4_vela_glitch_plot_fig_13.py for figures 11 and 13.The first three files (ps_cand2...) contain the spectra of the original data and of the data after injecting two signals, slightly shifted w.r.t. the most significant search candidate, for figure 13.The fourth file (topt...) contains the CR values as a function of the observing window, after the injection of a signal with four different amplitudes, for figure 11.