Data Files to accompany the paper "All-sky search for short gravitational-wave
bursts in the first part of the fourth LIGO-Virgo-KAGRA observing run"
by LIGO Scientific Collaboration, Virgo Collaboration, and KAGRA Collaboration

Version 2
October 3, 2025

We provide machine-readable files (in csv format with a header row)
representing the data that was used to make the Tables I, II, III and
Figures 3, 4, 5, 6 in the paper.

Table I in the paper shows the h_rss values for which 50% detection efficiency
is achieved, for Gaussian (GA), Sine-Gaussian (SG), and White-noise burst
(WNB) waveforms with various parameters.  The file Table1_all_waveforms.csv
contains a machine-readable version of the table.  Because the different
waveform types have different parameters, each line of the file specifies the
relevant parameters by name (columns param1, param2, param3) as well as giving
their values (columns value1, value2, value3).  h_rss 50% values in the file
are in dimensionless units without factoring out 1e-22 as was done for the
table in the paper.  If a given waveform was not analyzed by some pipeline,
the element is blank in the file.

Table II in the paper shows GW emitted energy values (E_GW) corresponding to
50% detection efficiency for the analyzed set of elliptically polarized
sine-Gaussian waveforms.  Energy values in the file Table2_EGW.csv are given
as multiples of the Solar rest mass energy, $M_{\odot} c^2$, without factoring
out 1e-10 and without the rounding that was used to construct Table II in the
paper.  A value is given for each analyzed waveform using the three pipelines
in the O4a search and from the previously published O3 search.  If a given
waveform was not analyzed by some pipeline, the element is blank in the file.

Table III in the paper reports the percentage of Galactic core-collapse
supernovae that are detectable by each pipeline for seven different supernova
GW waveform models.  The file Table3_coverage_fraction.csv contains a
machine-readable version of the table with decimal values which are fractions,
not percentages.  The "< 0.1%" entries in the table are represented as 0.001
in the file.  Two waveforms were not evaluated using O3 data and thus have
blank elements in the file.

Figure 3 in the paper has four panels for the four analyses performed for the
search, namely the three low-frequency (16-2048 Hz) analyses using different
pipelines and the high-frequency (1600-4096 Hz) 2G+XGB analysis. Two data files
are provided for each of those four analyses, each containing a csv table with
the inverse false alarm rate (IFAR) of each candidate in units of years and the
cumulative number of events, sorted by IFAR in descending order:
  Fig3_2G+XGB_LF_Search_sorted.csv
  Fig3_2G+XGB_LF_NoCBC_sorted.csv
  Fig3_XP+XGB_LF_Search_sorted.csv
  Fig3_XP+XGB_LF_NoCBC_sorted.csv
  Fig3_2G+GMM_LF_Search_sorted.csv
  Fig3_2G+GMM_LF_NoCBC_sorted.csv
  Fig3_2G+XGB_HF_Search_sorted.csv
  Fig3_2G+XGB_HF_NoCBC_sorted.csv
The files with 'Search' in their names represent the results plotted with
triangles while the files with 'NoCBC' in their names represent the results
plotted with circular points.  For the 2G+XGB high-frequency analysis the two
files are identical.

Figure 4 in the paper shows rate density upper limits (at 90% confidence), in
units of Gpc^-3 yr^-1, for different Sine-Gaussian frequencies and Q values.
To limit the number of overlapping symbols in the figure, only the best result
from among the three O4a pipelines was plotted for each (frequency,Q)
combination, along with an O3 comparison in the 6 cases for which it is
available.  Files Figure4_2G+XGB.csv, Figure4_2G+GMM.csv, Figure4_XP+XGB.csv
and Figure4_O3_reference.csv contain the full results from all pipelines.

Figure 5 in the paper shows the sensitivity of each all-sky GW search pipeline
to core-collapse supernova events for different emission models.  The file
Figure5_all_pipelines.csv contains, for all emission models and pipelines plus
an O3 reference (when available), the distances (in kpc) at which 90%, 50%,
and 10% detection is achieved.  (NOTE: the 90% distance is not reported in the
paper.)

Figure 6 in the paper shows the sensitivity (in terms of fractional glitch
size) of the high-frequency 2G+XGB analysis to neutron star glitches, assuming
different neutron star masses and two different equations of state (EOS).
Horizontal error bars are plotted to represent the range within the mass bin.
The file Figure6_all_ranges.csv contains a machine-readable version of the
data used to plot the error bars as (min,mean,max) triplets, for each EOS and
mass bin and for the earlier O3 run as well as O4a.  It also contains columns
with median and standard deviation values.