# The First _Insight-_ HXMT Gamma-Ray Burst Catalog: The First Four Years

Xin-Ying Song  Key Laboratory of Particle Astrophysics, Institute of High
Energy Physics, Chinese Academy of Sciences, Beijing 100049, China  Shao-Lin
Xiong  Key Laboratory of Particle Astrophysics, Institute of High Energy
Physics, Chinese Academy of Sciences, Beijing 100049, China  Shuang-Nan Zhang
Key Laboratory of Particle Astrophysics, Institute of High Energy Physics,
Chinese Academy of Sciences, Beijing 100049, China  University of Chinese
Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China
Cheng-Kui Li  Key Laboratory of Particle Astrophysics, Institute of High
Energy Physics, Chinese Academy of Sciences, Beijing 100049, China  Xiao-Bo Li
Key Laboratory of Particle Astrophysics, Institute of High Energy Physics,
Chinese Academy of Sciences, Beijing 100049, China  Yue Huang  Key Laboratory
of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of
Sciences, Beijing 100049, China  Cristiano Guidorzi  Department of Physics and
Earth Science, University of Ferrara, Via Saragat 1, I-44122 Ferrara, Italy
INFN - Sezione di Ferrara, Via Saragat 1, I-44122 Ferrara, Italy  INAF -
Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Piero
Gobetti 101, I-40129 Bologna, Italy  Filippo Frontera  Department of Physics
and Earth Science, University of Ferrara, Via Saragat 1, I-44122 Ferrara,
Italy  INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna,
Via Piero Gobetti 101, I-40129 Bologna, Italy  Cong-Zhan Liu  Key Laboratory
of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of
Sciences, Beijing 100049, China  Xu-Fang Li  Key Laboratory of Particle
Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences,
Beijing 100049, China  Gang Li  Key Laboratory of Particle Astrophysics,
Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049,
China  Jin-Yuan Liao  Key Laboratory of Particle Astrophysics, Institute of
High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China  Ce
Cai  Key Laboratory of Particle Astrophysics, Institute of High Energy
Physics, Chinese Academy of Sciences, Beijing 100049, China  University of
Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049,
China  Qi Luo  Key Laboratory of Particle Astrophysics, Institute of High
Energy Physics, Chinese Academy of Sciences, Beijing 100049, China  University
of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049,
China  Shuo Xiao  Key Laboratory of Particle Astrophysics, Institute of High
Energy Physics, Chinese Academy of Sciences, Beijing 100049, China  University
of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049,
China  Qi-Bin Yi  Key Laboratory of Particle Astrophysics, Institute of High
Energy Physics, Chinese Academy of Sciences, Beijing 100049, China  Department
of Physics, Xiangtan University, Xiangtan, Hunan Province 411105, China  Yao-
Guang Zheng  Key Laboratory of Particle Astrophysics, Institute of High Energy
Physics, Chinese Academy of Sciences, Beijing 100049, China  College of
physics Sciences & Technology, Hebei University, No. 180 Wusi Dong Road, Lian
Chi District, Baoding City, Hebei Province 071002, China  Deng-Ke Zhou  Key
Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese
Academy of Sciences, Beijing 100049, China  University of Chinese Academy of
Sciences, Chinese Academy of Sciences, Beijing 100049, China  Jia-Cong Liu
Key Laboratory of Particle Astrophysics, Institute of High Energy Physics,
Chinese Academy of Sciences, Beijing 100049, China  University of Chinese
Academy of Sciences, Chinese Academy of Sciences, Beijing 100049, China  Wang-
Chen Xue  Key Laboratory of Particle Astrophysics, Institute of High Energy
Physics, Chinese Academy of Sciences, Beijing 100049, China  University of
Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing 100049,
China  Yan-Qiu Zhang  Key Laboratory of Particle Astrophysics, Institute of
High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
University of Chinese Academy of Sciences, Chinese Academy of Sciences,
Beijing 100049, China  Chao Zheng  Key Laboratory of Particle Astrophysics,
Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049,
China  University of Chinese Academy of Sciences, Chinese Academy of Sciences,
Beijing 100049, China  Zhi Chang  Key Laboratory of Particle Astrophysics,
Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049,
China  Zheng-Wei Li  Key Laboratory of Particle Astrophysics, Institute of
High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China  Xue-
Feng Lu  Key Laboratory of Particle Astrophysics, Institute of High Energy
Physics, Chinese Academy of Sciences, Beijing 100049, China  Ai-Mei Zhang  Key
Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese
Academy of Sciences, Beijing 100049, China  Yi-Fei Zhang  Key Laboratory of
Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of
Sciences, Beijing 100049, China  Yong-Jie Jin  Department of Engineering
Physics, Tsinghua University, Beijing 100084, China  Ti-Pei Li  Key Laboratory
of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of
Sciences, Beijing 100049, China  Department of Engineering Physics, Tsinghua
University, Beijing 100084, China  Fang-Jun Lu  Key Laboratory of Particle
Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences,
Beijing 100049, China  University of Chinese Academy of Sciences, Chinese
Academy of Sciences, Beijing 100049, China  Li-Ming Song  Key Laboratory of
Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of
Sciences, Beijing 100049, China  University of Chinese Academy of Sciences,
Chinese Academy of Sciences, Beijing 100049, China  Mei Wu  Key Laboratory of
Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of
Sciences, Beijing 100049, China  Yu-Peng Xu  Key Laboratory of Particle
Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences,
Beijing 100049, China  Xiang Ma  Key Laboratory of Particle Astrophysics,
Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049,
China  Ming-Yu Ge  Key Laboratory of Particle Astrophysics, Institute of High
Energy Physics, Chinese Academy of Sciences, Beijing 100049, China  Shu-Mei
Jia  Key Laboratory of Particle Astrophysics, Institute of High Energy
Physics, Chinese Academy of Sciences, Beijing 100049, China  Bing Li  Key
Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese
Academy of Sciences, Beijing 100049, China  Jian-Yin Nie  Key Laboratory of
Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of
Sciences, Beijing 100049, China  Ling-Jun Wang  Key Laboratory of Particle
Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences,
Beijing 100049, China  Juan Zhang  Key Laboratory of Particle Astrophysics,
Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049,
China  Shi-Jie Zheng  Key Laboratory of Particle Astrophysics, Institute of
High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China  Xue-
Juan Yang  Department of Physics, Xiangtan University, Xiangtan, Hunan
Province 411105, China  Rong-Jia Yang  College of physics Sciences &
Technology, Hebei University, No. 180 Wusi Dong Road, Lian Chi District,
Baoding City, Hebei Province 071002, China

###### Abstract

The Hard X-ray Modulation Telescope (_Insight-_ HXMT), is China’s first X-ray
astronomy satellite launched on June 15, 2017. The anti-coincidence CsI
detectors of the High Energy X-ray telescope (HE) onboard _Insight-_ HXMT
could serve as an all-sky gamma-ray monitor in about 0.2-3 MeV. In its first
four years of operation, _Insight-_ HXMT has detected 322 Gamma-Ray Bursts
(GRBs) by offline search pipeline including blind search and targeted search.
For the GOLDEN sample of _Insight-_ HXMT GRBs, joint analyses were performed
with other GRB missions, including _Fermi_ Gamma-ray Burst Monitor (_Fermi_
/GBM), Swift Burst Alert Telescope (_Swift_ /BAT) and Gravitational wave high-
energy Electromagnetic Counterpart All-sky Monitor (GECAM). It shows that
_Insight-_ HXMT can provide better constraint on GRB spectrum at higher energy
band. The properties of _Insight-_ HXMT GRBs are reported in detail, including
their trigger time, duration, spectral parameters, peak fluxes of different
time scales and fluence. This catalog is an official product of the _Insight-_
HXMT GRB team.

catalogs – gamma-ray burst: general

##  1 Introduction

The Hard X-ray Modulation Telescope (HXMT), dubbed _Insight-_ HXMT, launched
on June 15, 2017, is China’s first X-ray astronomy satellite devoted to broad
band observations in the 1-250 keV band. _Insight-_ HXMT consists of three
collimator-based telescopes: the High Energy X-ray Telescope (HE, Liu et al.,
2020), the Medium Energy X-ray Telescope (ME, Cao et al., 2020) and the Low
Energy X-ray Telescope (LE, Chen et al., 2020). _Insight-_ HXMT/HE adopts an
array of 18 NaI(Tl)/CsI(Na) phoswich detectors as the main detector plane,
with a total geometric area of about 5100 cm2 and a combined Field of View
(FOV) of about $5.7^{\circ}\times 5.7^{\circ}$ (FWHM)(HE, Liu et al., 2020).
The CsI(Na) (CsI for brevity) in the phoswich detector of HE can be also used
as an all-sky gamma-ray monitor in 0.2-3 MeV, since gamma-rays in this energy
range can penetrate the spacecraft and deposit energy in the CsI detecor. Thus
HE could play an important role in monitoring gamma-ray bursts (GRBs), MeV
pulsars, Solar Flares (SFL), Terrestrial Gamma-ray Flashes (TGF) and other
gamma-ray sources. The measured energy range (deposited energy) of CsI is
about 40-800 keV in the normal gain (NG) mode and about 200 keV- 3 MeV in low
gain (LG) mode. The NG and LG modes are achieved by adjusting the high voltage
of the PMTs which readout the NaI(Tl)/CsI(Na) phoswich detectors.

There is neither on-board GRB trigger system nor prompt data telemetry for
_Insight-_ HXMT, thus GRBs are unveiled on-ground using two pipelines: the
blind search is performed on all data acquired by _Insight-_ HXMT/HE CsI
detector; in addition, for each GRB detected by other astronomical satellites
or instruments (called external triggers hereafter, in contrast to the
internal triggers produced by _Insight-_ HXMT itself) reported through the
Gamma-ray Coordinates Network (GCN), the targeted search pipeline would be
launched to search CsI data around the trigger time of external triggers.

From June 26th in 2017 to June 30th 2021, GRBs and others bursts including
terrestrial gamma-ray flash (TGF), solar flares (SFL, Zhang et al., 2021) have
been detected by _Insight-_ HXMT, the gamma-ray counterparts of Gravitational
Wave (GW) events (Li et al., 2018a; Zhang et al., 2018; Li et al., 2017); Fast
radio bursts (FRB, Guidorzi et al., 2020) ) and High Energy Neutrino (HEN,
e.g. Zheng et al., 2020), have been monitored as well. During the first four
years of observation data, 660 bursts are found, where 322 are classified as
GRBs, 245 as TGFs, 4 as SFLs, 33 as charged particles and 56 as unclassified.
Targeted search were implemented for external triggers of great importance,
including 41 HENs, 48 GWs and 39 FRBs. For each GRB, the trigger time in
Universal Time Coordinated (UTC) and Mission Elapsed Time (MET) are recorded
and the event data is selected between $\rm T_{0}-100$s and $\rm T_{0}+300$s
in most cases, where $\rm T_{0}$ is trigger time from GCN or blind search. In
addition, quick-analysis tools for GRBs and joint spectral fitting with other
missions are developed for this catalog analysis, which are introduced in the
following sections.

We start with a brief description of the HXMT/CsI detectors and calibration in
Section 2 and refer Luo et al. (2020) for a more thorough and complete
description of the instrument and calibration respectively. This is followed,
in Section 3 the burst-searching algorithm and its up-to-date ability is
introduced in details. In Section 4, a description of the methodology used in
the production of this catalog is presented, including detector selection,
data types used, energy selection and background fitting, and the source
selection. In Section 5, catalog analysis and results are presented. In
Section 6, the distribution of duration, hardness are discussed and all the
GRBs catalog results are summarized.

##  2 Instrument

The High Energy X-ray Telescope (HE, Liu et al., 2020) consists of the main
detector (HED), high energy collimator (HEC), auto-gain control detector
(HGC), anti-coincidence shield detector (HVT), particle monitor (HPM), data
processing and control box (HEB) and power box (HEA). As the main detector of
HE, HED is responsible for the observation of celestial sources. It consists
of 18 NaI(Tl)/CsI(Na) phoswich detectors (labelled as HED-0, 1 … to 17), each
with a diameter of 190 mm and a collimator made of lead and tantalum. The NaI
detectors are sensitive to the hard X-rays in 20-250 keV, whereas the CsI acts
as an anti-coincidence detector to reduce the background of NaI. The thickness
of the NaI and CsI crystals are 3.5 mm and 40 mm, respectively. HGC provides
the auto-gain control and energy calibration for HED. HVTs act as an active
shielding system to reduce HED’s background caused by charged particles. HPMs
monitor the flux of charged particles and send out an alert to switch off the
high voltages of HEDs and HVTs in high flux regions to avoid potential damage
to the PMTs of these detectors. The overview of all telescopes aboard
_Insight-_ HXMT is shown in Figure 1.

_Insight-_ HXMT/HE can observe the high energy sky with two observation
scenarios (Zhang et al., 2020) which can work simultaneously:

  * (1)

Collimator-based (pointed or scan) observation: using NaI/CsI detectors, HE
can detect hard X-ray emission in 20-250 keV from the celestial sources within
the FOV defined by collimators. HE can do pointed observation to a specific
source, or scan observation to a small sky area.

  * (2)

Gamma-ray all-sky monitoring: Gamma-ray photons with energy higher than
$\sim$200 keV from all directions can penetrate the spacecraft and be detected
by the CsI detectors. CsI can monitor the gamma-ray all-sky with the only
exception of the occulted region by the Earth. This gamma-ray all-sky
monitoring is an extended capability for HE and inapplicable for ME or LE
telescopes aboard _Insight-_ HXMT.

The primary observation scenario of HE is the collimator-based observation
consisting of pointed observation and scan observation, both of which use the
NaI as the main detector and detect sources within the field of view (FOV) of
collimator in 20-250 keV. The CsI detectors mainly act as the anti-coincidence
and shielding to reduce the background of NaI. Due to the high thickness of
the CsI(Na) crystals, high energy (greater than about 200 keV) gamma-ray
photons can penetrate the spacecraft and be recorded by the CsI detectors,
thus the GRBs unocculted by the Earth can be detected. For each NaI/CsI
phoswich detector of HE, the event-by-event data (called EVT data hereafter)
is recorded and we can use the pulse width information in the EVT data to
distinguish between NaI events and CsI events. For this paper, we only select
these events recorded by CsI detectors by screening events with pulse width
greater than 75. The response and calibration of the CsI detectors are mainly
described in Section 4.1.

Figure 1: The illustration of the satellite platform and the payloads of
_Insight-_ HXMT. The coordinate system used in this study is shown on the
upper-left. It is adapted from Fig. 1 in Luo et al. (2020).

The gain of NaI/CsI detector is mainly controlled by the High Voltage of the
PMT which converts the scintillation light produced by NaI/CsI crystals to the
electric signals. To meet various observation requirements, two gain modes are
designed for the HE NaI/CsI detectors: normal gain (NG) mode and low gain (LG)
mode. The measured energy ranges for CsI detector are listed as bellow: the NG
mode in $40-800$ keV and the LG mode in 200-3000 keV (both refer to the
deposited energies). NG mode is the main working mode that the auto-gain
control system can keep the full-energy-peak of the 59.5 keV photons (emitted
from a radioactive source 241Am) in a fixed channel of the NaI detector. In LG
mode, the high voltage of the each _Insight-_ HXMT/HE detector is reduced and
the auto-gain control system is disabled to achieve a higher energy range
detection. As derived from the two-year observations since _Insight-_ HXMT has
operated in-orbit, the E-C relationships of each _Insight-_ HXMT/CsI detector
for both NG and LG modes vary over time, so calibration of the instrumental
response is of great importance.

##  3 Search for Bursts

A pipeline is developed to search for GRBs for blind search and the coherent
search method for targeted search (Cai et al., 2021). The blind search
software continually monitors each group (18 CsI detectors are divided into 6
groups, 3 in each group) of detectors count rates, for which the reason is to
reduce statistical fluctuations of one or a few detectors, one of the main
causes of false trigger. The pipeline is triggered when counts rates in the
EVT data of three or more groups of CsI detectors exceed the background counts
rates, by 3$\sigma$ on five timescales: 0.05s, 0.1s, 0.2s, 0.5s and 1s by
calculating an average of the counts rates of 10 s of the previous data as
background.

If a GRB detected by other external missions, falls in the field of view of
HE, but did not trigger the bind search, targeted search in HE/CsI data would
be launched. The targeted coherent search method is applied to the EVT data of
HE CsI detectors, which can recover true astrophysical bursts that are too
weak to trigger through blind search. This coherent method was originally
developed by Blackburn et al. (2015), improved by Goldstein et al. (2016),
Goldstein et al. (2019), and verified by Kocevski et al. (2018). From the
statistics of searched GRBs, we find the fluence (from GBM Burst Catalog) of
HE targeted search could reach $\sim 10^{-7}$ $\rm erg$ $\rm cm^{-2}$ (10
keV–1 MeV) in duration of 0.256 s. For this paper, 15 GRBs that are found from
targeted search are included and labeled in Table 3, while the rest are from
blind search. Details of burst search are presented in a separate paper (Cai
et al., 2021).

##  4 Catalog Analysis

###  4.1 Instrument Response

There are two parts in the instrumental response of CsI detectors: the energy
redistribution of the photons from incident energy to deposition energy that
is determined by the property of the CsI crystal and the mass distribution of
satellite; and the Energy-Channel (E-C) relationship that is determined by the
detectors and electronic system of the instrument. For the photon energy
redistribution, the reliability is mainly determined by the accuracy of the
mass model of the satellite and the payloads (Agostinelli et al., 2003). Based
on the initial mass model of the satellite platform (Xie et al., 2015), we
calibrate the mass model with the Crab pulse radiation as a standard candle
(Li et al., 2018b), to generate accurate instrumental response for the all sky
gamma-ray monitoring.

The in-flight E-C relationship and energy resolution of the instrument can be
obtained by analyzing the characteristic lines of the in-orbit observed and
the on-ground simulated background spectra (Li et al., 2019). The E-C
relationship varies over time, whereas the energy resolution remains stable
(Li et al., 2020). Therefore, we update the E-C relationship every month, and
take the average energy resolution of all calibration results to generate the
instrumental response.

After the above calibration, a new response matrix library is established and
a simulated spectral analysis is performed to test the HXMT/CsI spectroscopy
capabilities. Calibration of the instrumental response to GRB is carried out
with GRBs (Luo et al., 2020). In a GRB observation, the incident direction of
the GRB photons is supposed to be arbitrary, however, only the instrumental
response to several directions can be calibrated directly. A common method of
the instrumental response testing is the cross-calibration with other
instruments by comparing the energy spectrum of the simultaneously observed
GRB (Sakamoto et al., 2011; Tsujimoto et al., 2011; Tierney et al., 2010;
Ishida et al., 2014). The detection efficiency of HXMT/CsI is checked by the
joint spectral analyses with _Fermi_ /GBM, _Swift_ /BAT and Konus-_Wind_ , in
which we find that HXMT/CsI can provide better constraint on GRB spectrum at
higher energy band (Luo et al., 2020). The instrumental responses are mainly
obtained by Monte Carlo simulation with the Geant4 tool and the mass model of
both the satellite and all the payloads, which is updated and tested with the
Crab pulse emission in various incident directions. Both the Energy-Channel
relationship and the energy resolution are calibrated in two working modes (NG
mode and LG mode) with the different detection energy ranges. The simulated
spectral analyses show that HXMT/CsI can constrain the spectral parameters
much better in the high energy band than that in the low energy band. As
introduced in (Luo et al., 2020), the joint spectral analyses are performed to
ten bright GRBs observed simultaneously with HXMT/CsI and other instruments
(_Fermi_ /GBM, _Swift_ /BAT, Konus-_Wind_), and the results show that the GRB
flux given by HXMT/CsI is systematically higher by $7.0\pm 8.8\%$ than those
given by the other instruments. The HXMT/CsI-_Fermi_ /GBM joint fittings also
show that the high energy spectral parameter can be constrained much better as
the HXMT/CsI data are used in the joint fittings.

In summary, the instrumental responses of the HXMT/CsI detectors of _Insight-_
HXMT are well calibrated in aspects of mass model, E-C relationship and the
energy resolutions for both the NG and LG modes. Thanks to the large effective
area in the high-energy band, as shown in Figure 2, HXMT/CsI shows its
advantages in constraining the GRB spectra in high energy band, together with
other missions (such as _Fermi_ /GBM) which provide observations at lower
energies.

Figure 2:  Effective areas of HXMT/CsI, _Fermi_ /LAT, _Fermi_ /GBM, Konus-
_Wind_ , _Swift_ /BAT, _CALET_ /CGBM and _AstroSat_ /CZTI. The effective area
of _Fermi_ /GBM (NaI) is the averaged over the unocculted sky. It is adapted
from Fig. 13 in Luo et al. (2020).

Note that the the deposited energy range is usually very different from
incident energy bands due to the responses of HXMT/CsI detectors. Three types
of spectra are listed in Table 1, where the soft and middle spectra are with
BAND model, the hard spectra is with CPL model, and they are representative of
GRBs of different hardness; details of BAND and CPL model are clarified in
Section 4.7.1. They are simulated with the same amplitude in each type of
spectra (use $fakeit$ in Xspec 12.11.0, with all the model normalization
factors equal to 1), and convoluted with the total response of 18 HXMT/CsI
detectors. The deposited energy spectra of incident angle theta from
$0^{\circ}$ to $180^{\circ}$ are shown in NG mode (Figure 3) and in LG mode
(Figure 4) respectively, which shows the ranges of deposited energy.
Considering the deposited spectra and effective area shown in Figure 2, the
deposited energy range of HXMT/CsI data is determined to be about 150-800 keV
for NG mode and about 200-3000 keV for LG mode in the following spectra
analysis.

Table 1:  Three types of spectra and parameters. The soft and middle spectra are with BAND model, and the hard spectra is with CPL model. Types of spectra | $\alpha$ | $\beta$ |  $E_{\rm peak}$(keV)
---|---|---|---
SOFT | -1.9 | -3.7 | 70
MIDDLE | -1.0 | -2.0 | 230
HARD | -0.5 | - | 1500
Figure 3:  The deposited energy spectra of three types of BAND with incident
angle $\theta$ of $0^{\circ}$ to $180^{\circ}$ are shown in NG mode. The
azimuthal angle $\phi$ is $0^{\circ}$. Here the incident angle $\theta$ and
the azimuthal angle $\phi$ denote the direction of gamma rays in spherical
coordinates of HE/CsI detector. Figure 4:  The deposited energy spectra of
three types of BAND with incident angle $\theta$ of $0^{\circ}$ to
$180^{\circ}$ are shown in LG mode. The azimuthal angle $\phi$ is $0^{\circ}$.
Here the incident angle $\theta$ and the azimuthal angle $\phi$ denote the
direction of gamma rays in spherical coordinates of HE/CsI detector.

###  4.2 GRB Samples

In summary, we define three types of GRB samples as shown in Table 2. Only the
‘GOLDEN’ GRBs could be utilized in the joint analysis, which are required to
be located well and detected without saturation in HXMT/CsI data. The ‘SILVER’
samples denote those which are detected by other external missions, but not
located or lack of data for joint analysis. In this analysis, public data
offered by _Fermi_ /GBM, _Swift_ /BAT or GECAM are utilized for joint
analysis. The bursts which are only detected by HXMT are labeled as ‘BRONZE’.
The HXMT/HE data files will not be used if there is saturation in electronics
subsystem during the GRBs, or the data quality is not good (such as data
loss). Saturation is defined when the two following criteria are matched
simultaneously: firstly, total count rate of 18 CsI detectors exceeds 20000
counts/s, as evaluated over four different timescales: 0.1, 0.2, 0.5, and 1.0
s; secondly, in at least one of the three groups of 6 CsI detectors that share
the same Analog-to-Digital Converter (ADC) (Liu et al., 2020), the total light
curve has at least one 5-ms bin with zero counts. As shown in Table 2, this
kind of GRB samples are labeled as ‘IRON’, which are not utilized in the
following analysis.

Table 2:  Classification of four kinds of _Insight-_ HXMT GRB samples. Type | Location and data for joint analysis | External detected | Saturation in HXMT data | Utilized or not | Number
---|---|---|---|---|---
GOLDEN | Yes | Yes | No | Yes | 202
SILVER | No | Yes | No | No | 44
BRONZE | No | No | No | No | 50
IRON | Yes/No | Yes/No | Yes | No | 26

###  4.3 Suppression of Background From Charged Particles

Among the main detectors of the HE telescope, HVTs act as an active shielding
system to reduce HED background caused by charged particles (HE, Liu et al.,
2020). In order to suppress the background from charged particles, events
which are coincidence with signal in HVTs are removed since they are likely
produced by charged particles rather than gamma-rays. Besides, those events
which also have energy deposition in NaI (Tl) detectors are also eliminated,
because the signals of NaI (Tl) are mainly from the target source when we
perform pointed or scan observation. Response of 18 CsI detectors in HED
according to Section 2 are different but the discrepancy between them are
small (unlike the case in _Fermi_ /GBM or GECAM where detectors have different
orientations), therefore, all dat events in 18 CsI detectors are utilized in
this study.

###  4.4 Dead Time Correction

Dead time of HED detectors is complicated. According to Xiao et al. (2020),
every 6 detectors in 18 NaI (Tl)/CsI (Na) detectors in HE share one ADC read-
out electronics, thus a signal in any detector will cause dead time not only
to the incident detector itself, but also to the other 5 detectors of the same
ADC. The dead time of one event is normally about $4\sim 8$ $\mu$s, but it
will be longer for the signals generated by high energy charged particles.
There is a dead time counter in HEB for each HED, and the information is
recorded in the form of proportion of dead time. The proportion of dead time
in a time interval is determined with the method established in Xiao et al.
(2020). The correction factors on the light curves are determined by
$\frac{1}{1-P_{\rm dt}}$, where $P_{\rm dt}$ is the proportion of dead time in
every time bin with bin width of 10 ms. The light curves of each CsI detector
are corrected by multiplying with series of dead-time correction factors
before background fitting is performed. As shown in Figure 5, the comparison
between light curves with and without dead-time correction of a short GRB is
present, which shows that the dead-time correction is necessary for refined
analysis.

Figure 5:  A comparison between light curves with and without dead-time
correction of a short GRB triggered at 2019-11-05T06:11:08.65 UTC. The
histogram of red lines and error bars denote the light curve without dead-time
correction, while the black with dead-time correction. Here MET means the
mission elapsed time of HXMT.

###  4.5 Background Fitting

After the data have been selected for a given GRB, a background model in the
form of polynomial function with time, is computed separately for each
detector, based on user-selected time intervals for background region. Here we
use a pre-burst interval and a post-burst interval as user-selected background
regions. The order of polynomial is determined by the best goodness of fits
with polynomials of different orders, where the order could be 0, 1, 2
respectively. For each detector, background fitting is carried out for each
energy channel, and the background fit determined from pre-burst and post-
burst intervals are used to estimate the background counts in the signal
region of the burst. The net counts number of GRB in each channel is obtained
by subtracting the counts of background from the total counts number.
Background fitting is performed in each detector channel by channel in
deposited energy spectrum, until the net counts and background counts of all
channels for the given GRB are determined. Statistical errors of net counts
are determined by the root of the sum of squares of the statistical errors of
background estimation and Poisson errors of total counts (i.e. classical error
propagation). Note that all light curves for each energy channel in each
detector have been corrected with dead-time correction factors. The source
time intervals for all detectors are chosen to be same for the GRB data
analysis, thus data of all detectors could be added up to reduce the
statistical uncertainties.

###  4.6 Source Time Interval Selection

Source time interval selection may be different when we perform different
analyses. For the computation of duration, peak fluxes and fluence, the source
interval is loosely selected, by starting from several seconds before the
burst begins and ending at several seconds after the burst ends, and may have
overlaps with pre-burst and post-burst intervals for background selection. If
there exists difference of start- and end-time of a GRB between HXMT/CsI and
other missions due to the energy detection range, the loosest source interval
is applied for the joint data analysis of these missions. For the analysis of
time-average spectra, the source time interval is usually selected to be
narrower. The events in $T_{\rm 90}$ or the whole duration in some cases based
on deposited photon counts are selected for the time-averaged energy spectra.

In the case of joint analyses with other missions, the time delay due to the
different arrival times of two spacecrafts is considered. The method mentioned
in Hurley et al. (1999) is utilized to determine the time delay between HXMT
and other missions. Figure 6 shows the time delays of other missions relative
to HXMT for ‘GOLDEN’ GRB samples. The red histograms denote the time delays of
_Fermi_ /GBM, while the blue ones denote those of _Swift_ /BAT and the green
ones for those of GECAM. The negative values represent that GRBs arrived at
other missions earlier than HXMT, while the positive numbers means that the
GRB arrival time of HXMT is earlier. Some time delays reach up to tens of
milliseconds and must be considered, because the time scale (64 ms) of
deconvolved photon spectra is in the same order of magnitude.

Figure 6:  The distribution from ‘GOLDEN’ GRB samples of time delays of
_Fermi_ /GBM (dashed), _Swift_ /BAT (dotted), and GECAM (dot-dashed) relative
to HXMT are shown.

###  4.7 Duration, Fluence and Peak Flux

In order to take advantages of different missions and to reduce uncertainties
in determination of the parameters of GRBs, joint spectral analyses between
HXMT and _Fermi_ /GBM, _Swift_ /BAT and GECAM are applied on all ‘GOLDEN’
GRBs. This paper reports various measures of the duration, peak fluxes and
fluence of each burst. We take GRB 200125B (HEB200125863), GRB 210121A
(HEB2101210779) and GRB 210112A (HEB210112068) as samples to show the
procedures performed on all GRBs in Appendix A. The fits to time-averaged and
time-resolved spectra are all performed with Xspec 12.11.0.

####  4.7.1 Time-Average Spectrum

The time-averaged energy spectra are obtained from HXMT/CsI together with
other instruments. For example, from _Fermi_ /GBM, the spectra from two
NaI(Tl) scintillation detectors working at 8 keV $-$ 1 MeV and one BGO
scintillation detectors at $\sim 200$ keV to $\sim 4$ MeV are selected
according to the statistics of GRB signal. A joint fit with time-averaged
energy spectra from HXMT/CsI and three (two NaI and one BGO) spectra from
_Fermi_ /GBM are performed, where the parameters of GRB spectral shape are
shared but the amplitudes are set to be float for these four sets of data, to
compensate the possible lack information either in the adopted spectrum model
or the understanding of the instruments response. In most cases, the
amplitudes of fitted spectra are consistent well with each other within one
standard deviation.

To perform the joint fit, 6 models are chosen including a single power law
(PL), Band’s GRB function (BAND, Band et al. (1993)), an exponential cut-off
power law (CPL, also called Comptonized Model) and plus a component of black
body function (BB) of float amplitudes. The PL model is represented with
Equation 1 with two free parameters, where A denotes amplitude and $\alpha$ is
the spectral index.

$N_{\rm PL}(E)=AE^{\alpha}.$ (1)

The BAND function has four free parameters: low and high energy spectral
indices, denoted as $\alpha$ and $\beta$ respectively, the peak energy of $\nu
F_{\nu}$ spectrum, denoted as $E_{peak}$, and amplitude, as shown in Equation
2.

$\begin{split}&N_{\rm BAND}(E)=\\\ &A\begin{cases}\biggl{(}\frac{E}{100\ \rm
keV}\biggr{)}^{\alpha}\exp\biggl{[}-\frac{(\alpha+2)E}{E_{\rm
peak}}\biggr{]},\ E\geq\frac{(\alpha-\beta)\ E_{\rm peak}}{\alpha+2}\\\
\biggl{(}\frac{E}{100\ \rm
keV}\biggr{)}^{\beta}\exp(\beta-\alpha)\biggl{[}\frac{(\alpha-\beta)E_{\rm
peak}}{100\ \rm keV\ (\alpha+2)}\biggr{]}^{\alpha-\beta},\\\
E<\frac{(\alpha-\beta)\ E_{\rm peak}}{\alpha+2}.\end{cases}\end{split}$ (2)

CPL model is a subset of BAND model if $\beta$ is very small and the part of
$E<\frac{(\alpha-\beta)\ E_{\rm peak}}{\alpha+2}$ of BAND model is ignored.
There are three parameters in CPL model: the amplitude A, the lower energy
index $\alpha$, and the $\nu F_{\nu}$ peak energy, $E_{\rm peak}$, as shown in
Equation 3.

$N_{\rm COMP}(E)=A\ \Bigl{(}\frac{E}{E_{\rm
piv}}\Bigr{)}^{\alpha}\exp\Biggl{[}-\frac{(\alpha+2)\ E}{E_{\rm
peak}}\Biggr{]}.$ (3)

The Equation 4 for the photon spectrum of a black body usually used in the
spectral fitting, where $K=L_{\rm 39}/D^{2}_{\rm L,10kpc}$ is defined by the
blackbody luminosity L in units of $10^{39}$ erg s-1 in the GRB host galaxy
frame and the luminosity distance $D_{\rm L}$ in units of 10 kpc.

$N_{\rm BB}(E)=\frac{K\times 8.0525E^{2}}{(kT)^{4}[\exp(E/kT)-1]}.$ (4)

All models are formulated in units of photon flux with energy (E) in keV and
multiplied by a normalization constant A (ph s-1 cm-2 keV-1), and $kT$ and $E$
are measured in the observer’s frame. We determine the best spectral
parameters by optimizing the Castor C statistic value. Castor Cstat
(henceforth Cstat, Cash, 1979) is a likelihood technique modified for a
particular data set to converge to a $\chi^{2}$ with an increase of the
signal. $\chi^{2}$ is evaluated for each spectral fit that is performed
through minimizing C-Stat. Among these 6 models, the best model is determined
when a single additional parameter changes in $\chi^{2}$ by at least 6 since
the probability for achieving this difference is 0.01 as suggested by
Goldstein et al. (2012), which is a conservative threshold to avoid the false
positive rates of the extra component.

As shown in Figure 18 in Appendix A, for GRB 200125B (HEB200125863), joint
spectra fit with BAND model is the best model, with a reduced $\chi^{2}$ of
1.14. A BAND model of low energy spectral index $\alpha=-0.78\pm 0.01$, high
energy spectral index $\beta=-2.70\pm 0.03$, and the $\nu F_{\nu}$ peak
energy, $E_{peak}=200.8\pm 7.7$ keV, is determined. GRB 210121A is observed by
HXMT/CsI, _Fermi_ /GBM and GECAM, and joint analysis with the other two
missions is shown in Figure 21. $\alpha=-0.64\pm 0.01$, $\beta=-2.49\pm 0.03$
and $E_{peak}=932.4\pm 23.8$ keV are determined with a BAND model. Figure 22
shows the spectrum of GRB 210112A detected by _Swift_ /BAT and HXMT/CsI. The
best model is determined to be CPL, with $\alpha=-1.27\pm 0.03$, and
$E_{peak}=347.7\pm 49.7$ keV for the CPL component. In the case of utilizing
data of _Swift_ /BAT only, PL model is determined and the $E_{peak}$ is not
measured due to lack of information from higher energy band.

The distribution of energy spectra parameter of ‘GOLDEN’ GRBs are shown in
Figures 7, 8, 9. Up to 29% low energy spectral indices of the ‘GOLDEN’ samples
violate -2/3 synchrotron “line-of-death” (Preece et al., 1998), while an
additional 6% of the indices violate the -3/2 synchrotron cooling limit. The
distribution of high-energy indices in Figure 9 peaks at a slope slightly
steeper than -2 and have a extension toward steeper values. The $E_{peak}$
distribution generally peaks around 200 keV, and spans over two orders of
magnitude.

Figure 7: The distribution of low energy spectral index $\alpha$ of ‘GOLDEN’
GRBs from time-averaged spectral fits are shown. The blue solid lines denote
the total distribution of $\alpha$ from BAND model (red dashed lines), CPL
model (green dotted lines) and PL (orange dot-dashed lines).
Figure 8: The distribution of $\nu F_{\nu}$ peak energy $E_{peak}$ of ‘GOLDEN’
GRBs from time-averaged spectral fits are shown. The blue solid lines denote
the total distribution of $E_{peak}$ from BAND model (red dashed lines), CPL
model (green dotted lines).
Figure 9: The distribution of high energy spectral index $\beta$ of ‘GOLDEN’
GRBs from time-averaged spectral fits are shown.

####  4.7.2 Duration and Fluence

For ‘SILVER’ and ‘BRONZE’ samples, the burst durations are determined by
integrating the signal counts from GRBs with deposited energy in ranges of
40-800 keV in NG mode and 200-3000 keV in LG mode, respectively. The duration
$T_{\rm 50}$ and $T_{\rm 90}$ are determined from the interval between the
times where the burst has reached 25% (5%) and 75% (95%) of its maximum
counts. The method developed for BATSE (Koshut et al., 1996) are used to
determine the systematic error. Table 5 shows the values of durations of
‘SILVER’ and ‘BRONZE’ samples.

For ‘GOLDEN’ samples, the burst durations $T_{\rm 50}$ and $T_{\rm 90}$ are
computed in the 10-2000 keV energy range. They are determined using a method
similar to that developed for BATSE (Koshut et al., 1996), the counts spectra
of HXMT/CsI and the other missions in each time bin 64 ms are deconvolved and
the durations are computed from the time history of fitted photon spectra, as
shown in Figure 19 and 20. Peak fluxes of different time scales are naturally
obtained in the same analysis, and the fluence is obtained by integrating the
deconvolved flux history.

It is worth noting that, to avoid the failure of fit to each time bin, the
parameters of GRB shape are fixed to the best model determined in joint fit to
the time-averaged spectrum, while the amplitudes are set to be float.
Therefore, in addition to the systematic effects mentioned in Koshut et al.
(1996), an extra systematic error is introduced by fixed parameters. To
estimate the uncertainty from the fixed parameters, we simulate tens of sets
of parameters of the best GRB model by smearing the mean values with
covariance matrix within one standard deviation. Then the same procedures are
applied to calculate tens of sets of duration values. The maximum changes from
the duration values with the mean value are taken to be the systematic error
from fixed GRB parameters. The systematic uncertainties of peak fluxes and
fluences from the same source are also estimated in the same way. Note that in
most cases of spectral parameters that are well determined, the system
uncertainties of this kind are less than or numerically comparable with the
the systematic effects, which could be ignored. As a sample of GRB 200125B,
the total fluence (10-2000 keV) is 5.92e-05$\pm$4.54e-07 $\rm erg$ $\rm
cm^{-2}$, the peak flux ($\rm ph$ $\rm cm^{-2}$ s-1) in 10-2000 keV of
timescales of 64 ms, 256 ms, 1024 ms is 175.35$\pm$9.57, 149.25$\pm$3.78,
110.27$\pm$1.63 respectively.

##  5 CATALOG RESULTS

Table 3 lists the 322 searched bursts that are classified as GRBs. In the last
column of Table 3, abbreviation of GRBs types are given. Among 322 searched
bursts files, 202 ‘GOLDEN’ samples are analyzed and collected in all. 44
‘SILVER’ , 50 ‘BRONZE’ and 26 ‘IRON’ samples are also listed in Table 2.

The results of the duration of GRBs are derived from joint analyses of HXMT
with Fermi/GBM, Swift/BAT or GECAM discussed in 4.7, and shown in Table 4. The
values of $T_{\rm 50}$ and $T_{\rm 90}$ in 10-2000 keV energy range are listed
along with their respective statistical error estimates and start times
relative to the trigger time of HXMT. As part of the duration analysis, peak
fluxes and fluence are computed. Table 6 shows the total fluence and peak
fluxes of different time scales in 10-2000 keV. Table 5 lists the durations of
‘SILVER’ and ‘GOLDEN’ samples, which obtained from HXMT/CsI GRBs signal
counts.

##  6 DISCUSSION and SUMMARY

Histograms of the $T_{\rm 50}$ and $T_{\rm 90}$ distributions are shown in
10-2000 keV energy range in Figure 10. Using the conventional division between
the short and long GRB classes ($T_{\rm 90}$=2 s), we find 35 (17%) of the 202
‘GOLDEN’ GRBs to be in the short regime. Within the quoted duration errors,
the number of short GRB events ranges from 28 (14%) to 39 (19%). It is
consistent with the results from _Fermi_ /GBM GRB catalogs covering ten years
(von Kienlin et al., 2020), which has 395 (17%) short GRBs from statistics in
10-1000 keV. Due to the limited statistic of GRB numbers, we do not perform
lognormal fits to the distribution of durations.

Figure 16 shows the comparison of durations ($T_{\rm 90}$) from joint analyses
with other missions and those from HXMT/CsI GRBs data, where the red line
denotes the case of these two are equivalent to each other. Most GRBs are
below the red line, because energy range of HXMT/CsI is higher than those of
other missions, such as _Fermi_ /GBM and that GRBs tend to be shorter at
higher energy. Therefore, joint analysis is necessary for the measurement of
duration in 10-2000 keV.

Despite of the limited statistic of ‘GOLDEN’ GRBs, as shown in Figure 11,
anti-correlation of spectral hardness with duration is confirmed by the
relationship between the hardness and duration, where the hardness is
calculated as the ratio of the flux density from spectral parameters
determined from time-averaged spectral fits in 50-300 keV to that in 10-50
keV. We note that, here the durations are those from joint analyses in energy
range of 10-2000 keV, which also illustrates the anti-correlation between the
hardness of GRBs spectra and duration.

Distributions of GRBs fluence are shown in Figure 15. Peak fluxes on
timescales of 64 ms, 256 ms, 1024 ms are shown in Figure 12, Figure 13 and
Figure 14 respectively. These distributions are not consistent with those from
von Kienlin et al. (2020). The contributions are very small both below 10-7
$\rm erg$ $\rm cm^{-2}$ and 1 $\rm ph$ $\rm cm^{-2}$ s-1 in distributions of
fluence and peak fluxes. It could be explained by the sharply fall of
effective area below 100 keV. Weak short GRBs cannot cause enough statistics
in HXMT/CsI, and thus cannot be detected significantly. Extremely bright GRBs
would not be included in ‘GOLDEN’ samples because they are very likely to
cause data saturation in HXMT and be labeled as ‘IRON’ samples.

Figure 10:  Distributions of ‘GOLDEN’ GRB durations in the 10-2000 keV energy
range are shown. The upper plot shows $T_{\rm 50}$ and the lower plot shows
$T_{\rm 90}$.

Figure 11:  Scatter plots of spectral hardness vs. duration are shown for the
two duration measures $T_{\rm 50}$ (upper plot) and $T_{\rm 90}$ (lower plot)
as shown in Figure 10. The hardness is calculated as the ratio of the flux
density from spectral parameters determined from time-averaged spectral fits
in 50-300 keV to that in 10-50 keV. For clarity, the estimated errors are not
shown but can be quite large for the weak events. Nevertheless, the anti-
correlation of spectral hardness with burst duration is evident.  Figure 12:
Distribution of ‘GOLDEN’ GRBs peak flux on the 0.064 s timescale is shown in
energy range of 10-2000 keV. Figure 13:  Distribution of ‘GOLDEN’ GRBs peak
flux on the 0.256 s timescale is shown in energy range of 10-2000 keV. Figure
14:  Distribution of ‘GOLDEN’ GRBs peak flux on 1.024 s timescale is shown in
energy range of 10-2000 keV. Figure 15:  Distribution of ‘GOLDEN’ GRBs fluence
is shown in energy range of 10-2000 keV. Figure 16:  A comparison between the
durations ($T_{\rm 90}$) of ‘GOLDEN’ GRBs from joint analysis and those
obtained from HXMT/CsI GRBs counts are shown. The red line denotes the case of
these two are equal to each other.

This work made use of the data from the _Insight-_ HXMT mission, a project
funded by China National Space Administration (CNSA) and the Chinese Academy
of Sciences (CAS). The authors thank supports from the National Program on Key
Research and Development Project (Grants No. 2016YFA0400801, 2021YFA0718500),
the National Natural Science Foundation of China under Grants No. U1838113,
and the Strategic Priority Research Program on Space Science, the Chinese
Academy of Sciences (Grant No. XDB23040400, XDA15052700). The authors are very
grateful to the public data of _Fermi_ /GBM, _Swift_ /BAT and GECAM.

Table 3:  GRB Triggers: Locations and Trigger Characteristics. Trigger IDaaThe trigger ID starts with a ‘HEB’ label which means ‘HE-detected Burst’. | GRB Name | Trigger Time (UTC) | Search MethodbbAs clarified in Sec 3, BLIND: blind search, TARGETED: targeted search. | Gain Mode | RA(°) | DEC(°) | err(°) | location sourceccThe uncertainties of the locations from _Swift_ /BAT are 90% containment, including systematic uncertainty, while those from _Fermi_ /GBM and other detections are 1$\sigma$ containment, statistical only. If the location source is from interplanetary network (IPN) triangulation, the error is determined to be the maximum dimension of error box area. Instrument detections are defined as: Fermi/LAT: Large Area Telescope, IBIS: Imager on Board Integral Satellite in INTEGRAL.  | Kinds of GRB samplesddAs shown in Table 2, G: GOLDEN, S: SILVER, B: BRONZE, I: IRON.
---|---|---|---|---|---|---|---|---|---
HEB170626040 | GRB 170626B | 2017-06-26T00:57:55.80 | BLIND | NG | 289.8 | -19.2 | 5.0 | IPN | S
HEB170626400 | GRB 170626A | 2017-06-26T09:37:22.32 | BLIND | NG | 165.4 | 56.5 | 1.0 | Fermi/GBM | G
HEB170705115 | GRB 170705A | 2017-07-05T02:45:59.00 | BLIND | NG | 191.7 | 18.3 | 0.1 | Swift | G
HEB170708045 | GRB 170708A | 2017-07-08T01:06:11.25 | BLIND | LG | 335.8 | 19.8 | 4.6 | IPN | S
HEB170712139 | GRB 170712A | 2017-07-12T03:20:30.00 | BLIND | LG | - | - | - | - | B
HEB170714049 | GRB 170714B | 2017-07-14T01:10:51.10 | BLIND | NG | 18.2 | 29.5 | - | Fermi/GBM | G
HEB170718152 | - | 2017-07-18T03:39:30.00 | TARGETED | NG | 102.3 | -35.0 | - | Fermi/GBM | G
HEB170726248 | GRB 170726B | 2017-07-26T05:58:15.42 | BLIND | NG | 166.4 | -34.0 | 2.8 | Fermi/GBM | G
HEB170726793 | GRB 170726A | 2017-07-26T19:02:59.51 | BLIND | NG | 297.8 | 6.6 | - | Fermi/GBM | G
HEB170728960 | GRB 170728B | 2017-07-28T23:03:19.00 | BLIND | NG | 238.0 | 70.1 | - | Fermi/GBM | G
HEB170731751 | - | 2017-07-31T18:01:39.75 | BLIND | NG | 245.2 | 64.3 | 6.3 | Fermi/GBM | G
HEB170801208 | GRB 170801A | 2017-08-01T04:59:55.25 | BLIND | NG | - | - | - | - | B
HEB170802637 | GRB 170802A | 2017-08-02T15:18:26.00 | BLIND | NG | 52.3 | -39.2 | 2.1 | Fermi/GBM | G
HEB170803917 | GRB 170803B | 2017-08-03T22:00:31.00 | BLIND | NG | - | - | - | - | S
HEB170805596 | GRB 170805B | 2017-08-05T14:18:49.50 | BLIND | NG | 137.3 | 69.6 | 1.3 | IPN | S
HEB170805610 | GRB 170805A | 2017-08-05T14:38:34.00 | BLIND | NG | 269.2 | -18.3 | 4.6 | IPN | S
HEB170817908 | GRB 170817B | 2017-08-17T21:47:34.00 | BLIND | NG | 83.0 | 50.1 | 3.7 | Fermi/GBM | G
HEB170825306 | - | 2017-08-25T07:22:03.00 | BLIND | NG | 274.4 | -26.2 | 3.2 | Fermi/GBM | G
HEB170826818 | GRB 170826B | 2017-08-26T19:38:58.00 | BLIND | NG | 327.7 | -31.8 | 1.0 | Fermi/GBM | G
HEB170829270 | GRB 170829A | 2017-08-29T06:29:39.90 | BLIND | NG | - | - | - | - | S
HEB170901499 | GRB 170901B | 2017-09-01T11:59:56.50 | BLIND | NG | - | - | - | - | B
HEB170903534 | GRB 170903A | 2017-09-03T12:49:11.00 | BLIND | NG | 254.5 | 35.0 | 1.3 | Fermi/GBM | G
HEB170904406 | GRB 170904A | 2017-09-04T09:46.00.62 | BLIND | NG | 35.4 | -32.5 | 3.2 | IPN | S
HEB170904884 | - | 2017-09-04T21:13:07.10 | BLIND | NG | - | - | - | - | B
HEB170906029 | GRB 170906A | 2017-09-06T00:43:06.00 | BLIND | LG | 198.6 | -53.5 | 12.2 | Fermi/GBM | G
HEB170912984 | GRB 170912C | 2017-09-12T23:38:12.60 | BLIND | NG | 83.6 | 7.2 | - | Fermi/GBM | G
HEB170918905 | GRB 170918A | 2017-09-18T21:43:35.40 | BLIND | NG | - | - | - | - | B
HEB170921030 | GRB 170921C | 2017-09-21T00:43:37.00 | BLIND | NG | - | - | - | - | B
HEB170923188 | GRB 170923A | 2017-09-23T04:31:05.44 | BLIND | NG | 221.5 | 81.2 | 5.0 | Fermi/GBM | G
HEB170926340 | GRB 170926A | 2017-09-26T08:10:39.80 | BLIND | NG | - | - | - | - | B
HEB171007498 | GRB 171007A | 2017-10-07T11:57:38.27 | BLIND | NG | 135.6 | 42.8 | 0.1 | Swift | I
HEB171008079 | GRB 171008A | 2017-10-08T01:54:38.50 | BLIND | NG | 232.6 | 24.0 | - | Fermi/GBM | G
HEB171011045 | GRB 171011B | 2017-10-11T01:05:36.00 | BLIND | NG | 158.9 | 1.6 | 8.1 | IPN | I
HEB171013350 | GRB 171013B | 2017-10-13T08:24:42.11 | TARGETED | NG | 145.1 | -32.6 | 30.3 | Fermi/GBM | G
HEB171020963 | GRB 171020A | 2017-10-20T23:07:10.75 | BLIND | NG | 39.2 | 15.2 | 0.1 | Swift | G
HEB171030728 | GRB 171030A | 2017-10-30T17:29:45.00 | BLIND | NG | 74.1 | -19.5 | 23.4 | IPN | G
HEB171102106 | GRB 171102A | 2017-11-02T02:33:35.99 | BLIND | NG | 188.8 | 54.3 | 11.5 | IPN | S
HEB171103965 | GRB 171103A | 2017-11-03T23:10:30.04 | BLIND | NG | 249.5 | -10.2 | 3.0 | Fermi/GBM | G
HEB171108279 | GRB 171108B | 2017-11-08T06:42:24.00 | BLIND | NG | - | - | - | - | B
HEB171115217 | GRB 171115B | 2017-11-15T05:13:14.70 | BLIND | NG | - | - | - | - | B
HEB171120555 | GRB 171120A | 2017-11-20T13:20:02.00 | BLIND | NG | 163.8 | 22.5 | 0.1 | Swift | G
HEB171124234 | GRB 171124A | 2017-11-24T05:38:03.00 | BLIND | NG | 333.9 | 35.1 | 1.6 | Fermi/GBM | G
HEB171207054 | - | 2017-12-07T01:18:42.45 | TARGETED | NG | 314.4 | 51.7 | 9.5 | Fermi/GBM | G
HEB171209615 | GRB 171209A | 2017-12-09T14:46:16.22 | BLIND | NG | 139.4 | -30.5 | 0.1 | Swift | G
HEB171210492 | GRB 171210A | 2017-12-10T11:49:16.00 | BLIND | NG | 338.0 | 27.5 | 1.0 | Fermi/GBM | G
HEB171215705 | GRB 171215A | 2017-12-15T16:55:26.57 | BLIND | NG | 19.7 | 34.7 | 4.7 | Fermi/GBM | G
HEB171223818 | GRB 171223A | 2017-12-23T19:38:15.00 | BLIND | NG | 115.8 | -33.5 | 6.6 | Fermi/GBM | G
HEB171230955 | GRB 171230B | 2017-12-30T22:55:34.00 | BLIND | NG | 89.5 | -27.8 | 1.1 | Fermi/GBM | G
HEB180103047 | GRB 180103A | 2018-01-03T01:08:40.00 | BLIND | NG | 159.6 | -53.5 | 0.1 | Swift | S
HEB180103949 | - | 2018-01-03T22:47:12.00 | BLIND | NG | - | - | - | - | B
HEB180110608 | - | 2018-01-10T14:35:59.22 | BLIND | NG | 126.3 | 51.3 | 30.1 | Fermi/GBM | G
HEB180111695 | GRB 180111A | 2018-01-11T16:42:06.38 | BLIND | LG | 149.8 | 48.2 | 0.1 | Swift | G
HEB180112687 | GRB 180112A | 2018-01-12T16:30:38.00 | BLIND | LG | - | - | - | - | S
HEB180113011 | GRB 180113B | 2018-01-13T00:16:00.00 | BLIND | NG | 354.0 | 13.5 | 1.2 | Fermi/GBM | I
HEB180113418 | GRB 180113C | 2018-01-13T10:02:07.50 | BLIND | NG | 174.6 | -64.7 | 1.0 | Fermi/GBM | I
HEB180119836 | - | 2018-01-19T20:04:49.78 | BLIND | NG | 348.7 | -15.0 | 2.5 | Fermi/GBM | G
HEB180127049 | - | 2018-01-27T01:11:12.91 | BLIND | NG | 20.5 | 25.8 | 5.0 | Fermi/GBM | G
HEB180130744 | - | 2018-01-30T17:51:26.79 | TARGETED | NG | 136.8 | 52.7 | 68.1 | Fermi/GBM | G
HEB180202211 | GRB 180202A | 2018-02-02T05:04:28.00 | BLIND | NG | - | - | - | - | S
HEB180208764 | - | 2018-02-08T18:20:50.30 | TARGETED | NG | 196.6 | 8.2 | 5.1 | Fermi/GBM | G
HEB180210517 | GRB 180210A | 2018-02-10T12:24:44.00 | BLIND | NG | 3.3 | 21.0 | 1.5 | Fermi/GBM | G
HEB180210728 | - | 2018-02-10T17:29:06.00 | BLIND | NG | - | - | - | - | B
HEB180218634 | GRB 180218A | 2018-02-18T15:14:05.49 | BLIND | NG | 47.2 | 46.6 | 4.4 | Fermi/GBM | I
HEB180219482 | GRB 180219A | 2018-02-19T11:34:39.00 | BLIND | NG | 86.2 | 32.3 | 1.0 | Fermi/GBM | I
HEB180221520 | GRB 180221B | 2018-02-21T12:30:01.00 | BLIND | NG | - | - | - | - | S
HEB180226392 | - | 2018-02-26T09:24:58.73 | BLIND | NG | - | - | - | - | S
HEB180305393 | GRB 180305A | 2018-03-05T09:26:08.66 | BLIND | NG | 45.9 | 31.2 | 1.6 | Fermi/GBM | G
HEB180306972 | - | 2018-03-06T23:20:33.93 | TARGETED | NG | 196.8 | -32.2 | 14.8 | Fermi/GBM | G
HEB180309321 | - | 2018-03-09T07:43:10.62 | TARGETED | NG | 186.1 | 34.5 | 2.1 | Fermi/GBM | G
HEB180313977 | GRB 180313A | 2018-03-13T23:28:17.53 | BLIND | NG | 317.5 | -26.5 | 5.7 | Fermi/GBM | G
HEB180326143 | GRB 180326A | 2018-03-26T03:26:07.06 | BLIND | NG | 291.7 | -13.5 | 3.1 | IPN | S
HEB180330891 | - | 2018-03-30T21:23:15.52 | BLIND | NG | 164.2 | 83.9 | 3.7 | Fermi/GBM | G
HEB180331177 | GRB 180331A | 2018-03-31T04:14:55.70 | BLIND | NG | 66.0 | 13.4 | 0.1 | Swift | G
HEB180401279 | - | 2018-04-01T06:42:43.78 | BLIND | NG | 126.7 | 7.0 | 1.6 | Fermi/GBM | G
HEB180402406 | GRB 180402A | 2018-04-02T09:44:59.37 | BLIND | NG | 251.9 | -14.9 | 0.1 | Swift | G
HEB180404091 | GRB 180404B | 2018-04-04T02:11:38.64 | BLIND | NG | 53.0 | -49.3 | 1.2 | Fermi/GBM | G
HEB180405168 | - | 2018-04-05T04:02:53.06 | BLIND | NG | 123.6 | -33.5 | 2.2 | Fermi/GBM | S
HEB180409346 | GRB 180409A | 2018-04-09T08:18:18.67 | BLIND | LG | 178.2 | 36.0 | 1.0 | Fermi/GBM | G
HEB180411359 | GRB 180411B | 2018-04-11T08:37:29.76 | BLIND | NG | - | - | - | - | B
HEB180413117 | - | 2018-04-13T02:49:43.23 | BLIND | NG | 168.2 | -31.6 | 1.2 | Fermi/GBM | G
HEB180416923 | GRB 180416B | 2018-04-16T22:10:11.00 | BLIND | NG | 353.5 | 74.6 | 2.1 | Fermi/GBM | G
HEB180427442 | GRB 180427A | 2018-04-27T10:37:03.00 | BLIND | NG | 283.3 | 46.6 | 1.0 | Fermi/GBM | G
HEB180505539 | GRB 180505A | 2018-05-05T12:57:30.00 | BLIND | LG | 4.5 | -59.9 | 1.2 | Fermi/GBM | G
HEB180506902 | - | 2018-05-06T21:38:58.00 | BLIND | NG | 61.2 | -0.9 | 6.7 | Fermi/GBM | G
HEB180510808 | GRB 180510A | 2018-05-10T19:24:39.00 | BLIND | NG | 276.3 | -31.9 | 1.0 | Swift | G
HEB180523782 | - | 2018-05-23T18:46:28.00 | BLIND | LG | 168.4 | 49.4 | 12.9 | Fermi/GBM | G
HEB180525151 | - | 2018-05-25T03:37:59.05 | BLIND | NG | 103.3 | 19.9 | 14.9 | Fermi/GBM | G
HEB180603235 | - | 2018-06-03T05:39:50.00 | BLIND | LG | - | - | - | - | S
HEB180605457 | GRB 180605A | 2018-06-05T10:59:25.00 | BLIND | LG | 50.0 | -50.4 | 1.0 | Fermi/GBM | G
HEB180615462 | - | 2018-06-15T11:05:56.00 | BLIND | NG | 55.8 | 78.3 | 1.0 | Fermi/GBM | I
HEB180617871 | - | 2018-06-17T20:55:23.60 | BLIND | NG | - | - | - | - | B
HEB180618030 | GRB 180618A | 2018-06-18T00:43:13.00 | BLIND | NG | 169.9 | 73.8 | 0.1 | Swift | G
HEB180623696 | GRB 180623A | 2018-06-23T16:42:21.00 | BLIND | NG | 214.5 | -60.3 | 0.1 | Swift | G
HEB180625940 | - | 2018-06-25T22:34:41.50 | BLIND | NG | 39.1 | -62.3 | 6.4 | Fermi/GBM | G
HEB180626260 | GRB 180626D | 2018-06-26T06:15:14.00 | BLIND | NG | - | - | - | - | B
HEB180626391 | GRB 180626C | 2018-06-26T09:23:50.95 | BLIND | NG | 285.1 | 44.8 | 8.2 | Fermi/GBM | G
HEB180704233 | GRB 180704A | 2018-07-04T05:36:43.00 | BLIND | NG | 32.6 | 70.0 | 0.1 | Swift | G
HEB180704525 | GRB 180704B | 2018-07-04T12:36:33.00 | BLIND | NG | - | - | - | Fermi/GBM | S
HEB180715754 | GRB 180715A | 2018-07-15T18:07:05.00 | BLIND | NG | 231.8 | -4.4 | 4.8 | Fermi/GBM | G
HEB180718762 | GRB 180718B | 2018-07-18T18:18:24.00 | BLIND | NG | 44.7 | -31.5 | 0.6 | Fermi/LAT | G
HEB180720598 | GRB 180720B | 2018-07-20T14:21:39.65 | BLIND | LG | 0.5 | -2.9 | 1.2 | Fermi/GBM | I
HEB180722992 | GRB 180722B | 2018-07-22T23:49:13.00 | BLIND | NG | 55.3 | 41.7 | 3.5 | Fermi/GBM | G
HEB180724807 | GRB 180724A | 2018-07-24T19:22:31.00 | BLIND | LG | 285.2 | -33.7 | 1.0 | Fermi/GBM | G
HEB180730017 | - | 2018-07-30T00:25:40.00 | BLIND | NG | 98.0 | 44.5 | 8.3 | Fermi/GBM | G
HEB180801275 | - | 2018-08-01T06:37:03.51 | TARGETED | NG | 240.9 | -11.4 | 8.8 | Fermi/GBM | G
HEB180803590 | - | 2018-08-03T14:09:49.73 | BLIND | LG | 71.6 | 57.6 | 17.4 | Fermi/GBM | G
HEB180804554 | - | 2018-08-04T13:17:48.00 | BLIND | NG | - | - | - | - | B
HEB180804930 | - | 2018-08-04T22:20:38.28 | BLIND | NG | 109.4 | -69.3 | 1.8 | Fermi/GBM | G
HEB180816088 | - | 2018-08-16T02:07:18.91 | TARGETED | NG | 126.2 | -36.7 | 1.9 | Fermi/GBM | G
HEB180822561 | - | 2018-08-22T13:28:34.05 | TARGETED | NG | 185.2 | -61.5 | 2.2 | Fermi/GBM | G
HEB180828789 | GRB 180828A | 2018-08-28T18:57:26.58 | BLIND | NG | 270.7 | -23.9 | 1.2 | Fermi/GBM | G
HEB180912273 | - | 2018-09-12T06:34:15.40 | BLIND | NG | 202.0 | -26.2 | 2.1 | Fermi/GBM | I
HEB180914765 | GRB 180914B | 2018-09-14T18:22:48.00 | BLIND | NG | 332.4 | 24.9 | 0.3 | Fermi/LAT | I
HEB180922461 | - | 2018-09-22T11:03:52.02 | TARGETED | NG | 19.2 | -0.1 | 4.4 | Fermi/GBM | I
HEB180925407 | - | 2018-09-25T09:46:30.54 | TARGETED | NG | 181.9 | -25.4 | 9.3 | Fermi/GBM | G
HEB180925609 | GRB 180925A | 2018-09-25T14:37:27.90 | BLIND | NG | 315.2 | -64.4 | 0.1 | Swift | G
HEB180927992 | - | 2018-09-27T23:49:20.19 | BLIND | NG | 236.0 | -1.7 | 5.7 | Fermi/GBM | G
HEB180929453 | - | 2018-09-29T10:52:33.92 | BLIND | NG | 244.7 | -8.9 | 8.4 | Fermi/GBM | G
HEB181008269 | - | 2018-10-08T06:28:13.50 | BLIND | NG | 57.5 | 7.2 | 14.4 | Fermi/GBM | G
HEB181011181 | - | 2018-10-11T04:21:12.00 | BLIND | LG | - | - | - | - | S
HEB181014479 | - | 2018-10-14T11:30:23.00 | BLIND | NG | 228.9 | 16.5 | 1.3 | Fermi/GBM | G
HEB181028590 | GRB 181028A | 2018-10-28T14:09:43.00 | BLIND | LG | 88.9 | -21.2 | 2.5 | IPN | G
HEB181112582 | - | 2018-11-12T13:58:51.00 | BLIND | NG | - | - | - | - | I
HEB181119605 | GRB 181119A | 2018-11-19T14:32:17.13 | BLIND | NG | 86.4 | 37.1 | 1.8 | Fermi/GBM | G
HEB181121306 | - | 2018-11-21T07:21:29.27 | BLIND | NG | 130.9 | 31.5 | 18.3 | Fermi/GBM | G
HEB181122381 | - | 2018-11-22T09:09:03.06 | BLIND | LG | 93.7 | 34.4 | 4.2 | Fermi/GBM | G
HEB181123231 | GRB 181123B | 2018-11-23T05:33:03.09 | BLIND | NG | 184.3 | 14.6 | 0.1 | Swift | G
HEB181201111 | GRB 181201A | 2018-12-01T02:39:53.00 | BLIND | NG | 319.3 | -12.6 | 0.1 | IBIS | S
HEB181212692 | GRB 181212A | 2018-12-12T16:37:45.50 | BLIND | NG | 298.4 | -3.7 | 2.3 | Fermi/GBM | G
HEB181213540 | GRB 181213A | 2018-12-13T12:57:38.00 | BLIND | NG | 248.3 | 78.5 | 0.1 | Swift | G
HEB181217664 | GRB 181217A | 2018-12-17T15:56:57.00 | BLIND | NG | 332.2 | 29.9 | - | Fermi/GBM | G
HEB181222841 | GRB 181222B | 2018-12-22T20:11:37.00 | BLIND | NG | 311.1 | 22.9 | 1.6 | Fermi/GBM | I
HEB181225489 | GRB 181225A | 2018-12-25T11:44:10.00 | BLIND | LG | 348.1 | -9.5 | - | Fermi/GBM | G
HEB190102652 | - | 2019-01-02T15:40:17.27 | BLIND | NG | - | - | - | - | S
HEB190103695 | GRB 190103A | 2019-01-03T16:41:52.64 | BLIND | NG | 251.4 | 17.4 | 2.7 | IPN | I
HEB190103877 | GRB 190103B | 2019-01-03T21:03:50.00 | BLIND | NG | 212.6 | 35.3 | 0.1 | Swift | G
HEB190110725 | GRB 190110A | 2019-01-10T17:24:53.00 | BLIND | NG | 277.0 | -49.2 | 2.2 | Fermi/GBM | G
HEB190114872 | GRB 190114C | 2019-01-14T20:57:02.00 | BLIND | LG | 56.2 | -31.8 | 3.3 | Fermi/GBM | I
HEB190117608 | GRB 190117A | 2019-01-17T14:36:47.00 | BLIND | NG | - | - | - | - | S
HEB190131964 | GRB 190131A | 2019-01-31T23:08:35.00 | BLIND | NG | 42.3 | 35.5 | 2.2 | Fermi/GBM | G
HEB190203655 | - | 2019-02-03T15:44:09.00 | BLIND | NG | - | - | - | - | B
HEB190212129 | GRB 190212A | 2019-02-12T03:06:06.20 | BLIND | NG | - | - | - | - | S
HEB190215771 | GRB 190215A | 2019-02-15T18:31:22.48 | BLIND | NG | 342.3 | 36.2 | 1.0 | Fermi/GBM | G
HEB190218810 | - | 2019-02-18T19:27:40.00 | BLIND | NG | - | - | - | - | B
HEB190222537 | - | 2019-02-22T12:53:27.15 | BLIND | NG | 147.3 | 60.9 | 1.5 | Fermi/GBM | G
HEB190226515 | GRB 190226A | 2019-02-26T12:21:45.50 | BLIND | NG | 224.4 | -8.6 | - | Fermi/GBM | G
HEB190305545 | GRB 190305A | 2019-03-05T13:05:19.00 | BLIND | NG | - | - | - | - | I
HEB190306467 | GRB 190306B | 2019-03-06T11:13:27.95 | BLIND | NG | - | - | - | - | B
HEB190310398 | GRB 190310A | 2019-03-10T09:33:25.00 | BLIND | NG | 349.3 | 12.1 | 1.2 | Fermi/GBM | G
HEB190321931 | GRB 190321A | 2019-03-21T22:21:21.00 | BLIND | NG | - | - | - | - | S
HEB190323878 | GRB 190323D | 2019-03-23T21:05:24.00 | BLIND | NG | 34.7 | 10.3 | 1.1 | Fermi/GBM | S
HEB190324348 | GRB 190324B | 2019-03-24T08:21:21.00 | BLIND | NG | 81.0 | 12.0 | 1.0 | Fermi/GBM | G
HEB190324947 | GRB 190324A | 2019-03-24T22:44:20.50 | BLIND | NG | 49.6 | -47.2 | 0.1 | Swift | G
HEB190326313 | GRB 190326B | 2019-03-26T07:31:47.00 | BLIND | NG | 264.2 | 68.3 | 1.3 | Fermi/GBM | G
HEB190326316 | GRB 190326A | 2019-03-26T07:35:28.90 | BLIND | NG | 341.6 | 39.9 | 0.1 | Swift | G
HEB190330207 | - | 2019-03-30T04:59:27.70 | BLIND | NG | - | - | - | - | B
HEB190330694 | GRB 190330A | 2019-03-30T16:39:32.00 | BLIND | LG | 86.9 | 22.6 | 2.1 | Fermi/GBM | G
HEB190331093 | GRB 190331A | 2019-03-31T02:14:38.00 | BLIND | NG | 28.6 | 27.6 | 0.1 | Swift | G
HEB190331841 | GRB 190331C | 2019-03-31T20:12:00.10 | BLIND | NG | - | - | - | - | S
HEB190401139 | GRB 190401A | 2019-04-01T03:20:21.00 | BLIND | NG | 280.0 | 39.0 | 5.7 | Fermi/GBM | G
HEB190407671 | GRB 190407A | 2019-04-07T16:07:26.49 | TARGETED | NG | 181.8 | 40.6 | 4.5 | Fermi/GBM | G
HEB190411406 | GRB 190411A | 2019-04-11T09:45:46.00 | BLIND | NG | 286.0 | -36.3 | 4.8 | Fermi/GBM | I
HEB190415173 | GRB 190415A | 2019-04-15T04:09:49.90 | BLIND | NG | 26.9 | 13.9 | 6.6 | Fermi/GBM | I
HEB190422283 | - | 2019-04-22T06:48:17.50 | BLIND | NG | 306.7 | -73.0 | 1.8 | Fermi/GBM | G
HEB190424417 | GRB 190424A | 2019-04-24T10:00:42.00 | BLIND | NG | 48.7 | 20.2 | 0.1 | Swift | G
HEB190507269 | GRB 190507A | 2019-05-07T06:28:23.00 | BLIND | NG | 156.0 | -12.8 | 4.8 | Fermi/GBM | G
HEB190510119 | GRB 190510B | 2019-05-10T02:52:13.23 | TARGETED | NG | 124.5 | -53.1 | 1.2 | Fermi/GBM | S
HEB190515189 | GRB 190515A | 2019-05-15T04:33:03.00 | BLIND | NG | 137.2 | 39.3 | 5.0 | Fermi/GBM | G
HEB190525031 | GRB 190525A | 2019-05-25T00:45:47.65 | TARGETED | NG | 338.0 | 5.4 | 4.0 | Fermi/GBM | G
HEB190530429 | GRB 190530A | 2019-05-30T10:19:08.90 | BLIND | NG | 120.5 | 35.5 | 1.0 | Fermi/GBM | I
HEB190531840 | GRB 190531B | 2019-05-31T20:10:12.00 | BLIND | NG | 24.3 | -42.0 | 1.0 | Fermi/GBM | G
HEB190604446 | GRB 190604A | 2019-06-04T10:42:37.05 | BLIND | NG | 342.5 | 46.4 | 1.0 | Fermi/GBM | G
HEB190605110 | GRB 190605B | 2019-06-05T02:39:08.00 | BLIND | NG | - | - | - | - | B
HEB190606079 | GRB 190606A | 2019-06-06T01:55:07.78 | BLIND | NG | 76.6 | -0.6 | 6.0 | IPN | I
HEB190610477 | GRB 190610A | 2019-06-10T11:27:45.00 | BLIND | NG | 46.2 | -7.7 | 0.1 | Swift | S
HEB190613449 | GRB 190613B | 2019-06-13T10:47:00.00 | BLIND | NG | 305.4 | -4.6 | 0.1 | Swift | G
HEB190615612 | GRB 190615B | 2019-06-15T14:42:22.00 | BLIND | NG | - | - | - | - | B
HEB190615636 | GRB 190615A | 2019-06-15T15:16:27.00 | BLIND | NG | 191.4 | 49.4 | 2.3 | Fermi/GBM | G
HEB190619594 | GRB 190619B | 2019-06-19T14:16:37.00 | BLIND | NG | 291.1 | 20.2 | 1.8 | Fermi/GBM | G
HEB190620507 | GRB 190620A | 2019-06-20T12:10:19.50 | BLIND | NG | 166.2 | 26.8 | 4.4 | Fermi/GBM | G
HEB190706571 | GRB 190706C | 2019-07-06T13:42:25.95 | BLIND | NG | 351.7 | 24.7 | 2.6 | IPN | I
HEB190706710 | GRB 190706D | 2019-07-06T17:03:05.40 | BLIND | NG | 324.6 | 9.9 | 21.9 | IPN | S
HEB190719113 | GRB 190719A | 2019-07-19T02:44:08.00 | BLIND | NG | 123.9 | -30.8 | 5.2 | Fermi/GBM | B
HEB190720964 | GRB 190720B | 2019-07-20T23:08:39.50 | BLIND | NG | 138.9 | -55.6 | 2.3 | Fermi/GBM | G
HEB190723308 | GRB 190723A | 2019-07-23T07:24:16.00 | BLIND | NG | 289.5 | 25.2 | 10.5 | Fermi/GBM | G
HEB190724030 | GRB 190724A | 2019-07-24T00:43:56.75 | BLIND | NG | 170.3 | 15.1 | 13.6 | Fermi/GBM | G
HEB190726642 | GRB 190726A | 2019-07-26T15:24:59.20 | BLIND | NG | 310.3 | 34.3 | 1.2 | Fermi/GBM | G
HEB190806675 | GRB 190806A | 2019-08-06T16:12:33.32 | BLIND | NG | 121.1 | -75.4 | 4.3 | Fermi/GBM | G
HEB190813520 | GRB 190813A | 2019-08-13T12:29:09.94 | BLIND | NG | 106.4 | -23.3 | 10.4 | Fermi/GBM | G
HEB190814837 | GRB 190814A | 2019-08-14T20:05:21.00 | BLIND | NG | 60.4 | -60.3 | 30.2 | Fermi/GBM | G
HEB190825878 | GRB 190825B | 2019-08-25T21:04:54.50 | BLIND | NG | - | - | - | - | B
HEB190828783 | GRB 190828D | 2019-08-28T18:48:33.70 | BLIND | NG | 251.9 | -24.5 | 2.5 | IBIS | S
HEB190831271 | - | 2019-08-31T06:30:27.11 | BLIND | NG | - | - | - | - | S
HEB190901890 | GRB 190901A | 2019-09-01T21:21:57.80 | BLIND | NG | 230.6 | -3.0 | 18.8 | Fermi/GBM | G
HEB190903721 | GRB 190903A | 2019-09-03T17:19:36.26 | BLIND | NG | 70.5 | -49.0 | 6.4 | Fermi/GBM | G
HEB190906045 | GRB 190906A | 2019-09-06T01:04:50.90 | BLIND | NG | 267.6 | -11.9 | 6.0 | IPN | S
HEB190906767 | GRB 190906B | 2019-09-06T18:25:09.29 | BLIND | NG | 171.8 | -71.6 | 3.5 | Fermi/GBM | G
HEB190915239 | GRB 190915A | 2019-09-15T05:44:58.40 | BLIND | NG | 48.3 | 4.0 | 4.3 | Fermi/GBM | G
HEB190927106 | - | 2019-09-27T02:33:50.30 | BLIND | NG | - | - | - | - | B
HEB190928550 | GRB 190928A | 2019-09-28T13:12:14.00 | BLIND | NG | 36.6 | 29.5 | 18.4 | IPN | S
HEB190928551 | GRB 190928A | 2019-09-28T13:13:48.40 | BLIND | NG | 36.6 | 29.5 | 18.4 | IPN | S
HEB190929884 | - | 2019-09-29T21:13:49.66 | BLIND | NG | - | - | - | - | B
HEB191009297 | GRB 191009A | 2019-10-09T07:08:56.77 | BLIND | NG | 29.4 | 63.4 | 9.1 | Fermi/GBM | G
HEB191019970 | GRB 191019B | 2019-10-19T23:17:13.35 | BLIND | NG | 216.3 | -40.6 | 1.0 | Fermi/GBM | G
HEB191021831 | - | 2019-10-21T19:57:29.00 | BLIND | NG | - | - | - | - | B
HEB191025779 | GRB 191025B | 2019-10-25T18:42:09.10 | BLIND | NG | 60.1 | 56.5 | 3.9 | IPN | I
HEB191031182 | - | 2019-10-31T04:23:11.36 | BLIND | NG | - | - | - | - | S
HEB191031318 | GRB 191031E | 2019-10-31T07:38:55.54 | BLIND | NG | - | - | - | - | S
HEB191031780 | GRB 191031C | 2019-10-31T18:43:16.00 | BLIND | NG | 115.9 | -62.3 | 1.3 | Fermi/GBM | G
HEB191105257 | - | 2019-11-05T06:11:08.65 | BLIND | NG | 297.3 | 24.6 | 3.3 | Fermi/GBM | G
HEB191108003 | GRB 191108A | 2019-11-08T00:04:37.60 | BLIND | NG | 232.9 | 10.8 | 17.3 | Fermi/GBM | G
HEB191111364 | GRB 191111A | 2019-11-11T08:44:29.95 | BLIND | NG | 197.2 | -23.2 | 13.4 | Fermi/GBM | G
HEB191113578 | GRB 191113A | 2019-11-13T13:52:44.52 | BLIND | NG | 298.1 | 20.9 | 5.8 | Fermi/GBM | G
HEB191118925 | GRB 191118A | 2019-11-18T22:12:01.82 | BLIND | NG | 219.8 | -58.7 | 26.8 | Fermi/GBM | G
HEB191119445 | - | 2019-11-19T10:41:07.00 | BLIND | NG | - | - | - | - | B
HEB191130506 | - | 2019-11-30T12:09:34.90 | BLIND | NG | 345.5 | -4.4 | 14.2 | Fermi/GBM | G
HEB191202378 | - | 2019-12-02T09:05:40.50 | BLIND | NG | - | - | - | - | B
HEB191202867 | GRB 191202A | 2019-12-02T20:48:59.55 | BLIND | NG | 246.4 | 17.1 | 1.8 | Fermi/GBM | G
HEB191203289 | GRB 191203A | 2019-12-03T06:57:19.08 | BLIND | NG | 332.4 | 51.8 | 34.3 | Fermi/GBM | G
HEB191205740 | GRB 191205A | 2019-12-05T17:46:20.44 | BLIND | NG | 14.0 | -34.1 | 21.4 | Fermi/GBM | G
HEB191218112 | GRB 191218A | 2019-12-18T02:42:43.20 | BLIND | NG | 301.1 | -40.3 | 0.1 | Swift | G
HEB191221860 | GRB 191221B | 2019-12-21T20:39:10.70 | BLIND | NG | 154.8 | -38.1 | 0.1 | Swift | G
HEB191224829 | - | 2019-12-24T19:55:07.00 | BLIND | NG | - | - | - | - | B
HEB191227069 | GRB 191227A | 2019-12-27T01:39:34.40 | BLIND | NG | 319.2 | -16.7 | 0.1 | Swift | G
HEB191227723 | GRB 191227B | 2019-12-27T17:21:44.10 | BLIND | NG | 258.2 | -26.0 | 2.4 | Fermi/GBM | I
HEB200109073 | GRB 200109A | 2020-01-09T01:45:51.89 | BLIND | NG | 307.1 | 53.0 | 0.1 | Swift | G
HEB200111632 | GRB 200111A | 2020-01-11T15:11:07.61 | BLIND | NG | 104.5 | 31.7 | 3.5 | Fermi/GBM | G
HEB200114153 | GRB 200114A | 2020-01-14T03:40:45.50 | BLIND | NG | 199.4 | -0.3 | 2.6 | Fermi/GBM | G
HEB200120961 | GRB 200120A | 2020-01-20T23:04:58.60 | BLIND | NG | 139.4 | -70.7 | 1.0 | Fermi/GBM | G
HEB200125863 | GRB 200125B | 2020-01-25T20:43:31.90 | BLIND | NG | 7.5 | 64.7 | 1.0 | Fermi/GBM | G
HEB200211193 | - | 2020-02-11T04:38:56.10 | BLIND | NG | - | - | - | - | B
HEB200219998 | GRB 200219C | 2020-02-19T23:57:12.05 | BLIND | NG | 264.5 | 8.4 | 1.0 | Fermi/GBM | G
HEB200221161 | GRB 200221A | 2020-02-21T03:52:58.71 | BLIND | NG | 157.1 | 33.1 | 5.0 | Fermi/GBM | G
HEB200227305 | GRB 200227A | 2020-02-27T07:20:16.15 | BLIND | NG | 56.4 | 9.5 | 0.1 | Swift | G
HEB200313878 | - | 2020-03-13T21:04:58.00 | BLIND | NG | - | - | - | - | B
HEB200323782 | GRB 200323A | 2020-03-23T18:46:32.80 | BLIND | NG | 156.5 | -55.5 | 1.5 | Fermi/GBM | G
HEB200325137 | GRB 200325A | 2020-03-25T03:18:31.70 | BLIND | NG | 22.1 | -29.1 | 4.2 | Fermi/GBM | G
HEB200326421 | - | 2020-03-26T10:07:36.86 | BLIND | NG | - | - | - | - | S
HEB200326517 | GRB 200326A | 2020-03-26T12:24:47.90 | BLIND | NG | 245.3 | -21.1 | 6.9 | Fermi/GBM | G
HEB200412381 | GRB 200412B | 2020-04-12T09:08:45.80 | BLIND | NG | 279.8 | 64.1 | 1.0 | Fermi/GBM | G
HEB200413712 | - | 2020-04-13T17:06:38.00 | BLIND | NG | - | - | - | - | S
HEB200413743 | - | 2020-04-13T17:50:06.00 | BLIND | LG | - | - | - | - | B
HEB200415366 | GRB 200415A | 2020-04-15T08:48:05.55 | BLIND | NG | 6.1 | -32.0 | 2.0 | Fermi/GBM | I
HEB200416295 | GRB 200416A | 2020-04-16T07:05:17.17 | BLIND | NG | 335.7 | -7.5 | 0.1 | Swift | G
HEB200418864 | - | 2020-04-18T20:45:00.28 | BLIND | NG | 72.6 | -1.0 | - | Fermi/GBM | G
HEB200519472 | GRB 200519A | 2020-05-19T11:20:23.73 | BLIND | NG | 255.3 | -30.4 | 0.1 | Swift | G
HEB200521511 | GRB 200521A | 2020-05-21T12:16:41.26 | BLIND | NG | 169.5 | 7.2 | 4.3 | IPN | S
HEB200526628 | - | 2020-05-26T15:04:48.31 | BLIND | NG | - | - | - | - | B
HEB200601097 | GRB 200601A | 2020-06-01T02:19:56.50 | BLIND | NG | 36.7 | 33.5 | 1.7 | Fermi/GBM | G
HEB200609379 | GRB 200609A | 2020-06-09T09:06:48.05 | BLIND | LG | 16.3 | 67.4 | 1.5 | Fermi/GBM | G
HEB200617679 | GRB 200617A | 2020-06-17T16:18:05.80 | BLIND | NG | 359.1 | -59.8 | - | Fermi/GBM | G
HEB200619108 | GRB 200619A | 2020-06-19T02:36:11.60 | BLIND | NG | 101.3 | 56.7 | 4.0 | Fermi/GBM | G
HEB200707072 | GRB 200707A | 2020-07-07T01:44:02.54 | BLIND | NG | 80.8 | -14.9 | 3.1 | Fermi/GBM | G
HEB200711461 | GRB 200711A | 2020-07-11T11:04:32.93 | BLIND | NG | 292.1 | 1.2 | 5.6 | Fermi/GBM | G
HEB200716315 | GRB 200716B | 2020-07-16T07:34:29.50 | BLIND | LG | 350.7 | -21.8 | 13.8 | Fermi/GBM | G
HEB200716956 | GRB 200716C | 2020-07-16T22:57:41.18 | BLIND | NG | 195.6 | 25.1 | 3.5 | Fermi/GBM | G
HEB200801352 | GRB 200801A | 2020-08-01T08:27:14.08 | BLIND | NG | 321.1 | 85.3 | 11.3 | Fermi/GBM | G
HEB200806645 | GRB 200806A | 2020-08-06T15:28:49.91 | BLIND | LG | 52.9 | 37.1 | 0.1 | Swift | G
HEB200809653 | GRB 200809B | 2020-08-09T15:41:27.00 | BLIND | LG | 359.8 | -76.9 | 3.4 | Fermi/GBM | G
HEB200824594 | GRB 200824A | 2020-08-24T14:15:38.82 | BLIND | NG | 117.7 | 10.5 | 15.4 | Fermi/GBM | G
HEB200903112 | GRB 200903B | 2020-09-03T02:42:40.87 | BLIND | NG | 60.1 | -13.8 | 14.6 | Fermi/GBM | G
HEB200919964 | GRB 200919C | 2020-09-19T23:08:22.64 | BLIND | LG | 280.1 | -23.7 | 16.8 | Fermi/GBM | G
HEB200922504 | GRB 200922A | 2020-09-22T12:06:46.00 | BLIND | NG | 296.9 | -55.2 | 0.1 | Swift | G
HEB200928551 | GRB 200928B | 2020-09-28T13:14:44.75 | BLIND | NG | 85.7 | 2.3 | 17.8 | Fermi/GBM | G
HEB201013157 | GRB 201013A | 2020-10-13T03:46:30.20 | BLIND | NG | 107.4 | 57.0 | 0.1 | Swift | G
HEB201016019 | GRB 201016A | 2020-10-16T00:27:49.50 | BLIND | NG | 167.4 | 4.5 | 5.0 | Fermi/GBM | I
HEB201105229 | GRB 201105A | 2020-11-05T05:31:07.76 | BLIND | LG | 244.5 | 16.0 | 1.0 | Fermi/GBM | G
HEB201122355 | GRB 201122A | 2020-11-22T08:32:01.00 | BLIND | NG | - | - | - | - | S
HEB201209239 | GRB 201209A | 2020-12-09T05:44:52.53 | BLIND | NG | 23.1 | -1.7 | 0.1 | Swift | G
HEB201221591 | GRB 201221B | 2020-12-21T14:11:43.00 | BLIND | NG | 110.6 | 32.0 | 4.1 | Fermi/GBM | G
HEB201226553 | GRB 201226A | 2020-12-26T13:16:26.60 | BLIND | NG | 173.1 | -6.0 | - | Fermi/GBM | G
HEB201227634 | GRB 201227A | 2020-12-27T15:14:07.40 | BLIND | NG | 170.1 | -73.6 | 1.5 | IPN | I
HEB210112068 | GRB 210112A | 2021-01-12T01:38:06.55 | BLIND | NG | 219.0 | 33.1 | 0.1 | Swift | G
HEB210119120 | GRB 210119A | 2021-01-19T02:54:09.82 | BLIND | NG | 285.8 | -63.1 | 7.8 | Fermi/GBM | G
HEB210121779 | GRB 210121A | 2021-01-21T18:41:48.75 | BLIND | LG | 17.0 | -46.4 | 0.6 | IPN | G
HEB210123304 | GRB 210123A | 2021-01-23T07:19:10.35 | BLIND | LG | 345.1 | -56.9 | 1.1 | Fermi/GBM | G
HEB210124558 | GRB 210124B | 2021-01-24T13:23:48.40 | BLIND | LG | 274.3 | -0.4 | 0.4 | IPN | S
HEB210129908 | - | 2021-01-29T21:48:56.90 | BLIND | NG | - | - | - | - | B
HEB210207911 | GRB 210207B | 2021-02-07T21:52:49.60 | BLIND | LG | 270.6 | 53.7 | 0.1 | Swift | G
HEB210208564 | GRB 210208A | 2021-02-08T13:32:25.63 | BLIND | NG | 260.2 | -12.7 | 0.1 | IBIS | S
HEB210213286 | GRB 210213B | 2021-02-13T06:52:27.18 | BLIND | NG | - | - | - | - | S
HEB210225217 | GRB 210225A | 2021-02-25T05:13:36.00 | BLIND | NG | 333.4 | 28.4 | 3.4 | Fermi/GBM | G
HEB210227114 | - | 2021-02-27T02:45:09.42 | BLIND | NG | 115.8 | 61.1 | - | Fermi/GBM | G
HEB210228057 | GRB 210228B | 2021-02-28T01:22:53.90 | BLIND | NG | 283.5 | -43.1 | - | Fermi/GBM | G
HEB210306320 | - | 2021-03-06T07:41:07.50 | BLIND | NG | - | - | - | - | B
HEB210306879 | - | 2021-03-06T21:07:09.56 | BLIND | NG | - | - | - | - | B
HEB210307247 | GRB 210307B | 2021-03-07T05:56:37.94 | BLIND | LG | 125.6 | 17.5 | 7.3 | GECAM | G
HEB210323918 | GRB 210323A | 2021-03-23T22:02:18.40 | BLIND | NG | 317.9 | 25.4 | 0.1 | Swift | G
HEB210324468 | - | 2021-03-24T11:14:28.21 | BLIND | NG | 148.5 | 37.2 | - | Fermi/GBM | G
HEB210326057 | GRB 210326A | 2021-03-26T01:22:24.93 | BLIND | NG | 58.0 | 15.1 | 39.2 | Fermi/GBM | G
HEB210326890 | - | 2021-03-26T21:22:24.93 | BLIND | NG | - | - | - | - | B
HEB210328396 | - | 2021-03-28T09:30:52.77 | BLIND | NG | - | - | - | - | B
HEB210405507 | - | 2021-04-05T12:11:26.68 | BLIND | NG | - | - | - | - | B
HEB210406716 | GRB 210406A | 2021-04-06T17:11:28.92 | BLIND | NG | 132.5 | 76.5 | 0.1 | IBIS | S
HEB210409894 | GRB 210409A | 2021-04-09T21:28:26.86 | BLIND | NG | 70.9 | -58.3 | 2.9 | GECAM | G
HEB210411147 | GRB 210411A | 2021-04-11T03:31:41.10 | BLIND | NG | 259.4 | -27.4 | 3.0 | Fermi/GBM | G
HEB210421454 | GRB 210421B | 2021-04-21T10:54:44.81 | BLIND | NG | 272.1 | 57.2 | 2.1 | Fermi/GBM | G
HEB210422572 | GRB 210422B | 2021-04-22T13:44:37.13 | BLIND | NG | 116.6 | 24.7 | 2.1 | Fermi/GBM | G
HEB210427206 | GRB 210427A | 2021-04-27T04:57:12.99 | BLIND | NG | 177.3 | -53.4 | 1.1 | Fermi/GBM | G
HEB210429071 | - | 2021-04-29T01:43:11.33 | BLIND | NG | - | - | - | - | B
HEB210502295 | - | 2021-05-02T07:05:16.38 | BLIND | NG | - | - | - | - | B
HEB210504958 | - | 2021-05-04T23:00:47.17 | BLIND | NG | - | - | - | - | B
HEB210506027 | GRB 210506A | 2021-05-06T00:39:48.54 | BLIND | LG | 224.2 | -32.7 | 43.0 | IPN | B
HEB210511476 | GRB 210511B | 2021-05-11T11:26:39.26 | BLIND | NG | 316.2 | 61.7 | 1.0 | Fermi/GBM | G
HEB210511647 | - | 2021-05-11T15:32:56.10 | BLIND | NG | - | - | - | - | B
HEB210515546 | GRB 210515A | 2021-05-15T13:06:45.70 | BLIND | NG | 117.1 | 77.3 | 14.6 | Fermi/GBM | G
HEB210516982 | GRB 210516A | 2021-05-16T23:34:45.86 | BLIND | NG | 22.1 | 74.9 | 9.5 | Fermi/GBM | G
HEB210518544 | GRB 210518A | 2021-05-18T13:04:09.64 | BLIND | NG | 270.0 | 49.6 | 1.8 | Fermi/GBM | G
HEB210520796 | GRB 210520A | 2021-05-20T19:07:02.00 | BLIND | NG | 147.9 | -67.0 | 3.7 | Fermi/GBM | G
HEB210602502 | GRB 210602A | 2021-06-02T12:04:01.32 | BLIND | LG | 44.6 | -2.7 | 0.2 | MAXI/GSC | S
HEB210605214 | GRB 210605A | 2021-06-05T05:08:58.39 | BLIND | NG | 21.7 | -41.5 | 2.0 | Fermi/GBM | G
HEB210606120 | - | 2021-06-06T02:53:02.89 | BLIND | NG | - | - | - | - | B
HEB210606945 | GRB 210606B | 2021-06-06T22:41:05.24 | BLIND | NG | 87.5 | -18.4 | 1.2 | Fermi/GBM | G
HEB210607775 | GRB 210607B | 2021-06-07T18:37:17.80 | BLIND | NG | - | - | - | - | B
HEB210607902 | GRB 210607C | 2021-06-07T21:39:20.72 | BLIND | NG | - | - | - | - | B
HEB210610827 | GRB 210610B | 2021-06-10T19:51:05.05 | BLIND | NG | 243.9 | 14.4 | 0.1 | Swift | G
HEB210615891 | - | 2021-06-15T21:23:51.50 | BLIND | NG | - | - | - | - | B
HEB210615981 | GRB 210615A | 2021-06-15T23:33:53.60 | BLIND | NG | 342.9 | 62.2 | 7.5 | Fermi/GBM | G
HEB210622064 | GRB 210622A | 2021-06-22T01:32:35.94 | BLIND | NG | 242.1 | -14.1 | 6.1 | Fermi/GBM | G
HEB210622339 | - | 2021-06-22T08:09:30.61 | BLIND | NG | - | - | - | - | B
HEB210627311 | GRB 210627A | 2021-06-27T07:29:15.68 | BLIND | NG | 148.3 | 44.5 | 10.7 | Fermi/GBM | G
HEB210627813 | - | 2021-06-27T19:31:37.68 | BLIND | NG | - | - | - | - | B
Table 4: Durations (10-2000 keV) from joint analyses with ‘GOLDEN’ GRB samples. Trigger | Detectors | $T_{\rm 50}$ |  $T_{\rm 50}$ start | $T_{\rm 90}$ |  $T_{\rm 90}$ start |  $T_{\rm 90}$ only with HXMT/CsI counts
---|---|---|---|---|---|---
ID | Used | (s) | (s) | (s) | (s) | (s)
HEB170626400 | HXMT/CsI, Fermi-GBM (n0, n1, n2, b0) | 7.040$\pm$0.264 | 1.248 | 12.416$\pm$0.202 | 0.224 | 12.690$\pm$0.081
HEB170705115 | HXMT/CsI, Fermi-GBM (n8, nb, b1) | 33.792$\pm$3.714 | 0.496 | 68.672$\pm$1.601 | -6.416 | 18.460$\pm$6.340
HEB170714049 | HXMT/CsI, Fermi-GBM (n3, n7, b0, b1) | 0.128$\pm$0.064 | -0.156 | 0.448$\pm$0.143 | -0.412 | 0.835$\pm$0.220
HEB170718152 | HXMT/CsI, Fermi-GBM (n3, n4, b0) | 10.624$\pm$1.943 | -7.144 | 24.768$\pm$3.562 | -13.352 | 24.160$\pm$3.322
HEB170726248 | HXMT/CsI, Fermi-GBM (n9, n7) | 1.344$\pm$0.143 | -0.232 | 5.824$\pm$1.537 | -1.704 | 2.580$\pm$0.061
HEB170726793 | HXMT/CsI, Fermi-GBM (n8, n7, b1) | 10.432$\pm$0.272 | 1.364 | 26.240$\pm$2.689 | -5.612 | 22.871$\pm$0.901
HEB170728960 | HXMT/CsI, Fermi-GBM (n6, n9, b1) | 12.864$\pm$0.202 | 0.684 | 19.840$\pm$0.962 | 0.364 | 16.860$\pm$2.371
HEB170731751 | HXMT/CsI, Fermi-GBM (n0, n3, b0) | 41.664$\pm$1.604 | 4.336 | 59.584$\pm$3.623 | -2.768 | 28.141$\pm$6.360
HEB170802637 | HXMT/CsI, Fermi-GBM (n6, n8, b1) | 0.192$\pm$0.091 | 0.696 | 2.176$\pm$1.793 | -1.288 | 0.820$\pm$0.014
HEB170817908 | HXMT/CsI, Fermi-GBM (n0, n1, n2, n5, b0) | 1.472$\pm$0.143 | 0.544 | 2.688$\pm$0.202 | 0.288 | 2.620$\pm$0.081
HEB170825306 | HXMT/CsI, Fermi-GBM (n3, n7, b0, b1) | 3.328$\pm$0.181 | -0.713 | 11.712$\pm$2.244 | -2.441 | 7.340$\pm$1.872
HEB170826818 | HXMT/CsI, Fermi-GBM (na, nb, b1) | 5.952$\pm$0.091 | 1.424 | 11.392$\pm$0.264 | -0.432 | 9.537$\pm$0.161
HEB170903534 | HXMT/CsI, Fermi-GBM (n4, n8, b0, b1) | 11.328$\pm$1.414 | -2.502 | 26.048$\pm$1.414 | -6.022 | 19.050$\pm$3.960
HEB170906029 | HXMT/CsI, Fermi-GBM (n4, n3, b0) | 38.912$\pm$0.466 | 31.724 | 93.120$\pm$1.294 | 8.556 | 63.610$\pm$2.140
HEB170912984 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 1.728$\pm$1.154 | -1.680 | 2.880$\pm$0.834 | -2.256 | 4.005$\pm$0.708
HEB170923188 | HXMT/CsI, Fermi-GBM (n4, n7, b0) | 12.672$\pm$2.636 | 9.533 | 32.960$\pm$2.561 | -0.451 | 25.660$\pm$1.310
HEB171008079 | HXMT/CsI, Fermi-GBM (n4, n8, b0, b1) | 5.248$\pm$0.326 | 0.352 | 12.672$\pm$3.721 | -2.976 | 1.169$\pm$1.819
HEB171013350 | HXMT/CsI, Fermi-GBM (n2, n3, b0) | 13.312$\pm$0.345 | 6.296 | 32.000$\pm$0.771 | -2.920 | 22.710$\pm$5.620
HEB171020963 | HXMT/CsI, Swift/BAT | 6.400$\pm$1.231 | -2.416 | 10.176$\pm$0.091 | -5.040 | 9.620$\pm$2.070
HEB171030728 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 0.320$\pm$0.453 | 0.052 | 1.344$\pm$0.643 | -0.716 | 0.475$\pm$1.481
HEB171103965 | HXMT/CsI, Swift/BAT | 0.064$\pm$0.091 | 2.032 | 0.192$\pm$0.091 | 1.968 | 0.197$\pm$0.022
HEB171120555 | HXMT/CsI, Fermi-GBM (n0, n3, b0) | 39.488$\pm$0.143 | 1.312 | 52.160$\pm$1.601 | 0.480 | 43.461$\pm$9.610
HEB171124234 | HXMT/CsI, Fermi-GBM (n0, n3, b0) | 5.312$\pm$0.362 | -3.608 | 18.112$\pm$0.653 | -6.424 | 6.197$\pm$0.490
HEB171207054 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 0.192$\pm$0.091 | -0.104 | 4.864$\pm$2.625 | -1.320 | 3.010$\pm$0.358
HEB171209615 | HXMT/CsI, Swift/BAT | 61.376$\pm$1.358 | 11.792 | 93.696$\pm$2.567 | -0.944 | 84.781$\pm$10.092
HEB171210492 | HXMT/CsI, Fermi-GBM (n9, n1, b0, b1) | 48.128$\pm$1.414 | 7.544 | 108.224$\pm$3.137 | 1.592 | 15.950$\pm$1.773
HEB171215705 | HXMT/CsI, Fermi-GBM (n8, nb, b1) | 13.696$\pm$1.096 | 0.672 | 34.496$\pm$8.192 | -4.576 | 32.016$\pm$8.414
HEB171223818 | HXMT/CsI, Fermi-GBM (n7, n6, b1) | 1.088$\pm$0.219 | 0.632 | 1.216$\pm$0.219 | 0.632 | 0.160$\pm$0.014
HEB171230955 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 24.768$\pm$1.105 | 6.056 | 77.440$\pm$4.636 | -1.368 | 20.050$\pm$2.241
HEB180110608 | HXMT/CsI, Fermi-GBM (n7, n9, b1) | 7.488$\pm$3.393 | -0.712 | 13.952$\pm$0.580 | -4.424 | 14.290$\pm$2.930
HEB180111695 | HXMT/CsI, Swift/BAT | 9.920$\pm$0.091 | 2.604 | 27.008$\pm$3.073 | 0.108 | 21.040$\pm$6.820
HEB180119836 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 2.112$\pm$0.202 | 2.800 | 6.144$\pm$1.802 | 0.176 | 9.380$\pm$3.110
HEB180127049 | HXMT/CsI, Fermi-GBM (n3, n7, b0, b1) | 7.744$\pm$0.345 | 2.400 | 21.312$\pm$1.541 | -2.400 | 22.669$\pm$1.377
HEB180130744 | HXMT/CsI, Fermi-GBM (n6, n8, b1) | 0.064$\pm$0.264 | -0.148 | 1.280$\pm$1.154 | -0.148 | 1.997$\pm$0.516
HEB180208764 | HXMT/CsI, Fermi-GBM (na, nb, b1) | 4.544$\pm$0.547 | -1.896 | 27.328$\pm$1.856 | -15.976 | 5.603$\pm$0.283
HEB180210517 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 16.704$\pm$0.181 | 6.104 | 40.448$\pm$0.707 | -1.384 | 17.028$\pm$1.415
HEB180305393 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 4.096$\pm$0.091 | 3.768 | 10.944$\pm$0.453 | 1.464 | 4.002$\pm$0.283
HEB180306972 | HXMT/CsI, Fermi-GBM (n3, n5, b0) | 9.984$\pm$1.431 | 0.928 | 33.856$\pm$9.605 | -3.232 | 26.303$\pm$12.649
HEB180309321 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 16.832$\pm$1.694 | 5.344 | 44.608$\pm$2.248 | -1.504 | 50.456$\pm$5.352
HEB180313977 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 0.064$\pm$0.389 | -0.008 | 0.832$\pm$0.453 | -0.008 | 1.201$\pm$0.283
HEB180330891 | HXMT/CsI, Fermi-GBM (n1, n3, b0) | 4.800$\pm$0.580 | 1.168 | 15.168$\pm$1.282 | 0.144 | 5.860$\pm$1.180
HEB180331177 | HXMT/CsI, Swift/BAT | 16.320$\pm$1.350 | 1.232 | 29.568$\pm$2.499 | -4.272 | 35.780$\pm$9.670
HEB180401279 | HXMT/CsI, Fermi-GBM (n2, na, b0, b1) | 6.208$\pm$0.231 | 2.112 | 13.952$\pm$0.462 | -1.600 | 6.003$\pm$0.283
HEB180402406 | HXMT/CsI, Fermi-GBM (n6, n8, b1) | 0.128$\pm$0.091 | -0.048 | 0.384$\pm$0.326 | -0.304 | 0.411$\pm$0.007
HEB180404091 | HXMT/CsI, Fermi-GBM (n3, n4, b0) | 17.088$\pm$1.421 | 7.119 | 59.904$\pm$3.267 | 0.783 | 53.141$\pm$8.120
HEB180409346 | HXMT/CsI, Fermi-GBM (n9, b1) | 6.912$\pm$0.091 | 4.616 | 12.864$\pm$0.264 | 1.288 | 11.510$\pm$0.530
HEB180413117 | HXMT/CsI, Fermi-GBM (n6, n7, b1) | 21.760$\pm$1.002 | 0.304 | 84.352$\pm$7.059 | -25.296 | 21.010$\pm$5.206
HEB180416923 | HXMT/CsI, Fermi-GBM (n4, n7, b0, b1) | 28.352$\pm$1.860 | 3.896 | 74.816$\pm$1.473 | 0.376 | 27.250$\pm$2.330
HEB180427442 | HXMT/CsI, Fermi-GBM (n6, n4, b0, b1) | 9.280$\pm$0.202 | 3.952 | 29.824$\pm$1.218 | 0.816 | 7.240$\pm$0.311
HEB180505539 | HXMT/CsI, Fermi-GBM (n8, n4, b0, b1) | 4.224$\pm$0.091 | -3.032 | 28.096$\pm$1.159 | -20.376 | 27.751$\pm$9.580
HEB180506902 | HXMT/CsI, Fermi-GBM (n2, n5, b0, b1) | 13.888$\pm$0.528 | 1.504 | 21.760$\pm$0.905 | -2.720 | 17.409$\pm$6.280
HEB180510808 | HXMT/CsI, Swift/BAT | 2.752$\pm$0.091 | 0.688 | 39.744$\pm$4.224 | -9.296 | 20.526$\pm$8.569
HEB180523782 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 1.728$\pm$0.547 | -0.968 | 7.936$\pm$1.118 | -3.720 | 6.702$\pm$4.189
HEB180525151 | HXMT/CsI, Fermi-GBM (n4, n5, b0, b1) | 0.064$\pm$0.091 | 0.012 | 0.320$\pm$0.264 | -0.052 | 0.361$\pm$0.076
HEB180605457 | HXMT/CsI, Fermi-GBM (n0, n2, b0) | 9.408$\pm$0.202 | 4.256 | 22.784$\pm$1.601 | 0.736 | 17.670$\pm$0.670
HEB180618030 | HXMT/CsI, Fermi-GBM (n4, n5, b0, b1) | 0.576$\pm$0.143 | -0.288 | 5.056$\pm$0.716 | -3.488 | 3.501$\pm$0.855
HEB180623696 | HXMT/CsI, Swift/BAT | 18.624$\pm$2.057 | -6.976 | 64.768$\pm$0.453 | -24.960 | 64.811$\pm$3.820
HEB180625940 | HXMT/CsI, Fermi-GBM (n4, n8, b0) | 0.256$\pm$0.091 | 0.120 | 2.048$\pm$0.962 | -0.776 | 0.310$\pm$0.071
HEB180626391 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 0.320$\pm$0.091 | -0.340 | 0.768$\pm$0.453 | -0.340 | 0.770$\pm$0.070
HEB180704233 | HXMT/CsI, Swift/BAT | 18.368$\pm$0.320 | -18.880 | 32.384$\pm$1.833 | -28.992 | 20.030$\pm$1.414
HEB180715754 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 0.448$\pm$0.091 | -0.004 | 1.280$\pm$0.870 | -0.580 | 0.640$\pm$0.175
HEB180718762 | HXMT/CsI, Fermi-GBM (n0, n2, b0) | 23.232$\pm$1.231 | 6.312 | 59.776$\pm$3.142 | 1.512 | 21.550$\pm$0.500
HEB180722992 | HXMT/CsI, Fermi-GBM (n2, n1, b0) | 41.920$\pm$0.975 | 13.312 | 116.800$\pm$4.740 | 1.024 | 90.122$\pm$0.689
HEB180724807 | HXMT/CsI, Fermi-GBM (na, nb, b1) | 17.792$\pm$0.590 | 6.584 | 52.224$\pm$1.921 | 1.400 | 53.066$\pm$14.026
HEB180730017 | HXMT/CsI, Fermi-GBM (n4, n5, b0) | 0.000$\pm$0.962 | 0.312 | 1.664$\pm$1.601 | 0.248 | 0.100$\pm$1.561
HEB180801275 | HXMT/CsI, Fermi-GBM (n6, n7, b1) | 0.192$\pm$0.091 | -0.008 | 0.704$\pm$0.264 | -0.456 | 0.550$\pm$0.114
HEB180803590 | HXMT/CsI, Fermi-GBM (n3, n4, b0) | 0.128$\pm$0.091 | -0.240 | 0.256$\pm$0.516 | -0.304 | 0.350$\pm$0.071
HEB180804930 | HXMT/CsI, Fermi-GBM (n8, nb, b1) | 5.824$\pm$0.771 | 0.496 | 23.040$\pm$1.802 | -3.472 | 4.620$\pm$0.240
HEB180816088 | HXMT/CsI, Fermi-GBM (n2, n1, b0) | 15.040$\pm$0.320 | 9.015 | 39.168$\pm$2.180 | -0.137 | 59.074$\pm$5.031
HEB180822561 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 2.816$\pm$0.286 | -0.344 | 13.568$\pm$2.463 | -3.480 | 4.506$\pm$1.119
HEB180828789 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 4.032$\pm$0.091 | 4.512 | 8.448$\pm$0.143 | 1.440 | 7.750$\pm$0.122
HEB180925407 | HXMT/CsI, Fermi-GBM (n4, n5, b0) | 2.496$\pm$0.405 | -2.952 | 5.440$\pm$2.308 | -4.808 | 5.601$\pm$1.360
HEB180925609 | HXMT/CsI, Swift/BAT | 13.312$\pm$0.286 | 3.304 | 33.664$\pm$1.484 | -5.080 | 10.640$\pm$0.940
HEB180927992 | HXMT/CsI, Fermi-GBM (n1, n5, b0) | 3.392$\pm$0.590 | -0.264 | 11.584$\pm$2.753 | -2.568 | 3.380$\pm$0.256
HEB180929453 | HXMT/CsI, Fermi-GBM (n1, n2, b0) | 2.368$\pm$0.091 | -0.008 | 3.008$\pm$0.143 | -0.264 | 2.850$\pm$0.190
HEB181008269 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 11.264$\pm$0.362 | -3.384 | 49.920$\pm$3.014 | -24.312 | 31.039$\pm$1.583
HEB181014479 | HXMT/CsI, Fermi-GBM (n1, n4, b0) | 8.128$\pm$0.405 | -4.248 | 25.728$\pm$2.755 | -9.432 | 23.507$\pm$3.042
HEB181028590 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 14.784$\pm$0.429 | 9.360 | 33.088$\pm$1.358 | 1.040 | 29.061$\pm$3.021
HEB181119605 | HXMT/CsI, Fermi-GBM (n7, n9, b1) | 8.960$\pm$0.181 | 5.714 | 18.432$\pm$0.389 | 0.146 | 15.090$\pm$0.871
HEB181121306 | HXMT/CsI, Fermi-GBM (n8, b1) | 0.384$\pm$0.326 | -0.240 | 0.576$\pm$0.143 | -0.304 | 0.621$\pm$0.822
HEB181122381 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 15.232$\pm$1.645 | 4.872 | 40.768$\pm$7.040 | 0.136 | 21.491$\pm$5.498
HEB181123231 | HXMT/CsI, Swift/BAT | 0.128$\pm$0.090 | 0.090 | 0.256$\pm$0.090 | 0.024 | 0.370$\pm$0.330
HEB181212692 | HXMT/CsI, Fermi-GBM (n2, n5, b0) | 8.768$\pm$1.218 | 2.512 | 58.752$\pm$3.585 | 0.848 | 47.059$\pm$7.509
HEB181213540 | HXMT/CsI, Swift/BAT | 11.392$\pm$0.905 | 2.592 | 22.720$\pm$2.177 | 0.480 | 21.527$\pm$3.540
HEB181217664 | HXMT/CsI, Fermi-GBM (n2, na, b0) | 8.256$\pm$0.389 | 11.440 | 33.088$\pm$4.100 | 2.736 | 25.630$\pm$2.580
HEB181225489 | HXMT/CsI, Fermi-GBM (n3, n7, b0) | 9.344$\pm$0.264 | 1.312 | 35.776$\pm$2.817 | 0.672 | 10.110$\pm$0.440
HEB190103877 | HXMT/CsI, Swift/BAT | 9.856$\pm$0.345 | 1.440 | 24.448$\pm$3.216 | -7.776 | 10.202$\pm$0.224
HEB190110725 | HXMT/CsI, Fermi-GBM (n3, n5, b0, b1) | 3.456$\pm$0.181 | -2.536 | 11.904$\pm$2.244 | -5.096 | 6.838$\pm$1.085
HEB190131964 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 12.800$\pm$0.859 | 4.136 | 36.544$\pm$5.824 | 0.744 | 23.620$\pm$1.290
HEB190215771 | HXMT/CsI, Fermi-GBM (n1, n3, b0) | 8.064$\pm$0.326 | 3.896 | 25.216$\pm$2.369 | 0.760 | 15.010$\pm$2.470
HEB190222537 | HXMT/CsI, Fermi-GBM (n9, nb, b1) | 6.208$\pm$0.516 | 1.448 | 28.992$\pm$3.009 | -0.088 | 4.802$\pm$0.633
HEB190226515 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 0.064$\pm$0.091 | 0.160 | 0.192$\pm$0.389 | 0.096 | 0.470$\pm$0.125
HEB190310398 | HXMT/CsI, Fermi-GBM (n3, n5, b0, b1) | 6.720$\pm$0.143 | -1.696 | 75.072$\pm$1.537 | -51.680 | 64.080$\pm$27.038
HEB190324348 | HXMT/CsI, Fermi-GBM (n1, na, b0, b1) | 16.896$\pm$1.541 | 3.456 | 51.136$\pm$1.569 | -1.152 | 49.562$\pm$4.036
HEB190324947 | HXMT/CsI, Fermi-GBM (n6, n7, b1) | 5.056$\pm$0.202 | 1.664 | 12.736$\pm$0.580 | -0.256 | 6.700$\pm$0.501
HEB190326313 | HXMT/CsI, Fermi-GBM (n0, n3, b0) | 25.792$\pm$4.740 | 22.749 | 68.160$\pm$5.874 | -5.283 | 60.111$\pm$12.830
HEB190326316 | HXMT/CsI, Swift/BAT | 0.064$\pm$0.389 | -0.040 | 0.576$\pm$0.429 | -0.232 | 0.325$\pm$0.011
HEB190330694 | HXMT/CsI, Fermi-GBM (n1, n9, b0) | 23.808$\pm$1.409 | 1.648 | 45.760$\pm$2.113 | 0.432 | 8.080$\pm$0.860
HEB190331093 | HXMT/CsI, Fermi-GBM (n0, n3) | 18.176$\pm$2.147 | -15.728 | 35.008$\pm$2.947 | -24.496 | 18.022$\pm$1.805
HEB190401139 | HXMT/CsI, Fermi-GBM (n6, n7, b1) | 10.944$\pm$0.326 | 3.568 | 31.104$\pm$1.154 | 0.112 | 21.020$\pm$3.900
HEB190407671 | HXMT/CsI, Fermi-GBM (n8, n9, b1) | 6.848$\pm$0.264 | 1.136 | 14.400$\pm$0.643 | -1.808 | 4.506$\pm$0.707
HEB190422283 | HXMT/CsI, Fermi-GBM (n4, n8, b0) | 61.312$\pm$0.590 | 13.288 | 86.976$\pm$1.620 | -1.624 | 64.321$\pm$6.352
HEB190424417 | HXMT/CsI, Swift/BAT | 12.928$\pm$0.405 | 1.000 | 31.040$\pm$2.180 | -2.904 | 23.410$\pm$4.840
HEB190507269 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 7.488$\pm$0.716 | 0.761 | 18.560$\pm$1.282 | -1.159 | 12.180$\pm$3.861
HEB190515189 | HXMT/CsI, Fermi-GBM (n6, n9, b1) | 0.192$\pm$0.091 | 0.160 | 0.448$\pm$0.091 | 0.032 | 0.400$\pm$0.087
HEB190525031 | HXMT/CsI, Fermi-GBM (na, n9, b1) | 0.512$\pm$0.091 | 0.064 | 1.344$\pm$0.516 | -0.064 | 1.750$\pm$0.757
HEB190531840 | HXMT/CsI, Fermi-GBM (n0, n3, b0) | 13.632$\pm$0.091 | 18.360 | 37.248$\pm$4.224 | 7.544 | 29.390$\pm$1.400
HEB190604446 | HXMT/CsI, Fermi-GBM (n4, n3, b0) | 4.480$\pm$0.143 | 3.052 | 13.184$\pm$0.834 | 0.044 | 9.902$\pm$2.721
HEB190613449 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 1.408$\pm$0.143 | 0.880 | 2.816$\pm$0.264 | 0.112 | 2.340$\pm$0.022
HEB190615636 | HXMT/CsI, Fermi-GBM (nb, n8, b1) | 8.256$\pm$0.373 | 0.736 | 21.888$\pm$1.132 | -8.480 | 8.820$\pm$0.780
HEB190619594 | HXMT/CsI, Fermi-GBM (nb, n7, b1) | 70.080$\pm$1.874 | 4.768 | 136.128$\pm$5.089 | -8.736 | 131.664$\pm$22.033
HEB190620507 | HXMT/CsI, Fermi-GBM (n3, n4, b0) | 16.320$\pm$0.834 | 3.824 | 55.936$\pm$1.275 | -2.896 | 54.568$\pm$1.805
HEB190720964 | HXMT/CsI, Fermi-GBM (n3, n4, b0) | 3.264$\pm$0.326 | 0.173 | 11.520$\pm$2.305 | -1.171 | 7.509$\pm$1.583
HEB190723308 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 16.640$\pm$0.643 | 0.848 | 27.136$\pm$3.841 | -4.144 | 18.022$\pm$2.064
HEB190724030 | HXMT/CsI, Fermi-GBM (n0, n5, b1) | 0.064$\pm$0.091 | -0.004 | 0.192$\pm$0.143 | -0.132 | 0.430$\pm$0.032
HEB190726642 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 4.096$\pm$0.202 | -1.576 | 17.472$\pm$1.958 | -7.144 | 4.570$\pm$0.530
HEB190806675 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 8.960$\pm$0.429 | 2.241 | 24.384$\pm$3.585 | -0.063 | 16.020$\pm$0.708
HEB190813520 | HXMT/CsI, Fermi-GBM (n2, n9, b0) | 0.064$\pm$0.143 | -0.072 | 0.640$\pm$0.771 | -0.072 | 1.200$\pm$0.022
HEB190814837 | HXMT/CsI, Fermi-GBM (nb, n9, b1) | 4.928$\pm$0.653 | 0.485 | 13.184$\pm$3.009 | -3.035 | 5.910$\pm$0.430
HEB190901890 | HXMT/CsI, Fermi-GBM (n3, n4, b0) | 7.872$\pm$0.202 | 0.656 | 23.360$\pm$1.096 | -5.808 | 16.620$\pm$3.221
HEB190903721 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 0.192$\pm$0.091 | -0.212 | 0.320$\pm$0.389 | -0.276 | 0.450$\pm$0.461
HEB190906767 | HXMT/CsI, Fermi-GBM (n4, n8, b0) | 23.424$\pm$0.643 | 0.440 | 38.336$\pm$2.497 | -0.072 | 16.710$\pm$4.870
HEB190915239 | HXMT/CsI, Fermi-GBM (nb, n8, b1) | 6.656$\pm$0.590 | 1.064 | 15.488$\pm$0.854 | -1.432 | 7.230$\pm$0.830
HEB191009297 | HXMT/CsI, Fermi-GBM (n9, b1) | 48.192$\pm$6.977 | 7.400 | 88.128$\pm$3.992 | 0.424 | 53.566$\pm$18.050
HEB191019970 | HXMT/CsI, Fermi-GBM (n0, n5, b0, b1) | 104.256$\pm$0.692 | 22.991 | 142.976$\pm$2.636 | 7.311 | 136.833$\pm$16.050
HEB191031780 | HXMT/CsI, Fermi-GBM (n0, n6, b0, b1) | 21.952$\pm$0.516 | 26.159 | 75.264$\pm$6.849 | 0.623 | 49.951$\pm$4.510
HEB191105257 | HXMT/CsI, Fermi-GBM (n4, n8) | 0.064$\pm$0.091 | 0.024 | 0.192$\pm$0.091 | -0.040 | 0.145$\pm$0.007
HEB191108003 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 94.784$\pm$2.273 | 19.596 | 164.736$\pm$7.700 | -3.572 | 116.579$\pm$16.204
HEB191111364 | HXMT/CsI, Fermi-GBM (n4, b0) | 33.216$\pm$0.659 | 26.808 | 99.264$\pm$0.668 | -6.280 | 96.016$\pm$17.567
HEB191113578 | HXMT/CsI, Fermi-GBM (n4, n8, b0) | 10.432$\pm$3.521 | 0.672 | 19.008$\pm$0.834 | 0.160 | 24.530$\pm$4.615
HEB191118925 | HXMT/CsI, Fermi-GBM (n2, n5, b0) | 13.824$\pm$1.793 | 6.520 | 75.968$\pm$7.745 | 1.080 | 15.390$\pm$1.760
HEB191130506 | HXMT/CsI, Fermi-GBM (n0, n9, b0, b1) | 17.024$\pm$0.854 | 3.304 | 46.720$\pm$5.422 | -0.664 | 46.057$\pm$10.025
HEB191202867 | HXMT/CsI, Fermi-GBM (n0, n3, b0) | 6.656$\pm$0.462 | -2.008 | 33.408$\pm$2.499 | -7.768 | 4.180$\pm$1.145
HEB191203289 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 0.192$\pm$0.091 | -0.338 | 0.448$\pm$0.516 | -0.466 | 0.695$\pm$0.276
HEB191205740 | HXMT/CsI, Fermi-GBM (n3, n4, b0) | 2.496$\pm$0.466 | -3.892 | 3.840$\pm$0.962 | -4.084 | 3.920$\pm$0.581
HEB191218112 | HXMT/CsI, Swift/BAT | 41.664$\pm$0.345 | 3.112 | 53.824$\pm$2.689 | -0.216 | 49.811$\pm$1.240
HEB191221860 | HXMT/CsI, Swift/BAT | 4.096$\pm$0.091 | 1.944 | 13.632$\pm$0.962 | -1.960 | 13.016$\pm$1.119
HEB191227069 | HXMT/CsI, Fermi-GBM (n2, n1, b0) | 8.256$\pm$0.202 | 0.808 | 28.032$\pm$1.562 | -6.872 | 24.030$\pm$1.583
HEB200109073 | HXMT/CsI, Fermi-GBM (n5, n2, b0) | 24.704$\pm$1.489 | 2.720 | 40.256$\pm$1.869 | -4.512 | 25.540$\pm$5.260
HEB200111632 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 5.184$\pm$0.091 | 0.760 | 10.240$\pm$1.665 | -3.528 | 11.500$\pm$2.501
HEB200114153 | HXMT/CsI, Fermi-GBM (n2, na, b0, b1) | 26.048$\pm$0.590 | 0.304 | 42.496$\pm$6.529 | -2.512 | 28.035$\pm$5.105
HEB200120961 | HXMT/CsI, Fermi-GBM (n6, na, b1) | 4.160$\pm$0.231 | -2.700 | 14.400$\pm$2.369 | -6.732 | 14.660$\pm$1.354
HEB200125863 | HXMT/CsI, Fermi-GBM (n0, n1, b0, b1) | 2.624$\pm$0.091 | 0.888 | 6.400$\pm$0.202 | -0.072 | 4.240$\pm$0.330
HEB200219998 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 9.920$\pm$0.707 | 0.744 | 22.784$\pm$0.580 | -0.920 | 3.760$\pm$3.660
HEB200221161 | HXMT/CsI, Fermi-GBM (n8, nb, b1) | 0.512$\pm$0.143 | -0.264 | 8.128$\pm$0.771 | -4.616 | 1.460$\pm$0.121
HEB200227305 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 7.936$\pm$0.286 | -1.072 | 23.488$\pm$2.627 | -7.536 | 19.450$\pm$2.240
HEB200323782 | HXMT/CsI, Fermi-GBM (n7, n9, b1) | 0.768$\pm$0.091 | 0.440 | 1.664$\pm$0.264 | 0.056 | 1.601$\pm$0.141
HEB200325137 | HXMT/CsI, Fermi-GBM (n3, n5, b0) | 0.576$\pm$0.143 | 0.120 | 1.728$\pm$1.154 | -0.008 | 1.210$\pm$0.014
HEB200326517 | HXMT/CsI, Fermi-GBM (n9, nb, b1) | 1.728$\pm$0.405 | -0.636 | 2.816$\pm$1.032 | -1.020 | 2.410$\pm$1.131
HEB200412381 | HXMT/CsI, Fermi-GBM (n6, n8, b1) | 1.920$\pm$0.091 | 2.820 | 7.616$\pm$0.389 | -0.444 | 6.360$\pm$0.139
HEB200416295 | HXMT/CsI, Fermi-GBM (n2, n5) | 3.328$\pm$0.264 | 0.160 | 7.616$\pm$1.473 | -1.888 | 6.310$\pm$2.181
HEB200418864 | HXMT/CsI, Fermi-GBM (n3, n4, b0) | 15.360$\pm$4.420 | 5.736 | 38.080$\pm$3.905 | 0.680 | 12.900$\pm$8.113
HEB200519472 | HXMT/CsI, Swift/BAT | 5.760$\pm$0.604 | 21.168 | 32.832$\pm$2.052 | 8.560 | 30.890$\pm$2.520
HEB200601097 | HXMT/CsI, Fermi-GBM (n1, n5, b0) | 119.296$\pm$0.716 | 12.512 | 158.144$\pm$4.612 | -3.104 | 10.570$\pm$8.741
HEB200609379 | HXMT/CsI, Fermi-GBM (n0, n4, b0) | 27.584$\pm$1.319 | 2.576 | 93.248$\pm$3.912 | -44.400 | 88.071$\pm$8.960
HEB200617679 | HXMT/CsI, Fermi-GBM (n8, n4, b0) | 0.192$\pm$0.091 | -0.136 | 1.024$\pm$1.729 | -0.776 | 0.910$\pm$0.028
HEB200619108 | HXMT/CsI, Fermi-GBM (n5, n4, b0) | 8.640$\pm$0.607 | 1.532 | 28.672$\pm$6.528 | 0.188 | 27.534$\pm$7.027
HEB200707072 | HXMT/CsI, Fermi-GBM (n3, n1) | 7.360$\pm$1.368 | 3.128 | 20.224$\pm$2.191 | -0.776 | 16.521$\pm$6.028
HEB200711461 | HXMT/CsI, Fermi-GBM (n7, n9, b1) | 14.720$\pm$0.580 | 3.560 | 29.376$\pm$1.478 | 0.488 | 12.190$\pm$6.180
HEB200716315 | HXMT/CsI, Fermi-GBM (n6, n7, b1) | 22.528$\pm$0.968 | 2.000 | 43.968$\pm$2.241 | -0.624 | 42.053$\pm$13.026
HEB200716956 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 1.920$\pm$0.091 | 0.320 | 4.416$\pm$0.707 | 0.192 | 2.140$\pm$0.014
HEB200801352 | HXMT/CsI, Fermi-GBM (n6, n8) | 16.320$\pm$2.360 | -3.288 | 34.240$\pm$4.394 | -10.072 | 24.470$\pm$4.150
HEB200806645 | HXMT/CsI, Swift/BAT | 10.816$\pm$0.429 | 15.312 | 37.376$\pm$5.130 | 0.848 | 33.050$\pm$2.060
HEB200809653 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 5.120$\pm$0.707 | 0.280 | 14.656$\pm$3.334 | -1.000 | 17.522$\pm$2.553
HEB200824594 | HXMT/CsI, Fermi-GBM (n0, n3) | 0.320$\pm$0.834 | -0.456 | 1.664$\pm$0.707 | -0.840 | 0.850$\pm$0.112
HEB200903112 | HXMT/CsI, Fermi-GBM (n7, b1) | 38.528$\pm$2.589 | 4.056 | 89.152$\pm$3.917 | -16.424 | 40.026$\pm$2.809
HEB200919964 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 36.224$\pm$0.716 | 11.152 | 57.280$\pm$1.444 | 1.680 | 58.261$\pm$7.300
HEB200922504 | HXMT/CsI, Swift/BAT | 7.552$\pm$1.096 | 0.504 | 16.512$\pm$1.118 | -2.760 | 4.440$\pm$1.192
HEB200928551 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 7.872$\pm$0.231 | -2.720 | 19.584$\pm$2.627 | -6.112 | 15.160$\pm$1.990
HEB201013157 | HXMT/CsI, Swift/BAT | 1.856$\pm$0.326 | 0.560 | 6.912$\pm$0.202 | 0.048 | 2.010$\pm$0.022
HEB201105229 | HXMT/CsI, Fermi-GBM (n3, n5, b0) | 5.184$\pm$0.202 | 2.744 | 16.384$\pm$1.282 | 0.952 | 12.010$\pm$0.960
HEB201209239 | HXMT/CsI, Swift/BAT | 14.976$\pm$2.988 | -7.104 | 45.632$\pm$1.843 | -24.064 | 12.370$\pm$0.466
HEB201221591 | HXMT/CsI, Fermi-GBM (na, nb) | 0.010$\pm$0.014 | 0.048 | 0.050$\pm$0.045 | 0.038 | 0.035$\pm$0.007
HEB201226553 | HXMT/CsI, Fermi-GBM (n2, na) | 52.544$\pm$1.088 | 8.464 | 71.360$\pm$0.842 | -1.584 | 71.022$\pm$5.270
HEB210112068 | HXMT/CsI, Swift/BAT | 6.784$\pm$0.143 | 1.792 | 96.512$\pm$0.771 | -58.496 | 12.500$\pm$2.060
HEB210119120 | HXMT/CsI, Fermi-GBM (n1, n3, b0) | 0.032$\pm$0.091 | -0.032 | 0.064$\pm$0.091 | -0.032 | 0.060$\pm$0.061
HEB210121779 | HXMT/CsI, Fermi-GBM (n0, n3, b0) | 7.040$\pm$0.453 | 1.528 | 15.424$\pm$0.643 | 0.312 | 13.980$\pm$0.170
HEB210123304 | HXMT/CsI, Fermi-GBM (n2, n5, b0) | 5.888$\pm$0.231 | -2.928 | 15.488$\pm$1.282 | -6.896 | 12.330$\pm$0.990
HEB210207911 | HXMT/CsI, Swift/BAT | 27.968$\pm$0.202 | -26.192 | 43.584$\pm$0.389 | -40.400 | 42.501$\pm$0.631
HEB210225217 | HXMT/CsI, Fermi-GBM (n1, n5, b0) | 6.720$\pm$0.286 | 1.432 | 19.392$\pm$4.615 | -1.000 | 10.100$\pm$3.340
HEB210227114 | HXMT/CsI, Fermi-GBM (n9, n6, b1) | 10.880$\pm$1.833 | 4.664 | 25.088$\pm$1.409 | 1.272 | 10.704$\pm$1.903
HEB210228057 | HXMT/CsI, Fermi-GBM (n4, n5, b0) | 0.640$\pm$0.091 | 0.056 | 1.408$\pm$0.516 | -0.200 | 1.620$\pm$0.370
HEB210307247 | HXMT/CsI, GECAM | 0.896$\pm$0.091 | 0.216 | 1.216$\pm$0.771 | -0.040 | 0.190$\pm$0.014
HEB210323918 | HXMT/CsI, Fermi-GBM (n0, n1, n2, n5, b0) | 0.128$\pm$0.091 | -0.008 | 0.832$\pm$0.453 | -0.392 | 1.240$\pm$0.990
HEB210324468 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 16.768$\pm$0.362 | 4.448 | 34.432$\pm$1.282 | -3.808 | 33.109$\pm$10.330
HEB210326057 | HXMT/CsI, Fermi-GBM (n4, n5, b0) | 0.128$\pm$0.143 | -0.080 | 1.024$\pm$0.923 | -0.656 | 0.900$\pm$0.412
HEB210409894 | HXMT/CsI, GECAM | 13.248$\pm$2.503 | 1.496 | 38.336$\pm$4.162 | -0.936 | 13.022$\pm$4.535
HEB210411147 | HXMT/CsI, Fermi-GBM (n8, n7) | 36.672$\pm$0.345 | -36.736 | 52.480$\pm$6.503 | -44.160 | 4.507$\pm$1.120
HEB210421454 | HXMT/CsI, Fermi-GBM (n3, n6, b0) | 6.336$\pm$1.843 | -3.816 | 29.568$\pm$5.257 | -22.184 | 8.820$\pm$0.292
HEB210422572 | HXMT/CsI, Fermi-GBM (n0, n1, b0) | 6.528$\pm$1.180 | 3.040 | 38.464$\pm$6.728 | -14.944 | 32.053$\pm$4.789
HEB210427206 | HXMT/CsI, Fermi-GBM (n8, nb, b1) | 8.064$\pm$0.264 | 1.752 | 32.000$\pm$3.019 | -5.032 | 10.067$\pm$2.838
HEB210511476 | HXMT/CsI, Fermi-GBM (n3, n5, b0) | 1.792$\pm$0.091 | 3.176 | 5.824$\pm$0.580 | 1.064 | 5.008$\pm$0.708
HEB210515546 | HXMT/CsI, Fermi-GBM (n9, na, b1) | 0.960$\pm$0.286 | -0.984 | 5.632$\pm$4.800 | -1.176 | 10.017$\pm$4.480
HEB210516982 | HXMT/CsI, Fermi-GBM (n2, na, b0) | 2.816$\pm$0.453 | 5.308 | 7.872$\pm$0.389 | 4.924 | 7.012$\pm$2.065
HEB210518544 | HXMT/CsI, Fermi-GBM (n8, nb, b1) | 3.968$\pm$0.143 | 1.384 | 9.856$\pm$0.604 | -2.264 | 12.521$\pm$5.394
HEB210520796 | HXMT/CsI, Fermi-GBM (n0, n3, b0) | 34.752$\pm$3.223 | 3.752 | 67.200$\pm$15.169 | 0.616 | 67.522$\pm$36.412
HEB210605214 | HXMT/CsI, Fermi-GBM (n7, n8, b1) | 0.192$\pm$0.091 | -0.008 | 1.984$\pm$1.218 | -0.072 | 0.200$\pm$0.014
HEB210606945 | HXMT/CsI, Fermi-GBM (n3, n5, b0) | 199.616$\pm$2.561 | 8.888 | 246.848$\pm$1.601 | 3.896 | 22.537$\pm$3.046
HEB210610827 | HXMT/CsI, Fermi-GBM (n6, nb, b1) | 17.344$\pm$0.202 | 5.264 | 67.392$\pm$3.917 | -6.512 | 33.556$\pm$3.541
HEB210615981 | HXMT/CsI, Fermi-GBM (n0, n3, b0) | 0.832$\pm$0.143 | -1.040 | 4.864$\pm$2.497 | -3.920 | 5.008$\pm$1.120
HEB210622064 | HXMT/CsI, Fermi-GBM (na, n8, b1) | 27.456$\pm$5.588 | 1.072 | 48.256$\pm$5.824 | -0.208 | 48.078$\pm$5.033
HEB210627311 | HXMT/CsI, Fermi-GBM (n4, n5) | 3.776$\pm$0.326 | -0.216 | 9.024$\pm$0.516 | -3.352 | 8.303$\pm$2.609

Table 5:  Durations (40-800 keV for NG mode, 200-3000 keV for LG mode) of ‘SILVER’ and ‘BRONZE’ GRB samples Trigger | Detectors | $T_{\rm 50}$ |  $T_{\rm 50}$ start | $T_{\rm 90}$ |  $T_{\rm 90}$ start
---|---|---|---|---|---
ID | Used | (s) | (s) | (s) | (s)
HEB170626040 | HXMT/CsI | 2.504$\pm$0.707 | 3.840 | 6.511$\pm$1.120 | 1.836
HEB170708045 | HXMT/CsI | 0.050$\pm$0.014 | -0.004 | 0.200$\pm$0.022 | -0.034
HEB170712139 | HXMT/CsI | 3.504$\pm$0.708 | -2.628 | 8.511$\pm$1.119 | -5.631
HEB170801208 | HXMT/CsI | 0.020$\pm$0.014 | 0.009 | 0.460$\pm$0.750 | -0.421
HEB170803917 | HXMT/CsI | 0.160$\pm$0.014 | 0.837 | 0.260$\pm$0.014 | 0.787
HEB170805596 | HXMT/CsI | 0.040$\pm$0.032 | 0.192 | 0.270$\pm$0.487 | -0.028
HEB170805610 | HXMT/CsI | 0.300$\pm$0.141 | 0.476 | 2.000$\pm$0.141 | -1.024
HEB170829270 | HXMT/CsI | 2.002$\pm$0.707 | 0.374 | 5.507$\pm$2.696 | -0.627
HEB170901499 | HXMT/CsI | 8.020$\pm$2.832 | 3.274 | 46.118$\pm$28.143 | -0.736
HEB170904406 | HXMT/CsI | 5.901$\pm$0.224 | 2.475 | 11.403$\pm$0.608 | 0.175
HEB170904884 | HXMT/CsI | 2.002$\pm$0.707 | 10.888 | 10.012$\pm$3.645 | 7.384
HEB170918905 | HXMT/CsI | 0.540$\pm$0.033 | 0.312 | 1.929$\pm$0.310 | 0.162
HEB170921030 | HXMT/CsI | 0.500$\pm$0.071 | -0.012 | 1.150$\pm$0.112 | -0.312
HEB170926340 | HXMT/CsI | 89.223$\pm$5.111 | 0.750 | 108.270$\pm$18.073 | -0.252
HEB171102106 | HXMT/CsI | 25.532$\pm$3.540 | 8.387 | 50.563$\pm$10.025 | 1.379
HEB171108279 | HXMT/CsI | 1.000$\pm$0.707 | 1.154 | 2.501$\pm$0.707 | 0.154
HEB171115217 | HXMT/CsI | 22.532$\pm$16.030 | 0.891 | 47.066$\pm$9.027 | -14.130
HEB180103047 | HXMT/CsI | 43.310$\pm$33.511 | -7.728 | 55.813$\pm$3.516 | -16.630
HEB180103949 | HXMT/CsI | 0.160$\pm$0.014 | 0.928 | 0.430$\pm$0.149 | 0.888
HEB180112687 | HXMT/CsI | 138.168$\pm$1.119 | 1.380 | 158.193$\pm$26.537 | -4.127
HEB180202211 | HXMT/CsI | 2.503$\pm$0.708 | 2.378 | 8.511$\pm$1.119 | -0.125
HEB180210728 | HXMT/CsI | 4.005$\pm$2.064 | 0.876 | 14.018$\pm$4.036 | -0.125
HEB180221520 | HXMT/CsI | 11.503$\pm$2.802 | 7.277 | 32.208$\pm$6.902 | 1.776
HEB180226392 | HXMT/CsI | 0.200$\pm$0.141 | 0.476 | 1.400$\pm$0.412 | 0.376
HEB180326143 | HXMT/CsI | 7.017$\pm$2.242 | 3.759 | 14.035$\pm$1.414 | 2.757
HEB180405168 | HXMT/CsI | 9.011$\pm$2.064 | 6.382 | 22.528$\pm$3.540 | 0.875
HEB180411359 | HXMT/CsI | 47.559$\pm$2.239 | 39.928 | 94.617$\pm$5.529 | 6.386
HEB180603235 | HXMT/CsI | 0.200$\pm$0.071 | 0.088 | 0.450$\pm$0.461 | -0.012
HEB180617871 | HXMT/CsI | 0.200$\pm$0.141 | -0.131 | 1.200$\pm$0.141 | -1.031
HEB180626260 | HXMT/CsI | 19.048$\pm$1.416 | 0.751 | 25.063$\pm$8.267 | -2.256
HEB180704525 | HXMT/CsI | 5.012$\pm$1.416 | 1.752 | 13.032$\pm$4.133 | -1.256
HEB180804554 | HXMT/CsI | 10.025$\pm$1.416 | 0.751 | 27.067$\pm$3.169 | -9.273
HEB181011181 | HXMT/CsI | 4.010$\pm$1.416 | 1.753 | 8.020$\pm$1.416 | 0.750
HEB181201111 | HXMT/CsI | 5.401$\pm$0.141 | 4.177 | 20.605$\pm$1.118 | -1.324
HEB190102652 | HXMT/CsI | 1.898$\pm$0.122 | 4.059 | 2.918$\pm$0.349 | 3.449
HEB190117608 | HXMT/CsI | 15.704$\pm$0.412 | 2.176 | 21.805$\pm$1.504 | 0.375
HEB190203655 | HXMT/CsI | 25.062$\pm$2.241 | -22.307 | 60.149$\pm$14.071 | -42.357
HEB190212129 | HXMT/CsI | 0.045$\pm$0.090 | -0.007 | 0.180$\pm$0.335 | -0.027
HEB190218810 | HXMT/CsI | 16.704$\pm$6.802 | 6.177 | 29.807$\pm$7.803 | 0.175
HEB190306467 | HXMT/CsI | 19.048$\pm$2.241 | 0.751 | 29.073$\pm$7.635 | -4.261
HEB190321931 | HXMT/CsI | 4.506$\pm$0.707 | 0.877 | 8.511$\pm$1.119 | 0.377
HEB190323878 | HXMT/CsI | 14.017$\pm$0.708 | 1.878 | 25.031$\pm$3.206 | -3.629
HEB190330207 | HXMT/CsI | 0.520$\pm$0.360 | -0.473 | 3.400$\pm$1.840 | -1.453
HEB190331841 | HXMT/CsI | 0.050$\pm$0.071 | 0.039 | 0.850$\pm$0.255 | -0.761
HEB190510119 | HXMT/CsI | 47.117$\pm$9.078 | 11.780 | 76.190$\pm$11.073 | 0.752
HEB190605110 | HXMT/CsI | 6.402$\pm$0.707 | 2.676 | 15.704$\pm$2.702 | 0.275
HEB190610477 | HXMT/CsI | 0.200$\pm$0.141 | 1.075 | 0.500$\pm$0.141 | 0.975
HEB190615612 | HXMT/CsI | 20.050$\pm$1.416 | 1.753 | 29.072$\pm$4.133 | 0.751
HEB190706710 | HXMT/CsI | 1.502$\pm$0.708 | -0.125 | 2.503$\pm$0.707 | -0.125
HEB190719113 | HXMT/CsI | 6.007$\pm$3.645 | -6.131 | 10.513$\pm$2.239 | -7.132
HEB190825878 | HXMT/CsI | 14.035$\pm$1.416 | 2.757 | 28.070$\pm$5.111 | -0.251
HEB190828783 | HXMT/CsI | 3.004$\pm$0.707 | 0.375 | 5.006$\pm$0.708 | -0.125
HEB190831271 | HXMT/CsI | 0.400$\pm$0.141 | 1.077 | 2.601$\pm$0.141 | -1.024
HEB190906045 | HXMT/CsI | 0.030$\pm$0.014 | 0.019 | 0.060$\pm$0.014 | -0.001
HEB190927106 | HXMT/CsI | 20.050$\pm$2.241 | 5.765 | 34.085$\pm$6.340 | 1.755
HEB190928550 | HXMT/CsI | 5.012$\pm$1.416 | 97.993 | 27.067$\pm$2.242 | 81.953
HEB190928551 | HXMT/CsI | 5.006$\pm$0.707 | 3.881 | 21.026$\pm$0.708 | -7.133
HEB190929884 | HXMT/CsI | 16.040$\pm$1.418 | -2.256 | 43.108$\pm$3.170 | -23.309
HEB191021831 | HXMT/CsI | 2.503$\pm$0.708 | 0.375 | 9.011$\pm$0.708 | -5.131
HEB191031182 | HXMT/CsI | 3.101$\pm$0.316 | 1.876 | 9.502$\pm$0.447 | 0.275
HEB191031318 | HXMT/CsI | 3.007$\pm$1.418 | 4.761 | 9.022$\pm$1.416 | 0.751
HEB191119445 | HXMT/CsI | 0.040$\pm$0.007 | 0.019 | 0.095$\pm$0.007 | 0.004
HEB191202378 | HXMT/CsI | 3.008$\pm$1.414 | -3.259 | 3.008$\pm$1.414 | -3.259
HEB191224829 | HXMT/CsI | 1.700$\pm$0.224 | 0.476 | 2.901$\pm$0.922 | -0.524
HEB200211193 | HXMT/CsI | 0.000$\pm$2.242 | -0.249 | 3.007$\pm$1.416 | -2.254
HEB200313878 | HXMT/CsI | 1.850$\pm$0.212 | 0.238 | 3.300$\pm$0.552 | -0.112
HEB200326421 | HXMT/CsI | 77.628$\pm$9.070 | 9.350 | 97.160$\pm$16.034 | 1.838
HEB200413712 | HXMT/CsI | 0.900$\pm$0.224 | 0.075 | 2.201$\pm$0.316 | -0.125
HEB200413743 | HXMT/CsI | 2.501$\pm$0.825 | -0.124 | 8.702$\pm$0.721 | -2.224
HEB200521511 | HXMT/CsI | 0.150$\pm$0.014 | -0.587 | 0.590$\pm$0.041 | -0.647
HEB200526628 | HXMT/CsI | 7.017$\pm$1.418 | 62.907 | 73.182$\pm$12.072 | 3.759
HEB201122355 | HXMT/CsI | 6.511$\pm$0.708 | 1.338 | 9.516$\pm$2.554 | 0.837
HEB210124558 | HXMT/CsI | 0.020$\pm$0.014 | 3.069 | 0.500$\pm$0.114 | 2.769
HEB210129908 | HXMT/CsI | 2.401$\pm$0.224 | 0.667 | 18.606$\pm$4.806 | -0.433
HEB210208564 | HXMT/CsI | 24.216$\pm$1.020 | 0.738 | 25.216$\pm$1.078 | 0.337
HEB210213286 | HXMT/CsI | 10.934$\pm$1.729 | 3.182 | 18.886$\pm$2.225 | 1.194
HEB210306320 | HXMT/CsI | 8.027$\pm$2.242 | 5.685 | 29.097$\pm$1.417 | 1.671
HEB210306879 | HXMT/CsI | 3.010$\pm$1.414 | 1.673 | 8.027$\pm$1.417 | -0.334
HEB210326890 | HXMT/CsI | 11.037$\pm$2.838 | -4.349 | 13.043$\pm$3.173 | -5.353
HEB210328396 | HXMT/CsI | 3.101$\pm$2.885 | -1.934 | 5.002$\pm$0.671 | -2.235
HEB210405507 | HXMT/CsI | 2.000$\pm$0.071 | -1.267 | 7.051$\pm$1.801 | -3.017
HEB210406716 | HXMT/CsI | 8.504$\pm$1.119 | 3.776 | 17.008$\pm$3.537 | 0.774
HEB210429071 | HXMT/CsI | 10.517$\pm$1.584 | 1.840 | 34.056$\pm$9.529 | -9.679
HEB210502295 | HXMT/CsI | 2.003$\pm$1.120 | 1.838 | 8.013$\pm$0.708 | 1.337
HEB210504958 | HXMT/CsI | 14.023$\pm$7.529 | 2.337 | 54.090$\pm$14.104 | -9.182
HEB210506027 | HXMT/CsI | 0.400$\pm$0.453 | -0.415 | 1.200$\pm$0.255 | -1.215
HEB210511647 | HXMT/CsI | 10.033$\pm$6.103 | 6.688 | 45.150$\pm$9.085 | 0.668
HEB210602502 | HXMT/CsI | 0.501$\pm$0.707 | 1.335 | 2.003$\pm$0.707 | 0.834
HEB210606120 | HXMT/CsI | 2.200$\pm$0.071 | 1.784 | 4.951$\pm$0.255 | 0.834
HEB210607775 | HXMT/CsI | 9.030$\pm$3.172 | 0.667 | 15.050$\pm$5.676 | -0.336
HEB210607902 | HXMT/CsI | 7.202$\pm$0.224 | 0.370 | 16.705$\pm$2.603 | -2.831
HEB210615891 | HXMT/CsI | 13.043$\pm$6.103 | -0.335 | 24.080$\pm$6.731 | -1.338
HEB210622339 | HXMT/CsI | 2.001$\pm$0.224 | 3.068 | 6.402$\pm$1.265 | 0.367
HEB210627813 | HXMT/CsI | 79.264$\pm$26.106 | 3.678 | 104.347$\pm$11.218 | -8.362

Table 6:  Fluence and Peak Flux (10–2000 keV) from joint analyses with ‘GOLDEN’ GRB samples. Trigger | Fluence | PF64 | PF256 | PF1024
---|---|---|---|---
ID | ($\rm erg$ $\rm cm^{-2}$) | ($\rm ph$ $\rm cm^{-2}$ $\rm s^{-1}$) | ($\rm ph$ $\rm cm^{-2}$ $\rm s^{-1}$) | ($\rm ph$ $\rm cm^{-2}$ $\rm s^{-1}$)
HEB170626400 | 1.54e-05$\pm$1.43e-07 | 41.78$\pm$3.65 | 38.89$\pm$1.64 | 32.66$\pm$0.68
HEB170705115 | 2.03e-05$\pm$6.04e-07 | 40.64$\pm$7.53 | 32.12$\pm$3.08 | 21.31$\pm$1.22
HEB170714049 | 2.31e-07$\pm$2.72e-08 | 6.08$\pm$1.26 | 2.52$\pm$0.38 | 0.85$\pm$0.11
HEB170718152 | 2.29e-06$\pm$5.94e-08 | 3.50$\pm$0.75 | 2.21$\pm$0.31 | 1.57$\pm$0.12
HEB170726248 | 1.50e-06$\pm$1.01e-07 | 4.55$\pm$0.92 | 3.07$\pm$0.43 | 2.19$\pm$0.18
HEB170726793 | 8.23e-06$\pm$1.08e-07 | 11.03$\pm$1.07 | 7.71$\pm$0.43 | 3.79$\pm$0.16
HEB170728960 | 4.36e-06$\pm$9.99e-08 | 24.14$\pm$2.25 | 21.56$\pm$1.09 | 11.19$\pm$0.38
HEB170731751 | 3.07e-06$\pm$9.91e-07 | 1.89$\pm$0.51 | 1.10$\pm$0.21 | 0.75$\pm$0.08
HEB170802637 | 3.13e-06$\pm$1.78e-07 | 36.30$\pm$3.41 | 26.20$\pm$1.38 | 8.57$\pm$0.39
HEB170817908 | 5.50e-06$\pm$9.30e-08 | 14.55$\pm$0.86 | 10.09$\pm$0.42 | 6.79$\pm$0.17
HEB170825306 | 7.82e-06$\pm$1.68e-07 | 9.55$\pm$1.40 | 7.81$\pm$0.62 | 6.60$\pm$0.29
HEB170826818 | 3.90e-05$\pm$3.48e-07 | 47.94$\pm$3.55 | 40.70$\pm$1.58 | 28.39$\pm$0.65
HEB170903534 | 5.70e-06$\pm$9.44e-08 | 4.55$\pm$0.31 | 3.25$\pm$0.15 | 2.72$\pm$0.07
HEB170906029 | 1.46e-04$\pm$7.09e-07 | 32.61$\pm$3.52 | 30.36$\pm$1.50 | 24.44$\pm$0.66
HEB170912984 | 1.68e-06$\pm$2.14e-07 | 4.44$\pm$0.78 | 2.12$\pm$0.30 | 0.65$\pm$0.09
HEB170923188 | 4.86e-06$\pm$1.20e-07 | 7.19$\pm$0.38 | 4.95$\pm$0.16 | 3.68$\pm$0.08
HEB171008079 | 1.60e-06$\pm$9.14e-08 | 4.53$\pm$0.71 | 3.85$\pm$0.33 | 1.59$\pm$0.11
HEB171013350 | 2.19e-05$\pm$2.65e-07 | 11.40$\pm$2.10 | 8.70$\pm$0.91 | 7.67$\pm$0.43
HEB171020963 | 3.75e-06$\pm$1.39e-07 | 21.76$\pm$2.22 | 10.98$\pm$0.84 | 4.78$\pm$0.32
HEB171030728 | 1.92e-07$\pm$2.22e-08 | 8.26$\pm$1.05 | 4.17$\pm$0.38 | 1.08$\pm$0.09
HEB171103965 | 2.82e-06$\pm$8.49e-08 | 14.01$\pm$0.83 | 10.49$\pm$0.41 | 3.16$\pm$0.11
HEB171120555 | 2.95e-05$\pm$3.04e-07 | 87.57$\pm$6.19 | 78.60$\pm$2.98 | 45.05$\pm$1.02
HEB171124234 | 2.06e-05$\pm$4.72e-07 | 4.21$\pm$0.60 | 3.30$\pm$0.25 | 2.39$\pm$0.10
HEB171207054 | 6.60e-07$\pm$5.57e-08 | 5.78$\pm$0.53 | 4.00$\pm$0.27 | 1.25$\pm$0.08
HEB171209615 | 9.77e-06$\pm$2.53e-07 | 5.03$\pm$0.56 | 3.34$\pm$0.23 | 1.73$\pm$0.16
HEB171210492 | 1.24e-04$\pm$6.12e-07 | 15.06$\pm$1.96 | 13.21$\pm$0.81 | 12.68$\pm$0.37
HEB171215705 | 7.76e-06$\pm$1.35e-07 | 3.55$\pm$0.64 | 2.50$\pm$0.23 | 2.11$\pm$0.11
HEB171223818 | 1.33e-08$\pm$7.50e-09 | 1.26$\pm$0.46 | 0.76$\pm$0.20 | 0.09$\pm$0.07
HEB171230955 | 2.39e-05$\pm$2.82e-07 | 8.74$\pm$1.50 | 6.85$\pm$0.77 | 5.85$\pm$0.34
HEB180110608 | 2.01e-06$\pm$1.16e-07 | 3.57$\pm$0.81 | 2.83$\pm$0.37 | 1.70$\pm$0.14
HEB180111695 | 6.22e-05$\pm$1.10e-06 | 56.11$\pm$9.30 | 42.25$\pm$3.60 | 33.46$\pm$1.63
HEB180119836 | 2.86e-06$\pm$8.67e-08 | 6.98$\pm$0.58 | 5.77$\pm$0.25 | 4.56$\pm$0.11
HEB180127049 | 5.47e-06$\pm$1.60e-07 | 4.19$\pm$0.41 | 2.79$\pm$0.29 | 2.36$\pm$0.16
HEB180130744 | 1.62e-07$\pm$2.19e-08 | 4.36$\pm$0.55 | 2.54$\pm$0.22 | 0.75$\pm$0.06
HEB180208764 | 4.91e-06$\pm$3.92e-07 | 4.06$\pm$0.58 | 2.95$\pm$0.82 | 2.26$\pm$0.33
HEB180210517 | 5.60e-05$\pm$4.09e-07 | 28.01$\pm$3.27 | 24.69$\pm$1.41 | 18.70$\pm$0.66
HEB180305393 | 8.20e-05$\pm$8.81e-07 | 44.44$\pm$4.73 | 42.08$\pm$2.29 | 36.97$\pm$1.07
HEB180306972 | 2.85e-06$\pm$8.88e-08 | 1.87$\pm$0.40 | 1.18$\pm$0.15 | 0.78$\pm$0.06
HEB180309321 | 9.51e-06$\pm$1.64e-07 | 5.73$\pm$1.66 | 4.24$\pm$0.60 | 3.43$\pm$0.27
HEB180313977 | 6.39e-07$\pm$1.10e-07 | 14.12$\pm$2.27 | 4.34$\pm$0.66 | 1.20$\pm$0.18
HEB180330891 | 8.47e-06$\pm$1.93e-07 | 11.90$\pm$1.31 | 10.72$\pm$0.54 | 9.88$\pm$0.26
HEB180331177 | 2.08e-06$\pm$7.76e-08 | 1.51$\pm$0.27 | 0.76$\pm$0.10 | 0.33$\pm$0.04
HEB180401279 | 8.81e-06$\pm$2.53e-07 | 7.06$\pm$1.31 | 6.50$\pm$0.81 | 4.07$\pm$0.32
HEB180402406 | 8.02e-07$\pm$5.41e-08 | 7.83$\pm$0.98 | 4.43$\pm$0.33 | 1.22$\pm$0.08
HEB180404091 | 2.11e-05$\pm$1.47e-07 | 5.83$\pm$0.64 | 4.99$\pm$0.31 | 4.24$\pm$0.14
HEB180409346 | 3.32e-05$\pm$4.14e-07 | 118.01$\pm$11.41 | 91.04$\pm$4.74 | 56.26$\pm$1.78
HEB180413117 | 7.18e-06$\pm$1.97e-06 | 4.29$\pm$0.92 | 3.34$\pm$0.44 | 2.70$\pm$0.19
HEB180416923 | 3.45e-05$\pm$4.21e-07 | 9.31$\pm$1.22 | 8.26$\pm$0.57 | 5.88$\pm$0.26
HEB180427442 | 5.67e-05$\pm$6.24e-07 | 41.34$\pm$6.21 | 38.76$\pm$3.33 | 35.75$\pm$1.50
HEB180505539 | 2.68e-05$\pm$1.76e-07 | 53.94$\pm$1.88 | 49.43$\pm$1.14 | 37.11$\pm$0.49
HEB180506902 | 3.38e-06$\pm$6.13e-08 | 4.08$\pm$0.68 | 2.85$\pm$0.29 | 2.52$\pm$0.13
HEB180510808 | 7.00e-06$\pm$4.98e-07 | 19.59$\pm$3.94 | 18.01$\pm$2.18 | 12.69$\pm$0.81
HEB180523782 | 1.57e-06$\pm$5.40e-08 | 7.06$\pm$0.80 | 4.52$\pm$0.33 | 2.55$\pm$0.13
HEB180525151 | 4.32e-07$\pm$3.67e-08 | 8.90$\pm$1.18 | 4.10$\pm$0.39 | 1.18$\pm$0.10
HEB180605457 | 2.37e-05$\pm$2.79e-07 | 16.99$\pm$1.36 | 12.39$\pm$0.66 | 6.48$\pm$0.25
HEB180618030 | 3.23e-06$\pm$9.93e-08 | 15.00$\pm$0.83 | 12.74$\pm$0.33 | 4.52$\pm$0.15
HEB180623696 | 2.28e-05$\pm$5.31e-07 | 10.11$\pm$1.79 | 7.95$\pm$0.96 | 6.53$\pm$0.43
HEB180625940 | 1.36e-06$\pm$1.66e-07 | 5.32$\pm$2.01 | 4.31$\pm$0.79 | 1.95$\pm$0.25
HEB180626391 | 6.60e-07$\pm$4.14e-08 | 16.39$\pm$1.84 | 4.88$\pm$0.50 | 2.67$\pm$0.19
HEB180704233 | 1.28e-05$\pm$1.88e-07 | 5.25$\pm$0.78 | 4.14$\pm$0.36 | 3.30$\pm$0.16
HEB180715754 | 1.49e-06$\pm$7.43e-08 | 5.00$\pm$0.86 | 4.07$\pm$0.39 | 2.18$\pm$0.13
HEB180718762 | 2.73e-05$\pm$1.82e-06 | 5.34$\pm$1.00 | 4.31$\pm$0.54 | 3.71$\pm$0.25
HEB180722992 | 2.93e-05$\pm$1.84e-07 | 10.41$\pm$1.43 | 8.89$\pm$0.61 | 8.26$\pm$0.30
HEB180724807 | 5.73e-05$\pm$4.46e-07 | 16.05$\pm$1.84 | 13.90$\pm$0.87 | 12.89$\pm$0.45
HEB180730017 | 2.32e-07$\pm$9.46e-08 | 11.60$\pm$1.08 | 5.39$\pm$0.54 | 1.19$\pm$0.19
HEB180801275 | 9.74e-07$\pm$6.16e-08 | 6.67$\pm$0.80 | 4.36$\pm$0.34 | 1.85$\pm$0.11
HEB180803590 | 1.82e-07$\pm$1.93e-08 | 3.25$\pm$0.57 | 2.02$\pm$0.23 | 0.61$\pm$0.06
HEB180804930 | 7.25e-06$\pm$1.19e-07 | 10.53$\pm$1.21 | 9.99$\pm$0.61 | 7.34$\pm$0.24
HEB180816088 | 2.21e-05$\pm$2.07e-07 | 21.94$\pm$2.73 | 18.92$\pm$1.30 | 15.40$\pm$0.57
HEB180822561 | 3.65e-06$\pm$9.97e-08 | 4.75$\pm$0.96 | 3.98$\pm$0.42 | 3.30$\pm$0.18
HEB180828789 | 3.41e-05$\pm$3.65e-07 | 48.57$\pm$4.57 | 39.89$\pm$1.88 | 34.42$\pm$0.84
HEB180925407 | 7.12e-07$\pm$3.94e-08 | 3.10$\pm$0.46 | 1.91$\pm$0.17 | 0.75$\pm$0.06
HEB180925609 | 1.42e-05$\pm$2.73e-07 | 27.34$\pm$3.14 | 23.90$\pm$1.48 | 12.13$\pm$0.55
HEB180927992 | 2.54e-06$\pm$9.05e-08 | 7.12$\pm$0.95 | 5.84$\pm$0.38 | 4.41$\pm$0.18
HEB180929453 | 1.57e-06$\pm$6.08e-08 | 6.47$\pm$0.90 | 5.47$\pm$0.38 | 3.14$\pm$0.15
HEB181008269 | 1.63e-05$\pm$1.30e-07 | 15.12$\pm$1.65 | 13.21$\pm$0.86 | 12.62$\pm$0.40
HEB181014479 | 1.65e-05$\pm$1.56e-07 | 6.50$\pm$0.68 | 5.66$\pm$0.36 | 5.05$\pm$0.18
HEB181028590 | 2.76e-05$\pm$1.98e-07 | 13.74$\pm$1.11 | 11.80$\pm$0.59 | 9.63$\pm$0.27
HEB181119605 | 2.05e-05$\pm$2.16e-07 | 39.74$\pm$3.90 | 33.25$\pm$1.96 | 21.97$\pm$0.67
HEB181121306 | 6.90e-07$\pm$1.17e-07 | 3.83$\pm$1.15 | 3.02$\pm$0.67 | 1.10$\pm$0.19
HEB181122381 | 8.18e-06$\pm$2.08e-07 | 10.88$\pm$1.59 | 8.80$\pm$0.68 | 4.15$\pm$0.21
HEB181123231 | 6.71e-07$\pm$4.43e-08 | 6.41$\pm$0.32 | 5.00$\pm$0.40 | 1.64$\pm$0.11
HEB181212692 | 2.24e-05$\pm$1.82e-07 | 61.54$\pm$3.12 | 59.15$\pm$1.56 | 52.87$\pm$0.81
HEB181213540 | 7.43e-06$\pm$2.70e-07 | 7.95$\pm$1.62 | 3.43$\pm$0.53 | 2.24$\pm$0.21
HEB181217664 | 1.31e-05$\pm$2.38e-07 | 18.60$\pm$2.40 | 7.81$\pm$0.73 | 6.69$\pm$0.35
HEB181225489 | 1.12e-05$\pm$3.06e-07 | 10.46$\pm$1.55 | 8.99$\pm$0.70 | 7.62$\pm$0.29
HEB190103877 | 2.46e-05$\pm$3.88e-07 | 2.77$\pm$0.33 | 2.51$\pm$0.19 | 2.25$\pm$0.09
HEB190110725 | 4.38e-06$\pm$7.96e-08 | 13.22$\pm$1.22 | 12.17$\pm$0.66 | 9.64$\pm$0.32
HEB190131964 | 8.52e-06$\pm$1.14e-07 | 1.72$\pm$0.23 | 1.28$\pm$0.11 | 1.05$\pm$0.05
HEB190215771 | 1.59e-05$\pm$1.30e-07 | 8.95$\pm$0.82 | 8.53$\pm$0.53 | 8.09$\pm$0.24
HEB190222537 | 2.96e-05$\pm$7.61e-07 | 23.19$\pm$4.54 | 18.91$\pm$2.11 | 16.31$\pm$1.00
HEB190226515 | 1.26e-06$\pm$1.09e-07 | 11.37$\pm$1.73 | 8.92$\pm$0.72 | 2.43$\pm$0.19
HEB190310398 | 2.41e-05$\pm$2.51e-07 | 28.43$\pm$2.97 | 26.74$\pm$1.43 | 25.69$\pm$0.79
HEB190324348 | 2.44e-05$\pm$1.78e-07 | 8.43$\pm$0.81 | 7.53$\pm$0.43 | 6.96$\pm$0.20
HEB190324947 | 1.86e-05$\pm$2.39e-07 | 28.98$\pm$3.78 | 26.53$\pm$1.57 | 22.22$\pm$0.65
HEB190326313 | 1.39e-05$\pm$1.35e-07 | 11.25$\pm$1.03 | 9.30$\pm$0.50 | 7.24$\pm$0.23
HEB190326316 | 1.32e-07$\pm$1.57e-08 | 2.21$\pm$0.36 | 0.70$\pm$0.10 | 0.22$\pm$0.03
HEB190330694 | 1.09e-05$\pm$1.63e-07 | 8.19$\pm$1.24 | 7.42$\pm$0.50 | 6.80$\pm$0.24
HEB190331093 | 3.17e-06$\pm$1.07e-07 | 2.15$\pm$0.49 | 1.76$\pm$0.23 | 1.01$\pm$0.08
HEB190401139 | 1.94e-05$\pm$1.73e-07 | 19.20$\pm$1.93 | 16.36$\pm$1.13 | 14.34$\pm$0.51
HEB190407671 | 1.13e-05$\pm$2.70e-07 | 23.27$\pm$3.59 | 13.65$\pm$1.32 | 11.23$\pm$0.57
HEB190422283 | 3.09e-05$\pm$1.94e-07 | 16.17$\pm$1.77 | 15.35$\pm$0.86 | 12.94$\pm$0.39
HEB190424417 | 1.17e-05$\pm$4.28e-07 | 22.26$\pm$3.40 | 10.24$\pm$1.46 | 6.58$\pm$0.59
HEB190507269 | 3.31e-06$\pm$6.19e-08 | 5.10$\pm$0.87 | 3.94$\pm$0.38 | 3.16$\pm$0.16
HEB190515189 | 8.68e-07$\pm$5.45e-08 | 4.59$\pm$0.56 | 4.18$\pm$0.35 | 1.56$\pm$0.10
HEB190525031 | 1.93e-06$\pm$8.58e-08 | 7.06$\pm$0.94 | 5.41$\pm$0.40 | 3.03$\pm$0.14
HEB190531840 | 1.08e-04$\pm$4.73e-07 | 51.13$\pm$2.41 | 45.02$\pm$1.14 | 39.16$\pm$0.59
HEB190604446 | 2.26e-05$\pm$2.77e-07 | 18.51$\pm$2.13 | 17.25$\pm$0.97 | 13.67$\pm$0.46
HEB190613449 | 5.45e-06$\pm$1.52e-07 | 3.01$\pm$0.39 | 2.21$\pm$0.17 | 1.74$\pm$0.07
HEB190615636 | 1.20e-05$\pm$3.67e-07 | 7.05$\pm$1.45 | 5.41$\pm$0.71 | 4.31$\pm$0.36
HEB190619594 | 4.04e-05$\pm$3.76e-07 | 20.59$\pm$3.09 | 16.21$\pm$1.14 | 14.13$\pm$0.55
HEB190620507 | 5.95e-05$\pm$2.93e-07 | 18.17$\pm$1.30 | 16.91$\pm$0.69 | 16.09$\pm$0.35
HEB190720964 | 3.51e-06$\pm$7.89e-08 | 5.61$\pm$0.84 | 4.82$\pm$0.42 | 4.52$\pm$0.19
HEB190723308 | 3.29e-06$\pm$9.60e-08 | 4.10$\pm$0.75 | 3.46$\pm$0.35 | 2.61$\pm$0.16
HEB190724030 | 3.94e-07$\pm$2.15e-08 | 9.93$\pm$0.62 | 3.26$\pm$0.19 | 0.84$\pm$0.05
HEB190726642 | 1.73e-05$\pm$2.36e-07 | 21.73$\pm$3.33 | 20.74$\pm$1.49 | 19.26$\pm$0.67
HEB190806675 | 8.17e-06$\pm$1.16e-07 | 4.31$\pm$0.68 | 3.30$\pm$0.24 | 2.54$\pm$0.11
HEB190813520 | 3.99e-07$\pm$6.00e-08 | 9.41$\pm$2.10 | 3.58$\pm$0.60 | 1.03$\pm$0.16
HEB190814837 | 1.85e-06$\pm$5.81e-08 | 1.62$\pm$0.32 | 1.16$\pm$0.13 | 0.97$\pm$0.06
HEB190901890 | 4.38e-05$\pm$3.68e-07 | 19.34$\pm$1.86 | 16.48$\pm$0.93 | 15.77$\pm$0.45
HEB190903721 | 4.43e-07$\pm$2.49e-08 | 2.99$\pm$0.35 | 1.82$\pm$0.13 | 0.67$\pm$0.04
HEB190906767 | 4.91e-06$\pm$3.40e-07 | 10.55$\pm$1.01 | 8.50$\pm$0.43 | 5.48$\pm$0.20
HEB190915239 | 7.11e-06$\pm$2.21e-07 | 6.74$\pm$1.77 | 5.29$\pm$0.67 | 4.46$\pm$0.31
HEB191009297 | 1.90e-05$\pm$5.31e-07 | 2.84$\pm$0.74 | 2.05$\pm$0.31 | 1.72$\pm$0.15
HEB191019970 | 3.80e-05$\pm$2.53e-07 | 7.56$\pm$1.02 | 6.71$\pm$0.50 | 6.15$\pm$0.23
HEB191031780 | 1.14e-05$\pm$1.34e-07 | 6.46$\pm$1.03 | 4.64$\pm$0.40 | 3.78$\pm$0.18
HEB191105257 | 6.39e-06$\pm$6.99e-08 | 60.97$\pm$0.94 | 45.59$\pm$0.38 | 11.92$\pm$0.12
HEB191108003 | 2.28e-05$\pm$3.92e-07 | 7.96$\pm$2.45 | 5.64$\pm$0.93 | 3.85$\pm$0.40
HEB191111364 | 2.29e-05$\pm$2.60e-07 | 28.32$\pm$4.07 | 17.58$\pm$1.57 | 12.28$\pm$0.64
HEB191113578 | 1.06e-06$\pm$6.93e-08 | 10.79$\pm$1.97 | 6.66$\pm$0.78 | 4.94$\pm$0.33
HEB191118925 | 6.14e-06$\pm$1.09e-07 | 4.39$\pm$0.79 | 3.28$\pm$0.31 | 2.94$\pm$0.15
HEB191130506 | 9.57e-06$\pm$1.51e-07 | 3.47$\pm$0.56 | 2.34$\pm$0.22 | 1.91$\pm$0.10
HEB191202867 | 2.86e-05$\pm$3.29e-07 | 42.80$\pm$4.69 | 38.55$\pm$2.02 | 28.30$\pm$0.89
HEB191203289 | 3.68e-07$\pm$4.30e-08 | 2.62$\pm$0.74 | 1.99$\pm$0.33 | 0.88$\pm$0.10
HEB191205740 | 9.49e-07$\pm$6.24e-08 | 4.73$\pm$0.79 | 3.31$\pm$0.34 | 1.59$\pm$0.13
HEB191218112 | 2.70e-05$\pm$2.27e-07 | 7.06$\pm$0.92 | 6.30$\pm$0.41 | 5.81$\pm$0.20
HEB191221860 | 6.98e-05$\pm$6.41e-07 | 48.23$\pm$4.60 | 45.41$\pm$2.25 | 35.96$\pm$0.95
HEB191227069 | 6.11e-05$\pm$2.67e-07 | 42.03$\pm$1.88 | 37.79$\pm$0.99 | 31.34$\pm$0.46
HEB200109073 | 5.49e-06$\pm$2.20e-07 | 2.50$\pm$1.04 | 1.46$\pm$0.36 | 1.09$\pm$0.14
HEB200111632 | 6.22e-06$\pm$1.71e-07 | 20.45$\pm$2.09 | 17.01$\pm$0.96 | 10.95$\pm$0.39
HEB200114153 | 6.83e-06$\pm$1.43e-07 | 2.43$\pm$0.63 | 2.19$\pm$0.28 | 1.84$\pm$0.12
HEB200120961 | 1.24e-05$\pm$2.82e-07 | 38.90$\pm$6.14 | 25.40$\pm$1.85 | 18.08$\pm$0.83
HEB200125863 | 5.92e-05$\pm$4.54e-07 | 175.35$\pm$9.57 | 149.25$\pm$3.78 | 110.27$\pm$1.63
HEB200219998 | 3.21e-05$\pm$3.67e-07 | 32.78$\pm$2.79 | 29.51$\pm$1.56 | 25.39$\pm$0.73
HEB200221161 | 2.50e-06$\pm$2.37e-07 | 6.13$\pm$2.10 | 5.09$\pm$0.93 | 2.78$\pm$0.30
HEB200227305 | 1.26e-05$\pm$1.20e-07 | 10.07$\pm$1.10 | 7.57$\pm$0.53 | 6.81$\pm$0.24
HEB200323782 | 4.06e-06$\pm$1.07e-07 | 37.44$\pm$3.94 | 33.41$\pm$1.97 | 26.08$\pm$0.91
HEB200325137 | 2.92e-06$\pm$1.06e-07 | 9.81$\pm$1.00 | 7.43$\pm$0.43 | 4.91$\pm$0.17
HEB200326517 | 7.86e-07$\pm$3.70e-08 | 0.98$\pm$0.16 | 0.77$\pm$0.08 | 0.46$\pm$0.03
HEB200412381 | 8.70e-05$\pm$5.97e-07 | 157.21$\pm$8.23 | 155.41$\pm$3.77 | 115.72$\pm$1.58
HEB200416295 | 1.36e-06$\pm$4.05e-08 | 5.44$\pm$0.48 | 4.37$\pm$0.22 | 3.28$\pm$0.09
HEB200418864 | 1.85e-06$\pm$1.10e-07 | 5.33$\pm$1.44 | 3.39$\pm$0.59 | 2.02$\pm$0.23
HEB200519472 | 1.06e-05$\pm$3.27e-07 | 9.88$\pm$1.77 | 8.16$\pm$0.90 | 7.09$\pm$0.41
HEB200601097 | 5.41e-05$\pm$5.02e-07 | 7.88$\pm$1.82 | 5.44$\pm$0.72 | 4.80$\pm$0.31
HEB200609379 | 3.13e-05$\pm$2.80e-07 | 4.49$\pm$0.76 | 4.07$\pm$0.32 | 3.28$\pm$0.14
HEB200617679 | 1.81e-06$\pm$2.20e-07 | 5.09$\pm$1.10 | 4.06$\pm$0.50 | 1.98$\pm$0.20
HEB200619108 | 9.97e-06$\pm$1.30e-07 | 4.48$\pm$0.43 | 4.09$\pm$0.23 | 3.62$\pm$0.11
HEB200707072 | 4.18e-06$\pm$1.11e-07 | 2.47$\pm$0.58 | 1.88$\pm$0.22 | 1.27$\pm$0.09
HEB200711461 | 3.00e-05$\pm$4.65e-07 | 28.38$\pm$3.22 | 25.64$\pm$1.56 | 19.43$\pm$0.68
HEB200716315 | 4.07e-05$\pm$4.25e-07 | 11.31$\pm$1.48 | 9.04$\pm$0.58 | 7.90$\pm$0.27
HEB200716956 | 2.00e-05$\pm$3.78e-07 | 34.45$\pm$1.42 | 23.98$\pm$0.63 | 7.99$\pm$0.18
HEB200801352 | 4.38e-06$\pm$8.90e-08 | 1.30$\pm$0.28 | 0.83$\pm$0.10 | 0.61$\pm$0.04
HEB200806645 | 1.37e-05$\pm$1.99e-07 | 11.20$\pm$1.50 | 9.68$\pm$0.62 | 6.39$\pm$0.25
HEB200809653 | 3.77e-06$\pm$8.93e-08 | 8.01$\pm$0.74 | 5.73$\pm$0.31 | 4.24$\pm$0.14
HEB200824594 | 3.06e-07$\pm$3.02e-08 | 1.62$\pm$0.28 | 1.29$\pm$0.15 | 0.77$\pm$0.06
HEB200903112 | 1.15e-05$\pm$2.16e-07 | 2.15$\pm$0.62 | 1.78$\pm$0.30 | 1.40$\pm$0.13
HEB200919964 | 8.60e-05$\pm$6.26e-07 | 24.42$\pm$2.36 | 17.77$\pm$0.98 | 14.62$\pm$0.52
HEB200922504 | 2.58e-06$\pm$9.06e-08 | 2.58$\pm$0.50 | 1.91$\pm$0.20 | 1.56$\pm$0.10
HEB200928551 | 7.23e-06$\pm$9.80e-08 | 8.70$\pm$0.92 | 6.24$\pm$0.37 | 4.09$\pm$0.18
HEB201013157 | 1.56e-05$\pm$1.72e-07 | 41.55$\pm$2.06 | 40.47$\pm$1.05 | 33.90$\pm$0.54
HEB201105229 | 3.91e-05$\pm$2.84e-07 | 28.91$\pm$2.38 | 27.41$\pm$1.08 | 25.41$\pm$0.51
HEB201209239 | 1.60e-05$\pm$5.13e-07 | 4.86$\pm$1.15 | 3.29$\pm$0.43 | 2.71$\pm$0.19
HEB201221591 | 5.96e-07$\pm$4.37e-08 | 45.36$\pm$2.95 | 12.27$\pm$0.93 | 3.77$\pm$0.32
HEB201226553 | 8.34e-06$\pm$1.24e-07 | 2.19$\pm$0.43 | 1.81$\pm$0.19 | 1.31$\pm$0.08
HEB210112068 | 5.71e-05$\pm$1.06e-06 | 85.78$\pm$11.81 | 67.83$\pm$5.27 | 40.40$\pm$2.00
HEB210119120 | 2.37e-07$\pm$3.17e-08 | 10.73$\pm$1.43 | 2.85$\pm$0.38 | 0.71$\pm$0.10
HEB210121779 | 1.19e-04$\pm$5.64e-07 | 32.48$\pm$2.08 | 27.75$\pm$0.82 | 25.45$\pm$0.39
HEB210123304 | 2.22e-05$\pm$2.21e-07 | 37.27$\pm$3.04 | 29.43$\pm$1.36 | 25.53$\pm$0.68
HEB210207911 | 1.05e-04$\pm$1.66e-06 | 120.06$\pm$14.20 | 102.50$\pm$7.03 | 74.98$\pm$2.84
HEB210225217 | 6.73e-06$\pm$1.04e-07 | 4.32$\pm$0.80 | 3.72$\pm$0.31 | 3.19$\pm$0.15
HEB210227114 | 1.46e-05$\pm$3.48e-07 | 2.09$\pm$0.45 | 1.94$\pm$0.20 | 1.40$\pm$0.09
HEB210228057 | 4.76e-06$\pm$1.30e-07 | 9.87$\pm$1.08 | 7.77$\pm$0.51 | 6.03$\pm$0.22
HEB210307247 | 8.97e-07$\pm$7.74e-08 | 5.94$\pm$1.31 | 3.40$\pm$0.52 | 1.36$\pm$0.15