J/ApJS/249/32 The Multi-INstrument Burst ARchive (MINBAR) (Galloway+, 2020)
The Multi-INstrument Burst ARchive (MINBAR).
Galloway D.K., in 't Zand J., Chenevez J., Worpel H., Keek L., Ootes L.,
Watts A.L., Gisler L., Sanchez-Fernandez C., Kuulkers E.
<Astrophys. J. Suppl. Ser., 249, 32 (2020)>
=2020ApJS..249...32G 2020ApJS..249...32G
ADC_Keywords: Binaries, X-ray; X-ray sources; References
Keywords: X-ray bursts ; X-ray bursters ; X-ray transient sources ; Catalogs ;
Astrophysical explosive burning ; Neutron stars ; Nuclear astrophysics
Abstract:
We present the largest sample of type I (thermonuclear) X-ray bursts
yet assembled, comprising 7083 bursts from 85 bursting sources. The
sample is drawn from observations with Xenon-filled proportional
counters on the long-duration satellites RXTE, BeppoSAX, and
International Gamma-Ray Astrophysics Laboratory between 1996 February
8 and 2012 May 3. The burst sources were drawn from a comprehensive
catalog of 115 burst sources, assembled from earlier catalogs and the
literature. We carried out a consistent analysis for each burst light
curve (normalized to the relative instrumental effective area) and
provide measurements of rise time, peak intensity, burst timescale,
and fluence. For bursts observed with the RXTE/PCA and BeppoSAX/Wide
Field Camera we also provide time-resolved spectroscopy, including
estimates of bolometric peak flux and fluence, and spectral parameters
at the peak of the burst. For 950 bursts observed with the PCA from
sources with previously detected burst oscillations, we include an
analysis of the high time resolution data, providing information on
the detectability and amplitude of the oscillations, as well as where
in the burst they are found. We also present analysis of 118,848
observations of the burst sources within the sample time frame. We
extracted 3-25keV X-ray spectra from most observations, and (for
observations meeting our signal-to-noise criterion) we provide
measurements of the flux, spectral colors, and, for selected sources,
the position on the color-color diagram, for the best-fit spectral
model. We present a description of the sample, a summary of the
science investigations completed to date, and suggestions for further
studies.
Description:
The Rossi X-ray Timing Explorer (RXTE) was launched into an
approximately 90-minute low Earth orbit on 1995 December 30 and
operated until the end of the mission on 2012 January 3. The
spacecraft featured three science instruments: the All-Sky Monitor
(ASM), the High-Energy X-ray Timing Experiment (HEXTE), and the
Proportional Counter Array (PCA). We used PCA data for the principal
analysis for this paper. See Section 3.1.
The BeppoSAX broadband X-ray observatory was launched on 1996 April
30. It became operational 2 months later and remained active until
2002 May 1. The WFC is the primary instrument adopted for the
Multi-INstrument Burst ARchive (MINBAR). See Section 3.2.
The hard X-ray and γ-ray observatory INTEGRAL has been orbiting
the Earth about every 3 days since launch on 2002 October 17. The
satellite carries, besides an optical monitor camera, three coded-mask
instruments operating simultaneously and covering different energy
bands from 3keV up to 10MeV. In the present work we use data from the
X-ray monitor JEM-X. See Section 3.3.
Data release 1 of MINBAR consists of 7083 unique bursts, detected
within 118848 observations of 85 burst sources made between 1996
February 8, and 2012 May 3.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 143 115 Known low-mass X-ray binaries (LMXBs) exhibiting
type I X-ray bursts and their representation
in the MINBAR sample
table11.dat 327 7111 MINBAR table of thermonuclear bursts
table14.dat 128 950 Burst oscillation analysis table
table16.dat 419 118848 MINBAR table of observations
refs.dat 102 282 References
datafile2.fits 2880 234 The 115 MINBAR LMXBs Table 2 in FITS format
--------------------------------------------------------------------------------
See also:
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
VII/202 : Globular Clusters in the Milky Way (Harris, 1997)
J/AJ/109/1154 : JHK Photometry of Liller 1 (Frogel+ 1995)
J/MNRAS/351/31 : XMM-Newton Galactic Plane Survey (XGPS) (Hands+, 2004)
J/PAZh/32/508 : Hard X-ray Bursts by INTEGRAL; 2003-2004 (Chelovekov+, 2006)
J/A+A/458/21 : INTEGRAL burst observations of 4U 1728-34 (Falanga+, 2006)
J/A+A/469/807 : Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)
J/AJ/133/1287 : JHK phot. of 24 Galactic globular clusters (Valenti+, 2007)
J/A+A/484/783 : Spectroscopy of 7 INTEGRAL X-ray sources (Chaty+, 2008)
J/ApJS/179/360 : Thermonuclear X-ray bursts with RXTE (Galloway+, 2008)
J/ApJS/181/110 : Galactic center X-ray sources (Muno+, 2009)
J/ApJS/186/1 : 4th IBIS/ISGRI soft gamma-ray survey catalog (Bird+, 2010)
J/MNRAS/402/1729 : JHK phot. of 36 Galactic globular clusters (Valenti+ 2010)
J/PAZh/37/651 : Hard X-ray bursts by INTEGRAL; 2003-2009 (Chelovekov+, 2011)
J/ApJ/756/27 : Classif. of sources from the 2XMMi-DR3 cat. (Lin+, 2012)
J/MNRAS/449/268 : Type II bursts in the Rapid Burster (Bagnoli+, 2015)
J/ApJ/812/149 : HSTPROMO. III. Dynamical distances (Watkins+, 2015)
J/ApJ/826/228 : The Fermi-GBM three-year X-ray burst catalog (Jenke+, 2016)
J/PAZh/43/859 : ISGRI type I X-ray bursts (2003-2015) (Chelovekov+, 2017)
J/A+A/606/A130 : List of 1254 X-ray bursts (in't Zand+, 2017)
J/ApJS/245/19 : Thermonuclear burst oscillations with RXTE (Bilous+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 22 A22 --- Name Main name of the source
24 A1 --- f_Name [d] Flag on Name (1)
26- 28 A3 --- Inst Instrument with which the burst behavior
was first detected (2)
29- 32 I4 yr Year Year of first burst behavior detection
with Inst
34- 44 A11 --- Type Source type(s) adapted
from Liu+, J/A+A/469/807 (3)
46- 47 I2 h RAh Hour of right ascension (J2000)
49- 50 I2 min RAm Minute of right ascension (J2000)
52- 58 F7.4 s RAs Second of right ascension (J2000)
60 A1 --- DE- Sign of declination (J2000)
61- 62 I2 deg DEd Degree of declination (J2000)
64- 65 I2 arcmin DEm Arcminute of declination (J2000)
67- 72 F6.3 arcsec DEs Arcsecond of declination (J2000)
74- 81 F8.3 arcsec errPos [0.007/3600] Position error
83- 84 I2 % Conf [68/99]? Confidence
86- 92 F7.3 h Per [0.17/578]? Binary orbital period Porb
93 A1 --- u_Per [?] Uncertainty flag on Per
95-101 F7.4 10+22/cm2 NH [0.03/33]? Line-of-sight Hydrogen
column density NH
103-107 F5.2 Ms Time [1.12/25.7]? Time (4)
109 A1 --- f_Time [e] Flag on Time (1)
111-114 I4 --- Nb [0/1173]? Number of unique bursts detected
from each source through 2012 May 3
(MJD 56050)
116 A1 --- l_Rate Limit flag on Rate
118-124 F7.5 h-1 Rate [0.0004/1.9]? Mean burst rate (5)
126-143 A18 --- Ref Reference(s) from which the first detection
of bursts, position, orbital period, and
NH values are drawn (see refs.dat file)
--------------------------------------------------------------------------------
Note (1): Flag as follows:
d = These sources are indistinguishable from the next nearest source, and
so we cannot separate the bursts; we attribute all the observed events
to the neighbor (SLX 1744-300 in the case of SLX 1744-200, and
1A 1742-289 in the case of AX J1745.6-2901).
e = The observation table entries for these systems are not complete and
may be attributed to their nearby neighbor. We thus adopt the maximum
exposure for any of the nearby sources as the common value for the
group.
Note (2): Instrument as follows:
WFC = Wide Field Camera (24 bursts)
NFI = BeppoSAX Narrow Field Instruments (1 burst)
XTE = RXTE Proportional Counter Array (PCA; 10 bursts)
JEM = INTEGRAL Joint European X-Ray Monitor (JEM-X; 10 bursts)
IBI = INTEGRAL Imager on Board the INTEGRAL Satellite (IBIS; 1 burst)
SAS = Small Astronomy Satellite 3 (SAS-3; 13 bursts)
BAT = Swift Burst Alert Telescope (9 bursts)
XRT = Swift X-Ray Telescope (6 bursts)
EXO = European X-Ray Observatory Satellite (EXOSAT; 5 bursts)
OS8 = Orbiting Solar Observatory 8 (OSO-8; 5 bursts)
HAK = Hakucho (5 bursts)
TTM = Mir-Kvant Coded Mask Imaging Spectrometer (COMIS; 3 bursts)
GIN = Ginga/LAC (3 bursts)
EIN = Einstein X-ray Observatory (3 bursts)
ASC = Advanced Satellite for Cosmology and Astrophysics (ASCA; 3 bursts)
VEL = Vela (2 bursts)
MAX = ISS Monitor of All-Sky X-ray Image (MAXI; 2 bursts)
NIC = ISS Neutron star Interior Composition Explorer (NICER; 2 bursts)
NUS = Nuclear Spectroscopic Telescope Array (NuSTAR; 1 burst)
SLX = Spacelab-2 (1 burst)
AGI = Astro-rivelatore Gamma a Immagini Leggero (AGILE; 1 burst)
ANS = Astronomical Netherlands Satellite (1 burst)
GRA = Granat Astrophysical Roentgen Telescope (ART-P; 1 burst)
HET = High-Energy Transient Explorer 2 (HETE-2; 1 burst)
UHU = Uhuru (1 burst)
OPT = High time resolution optical photometry (Mason+ 1980Natur.287..516M 1980Natur.287..516M)
for 4U 1254-69
Note (3): Type as follows:
A = atoll source,
C = "ultracompact" X-ray binary (UCXB; including candidates),
D = "dipper"
E = eclipsing,
G = globular cluster association,
I = intermittent pulsar,
M = microquasar,
O = burst oscillation,
P = pulsar,
R = radio-loud X-ray binary,
S = superburst,
T = transient,
Z = Z-source.
We omit the "B" designation indicating a burst source.
Note (4): For sources with a neighbor within 1°, we combine all RXTE
observations that include this source within the FOV (possibly
including observations of the neighbor).
Note (5): For systems with no bursts detected in the MINBAR sample, we
calculate the 95% upper limit on the average burst rate, assuming a
Poisson-distributed number of bursts.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table11.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 21 A21 --- Name Likely burst origin
23- 25 A3 --- Inst Instrument label (G1)
27- 41 A15 --- obsid Observation ID
43- 53 F11.5 d Time [50121.6/56033.4] Burst start time (MJD UT)
55- 58 I4 --- Seq [1/8796] MINBAR burst ID
60- 65 I6 --- SeqID [77/277779] MINBAR observation ID
in which this burst falls
67- 69 I3 --- bnum [-1/383] Order of the event
within the observation
71- 74 I4 --- xref [0/1925]? Burst ID in external catalog
(G08 or C17) (1)
76- 76 I1 --- mult [1/2] Number of MINBAR instruments which
detected this event
78- 84 F7.2 arcmin angle [0/1296.25] Angle between the source
position and pointing axis
86- 90 F5.3 --- VigCor [0/1] Vignetting correction factor
92- 96 A5 --- sflag Data quality/analysis flags (G2)
98-102 F5.2 --- rexp [-1/3] Photospheric radius-expansion
flag (2)
104-108 F5.2 s rise [0/99.99] Burst rise time (G3)
110-114 F5.1 s tau [0.4/999.9]?=0 Ratio of fluence to peak
flux, tau (G3)
116-120 F5.1 s e_tau [0.1/999.9]?=0 Uncertainty on tau (G3)
122-127 F6.1 s dur [1/9999.9]?=0 Burst duration (G3)
129-134 F6.1 s e_dur [1/9999.9]?=0 Uncertainty on dur (G3)
136-141 F6.1 s edt [0.3/9999.9]?=0 Decay constant for
exponential fit to profile (G3)
143-149 F7.3 s e_edt [0.001/999.999]?=0 Error on edt (G3)
151-158 F8.1 h tdel [0.1/135444]?=0 Time since previous burst
from this source
160-163 F4.1 h trec [0.1/29.8]?=0 Inferred recurrence time
165-170 F6.3 10-9mW/m2 perflx [0.002/25.6]?=0 Persistent 3-25keV flux
prior to the burst, F_per
172-177 F6.3 10-9mW/m2 e_perflx [0.001/76.3]?=0 Uncertainty on perflx
179-184 F6.1 --- alpha [0.2/5708.5]?=0 Ratio of integrated
persistent flux to burst fluence, alpha
186-191 F6.1 --- e_alpha [0.1/1240.7]?=0 Uncertainty on alpha
193-197 F5.3 --- bc [1/2.14]?=0 Bolometric correction adopted
for persistent flux
199-203 F5.3 --- e_bc [0.001/0.14]?=0 Uncertainty on bc
205-210 F6.4 --- gamma [0.0001/4.52]?=0 Ratio of persistent flux
to peak PRE burst flux, gamma
212-217 F6.3 --- sc [0.012/99.999]?=0 Soft colour (G3)
219-224 F6.3 --- hc [0.008/24.27]?=0 Hard colour
226-230 F5.3 --- sZ [0.55/2.8]?=0 Position on the color-color
diagram, SZ
232-236 F5.2 ct/cm2/s pflux [0.01/19.3]?=0 Peak photon flux
238-241 F4.2 ct/cm2/s e_pflux [0.01/6.73]?=0 Uncertainty on pflux
243-250 F8.3 ct/cm2 fluen [0.05/2456]?=0 Integrated photon flux
252-258 F7.3 ct/cm2 e_fluen [0.002/833]?=0 Uncertainty on fluen
260-265 F6.2 10-9mW/m2 bpflux [0.18/999.99]?=0 Bolometric peak flux
(from blackbody fit) (G3)
267-271 F5.2 10-9mW/m2 e_bpflux [0.02/99.99]?=0 Uncertainty on bpflux (G3)
273-276 F4.2 keV kT [0.2/7]?=0 Blackbody temperature kT
at burst peak
278-281 F4.2 keV e_kT [0.01/3.1]?=0 Uncertainty on kT
283-288 F6.1 --- rad [0.3/4343]?=0 Blackbody normalisation
at burst peak (3)
290-293 F4.1 --- e_rad [0.1/81.4]?=0 Uncertainty on rad (3)
295-300 F6.4 10-6mJ/m2 bfluen [0.001/9.9999]?=0 Bolometric fluence
(integrated bolometric flux), E_b
302-307 F6.4 10-6mJ/m2 e_bfluen [0.0002/2.4]?=0 Uncertainty on bfluen
309-327 A19 --- Ref References for this burst
(see refs.dat file)
--------------------------------------------------------------------------------
Note (1): This work is an extension of previous studies of large databases,
such as that based on RXTE/PCA observations through 2008
(G08 = Galloway+ 2008, J/ApJS/179/360) or on all observations with the
BeppoSAX/WFCs (Cornelisse+ 2003A&A...405.1033C 2003A&A...405.1033C).
Note (2): This attribute indicates the presence of "photospheric radius
expansion" (PRE) burst, determined as described in Section 5.1.
The possible values are as follows:
2.00 = confirmed presence
1.00 = confirmed absence
range 1.0-2.0 = probability pi=rexp-1 (according to a machine-learning
classification scheme) that the burst exhibits radius
expansion
3.00 = marginal evidence
-1.00 = insufficient data to assess
Note (3): Units of (R/d), where R is in km and distance d in units of 10kpc,
as for the bbodyrad model in XSpec; Dorman & Arnaud (2001ASPC..238..415D 2001ASPC..238..415D).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table14.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Name Likely burst origin
19- 21 A3 --- Inst Instrument label (1)
23- 37 A15 --- obsid Observation ID
39- 42 I4 --- Seq [2204/8769] MINBAR burst ID
44- 49 I6 --- SeqID [14292/275831] MINBAR observation ID
in which this burst falls
51- 63 F13.3 s Time Start time of the bin with the most
significant signal
65- 69 F5.2 s Dur [0.11/12.8] Duration of the bin
71- 72 I2 --- Nbin [1/54] Number of time bins exceeding the
count threshold
74- 80 F7.1 ct/s BRate [38.5/11383.5] Background rate (per PCU)
estimated from the pre-burst emission
82- 82 I1 --- Det [0/1] Detection flag on burst oscillation;
1 for detection, 0 otherwise
84- 84 A1 --- Phase Phase during which oscillation was detected (2)
86- 86 I1 --- Crit [1/5] Detection criterion by which the
highest-power signal was selected (3)
88- 88 I1 --- fbin [0/1] Flag for signal in the first bin
after the start; 1=yes, 0=no
90- 94 F5.2 % Amp [4.17/21.92]?=0 Amplitude of detected
burst oscillation
96- 99 F4.2 % e_Amp [0.95/2.7]?=0 Lower uncertainty limit on Amp
101-104 F4.2 % E_Amp [1.13/3.2]?=0 Upper uncertainty limit on Amp
106-110 F5.2 % AmpLim [4.94/67.61]?=0 3-sigma upper limit on amplitude
in the absence of a detected oscillation
112-116 F5.1 Hz Freq [245/624]?=0 Frequency of the detected signal
118-122 F5.1 --- Pow [12.9/143.6]?=0 Signal power of the
detected burst oscillation
124-128 F5.1 --- PowMin [2.3/144.6] Measured power of the
most-significant detected signal
--------------------------------------------------------------------------------
Note (1): XPn for RXTE/PCA bursts, where n specifies the number of active
PCUs. Single-PCU cases are numbered as for the PCUs, 0..4; or a for all
PCUs active (see the paper for other possibilities).
Note (2): n = none, r = rise, p = peak (corresponding to the interval during
which the countrate was above 90% of the maximum), t = tail
Note (3): The detection criterion is present only if the amplitude is
greater than zero, and can take the values 1 (single bin, not in the
first second); 2 (single bin, signal in the first second); 3-5 (double
time-frequency bin). See the article for more details.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table16.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 21 A21 --- Name Burster name
23- 25 A3 --- Inst Instrument label (G1)
27- 41 A15 --- obsid Observation ID
43- 48 I6 --- Seq [8/277779] MINBAR observation ID
50- 54 A5 --- sflag Data quality/analysis flags (G2)
56- 66 F11.5 d tstart [50117.5/56050.74] Observation start time
68- 78 F11.5 d tstop [50117.5/56050.8] Observation stop time
80- 84 I5 s Exp [0/73840] Total exposure
86- 92 F7.2 arcmin Angle [0/1572] Angle between the source position
and pointing axis
94- 98 F5.3 --- VigCor [0.002/1] Vignetting correction factor
100-101 I2 --- Nb [0/31] Number of (type-I) bursts detected
in the observation
103-108 F6.3 ct/cm2/s Count [-0.3/96.1] Background-subtracted mean
rate for target source
110-114 F5.3 ct/cm2/s e_Count [0.001/3.6]?=0 Uncertainty on Count
116-121 F6.1 --- Sig [0.1/9999.9]?=0 Detection significance
for this observation (G3)
123-128 F6.3 10-9mW/m2 Flux [0.001/99.999]?=0 Mean flux over the
observation (G3)
130-134 F5.3 10-9mW/m2 e_Flux [0.001/5]?=0 Estimated uncertainty on Flu
136-141 F6.4 --- gamma [0.0001/9.9999]?=0 Ratio of persistent
flux to mean peak flux of
radius-expansion bursts (G3)
143-148 F6.3 --- sc [0.006/99.999]?=0 Soft colour (G3)
150-155 F6.3 --- hc [0.001/34.7]?=0 Hard colour
157-161 F5.3 --- sZ [0.45/2.8]?=0 SZ value, giving position
in the colour-colour diagram
163-185 A23 --- model Spectral model (XSpec syntax)
187-193 F7.4 --- plind [-3/10]?=0 Spectral index Gamma of
power law (where present)
195-202 E8.3 --- e_plind [5e-6/9.2]?=0 Uncertainty on plind (1)
204-211 E8.3 --- plnorm [1.4e-22/362000]?=0 Normalisation of
power law (2)
213-220 E8.3 --- e_plnorm [5.6e-9/48200]?=0 Uncertainty on plnorm (1)
222-229 F8.5 keV kT [0.0001/11]?=0 Temperature kT of
blackbody component (where present)
231-238 E8.3 keV e_kT [1e-5/7.8]?=0 Uncertainty on kT (1)
240-256 E17.3 --- bbnorm [2e-5/5.2e+23]?=0 Normalisation of blackbody
component (3)
258-275 E18.3 --- e_bbnorm [7e-6/8.3e+21]?=0 Uncertainty on bbnorm (1)
277-283 F7.5 keV T0 [0.001/6.6]?=0 Input soft photon (Wien)
temperature of Comptonisation component
(where present)
285-292 E8.3 keV e_T0 [2.4e-6/7430]?=0 Uncertainty on T0 (1)
294-300 F7.3 keV kTe [0.4/500]?=0 Plasma temperature of
Comptonisation component
302-309 E8.3 keV e_kTe [1.4e-5/2190]?=0 Uncertainty on kTe (1)
311-319 F9.5 --- tau [0.003/200]?=0 Plasma optical depth tau
of Comptonisation component
321-328 E8.3 --- e_tau [1.4e-7/1900]?=0 Uncertainty on tau (1)
330-339 E10.3 --- cnorm [5e-5/6e+7]?=0 Normalisation of
Comptonisation component
341-357 E17.3 --- e_cnorm [5.4e-6/1.4e+14]?=0 Uncertainty on cnorm (1)
359-362 F4.2 keV line [6/7.1]?=0 Line energy for Gaussian
component (where present)
364-371 E8.3 keV e_line [5.8e-6/3.6]?=0 Uncertainty on line (1)
373-380 E8.3 keV sigma [1e-5/5]?=0 Line width for Gaussian component
382-389 E8.3 keV e_sigma [7.6e-7/3.6]?=0 Uncertainty on sigma (1)
391-398 E8.3 ph/cm2/s gnorm [1e-05/1.1]?=0 Normalisation for Gaussian
component
400-407 E8.3 ph/cm2/s e_gnorm [3.8e-7/0.6]?=0 Uncertainty on gnorm (1)
409-413 F5.2 --- chi2 [0.01/99.99]?=0 (Mean) reduced chi2
of spectral fits (where >1 instrument) (G3)
415-419 F5.2 --- e_chi2 [0.01/99.99]?=0 Standard deviation of
chi2 from spectral fits, if relevant (G3)
--------------------------------------------------------------------------------
Note (1): Uncertainties are at the 1-sigma (68%) confidence level
Note (2): Power-law component normalisation has units of photons/keV/cm2/s at
1keV, as for XSpec; Dorman & Arnaud (2001ASPC..238..415D 2001ASPC..238..415D)
Note (3): Units of (R/d)^2, where R is in km and distance d in units of 10kpc,
as for the bbodyrad model
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Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Ref Reference code
5- 28 A24 --- Auth Author's name(s)
30- 48 A19 --- BibCode Bibcode of the reference
50-102 A53 --- Comm Comment
--------------------------------------------------------------------------------
Global notes:
Note (G1): XPn for RXTE/PCA bursts, where n specifies the number of PCUs on (see
the paper); SWc for BeppoSAX/WFC bursts, where c gives the camera
number; IJu for INTEGRAL/JEM-X bursts, with u the unit number, or X
where both units were active
Note (G2): Analysis flag as follows:
a = The burst was observed during a slew, and thus offset from the
source position; fluxes and fluence have been scaled
by 1/(1-Δθ) -- PCA instrument.
b = The observation was offset from the source position; flux and fluence
have been adjusted via setting the source position for response
matrix generation -- PCA instrument.
c = The origin of the burst is uncertain; the burst may have been from
another source in the FOV. If the origin is not the center of the FOV,
the flux and fluence have been adjusted by calculating the response
for the assumed source position -- PCA instrument.
d = Buffer overruns (or some other instrumental effect) caused gaps in
the high time resolution data, affecting the time-resolved
spectroscopic analysis -- PCA, WFC instruments.
e = The burst was so faint that only the peak flux could be measured, and
not the fluence or other parameters; or, alternatively, that the burst
was cut off by the end of the observation, so that the fluence is
an underestimate -- PCA, WFC instruments.
f = An extremely faint burst or possibly problems with the background
subtraction, resulting in no time-resolved spectral fit results
-- PCA instrument.
g = The full burst profile was not observed, so that the event can be
considered an unconfirmed burst candidate. Typically in these cases the
initial burst rise is missed, so that the measured peak flux and fluence
are lower limits only. Also includes long bursts observed with
INTEGRAL/JEM-X spanning multiple science windows (observations)
-- all instruments.
h = High time resolution modes do not cover burst, preventing any
time-resolved spectroscopic results and oscillation search
-- PCA instrument.
Note (G3): Values at that maximum of the column range and have values such as
99.99, 999.9, 999.999, 9999.9 exceed the format specification.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 27-Oct-2020