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The Burst Alert Telescope (BAT) is a highly sensitive, large FOVinstrument designed to provide critical GRB triggers and 4-arcminpositions. It is a coded aperture imaging instrument with a 1.4steradian field-of-view (half coded). The energy range is 15-150 keVfor imaging with a non-coded response up to 500 keV. Within severalseconds of detecting a burst, the BAT calculates an initial position,decides whether the burst merits a spacecraft slew and, if so, sendsthe position to the spacecraft.

In order to study bursts with a variety of intensities,durations, and temporal structures, the BAT must have a large dynamicrange and trigger capabilities. The BAT uses a two-dimensional codedaperture mask and a large area solid state detector array to detectweak bursts, and has a large FOV to detect a good fraction of brightbursts. Since the BAT coded aperture FOV always includes the XRT andUVOT fields-of-view, long duration gamma-ray emission from the burstcan be studied simultaneously with the X-ray and UV/opticalemission. The data from the BAT can also produce a sensitive hardX-ray all-sky survey over the course of Swift's two yearmission. Below is a cut-away drawing of the BAT, and a table listingthe BAT's parameters. Further information on the BAT is given byBarthelmy (2000; 2005).

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The BAT's 32,768 pieces of 4 x 4 x 2 mm CdZnTe (CZT) form a 1.2 x0.6 m sensitive area in the detector plane. Groups of 128 detectorelements are assembled into 8 x 16 arrays, each connected to128-channel readout Application Specific Integrated Circuits(ASICs). Detector modules, each containing two such arrays, arefurther grouped by eights into blocks. This hierarchical structure,along with the forgiving nature of the coded aperture technique, meansthat the BAT can tolerate the loss of individual pixels, individualdetector modules, and even whole blocks without losing the ability todetect bursts and determine locations. The CZT array has a nominaloperating temperature of 20 degrees C, and its thermal gradients(temporal and spatial) are kept to within 1 C. Thetypical bias voltage is -200 V, with a maximum of -300 V.

A figure-of-merit (FOM) algorithm resides within the BAT flightsoftware and decides if a burst detected by the BAT is worthrequesting a slew maneuver by the spacecraft. If the new burst hasmore "merit" than the pre-programmed observations, a slewrequest is sent to the spacecraft. Uploaded, rapid-reaction positionsare processed exactly the same as events discovered by the BAT. TheFOM is implemented entirely in software and can be changed either byadjusting the parameters of the current criteria or by adding newcriteria.

The BAT runs in two modes: burst mode, which produces burstpositions, and survey mode, which produces hard X-ray surveydata. In the survey mode the instrument collects count-rate data infive-minute time bins for 80 energy intervals. When a burst occurs itswitches into a photon-by-photon mode with a ring-buffer to savepre-burst information.

While searching for bursts, the BAT performs an all-sky hardX-ray survey and monitors for hard X-ray transients.The BAT accumulates detector plane maps every five minutes, which areincluded in the normal spacecraft telemetry stream. Sky images aresearched to detect and position sources. The 5-sigma sensitivity ofthe survey is about 0.8 mCrab in the 15-150 keV band for 2 years. Forregions where there are perpetually numerous strong sources in the BATFOV (i.e. the Galactic Center), the limiting sensitivity will be about50% greater.

The combination of the 4 mm square CZT pieces, plus the 5 mmsquare mask cells and the 1 m detector-to-mask separation gives aninstrumental angular resolution of 20 arcmin FWHM, yielding aconservative 4 arcmin centroiding capability for bursts andsteady-state sources given an 8 sigma burst threshold.

I use this feature quite a bit on our R6 mark II and have no problems extracting Raw files from the rolls in DPP 4 on my Windows 10 pro laptop. I usually keep my bursts short, like 1 or 2 seconds, and that is still 30-40 shots, including pre-burst, and makes for a 400-500mb file.

Have you tried increasing the amount of memory available in DPP (Tools/Preferences/General settings). Also, as a test, reduce your burst size. 1-2GB is a big file and DPP can be quirky. As mentioned, my files are typically under 500MB and I have no problems, so see if you can replicate that with a smaller roll file. I know, that's not how you shoot, but we can see if it's size related.

DPP doesn't really care how the photos were acquired whether burst or a big folder of single shots. I shoot sports using three 1DX bodies at an event and although I leave the bodies in high speed drive mode the image files are a combination of bursts and single to three shot. The last basketball event I shot was senior night with both boys and girls games and the DPP folder is 67.6 GB in size and it had no problem with it.

I'm pretty sure the OP is having problems extracting individual shots from a camera roll file. I'm not that familiar with the 1DX series, so not sure they will record Raw burst in rolls. So, sorry if I'm telling you something you already know If you enable the feature in camera, the burst is combined into a single roll and comes into DPP as one file and you have to open the Raw burst image tool to extract and edit individual Raw files within the roll. There is no conversion option, only Raw extraction and if you try a Batch operation, only the first image in the roll will be converted.

My wife and I both shoot bursts as a routine, not just for action. Usually, after two or three in the burst, the shot we want will be there. We both are unsteady and it usually takes a few frames for our "shake's" to settle down, even with proper holding technique. We can scroll through the file, extract the one or two we want, then dispose of the roll. Burst in general really helps us overcome our physical issues but I can see it helping anyone to get sharper images. Another feature of the film roll burst, at least on the R6 mark II, is pre-burst (when enabled). Man, do I like that! A half press takes 0.5 seconds of burst, which is about 8-11 shots depending on your exposure. How many times has your subject left in the middle of catching focus? Yes, the first few frames are soft, but the AF of these newer R's is nothing short of amazing and catches up by frame 3. Unfortunately, film roll isn't a feature (yet) of my R5, so I just have to edit and delete the regular way... Awwwww, poor me

I like to kick things off here with a slightly spicy garlic oil. My garlic sauce pasta is always a huge hit, and I wanted to take some notes of flavor from that. So we start with a bunch of garlic cloves and red pepper flakes. Then let the tomatoes burst in that incredible oil. They take on so much flavor while at the same time melting into the oil. It sort of creates a burst tomato oil in a way, with hints of garlic and spice.

Every Widget datasheet I've worked with used the term "SPI burst mode" to refer to writing more than 1 byte of data per sequence of "CSnot line low, Transmit setup like Mode byte, Address byte(s)", then "burst" N-bytes, then CSnot line high. The ST sample apps clearly show configuring a SPI for 8-bit mode, so you're done before you've even begun

Using bursting can save you and your team hours of time by running a report once and then dividing the results for recipients who each view a subset of data based on criteria you give it. For example, salespeople in different regions each need a report showing the sales target for their country or region. You use burst reports to send each salesperson only the information they need.

This how-to guide will walk you through how to setup and run burst reports in Cognos 11. If you find it helpful or have feedback (or questions), please let us know in the comments below! Visit the Reporting Hub for additional resources like guides, demo videos, and quick tips.

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This table lists all of the triggers observed by a subset of the 14 GBMdetectors (12 NaI and 2 BGO) which have been classified as gamma-ray bursts(GRBs). Note that there are two Browse catalogs resulting from GBM triggers. AllGBM triggers are entered in the Fermi GBM Trigger Catalog,while only those triggers classified as bursts are entered in the BurstCatalog. Thus, a burst will be found in both the Trigger and Burst Catalogs.The Burst Catalog analysis requires human intervention; therefore, GRBs willbe entered in the Trigger Catalog before the Burst Catalog. The latencyrequirements are 1 day for triggers and 3 days for bursts. There are fourfewer bursts in the online catalog than in the Gruber et al. 2014 paper. Thefour missing events (081007224, 091013989, 091022752, and 091208623) have notbeen classified with certainty as GRBs and are not included in the generalGRB catalog. This classification may be revised at a later stage.The GBM consists of an array of 12 sodium iodide (NaI) detectors which coverthe lower end of the energy range up to 1 MeV. The GBM triggers off of therates in the NaI detectors, with some Terrestrial Gamma-ray Flash(TGF)-specific algorithms using the bismuth germanate (BGO) detectors,sensitive to higher energies, up to 40 MeV. The NaI detectors are placedaround the Fermi spacecraft with different orientations to provide therequired sensitivity and FOV. The cosine-like angular response of the thinNaI detectors is used to localize burst sources by comparing rates fromdetectors with different viewing angles. The two BGO detectors are placed onopposite sides of the spacecraft so that all sky positions are visible to atleast one BGO detector.The signals from all 14 GBM detectors are collected by a central DataProcessing Unit (DPU). This unit digitizes and time-tags the detectors' pulseheight signals, packages the resulting data into several different types fortransmission to the ground (via the Fermi spacecraft), and performs variousdata processing tasks such as autonomous burst triggering.The GRB science products are transmitted to the FSSC in two types of files.The first file, called the "bcat" file, provides basic burst parameters suchas duration, peak flux and fluence, calculated from 8-channel data usinga spectral model which has a power-law in energy that falls exponentiallyabove an energy EPeak, known as the Comptonized model. The crude 8-channelbinning and the simple spectral model allow data fits in batch mode overnumerous time bins in an efficient and robust fashion, including intervalswith little or no flux, yielding both values for the burst duration, anddeconvolved lightcurves for the detectors included in the fit. The bcat fileincludes two extensions. The first, containing detailed information aboutenergy channels and detectors used in the calculations, is detector-specific,and includes the time history of the deconvolved flux over the time intervalsof the burst. The second shows the evolution of the spectral parametersobtained in a joint fit of the included detectors for the model used, usuallythe Comptonized model described above. The bcat files and their time-varyingquantities contained in these two extensions are available at the HEASARC FTPsite. Quantities derived from these batch fits are given in the bcat primaryheader and presented in the Browse table, as described below. The mainpurpose of the analysis contained in the bcat file is to produce a measure ofthe duration of the burst after deconvolving the instrument response. Theduration quantities are: * 't50' - the time taken to accumulate 50% of the burst fluence starting at the 25% fluence level. * 't90' - the time taken to accumulate 90% of the burst fluence starting at the 5% fluence level.By-products of this analysis include fluxes on various timescales andfluences, both obtained using the simple Comptonized model described above.These quantities are detailed in the Browse table using the following prefixes: * 'flux' - the peak flux over 3 different timescales obtained in the batch mode fit used to calculate t50/t90. * 'fluence' - the total fluence accumulated in the t50/t90 calculation.The fluxes and fluences derived from the 8-channel data for these bcat filesshould be considered less reliable than those in the spectral analysis filesdescribed below.Analysis methods used in obtaining these quantities are detailed in the firstGBM GRB Catalog (Paciesas et al. 2011). Updates of bcat files will be sent(with new version numbers) as these parameters are refined. This "bcat" fileis produced for triggers that are classified as GRBs (with exceptions asdescribed below), and supplements the initial data in the trigger or "tcat"file that is produced for all triggers.The second type of file (the spectrum or "scat" file) provides parametervalues and goodness-of-fit measures for different types of spectral fits andmodels. These fits are performed using 128-channel data, either CSPEC or, forshort bursts, TTE data. The type and model are coded into the file name. Thereare currently two spectrum categories: * Peak flux ('pflx') - a single spectrum over the time range of the peak flux of the burst * Fluence ('flnc') - a single spectrum over the entire burst duration selected by the duty scientist.Like the bcat files, the scat files have two extensions. The first extensiongives detector-specific information, including photon fluxes and fluences foreach detector, which are provided for each energy channel. The secondextension provides derived quantities such as flux, fluence and modelparameters for the joint fit of all included detectors. The scat files andtheir energy-resolved quantities contained in these two extensions areavailable in the Fermi data archive at the HEASARC. Quantities derived fromthese spectral fits are available in the Browse table, as described belowand in Goldstein et al. (2011).The spectra are fit with a number of models, with the signal-to-noise ratioof the spectrum often determining whether a more complex model isstatistically favored. The current set is: * Power law ('plaw'), * Comptonized (exponentially attenuated power law; 'comp') * Band ('band') * Smoothly broken power law ('sbpl')WarningsThe bcat and scat files result from two completely independent analyses,and consequently, it is possible that the same quantities might showdifferences. Indeed,1) the fluxes and fluences in the "scat" files should be considered morereliable than those in the "bcat" files, with the official fluxes andfluences being those yielded by the statistically favored model("Best_Fitting_Model" in the Browse table) and with the full energyresolution of the instrument;2) in both the bcat and scat analyses, the set of detectors used for thefits ("Scat_Detector_Mask" in the Browse table) may not be the same asthe set of detectors that triggered GBM ("Bcat_Detector_Mask" in theBrowse table);3) background definitions are different for the bcat and scat analysis(see References below).Finally, for weak events, it is not always possible to perform duration orspectral analyses, and some bursts occur too close in time to South AtlanticAnomaly entries or exits by Fermi with resultant data truncations that preventbackground determinations for the duration analysis. There is not an exactone-to-one correspondence between those events for which the duration analysisfails and those which are too weak to have a useful spectral characterization.This means that in the HEASARC Browse table there are a handful of GRBs whichhave duration parameters but not spectral fit parameters, and vice versa. Inthese cases, blank entries in the table indicate missing values where ananalysis was not possible. Values of 0.0 for the uncertainties on spectralparameters indicate those parameters have been fixed in the fit from which otherparameters or quantities in the table were derived. Missing values for model fitparameters indicate that the fit failed to converge for this model. This istrue mostly for the more complicated models (SBPL or BAND) when the fits failto converge for weaker bursts. Bad spectral fits can often result inunphysical flux and fluence values with undefined errors. We include thesebad fits but leave the error fields blank when they contain undefined values.The selection criteria used in the first catalog (Goldstein et al. 2011) forthe determination of the best-fit spectral model are different from those inthe second catalog (Gruber et al. 2014). The results using the two methodson the sample included in Goldstein et al. (2011) are compared in Gruber etal. (2014). The old catalog files can be retrieved using the HEASARC ftparchive tree, under "previous" directories. The values returned by Browsealways come from the "current" directories. The chi-squared statistic was notused in the 2nd catalog, either for parameter optimization or modelcomparison. The chi-squared values are missing for a few GRBs. This isbelieved to be because of a known software issue and should not be consideredindicative of a bad fit.The variable "scatalog" included in the Browse tables and in the FITS filesindicates which catalog a file belongs to, with 2 being the current catalog,and 1 (or absent) the first catalog (preliminary values may appear with value0).Catalog Bibcodes2020ApJ...893...46V

2016ApJS..223...28N

2014ApJS..211...13V

2014ApJS..211...12GBulletinThe FERMIGBRST database table was last updated on 3 January 2024.CaveatsPlease see the warnings on the GBM Caveats page, _caveats.html.References * The fourth (current) catalog is described in von Kienlin, A. et al. 2020. * The third general catalog is described in Bhat, P. et al. 2016. * The current (second) spectral catalog is described in Gruber, D. et al. 2014. * The second general catalog is described in von Kienlin, A. et al. 2014. * The first general catalog is described in Paciesas, W.S. et al. 2011, ApJS, 199, 18. * The first spectral catalog is described in Goldstein, A. et al. 2011, ApJS, 199, 19.Also, see the Fermi Science Data Product Interface Control Document.ProvenanceThe information in this table is provided by the Fermi Gamma-ray BurstMonitor Instrument Operations Center (GIOC) and the Fermi Science SupportCenter (FSSC). The values come from burst and spectral catalog entry FITSfiles provided by the GIOC to the FSSC. These FITS files may containadditional data and are available for download. This table is updatedautomatically within a day or so of new data files being processed and madeavailable.ParametersTrigger_Name

The Fermi trigger designation that is assigned for each new trigger detected. The name is the same as the one used in the Trigger Catalog. The naming scheme used is bnyymmddfff, where yymmdd is the date of the burst (yy, the year minus 2000; mm, the two-digit month; and dd, the two-digit day of the month) and fff = fraction of day.Name

The designation of the source of the burst. The name will initially be GRByymmddfff, where yymmdd is the 2-digit year, month and day of the burst and fff the fraction of the day, as assigned by pipeline processing. The name will eventually be changed to the GRByymmddx format, where x is null or 'A' or 'B' etc. Re-naming to this format requires human intervention, noting whether another burst was detected on the same day.RA

The Right Ascension of the burst in the selected equinox. This was given in J2000 decimal degree coordinates in the original data.Dec

The Declination of the burst in the selected equinox. This was given in J2000 decimal degree coordinates in the original data.LII

The Galactic Longitude of the burst, derived from the burst RA and Dec.BII

The Galactic Latitude of the burst, derived from the burst RA and Dec.Error_Radius

This parameter is the uncertainty in the position, in degrees. A value of 0 means that the source localization was done using something other than Fermi GBM (for example, Swift, XMM, Chandra, etc.), so that the error radius is negligible by GBM standards. A value of 50 means that the localization is not well determined. As noted in footnote (22) of von Kienlin et al. (2014), this error is the statistical 1-sigma error; the GBM errors are not symmetric, and the given value is the average of the error ellipse.Trigger_Time

The time at which the trigger occurred, originally provided in Fermi Mission Elapsed Time (MET) format and converted to UTC.Duration_Energy_Low

The lower limit of duration integration, in keV. This is a parameter, nominally 50 keV.Duration_Energy_High

The upper limit of duration integration, in keV. This is a parameter, nominally 300 keV.Back_Interval_Low_Start

The start of the pre-burst background interval (in seconds relative to trigger time) used as a plateau for the duration calculation. This value might not be used for the spectral analysis.Back_Interval_Low_Stop

The end of the pre-burst background interval (in seconds relative to trigger time) used as a plateau for the duration calculation. This value might not be used for the spectral analysis.Back_Interval_High_Start

The start of the post-burst background interval (in seconds relative to trigger time) used as a plateau for the duration calculation. This value might not be used for the spectral analysis.Back_Interval_High_Stop

The end of the post-burst background interval (in seconds relative to trigger time) used as a plateau for the duration calculation. This value might not be used for the spectral analysis.T50

The duration, in seconds, during which 50% of the burst fluence was accumulated. The start of the T50 interval is defined by the time at which 25% of the total fluence has been detected, and the end of the T50 interval is defined by the time at which 75% of the fluence been detected. The fluence for the T50 calculation is measured between duration_energy_low and duration_energy_high.T50_Error

The 1-sigma statistical uncertainty in the T50 duration.T50_Start

The start of the T50 interval (in seconds) relative to the trigger time.T90

The duration, in seconds, during which 90% of the burst fluence was accumulated. The start of the T90 interval is defined by the time at which 5% of the total fluence has been detected, and the end of the T90 interval is defined by the time at which 95% of the fluence been detected. The fluence for the T90 calculation is measured between duration_energy_low and duration_energy_high.T90_Error

The 1-sigma statistical uncertainty in the T90 duration.T90_Start

The start of T90 interval (in seconds) relative to the trigger time.Bcat_Detector_Mask

A mask, or string of 14 boolean flags (either '0' or 1'), that indicates which detectors were included in the fits for the duration calculation, with '1' representing inclusion. The mask reads from left to right: NaI 0 to NaI 11, then BGO 0 and 1.Flu_Low

The lower limit of flux/fluence integration, in keV. This is a parameter, nominally 10 keV.Flu_High

The upper limit of flux/fluence integration, in keV. This is a parameter, nominally 1000 keV.Fluence

The fluence (flux integrated over the burst duration, 100% level) in the flu_low - flu_high energy band, nominally 10-1000 keV, in erg/cm2.Fluence_Error

The 1-sigma statistical uncertainty of the fluence in the in the flu_low - flu_high energy band, nominally 10-1000 keV, in erg/cm2.Fluence_BATSE

The fluence (flux integrated over the burst duration, 100% level) in the BATSE standard 50-300 keV energy band, in erg/cm2.Fluence_BATSE_Error

The 1-sigma statistical uncertainty of the fluence in the BATSE standard 50-300 keV energy band, in erg/cm2.Flux_1024

The peak flux in the flu_low - flu_high energy band, nominally 10-1000 keV, (1024ms timescale).Flux_1024_Error

The 1-sigma statistical uncertainty in the in the flu_low - flu_high energy band, nominally 10-1000 keV, peak flux (1024ms timescale).Flux_1024_Time

The start time (in seconds relative to trigger time) of the interval for the peak flux (1024 ms timescale) in the flu_low - flu_high energy band, nominally 10-1000 keV.Flux_64

The peak flux in the flu_low - flu_high energy band, nominally 10-1000 keV, (64ms timescale).Flux_64_Error

The 1-sigma statistical uncertainty in the in the flu_low - flu_high energy band, nominally 10-1000 keV, peak flux (64ms timescale).Flux_64_Time

The start time (in seconds relative to trigger time) of the interval for the peak flux (64 ms timescale) in the flu_low - flu_high energy band, nominally 10-1000 keV.Flux_256

The peak flux in the flu_low - flu_high energy band, nominally 10-1000 keV, (256 ms timescale).Flux_256_Error

The 1-sigma statistical uncertainty in the in the flu_low - flu_high energy band, nominally 10-1000 keV, peak flux (256 ms timescale).Flux_256_Time

The start time (in seconds relative to trigger time) of the interval for the peak flux (256 ms timescale) in the flu_low - flu_high energy band, nominally 10-1000 keV.Flux_BATSE_1024

The peak flux in the BATSE standard 50-300 keV energy band (1024 ms timescale).Flux_BATSE_1024_Error

The 1-sigma statistical uncertainty in the 50-300 keV peak flux (1024 ms timescale).Flux_BATSE_1024_Time

The start time (in seconds relative to trigger time) of the interval for the peak flux (1024 ms timescale) in the BATSE standard 50-300 keV energy band.Flux_BATSE_64

The peak flux in the BATSE standard 50-300 keV energy band (64 ms timescale).Flux_BATSE_64_Error

The 1-sigma statistical uncertainty in the 50-300 keV peak flux (64 ms timescale).Flux_BATSE_64_Time

The start time (in seconds relative to trigger time) of the interval for the peak flux (64 ms timescale) in the BATSE standard 50-300 keV energy band.Flux_BATSE_256

The peak flux in the BATSE standard 50-300 keV energy band (256 ms timescale).Flux_BATSE_256_Error

The 1-sigma statistical uncertainty in the 50-300 keV peak flux (256 ms timescale).Flux_BATSE_256_Time

The start time (in seconds relative to trigger time) of the interval for the peak flux (256 ms timescale) in the BATSE standard 50-300 keV energy band.Actual_64ms_Interval

The actual length of nominal 64ms timescale for peak flux measurement.Actual_256ms_Interval

The actual length of nominal 256ms timescale for peak flux measurement.Actual_1024ms_Interval

The actual length of nominal 1024ms timescale for peak flux measurement.Scat_Detector_Mask

A mask, or string of 14 boolean flags (either '0' or 1'), that indicates which detectors were included in the spectral catalog fits, with '1' representing inclusion. The mask reads from left to right: NaI 0 to NaI 11, then BGO 0 and 1.Pflx_Spectrum_Start

The start of the interval (in seconds relative to trigger time) used in the spectral fits over the time range of the peak flux of the burst.Pflx_Spectrum_Stop

The end of the interval (in seconds relative to trigger time) used in the spectral fits over the time range of the peak flux of the burst.Pflx_PLaw_Ampl

The amplitude of a power law fit to a single spectrum over the time range of the peak flux of the burst, in photon/cm2/s/keV.Pflx_PLaw_Ampl_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the power law fit amplitude for the peak flux spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Pflx_PLaw_Ampl_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the power law fit amplitude for the peak flux spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Pflx_PLaw_Pivot

The pivot energy of a power law fit to a single spectrum over the time range of the peak flux of the burst, in keV. This parameter is typically fixed.Pflx_PLaw_Pivot_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the pivot energy of a power law fit for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_PLaw_Pivot_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the pivot energy of a power law fit for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_PLaw_Index

The power law index of a power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_PLaw_Index_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the power index of a power law fit for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_PLaw_Index_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the power index of a power law fit for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_PLaw_Phtflux

The photon flux, in photon/cm2/s, for a power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_PLaw_Phtflux_Error

The 1-sigma statistical error on the photon flux, in photon/cm2/s, for the power law peak flux spectrum.Pflx_PLaw_Phtflnc

The photon fluence, in photon/cm2, for a power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_PLaw_Phtflnc_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2, for the power law peak flux spectrum.Pflx_PLaw_Ergflux

The energy flux, in erg/cm2/s, for a power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_PLaw_Ergflux_Error

The 1-sigma statistical error on the energy flux, in erg/cm2/s, for the power law peak flux spectrum.Pflx_PLaw_Ergflnc

The energy fluence in erg/cm2 for a power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_PLaw_Ergflnc_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2, for the power law peak flux spectrum.Pflx_PLaw_Phtfluxb

The photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for a power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_PLaw_Phtfluxb_Error

The 1-sigma statistical error on the photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for the power law peak flux spectrum.Pflx_PLaw_Phtflncb

The photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for a power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_PLaw_Phtflncb_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for the power law peak flux spectrum.Pflx_PLaw_Ergflncb

The energy fluence in erg/cm2 between 50 and 300 keV (BATSE standard) for a power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_PLaw_Ergflncb_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for the power law peak flux spectrum.Pflx_PLaw_Redchisq

The reduced chi-squared statistic for the power law fit to the peak flux spectrum. This may not be the statistic used to determine the best fit parameters (see pflx_plaw_statistic), but it is used for model comparison purposes. This value of reduced chi-squared is calculated for the best-fit parameters evaluated using the pflx_plaw_statistic statistic. Using these best-fit parameters, a model is considered the best-fit model if it yields the lowest chi-squared value by a margin of at least 6 units for each extra parameter in the model.Pflx_PLaw_Redfitstat

The reduced fitting statistic for the power law fit to the peak flux spectrum. This is the value of the statistic used to determine the best fit parameters, specified in pflx_plaw_statistic.Pflx_PLaw_DoF

The degrees of freedom for the power law fit to the peak flux spectrum.Pflx_PLaw_Statistic

The statistical merit function for the power law fit to the peak flux spectrum.Pflx_Comp_Ampl

The amplitude of a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst, in photon/cm2/s/keV.Pflx_Comp_Ampl_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Comptonized model amplitude for the peak flux spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Pflx_Comp_Ampl_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Comptonized model amplitude for the peak flux spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Pflx_Comp_Epeak

The peak energy of a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst, in keV.Pflx_Comp_Epeak_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Comptonized model peak energy for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_Comp_Epeak_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Comptonized model peak energy for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_Comp_Index

The power law index of a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Comp_Index_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Comptonized model power law index for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_Comp_Index_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Comptonized model power law index for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_Comp_Pivot

The pivot energy of a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst, in keV. This parameter is typically fixed.Pflx_Comp_Pivot_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Comptonized model pivot energy for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_Comp_Pivot_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Comptonized model pivot energy for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_Comp_Phtflux

The photon flux, in photon/cm2/s, for a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Comp_Phtflux_Error

The 1-sigma statistical error on the photon flux, in photon/cm2/s, for the Comptonized model peak flux spectrum.Pflx_Comp_Phtflnc

The photon fluence in photon/cm2 for a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Comp_Phtflnc_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2, for the Comptonized model peak flux spectrum.Pflx_Comp_Ergflux

The energy flux, in erg/cm2/s, for a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Comp_Ergflux_Error

The 1-sigma statistical error on the energy flux, in erg/cm2/s, for the Comptonized model peak flux spectrum.Pflx_Comp_Ergflnc

The energy fluence in erg/cm2 for a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Comp_Ergflnc_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2, for the Comptonized model peak flux spectrum.Pflx_Comp_Phtfluxb

The photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Comp_Phtfluxb_Error

The 1-sigma statistical error on the photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for the Comptonized model peak flux spectrum.Pflx_Comp_Phtflncb

The photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Comp_Phtflncb_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for the Comptonized model peak flux spectrum.Pflx_Comp_Ergflncb

The energy fluence in erg/cm2 between 50 and 300 keV (BATSE standard) for a Comptonized model fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Comp_Ergflncb_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for the Comptonized model peak flux spectrum.Pflx_Comp_Redchisq

The reduced chi-squared statistic for the Comptonized fit to the peak flux spectrum. This may not be the statistic used to determine the best fit parameters (see pflx_comp_statistic), but it is used for model comparison purposes. This value of reduced chi-squared is calculated for the best-fit parameters evaluated using the pflx_comp_statistic statistic. Using these best-fit parameters, a model is considered the best-fit model if it yields the lowest chi-squared value by a margin of at least 6 units for each extra parameter in the model.Pflx_Comp_Redfitstat

The reduced fitting statistic for the Comptonized model fit to the peak flux spectrum. This is the value of the statistic used to determine the best fit parameters, specified in pflx_comp_statistic.Pflx_Comp_DoF

The degrees of freedom for the Comptonized model fit to the peak flux spectrum.Pflx_Comp_Statistic

The statistical merit function for the Comptonized model fit to the peak flux spectrum.Pflx_Band_Ampl

The amplitude of a Band function fit to a single spectrum over the time range of the peak flux of the burst, in photon/cm2/s/keV.Pflx_Band_Ampl_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Band function amplitude for the peak flux spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Pflx_Band_Ampl_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Band function amplitude for the peak flux spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Pflx_Band_Epeak

The peak energy of a Band function fit to a single spectrum over the time range of the peak flux of the burst, in keV.Pflx_Band_Epeak_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Band function peak energy for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_Band_Epeak_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Band function peak energy for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_Band_Alpha

The power law index, alpha, of a Band function fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Band_Alpha_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the to the Band function power law, alpha, for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_Band_Alpha_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the to the Band function power law, alpha, for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_Band_Beta

The power law index, beta, of a Band function fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Band_Beta_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the to the Band function power law, beta, for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_Band_Beta_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the to the Band function power law, beta, for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_Band_Phtflux

The photon flux, in photon/cm2/s, for a Band function fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Band_Phtflux_Error

The 1-sigma statistical error on the photon flux, in photon/cm2/s, for the Band function peak flux spectrum.Pflx_Band_Phtflnc

The photon fluence, in photon/cm2, for a Band function fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Band_Phtflnc_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2, for the Band function peak flux spectrum.Pflx_Band_Ergflux

The energy flux, in erg/cm2/s, for a Band function fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Band_Ergflux_Error

The 1-sigma statistical error on the energy flux, in erg/cm2/s, for the Band function peak flux spectrum.Pflx_Band_Ergflnc

The energy fluence in erg/cm2 for a Band function fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Band_Ergflnc_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2, for the Band function peak flux spectrum.Pflx_Band_Phtfluxb

The photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for a Band function fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Band_Phtfluxb_Error

The 1-sigma statistical error on the photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for the Band function peak flux spectrum.Pflx_Band_Phtflncb

The photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for a Band function fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Band_Phtflncb_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for the Band function peak flux spectrum.Pflx_Band_Ergflncb

The energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for a Band function fit to a single spectrum over the time range of the peak flux of the burst.Pflx_Band_Ergflncb_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for the Band function peak flux spectrum.Pflx_Band_Redchisq

The reduced chi-squared statistic for the Band function fit to the peak flux spectrum. This may not be the statistic used to determine the best fit parameters (see pflx_band_statistic), but it is used for model comparison purposes. This value of reduced chi-squared is calculated for the best-fit parameters evaluated using the pflx_band_statistic statistic. Using these best-fit parameters, a model is considered the best-fit model if it yields the lowest chi-squared value by a margin of at least 6 units for each extra parameter in the model.Pflx_Band_Redfitstat

The reduced fitting statistic for the Band function fit to the peak flux spectrum. This is the value of the statistic used to determine the best fit parameters, specified in pflx_band_statistic.Pflx_Band_DoF

The degrees of freedom for the Band function fit to the peak flux spectrum.Pflx_Band_Statistic

The statistical merit function for the Band function fit to the peak flux spectrum.Pflx_SBPL_Ampl

The amplitude of a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst, in photon/cm2/s/keV.Pflx_SBPL_Ampl_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law amplitude for the peak flux spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Ampl_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law amplitude for the peak flux spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Pivot

The pivot energy of a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst, in keV. Typically this parameter is fixed.Pflx_SBPL_Pivot_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law pivot energy for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Pivot_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law pivot energy for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Indx1

The 1st power law of a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_SBPL_Indx1_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law 1st power law for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Indx1_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law 1st power law for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Brken

The break energy of a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst, in keV.Pflx_SBPL_Brken_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law break energy for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Brken_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law break energy for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Brksc

The break scale of a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst, in keV. Typically, this parameter is fixed.Pflx_SBPL_Brksc_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law break scale for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Brksc_Neg_Err

The 1-sigma statistical negative error giving the upper bound to the smoothly broken power law break scale for the peak flux spectrum, in keV. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Indx2

The second power law of a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_SBPL_Indx2_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law 2nd power law for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Indx2_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law 2nd power law for the peak flux spectrum. An error of 0.0 implies a fixed parameter.Pflx_SBPL_Phtflux

The photon flux, in photon/cm2/s, for a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_SBPL_Phtflux_Error

The 1-sigma statistical error on the photon flux, in photon/cm2/s, for the smoothly broken power law peak flux spectrum.Pflx_SBPL_Phtflnc

The photon fluence in photon/cm2 for a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_SBPL_Phtflnc_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2, for the smoothly broken power law peak flux spectrum.Pflx_SBPL_Ergflux

The energy flux, in erg/cm2/s, for a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_SBPL_Ergflux_Error

The 1-sigma statistical error on the energy flux, in erg/cm2/s, for the smoothly broken power law peak flux spectrum.Pflx_SBPL_Ergflnc

The energy fluence, in erg/cm2, for a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_SBPL_Ergflnc_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2, for the smoothly broken power law peak flux spectrum.Pflx_SBPL_Phtfluxb

The photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_SBPL_Phtfluxb_Error

The 1-sigma statistical error on the photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for the smoothly broken power law peak flux spectrum.Pflx_SBPL_Phtflncb

The photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_SBPL_Phtflncb_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for the smoothly broken power law peak flux spectrum.Pflx_SBPL_Ergflncb

The energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for a smoothly broken power law fit to a single spectrum over the time range of the peak flux of the burst.Pflx_SBPL_Ergflncb_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for the smoothly broken power law peak flux spectrum.Pflx_SBPL_Redchisq

The reduced chi-squared statistic for the smoothly broken power law fit to the peak flux spectrum. This may not be the statistic used to determine the best fit parameters (see pflx_sbpl_statistic), but it is used for model comparison purposes. This value of reduced chi-squared is calculated for the best-fit parameters evaluated using the pflx_sbpl_statistic statistic. Using these best-fit parameters, a model is considered the best-fit model if it yields the lowest chi-squared value by a margin of at least 6 units for each extra parameter in the model.Pflx_SBPL_Redfitstat

The reduced fitting statistic for the smoothly broken power law fit to the peak flux spectrum. This is the value of the statistic used to determine the best fit parameters, specified in pflx_sbpl_statistic.Pflx_SBPL_DoF

The degrees of freedom for the smoothly broken power law fit to the peak flux spectrum.Pflx_SBPL_Statistic

The statistical merit function for the smoothly broken power law fit to the peak flux spectrum.Pflx_Best_Fitting_Model

The model which best fits the data for a spectrum accumulated over the peak flux of the burst. The determination of the best fitting model compares the values of the likelihood-based statistic CSTAT (or other statistic defined in pflx_xxxx_statistic) among the tested models. The COMP model is preferred over the PLAW model if there is a decrease in 8.58 units of CSTAT. The BAND or SBPL models are preferred over the COMP model if there is a decrease in 11.83 units of CSTAT, then the lower of BAND and SBPL is selected as best. For a model to be selected as best, its parameters must be well-determined, as follows: the low-energy power-law index must be known to at least 0.4 (68% CL); the high-energy power-law index within 1.0; all other parameters within 40% of their value.Pflx_Best_Model_Redchisq

The reduced chi-squared statistic for the model that provides the best fit to the peak flux spectrum using the parameters optimized using pfl_xxxx_statistic. This is not the statistic used to determine the best fit parameters but is provided as a "goodness-of-fit" estimate for the model.Flnc_Spectrum_Start

The start of the interval (in seconds relative to trigger time) used in the spectral fits over the duration of the burst.Flnc_Spectrum_Stop

The end of the interval (in seconds relative to trigger time) used in the spectral fits over the duration of the burst.Flnc_PLaw_Ampl

The amplitude of a power law fit to a single spectrum over the duration of the burst, in photon/cm2/s/keV.Flnc_PLaw_Ampl_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the power law fit amplitude for the fluence spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Flnc_PLaw_Ampl_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the power law fit amplitude for the fluence spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Flnc_PLaw_Pivot

The pivot energy of a power law fit to a single spectrum over the duration of the burst, in keV. This parameter is typically fixed.Flnc_PLaw_Pivot_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the pivot energy of a power law fit for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_PLaw_Pivot_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the pivot energy of a power law fit for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_PLaw_Index

The power law index of a power law fit to a single spectrum over the duration of the burst.Flnc_PLaw_Index_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the power index of a power law fit for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_PLaw_Index_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the power index of a power law fit for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_PLaw_Phtflux

The average photon flux, in photon/cm2/s, for a power law fit to a single spectrum over the duration of the burst.Flnc_PLaw_Phtflux_Error

The 1-sigma statistical error on the average photon flux, in photon/cm2/s, for the power law fluence spectrum.Flnc_PLaw_Phtflnc

The photon fluence, in photon/cm2, for a power law fit to a single spectrum over the duration of the burst.Flnc_PLaw_Phtflnc_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2, for the power law fluence spectrum.Flnc_PLaw_Ergflux

The average energy flux, in erg/cm2/s, for a power law fit to a single spectrum over the duration of the burst.Flnc_PLaw_Ergflux_Error

The 1-sigma statistical error on the average energy flux, in erg/cm2/s, for the power law fluence spectrum.Flnc_PLaw_Ergflnc

The energy fluence, in erg/cm2, for a power law fit to a single spectrum over the duration of the burst.Flnc_PLaw_Ergflnc_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2, for the power law fluence spectrum.Flnc_PLaw_Phtfluxb

The average photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for a power law fit to a single spectrum over the duration of the burst.Flnc_PLaw_Phtfluxb_Error

The 1-sigma statistical error on the average photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for the power law fluence spectrum.Flnc_PLaw_Phtflncb

The photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for a power law fit to a single spectrum over the duration of the burst.Flnc_PLaw_Phtflncb_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for the power law fluence spectrum.Flnc_PLaw_Ergflncb

The energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for a power law fit to a single spectrum over the duration of the burst.Flnc_PLaw_Ergflncb_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for the power law fluence spectrum.Flnc_PLaw_Redchisq

The reduced chi-squared statistic for the power law fit to the fluence spectrum. This may not be the statistic used to determine the best fit parameters (see flnc_plaw_statistic), but it is used for model comparison purposes. This value of reduced chi-squared is calculated for the best-fit parameters evaluated using the flnc_plaw_statistic statistic. Using these best-fit parameters, a model is considered the best-fit model if it yields the lowest chi-squared value by a margin of at least 6 units for each extra parameter in the model.Flnc_PLaw_Redfitstat

The reduced fitting statistic for the power law fit to the fluence spectrum. This is the value of the statistic used to determine the best fit parameters, specified in flnc_plaw_statistic.Flnc_PLaw_DoF

The degrees of freedom for the power law fit to the fluence spectrum.Flnc_PLaw_Statistic

The statistical merit function for the power law fit to the fluence spectrum.Flnc_Comp_Ampl

The amplitude of a Comptonized model fit to a single spectrum over the duration of the burst, in photon/cm2/s/keV.Flnc_Comp_Ampl_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Comptonized model amplitude for the fluence spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Flnc_Comp_Ampl_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Comptonized model amplitude for the fluence spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Flnc_Comp_Epeak

The peak energy of a Comptonized model fit to a single spectrum over the duration of the burst, in keV.Flnc_Comp_Epeak_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Comptonized model peak energy for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_Comp_Epeak_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Comptonized model peak energy for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_Comp_Index

The power law index of a Comptonized model fit to a single spectrum over the duration of the burst.Flnc_Comp_Index_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Comptonized model power law index for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_Comp_Index_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Comptonized model power law index for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_Comp_Pivot

The pivot energy of a Comptonized model fit to a single spectrum over the duration of the burst, in keV. This parameter is typically fixed.Flnc_Comp_Pivot_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Comptonized model pivot energy for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_Comp_Pivot_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Comptonized model pivot energy for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_Comp_Phtflux

The average photon flux, in photon/cm2/s, for a Comptonized model fit to a single spectrum over the duration of the burst.Flnc_Comp_Phtflux_Error

The 1-sigma statistical error on the average photon flux, in photon/cm2/s, for the Comptonized model fluence spectrum.Flnc_Comp_Phtflnc

The photon fluence, in photon/cm2, for a Comptonized model fit to a single spectrum over the duration of the burst.Flnc_Comp_Phtflnc_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2, for the power law fluence spectrum.Flnc_Comp_Ergflux

The average energy flux, in erg/cm2/s, for a Comptonized model fit to a single spectrum over the duration of the burst.Flnc_Comp_Ergflux_Error

The 1-sigma statistical error on the average energy flux, in erg/cm2/s, for the Comptonized model fluence spectrum.Flnc_Comp_Ergflnc

The energy fluence, in erg/cm2, for a Comptonized model fit to a single spectrum over the duration of the burst.Flnc_Comp_Ergflnc_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2, for the power law fluence spectrum.Flnc_Comp_Phtfluxb

The average photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for a Comptonized model fit to a single spectrum over the duration of the burst.Flnc_Comp_Phtfluxb_Error

The 1-sigma statistical error on the average photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for the Comptonized model fluence spectrum.Flnc_Comp_Phtflncb

The photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for a Comptonized model fit to a single spectrum over the duration of the burst.Flnc_Comp_Phtflncb_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for the power law fluence spectrum.Flnc_Comp_Ergflncb

The energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for a Comptonized model fit to a single spectrum over the duration of the burst.Flnc_Comp_Ergflncb_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for the power law fluence spectrum.Flnc_Comp_Redchisq

The reduced chi-squared statistic for the Comptonized model fit to the fluence spectrum. This may not be the statistic used to determine the best fit parameters (see flnc_comp_statistic), but it is used for model comparison purposes. This value of reduced chi-squared is calculated for the best-fit parameters evaluated using the flnc_comp_statistic statistic. Using these best-fit parameters, a model is considered the best-fit model if it yields the lowest chi-squared value by a margin of at least 6 units for each extra parameter in the model.Flnc_Comp_Redfitstat

The reduced fitting statistic for the Comptonized model fit to the fluence spectrum. This is the value of the statistic used to determine the best fit parameters, specified in flnc_comp_statistic.Flnc_Comp_DoF

The degrees of freedom for the Comptonized model fit to the fluence spectrum.Flnc_Comp_Statistic

The statistical merit function for the Comptonized model fit to the fluence spectrum.Flnc_Band_Ampl

The amplitude of a Band function fit to a single spectrum over the duration of the burst, in photon/cm2/s/keV.Flnc_Band_Ampl_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Band function amplitude for the fluence spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Flnc_Band_Ampl_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Band function amplitude for the fluence spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Flnc_Band_Epeak

The peak energy of a Band function fit to a single spectrum over the duration of the burst, in keV.Flnc_Band_Epeak_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the Band function peak energy for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_Band_Epeak_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the Band function peak energy for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_Band_Alpha

The power law index, alpha, of a Band function fit to a single spectrum over the duration of the burst.Flnc_Band_Alpha_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the to the Band function power law, alpha, for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_Band_Alpha_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the to the Band function power law, alpha, for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_Band_Beta

The power law index, beta, of a Band function fit to a single spectrum over the duration of the burst.Flnc_Band_Beta_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the to the Band function power law, beta, for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_Band_Beta_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the to the Band function power law, beta, for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_Band_Phtflux

The average photon flux, in photon/cm2/s, for a Band function law fit to a single spectrum over the duration of the burst.Flnc_Band_Phtflux_Error

The 1-sigma statistical error on the average photon flux, in photon/cm2/s, for the Band function fluence spectrum.Flnc_Band_Phtflnc

The photon fluence, in photon/cm2, for a Band function fit to a single spectrum over the duration of the burst.Flnc_Band_Phtflnc_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2, for the Band function peak flux spectrum.Flnc_Band_Ergflux

The average energy flux, in erg/cm2/s, for a Band function law fit to a single spectrum over the duration of the burst.Flnc_Band_Ergflux_Error

The 1-sigma statistical error on the average energy flux, in erg/cm2/s, for the Band function fluence spectrum.Flnc_Band_Ergflnc

The energy fluence, in erg/cm2, for a Band function fit to a single spectrum over the duration of the burst.Flnc_Band_Ergflnc_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2, for the Band function peak flux spectrum.Flnc_Band_Phtfluxb

The average photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for a Band function law fit to a single spectrum over the duration of the burst.Flnc_Band_Phtfluxb_Error

The 1-sigma statistical error on the average photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for the Band function fluence spectrum.Flnc_Band_Phtflncb

The photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for a Band function fit to a single spectrum over the duration of the burst.Flnc_Band_Phtflncb_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for the Band function peak flux spectrum.Flnc_Band_Ergflncb

The energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for a Band function fit to a single spectrum over the duration of the burst.Flnc_Band_Ergflncb_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for the Band function peak flux spectrum.Flnc_Band_Redchisq

The reduced chi-squared statistic for the Band function fit to the fluence spectrum. This may not be the statistic used to determine the best fit parameters (see flnc_band_statistic), but it is used for model comparison purposes. This value of reduced chi-squared is calculated for the best-fit parameters evaluated using the flnc_band_statistic statistic. Using these best-fit parameters, a model is considered the best-fit model if it yields the lowest chi-squared value by a margin of at least 6 units for each extra parameter in the model.Flnc_Band_Redfitstat

The reduced fitting statistic for the Band function fit to the fluence spectrum. This is the value of the statistic used to determine the best fit parameters, specified in flnc_band_statistic.Flnc_Band_DoF

The degrees of freedom for the Band function fit to the fluence spectrum.Flnc_Band_Statistic

The statistical merit function for the Band function fit to the fluence spectrum.Flnc_SBPL_Ampl

The amplitude of a smoothly broken power law fit to a single spectrum over the duration of the burst, in photon/cm2/s/keV.Flnc_SBPL_Ampl_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law fit amplitude for the fluence spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Ampl_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law fit amplitude for the fluence spectrum, in photon/cm2/s/keV. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Pivot

The pivot energy of a smoothly broken power law fit to a single spectrum over the duration of the burst, in keV. Typically this parameter is fixed.Flnc_SBPL_Pivot_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law pivot energy for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Pivot_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law pivot energy for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Indx1

The 1st power law of a smoothly broken power law fit to a single spectrum over the duration of the burst.Flnc_SBPL_Indx1_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law 1st power law for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Indx1_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law 1st power law for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Brken

The break energy of a smoothly broken power law fit to a single spectrum over the duration of the burst, in keV.Flnc_SBPL_Brken_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law break energy for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Brken_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law break energy for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Brksc

The break scale of a smoothly broken power law fit to a single spectrum over the duration of the burst, in keV. Typically, this parameter is fixed.Flnc_SBPL_Brksc_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law break scale for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Brksc_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law break scale for the fluence spectrum, in keV. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Indx2

The second power law of a smoothly broken power law fit to a single spectrum over the duration of the burst.Flnc_SBPL_Indx2_Pos_Err

The 1-sigma statistical positive error giving the upper bound to the smoothly broken power law 2nd power law for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Indx2_Neg_Err

The 1-sigma statistical negative error giving the lower bound to the smoothly broken power law 2nd power law for the fluence spectrum. An error of 0.0 implies a fixed parameter.Flnc_SBPL_Phtflux

The average photon flux, in photon/cm2/s, for a smoothly broken power law fit to a single spectrum over the duration of the burst.Flnc_SBPL_Phtflux_Error

The 1-sigma statistical error on the average photon flux, in photon/cm2/s, for the smoothly broken power law fluence spectrum.Flnc_SBPL_Phtflnc

The photon fluence, in photon/cm2, for a smoothly broken power law fit to a single spectrum over the duration of the burst.Flnc_SBPL_Phtflnc_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2, for the smoothly broken power law fluence spectrum.Flnc_SBPL_Ergflux

The average energy flux, in erg/cm2/s, for a smoothly broken power law fit to a single spectrum over the duration of the burst.Flnc_SBPL_Ergflux_Error

The 1-sigma statistical error on the average energy flux, in erg/cm2/s, for the smoothly broken power law fluence spectrum.Flnc_SBPL_Ergflnc

The energy fluence, in erg/cm2, for a smoothly broken power law fit to a single spectrum over the duration of the burst.Flnc_SBPL_Ergflnc_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2, for the smoothly broken power law fluence spectrum.Flnc_SBPL_Phtfluxb

The average photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for a smoothly broken power law fit to a single spectrum over the duration of the burst.Flnc_SBPL_Phtfluxb_Error

The 1-sigma statistical error on the average photon flux, in photon/cm2/s between 50 and 300 keV (BATSE standard), for the smoothly broken power law fluence spectrum.Flnc_SBPL_Phtflncb

The photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for a smoothly broken power law fit to a single spectrum over the duration of the burst.Flnc_SBPL_Phtflncb_Error

The 1-sigma statistical error in the photon fluence, in photon/cm2 between 50 and 300 keV (BATSE standard), for the smoothly broken power law fluence spectrum.Flnc_SBPL_Ergflncb

The energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for a smoothly broken power law fit to a single spectrum over the duration of the burst.Flnc_SBPL_Ergflncb_Error

The 1-sigma statistical error in the energy fluence, in erg/cm2 between 50 and 300 keV (BATSE standard), for the smoothly broken power law fluence spectrum.Flnc_SBPL_Redchisq

The reduced chi-squared statistic for the smoothly broken power law fit to the fluence spectrum. This may not be the statistic used to determine the best fit parameters (see flnc_sbpl_statistic), but it is used for model comparison purposes. This value of reduced chi-squared is calculated for the best-fit parameters evaluated using the flnc_sbpl_statistic statistic. Using these best-fit parameters, a model is considered the best-fit model if it yields the lowest chi-squared value by a margin of at least 6 units for each extra parameter in the model.Flnc_SBPL_Redfitstat

The reduced fitting statistic for the smoothly broken power law fit to the fluence spectrum. This is the value of the statistic used to determine the best fit parameters, specified in flnc_sbpl_statistic.Flnc_SBPL_DoF

The degrees of freedom for the smoothly broken power law fit to the fluence spectrum.Flnc_SBPL_Statistic

The statistical merit function for the smoothly broken power law fit to the fluence spectrum.Flnc_Best_Fitting_Model

The model which best fits the data for a spectrum accumulated over the duration of the burst. The determination of the best fitting model compares the values of the likelihood-based statistic CSTAT (or other statistic defined in flnc_xxxx_statistic), among the tested models. The COMP model is preferred over the PLAW model if there is a decrease in 8.58 units of CSTAT. The BAND or SBPL models are preferred over the COMP model if there is a decrease in 11.83 units of CSTAT, then the lower of BAND and SBPL is selected as best. For a model to be selected as best, its parameters must be well-determined, as follows: the low-energy power-law index must be known to at least 0.4 (68% CL); the high-energy power-law index within 1.0; all other parameters within 40% of their value.Flnc_Best_Model_Redchisq

The reduced chi-squared statistic for the model that provides the best fit to the fluence spectrum using the parameters optimized using flnc_xxxx_statistic. This is not the statistic used to determine the best fit parameters but is provided as a "goodness-of-fit" estimate for the model.Bcatalog

The burst catalog version of the file: zero for preliminary (unpublished) data, integer value (1, 2, 3, etc.) for official catalog releases.Scatalog

The spectral catalog version of the file: zero for preliminary (unpublished) data, integer value (1, 2, 3, etc.) for official catalog releases.Last_Modified

The time (in UTC) of the last modification to the burst information.Contact PersonQuestions regarding the FERMIGBRST database table can be addressed to theHEASARC User Hotline.Page Author: Browse Software Development Team

Last Modified: Monday, 01-Jun-2020 17:12:25 EDT A service of the Astrophysics Science Division at NASA/GSFC. 17dc91bb1f