BAT Digest

The pre-launch BAT spectral response file contained significant systematic errors. The response matrix model published with the public Swift software includes extra corrections to force the Crab to fit a canonical model, a power law with photon index 2.15 and normalization of 10.17 ph/cm²/s/keV at 1 keV. Figure 1 shows a fit to the Crab using the corrected response matrix and the estimated systematic error vector.

Corrections to Response

The extra corrections are: (a) addition of empirical absorption which shifts the low energy effective area by ~40% below 25 keV, and (b) a phenomenological adjustment to the effective area over the entire energy range, but which dominated at high energies (~20% for > 100 keV). Figure 2 shows the extent of these corrections in the BAT energy band. While it is believed that these errors are in part due to incorrect modeling of all the passive material in the beam, the exact details are not well understood.

Residual Features

Features at 17, 27, and 31 keV are still evident in Figure 3. The BAT CdZnTe detectors have K-edges at 27 keV (Cd) and at 31 keV (Te). The response matrix does not yet entirely account for spectral features resulting from these edges, so any such features at these energies should be interpreted with caution. There is also an as-yet unidentified feature at 17 keV.

Flux and Photon Index Systematic Errors

Systematic flux and spectral variations as a function of off-axis angle, theta, are shown in Figures 4 and 5 (as of version 008 of the response matrix parameter file). The Crab was observed using a set of 44 grid locations in the BAT FOV (including on-axis, and periodic spacings in tangent plane coordinates all the way out to the 0%-code edge of our field of view). The flux variations are approximately +/-5% peak to peak throughout the field of view. The user must be careful to avoid occultation by the earth/moon for off-axis angles larger than 30 degrees (see the "Occultation" analysis issue). Response matrices were generated for these fits using batdrmgen with the default method=MEAN parameter.

Hard Spectra

The response matrix was generated (a) from a set of ground calibrations with monochromatic lines from radioactive sources and (b) from a forced-adjustment fit to the canonical Crab spectrum (PLI=2.15, Norm=10.17). Given the deviation from ideal discussed above, we recommend caution when fitting sources that have significantly harder spectra than the Crab, in particular GRBs having spectral indices around 1.0 or flatter. While they were to some extent adjusted to match the Crab spectra, the large off-diagonal elements in the response matrix may not be correctly handling the scattering.

However, the fit to GRB 041223 shows the spectrum to be well fit by a simple power-law model, and the residuals show no sign of any bend in the spectrum (Figure 6). Also, the BAT spectrum for GRB 050326 agrees well with the KONUS spectrum (GCN Circ. #3152) for that burst (Figure 7).

Energy Range

Spectral analysis should be limited to channels between 14 keV and 150 keV. Due to varying threshold levels in individual detectors, channels below 14 keV should not be used for spectral anaylysis. Likewise, channels above 150 keV are unreliable due to a lack of calibration data at those energies.

Effective Area

Figure 8 shows the effective area for a source (a) on axis, and (b) a source 45 deg off-axis. This effective area contains the Mask transmission and the 56% efficiency factor due to the cross-correlation technique used for imaging and mask weighted flux determination. Edge features include 25.5 keV (Ag), 26.7 keV (Cd), 31.8 keV (Te), and 88 keV (Pb). The extra silver absorption used to fit the Crab may have produced an unrealistically pronounced silver K edge in the matrix.

Users can also estimate BAT count rates on-line using WebPIMMS.

The BAT team has delivered a systematic error vector to be used for all spectral fitting activities. Figure 9 shows this error as a function of energy. The error vector is a FITS file in CALDB containing a fractional systematic error SYS_ERR, and instructions are provided for applying this vector in the Science Analysis Issues section.

This systematic vector was constructed by assuming the correction vector was a constant fraction of the matrix corrections applied, with a minimum of 4% for the entire energy range. The error fraction was determined iteratively, in order to make the parameters derived from Crab on-axis and 30 degrees off-axis agree to within 1-2 sigma.

Users must use the following tools to obtain the correct energy scale:

1. bateconvert for event data (i.e. GRB data).

2. baterebin for binned data (i.e. survey DPH data).

Both of these tools apply a detector-dependent energy shift which accounts for the non-linear behavior of the detector electronics, as well as detector-to-detector offset shifts not currently accounted for by the on-board automatic calibration.

Figure 10 shows an on-board calibration spectrum with identified lines.

Without the correction, users can expect +/- 2 keV errors (90%, with maximum errors of 10 keV), and increased noise in detector images due to detector-to-detector gain variations.

With correction, users can expect +/- 0.1 keV errors. Figure 11 shows the on-board calibration spectrum after correction. The line centroids are consistent to within 0.1 keV, and the widths are consistent with the broadening derived by ground calibration.

WARNING: The SDC currently does not supply all of the gain/offset files required for energy correction of survey DPHs. Only the first gain/offset map is provided at the start of the observation, when in fact multiple calibrations can occur between snapshots. This will affect long observations the most. However, the gain behavior of the instrument does not appear to be a strong function of time. Using the first gain/offset map will degrade the energy scale, but only slightly.

Please use the newest software and calibration files, since these contain improvements to the energy scale. For event data, it is worthwhile to re-apply the correction since the SDC may not always be using the most recent software or calibration files.

As described above, and in Figure 10, the resolution is as expected from modeling of the ground calibration data. For example, the FWHM of the ²⁴¹Am line at 60 keV is <4 keV.

BAT positions are derived by generating a sky image using batfftimage and then fitting a point spread function to detected sources using batcelldetect. The BAT-to-spacecraft alignment was analyzed and checked using BAT observations detected in survey mode from approximately 2004-12-15 to 2005-01-15. The alignment data are stored in the BAT teldef and aperture files, and include rotation and focal length adjustments.

The residuals from the alignment calibration provide information on the centroiding error of the BAT. The residuals in Figure 12 were fit to a power law as a function of signal to noise. The best fit is:

      ERR_RAD = K x 6.1 SNR^(-0.7)   [arcmin; radius]  (equation 1)

where SNR is the signal to noise ratio reported by either batcelldetect or the BAT position message sent by TDRSS. This function is applicable for 6 < SNR < 100, but is poorly tested for partial coding fractions of less than ~25%.

For specific confidence limits, please use the values for K in Table 1. Also, representative error radii are given for 10 sigma and 20 sigma detections.

As of Spring 2006, it is now known that there are small scale but systematic image centroid shifts as a function of position in the BAT field of view. Based on 9 months of data from 2004-12-15 to 2005-09-15, the measured positions of known sources were compared to the known positions. The position offsets were preserved in instrument tangent-plane coordinates, and grouped by position in the field of view.

Figure 12 shows the resulting measured position offsets. This figure shows that beyond 45 degrees (IMR > 1), there are significant residuals, and within that angle, the residuals are negligible. The maximum residual offset is about 2 arcmin. Note that this effect is commonly only seen for very bright sources, or by averaging several faint source positions together.

The offsets appear to show a systematic but non-regular pattern. The current aperture+teldef model appears to help some, but does not remove the systematic offsets. Thus, a systematic distortion map was developed. This map is a thin-plate spline approximation to the measured offsets, which smooths over the noise in Figure 12, and interpolates between gaps. The resulting spline function is sampled on a regular grid and stored in the swbdistort* file. This file is used by source detection and mask weighting (ray tracing) tasks to produce more accurate fluxes and positions.

As shown, BAT point spread function is approximately a gaussian. The measured width of the point spread function is 22.5 arcminutes (FWHM on-axis). In tangent plane coordinates, the PSF shape is very uniform across the BAT field of view; i.e. the FWHM is tan(22.5') = 0.0065 in image coordinates. Figure 13 shows the point spread function for a bright source at two oversampling levels.

As a source moves farther off axis, the transformation between tangent projection and true spherical angles becomes more distorted. The width of the point spread function follows this model:

   FWHM_X = 22.5' / (1 + IMX^2)
   FWHM_Y = 22.5' / (1 + IMY^2)

where IMX and IMY are the tangent plane coordinates. This distortion occurs in celestial coordinates. The PSF shape and width are unchanged in instrument tangent plane coordinates.

BAT Timing: power spectrum problems with BAT event data

Event data from the BAT instrument is available for most gamma-ray bursts, failed triggers, and some special circumstances. There are cases where users may wish to search for periodic signatures, such as with a power spectrum analyais, or some other sensitive timing technique.

BAT time-stamps have a quantization of 100 microseconds, based on the BAT internal clock time resolution. This means that event times, expressed in MET, should be exact multiples of 100 microseconds.

However, the quantity 1 x 10^-4, and its multiples, and not exactly representable in the standard floating point representation used in FITS files and in most computers. In reality, BAT event times will not fall exactly on a 100 microsecond time marker. This effect is basically related to round-off error, and has a periodic structure over time (i.e. it is not random).

When software such as batbinevt or extractor attempts to make a light curve from this data, it will assign each event to a time bin based on its time value. Because of the round-off error effect noted above, events will be assigned to the wrong bin, in a systematically periodic way. The effect will be the strongest when users choose 100 microsecond time bins. A power spectrum of this light curve will produce many spurious "signals," as shown below.

Figure. Power spectrum of BAT event data, showing spurious signals produced by round-off problems.

In fact, this problem can apply to any mission. For RXTE, the most commonly used high resolution timing mission, time-stamp values are always a multiple of a power of 2, which is exactly representable in a computer. Other instruments, with other quantizations, will have this problem as well, but typically do not have the right count rates to produce visible artifacts.

WORKAROUND: The problem basically arises because events fall almost on multiples of 100 microsecond, but not exactly. Assuming that one chooses time bins which are a multiple of 100 microseconds, a workaround to the problem is to add a small offset time to each event before performing timing analysis. Our experiments show that a 5 microsecond offset is sufficient to remove the artifacts. The science is totally unaffected, since the offset of 5 microseconds is twenty times smaller than the event time quantization.

Here is an example command that will add 5 microseconds to each of the event time stamps in a file called old.evt, and saves the result in a file called new.evt.

ftcopy old.evt'[col *; TIME=TIME+5e-6]' new.evt

After doing so, the artifacts vanish, as shown below.

Figure. BAT power spectrum after applying a 5 microsecond time offset. The spurious signals have vanished.

A more generic solution is to add a random number between 0 and 100 microseconds for each event, which allows any arbitrary time bin size.

The BAT team is working with the SDC in order to apply a workaround correction automatically.

battblocks: duration uncertainties are unreliable

NOTE: this problem has been fixed in HEASoft version 6.4 (released December 2007).

Users can estimate gamma-ray burst durations such as "T50" and "T90" using the software task 'battblocks'. The T50 and T90 values are stored in the output file in the keywords T50DUR and T90DUR.

The task also provides estimates of the uncertainties in T50 and T90. However, the BAT team currently believes that these estimated uncertainties are too small, and cannot be relied upon.

Throughout the mission, the BAT team has estimated the uncertainties by visual inspection.

CALDB: BAT imaging tools need new teldef files

BAT imaging tools use a "TELDEF" file to describe the misalignment between the spacecraft and instrument coordinate systems. In the process of recovering from the safe-hold episode of Aug 2007, the Swift spacecraft coordinate system was redefined. The nature of the change was primarily in spacecraft "roll" angle, and the magnitude of the change was about 10 arcminutes.

As a result of this spacecraft-level redefinition, BAT data taken after August 28, 2007, will show systematic image shifts, especially in the outer parts of the field of view where the effect of a "roll" is greatest. (The shift should be approximately (10.6 arcmin)xsin(theta), where theta is the off-axis angle.)

New versions of the BAT TELDEF files are available which correct for the shift. They are available from the Swift CALDB area (BAT version 20070924 or later). Users of CALDB do not need to make any changes to their software or scripts, since the TELDEF files are indexed by observation time.

SPECIAL NOTE: The tool 'batmaskwtimg' may produce the wrong raytraced image after these CALDB changes. By default, this task does not require an input file (although the optional 'infile' parameter can be used). When no input is given, batmaskwtimg assumes the observation time is today. While this was not a problem up to August 2007, since the teldef file had not chainged up to that point, it will obviously fail for old observations processed with new teldef files today. This failure is silent. The workaround is to supply an input file. The next release of batmaskwtimg will make 'infile' a required parameter. Since the batmaskwtimg task has never been required for GRB analysis, it is likely that this interface change would have a low impact, and obviously would help the results to be more correct.

Analysis: Passive materials distort the off-axis counts/rates

The BAT image system works by forming shadow patterns cast by the mask onto the detector array. The mask is made from lead tiles. However, the mask support structure also contains significant absorbing materials. The edge of the support structure is a particular problem because (a) extra absorbing materials (e.g. epoxy) were applied, and (b) this material rises up above the plane of the mask. The net result is that for sensitive imaging and spectroscopy of off-axis sources, the full mask aperture cannot be used.

The BAT team has provided a new set of aperture files in CALDB, tied to the HEASoft 6.0.3 release. These apertures have been reduced in size to appropriately block out the shadows of most of the absorbing material. However, this does reduce solid angle sky coverage by 5-10%.

The aperture files are now divided into two classes:

• FLUX - reduced aperture for sensitive flux measurements (DEFAULT)

• DETECTION - full aperture for largest solid angle and most illuminated detectors, but reduced flux accuracy

We should note that the differences between these apertures are small. The "old" DETECTION apertures can still be used if desired, but the FLUX apertures are likely to be what most users want, and are thus the default. The aperture type is selectable in the raytracing tasks using aperture=CALDB:FLUX or aperture=CALDB:DETECTION.

batfftimage and batmaskwtimg: potentially incorrect derived attitude

Two imaging tasks assume that the spacecraft attitude is fixed during an observation: batfftimage (to make sky images) and batmaskwtimg (to make mask weighting maps for flux extraction). Both tasks take the time at the midpoint of the observation.

If there are gaps in the observation, i.e. multiple snapshots, then it is possible, even likely, that the midpoint time will fall within a gap. When this happens, the attitude may be erroneously interpolated.

The recommended solution is to use the 'aspect' tool to generate a revised attitude file. As of HEASoft 6.0, 'aspect' can create a new attitude file based on the median pointing direction during the observation good times only. You will also need to supply a good time interval extension to 'aspect', which should be available in the detector or sky images.

The 'aspect' command is:

aspect swNNNNNNNNNNNsat.fits none detimage.dpi'[STDGTI]' newattfile=detimage.att

where swNNNNNNNNNNNsat.fits is the spacecraft attitude file, detimage.dpi is the detector plane image (which should contain a GTI extension named STDGTI), and detimage.att is the new attitude file valid for the detimage.dpi only.

In the future the BAT team will investigate how feasible it is to incorporate 'aspect'-like functionality into the BAT imaging tools.

Updated (19 May 2005) - to recommend only the 'aspect' solution.
Updated (15 Oct 2005) - both batfftimage and batmaskwtimg now analyze the midpoint of the time interval

Analysis: Earth and Moon Occultation

The BAT field of view is large, approximately 120 x 60 degrees fully coded. The current spacecraft constraint excludes the sun with a 45 deg constraint cone, and the earth limb and moon with 30 degree constraints each.

Even so, the Earth and Moon may enter the BAT field of view. This will most commonly occur at edges of the "long" BAT axis (i.e. large IMX in the image plane). The effect will be to occult the flux of sources in that part of the sky. Since the Moon and (primarily) the Earth move as a function of time, the blockage may have the effect of reducing, but not totally eliminating the source on-time.

Example: in a 2000 second image, Sco X-1 might be blocked during the final 300 seconds.

The BAT team has released two tools to aid in correcting for occultation.

batoccultmap produces a fractional exposure map for a full sky image. Users provide the sky image and the prefilter attitude file ("SAO" file), and batoccultmap computes the fractional sky exposure in each pixel. This task should be used when users are interested many sources at one time.

NOTE: we suggest to only correct for earth occultation. Correcting for sun/moon occultation typically does not help, since it changes the image statistics in a non-smooth way.

batoccultgti produces a good time interval file (GTI file) for a known source. Good times are selected based on being unocculted and/or in a certain position in the field of view. This task should be used when users are interested in a particular source (i.e. not imaging), and should be used to filter the input data by time before further analysis.

Updated (15 Oct 2005) - to discuss the new occultation tasks

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