Документ взят из кэша поисковой машины. Адрес оригинального документа : http://hea.iki.rssi.ru/integral06/papers/J30_Bianchin01-16Feb07_12:32:07.pdf Дата изменения: Fri Feb 16 12:32:07 2007 Дата индексирования: Mon Oct 1 23:27:40 2012 Кодировка: Поисковые слова: apollo 13

IBIS/PICSIT STATUS
G. Di Cocco1 , V. Bianchin1 , L. Foschini1 , F. Gianotti1 , P. Laurent2 , G. Malaguti1 , L. Natalucci3 , and F. Schiavone1
1

INAF/IASF-Bologna, via Gobetti 101, 40129 Bologna, Italy (dicocco, bianchin @iasfbo.inaf.it) 2 Service d'Astrophysique ­ SAp-CEA, Saclay, France 3 INAF/IASF-Roma, Via Fosso del Cavaliere, 00100 Roma, Italy

ABSTRACT We report about the status of the PICsIT layer of the imager IBIS. The instrument has been tested in both Spectral Imaging and Spectral Timing Mode. PICsIT Single Events, Multiple and ISGRI data of the Crab are simultaneously fitted to a power law model and fit parameters are compared with the standard values. We present a joint fit of SPI, ISGRI, PICsIT data of the long GRB041219, that was seen by the PICsIT instrument in both Spectral Imaging and Spectral Timing acquisition modes. This allowed us to generate a preliminary version of the instrumental response matrices for the PICsIT Spectral Timing mode. Key words: gamma-ray telescopes - imaging detectors PICsIT.

pixels. Due to the electronic separation of semi-modules Multiple Events across semi-modules are treated as two separate Single Events (see [2]). Data acquisition and preprocessing follow two operational modes: Photon-by-Photon Mode (PPM) and Standard Mode (SM). In PPM the instrument reveals the complete photon information: event position, time delay between consecutive events and energy in 1024 channels for both Singles and Multiples. Because of the satellite telemetry restrictions the acquisition in PPM is activated only for Calibration purposes and during Slews ( 120 s). Moreover in PPM the energy of the transmitted data is limited to 1 MeV, again because of tight telemetry budget. During pointings, PICsIT is switched in its nominal operational mode, the SM, which is composed by two complementary Submodes: Spectral Imaging (SI) and Spectral Timing (ST). In SI the full spatial information on 64 в 64 pixels is kept but events are onboard integrated over 2 ks and stored in 256 energy channels. Conversely, ST mode allows a time binning from 0.97 ms to 500 ms, up to 8 energy bins, but no spatial resolution. From Revolution 441 (2006 May 24) the conversion table for ST (containing Singles and Multiples together) has been updated. Time binning is 16 ms in 8 energy bands: 208 - 260 keV, 260 - 312 keV, 312 - 364 keV, 364 - 468 keV, 468 - 572 keV, 572 - 780 keV, 780 - 1196 keV, 1196 - 2600 keV. More information on the status of the detector can be found at the IBIS/PICsIT web page in Bologna1

1.

PICSIT OUTLINE

PICsIT (Pixellated Imaging CsI Telescope) is the highenergy detector (175 keV-13 MeV) of the imager IBIS on board of the INTEGRAL satellite. The instrument provides fine imaging, good sensitivity and moderate energy resolution over a wide energy interval in the hard X/gamma-ray domain. PICsIT is composed by 4096 (64 в 64) CsI(Tl) crystals organised in 16 semimodules, with independent electronic units. The imager collects the shadowgram cast by the IBIS coded mask, covering a FOV=29 в 29 (zero response) sampled in 10 (see [1] for more details). Data are on-board equalised and pre-processed by means of the LUT (Look Up Tables) according to the event type and the detector operational mode. A valid PICsIT event is every signal that is not in coincidence with ISGRI events (Compton events), Calibration events or VETO strobes. PICsIT detects and stores separately two types of event: Single and Multiple Events. Single Events are made of detections in one single pixel, produced by energy deposits above the detector low threshold. The energy range for single events is 175 keV - 6.5 MeV. Multiple (Double) Events are generated by a photon energy deposit of 350 keV - 13 MeV across two or more

2.

THE CRAB SPECTRUM IMAGING MODE

IN

SPECTRAL

We tested the spectral capabilities of the IBIS/PICsIT layer on a joint fit of PICsIT and ISGRI data of the Crab. Spectral extraction can follow two methods: the first one is to run up to level SPE the pipeline of the Offline Scientific Analysis (OSA)2 , whose algorithms for IBIS are described in [3]. However, because of the generally low
1 http://www.iasfbo.inaf.it/index.php?option= com content&task=view&id=42&Itemid=49 2 http://isdc.unige.ch/?Soft+download


ISGRI (OSA 5.1)

PICsIT Single (OSA 6)

PICsIT Multiple (OSA 6)

39, 40, 41, 42, 45, 170, 239, 300, 365 and 422). Revolutions 102 and 103 have been neglected since the detector underwent high temperature fluctuations ( 10 ) that strongly affected imaging performances. Data have been downloaded from the ISDC data archive3 and we selected Observations in which PICsIT was in Standard operational Mode and where both Single and Multiple Events were collected. Data sample has been cleaned from ScWs where problems of different nature have been recognised: ScWs with exposure lower than 1ks, with missing calibration files, with badly downloaded histograms and so on.

Effective Area (cm2)

10

100

1000

100 Energy (keV)

1000

104

Figure 1. Effective area for IBIS instruments. For ISGRI we use the spectral response of OSA 5.1; PICsIT effective areas for Single and Multiple Events are the updated versions in OSA 6.
10



-2

0

2

10-5 10-4 10-3 0.01

PICsIT data analysis was carried out by means of OSA 6, running the pipeline on the 8 standard energy bins for single and multiple events [4]. The total mosaic of data set has been produced, with an effective exposure of 1.1 Ms. The long total exposure enhances the SNR and allows a full energy range investigation of the source spectrum. We included in the spectral analysis also data with very low values of the SNR since the Crab is a known source and we are mainly interested in analysing fit problems. For Single and Multiple events we used the newly released spectral responses (RMF/ARF), included in OSA 6 (see Fig.1).

counts s-1 keV-1

0.1

1

100 channel energy (keV)

1000

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Figure 2. Crab spectrum: joint fit of ISGRI (crosses), PICsIT singles (open triangles) and PICsIT multiples (filled triangles) data. Residuals are plotted in units.

signal/background ratio of sources in PICsIT operational energy range, this procedure works well with the integration of shadowgrams before spectral extraction. This is possible only in staring mode acquisition, while during scientific pointings the satellite usually takes a set of 2 ks acquisitions (Science Windows - ScWs) following a dither pattern. Improvements on this method are under development, but to date the most stable procedure is spectral extraction through the imaging pipeline. The scientific analysis software is run up to level IMA, when shadowgrams are deconvolved and images are obtained for each ScW. Subsequently the total mosaic of the whole data set is obtained by the varmosaic tool in HEASoft v.6.1.1. Counts and errors in each energy bin are then derived from the intensity and significance maps. It is important to remind that the low Signal to Noise Ratio (SNR) requires long exposure time. For this reason our data set covers all the Crab observations available up to date, from February 2003 to May 2005 (Revolutions

From the same data set we extracted the ISGRI spectrum running the OSA 5.1 pipeline up to level SPE. We used XSPEC v.11.3.2 to perform a joint fit of PICsIT Single, PICsIT Multiple and ISGRI data using a standard unabsorbed power law model (Fig.2). A systematic error of 1% is added to ISGRI data and a 5% systematic error is considered only in the first bin for PICsIT Single Events, which is strongly affected by cosmic rays induced events [5]. The best-fit model (2 = 23.8 for 20 dof, Prob.= 0.25) is a power-law with photon index = 2.11+0.09 and normalisation at 1 keV N = 8.1+4.9 -2 . 8 -0.08 ph cm-2 s-1 keV-1 . We obtain a good accordance with the "standard" values = 2.10 ± 0.03 and N = 9.7 ± 1.0 ph cm-2 s-1 keV-1 by [6]. A more recent analysis by [7], based on the observation of several satellites in the 0.1 - 1000 keV energy range, gave similar results ( = 2.08, N = 8.97 ph cm-2 s-1 keV-1 ). In the 20 keV - 10 MeV range the model flux is 0.26+0.31 -0.14 ph cm-2 s-1 , which is still in accordance with the expected value 0.33+0.12 ph cm-2 s-1 by [6], due -0.10 to the large error affecting the normalization parameter. The intercalibration coefficients for PICsIT single events (CS = 0.52+0.04 ) and for multiples (CM = 0.31 ± 0.06) -0.03 are sensibly low as compared with ISGRI (fixed to 1 as reference parameter). This problem requires a future deeper investigation on the response matrix for both PICsIT single and multiple events.


Figure 3. Image (252 - 336 keV) and lightcurves of the very long GRB041219, detected in both Spectral Imaging (left panel) and Spectral Timing (right panel). We extracted the spectrum of GRB041219 for ISGRI, SPI, PICsIT Single Events acquired in Spectral Imaging and PICsIT Spectral Timing. For ISGRI and SPI we run the standard OSA 5.1 pipeline up to level SPE, while for PICsIT SI we followed the procedure described above, deriving counts and errors from the image step. For PICsIT ST we extracted source plus background counts from the lightcurves of the ScW where the GRB occurred, while the background to be subtracted was extracted by using the ScWs before and after the event (see Fig. 3, right panel).
50 100 200 500 1000 channel energy (keV)

counts s-1 keV-1

-2

0

2

10-5

10-4

10-3

0.01

0.1

1

Figure 4. GRB041219 spectrum: joint fit of SPI (circles), ISGRI (crosses), PICsIT Spectral Imaging (triangles) and PICsIT Spectral Timing (stars) data. Residuals are given in units.

Using XSPEC we fitted data to an unabsorbed power law (Fig. 4). A first fit provides a rather poor 2 2. Most ~ of the problems are due to different systematic effects (cosmic-rays induced events in the low energy bins of PICsIT, the saturation of ISGRI during the GRB, other effects in SPI, etc...) and, therefore, for this preliminary analysis, we decided to assign an overall value of 7% for systematics. The best-fit model (2 = 31.1 for 26 dof with Prob. = 0.23) has photon index = 1.89 ± 0.05 and normalisation at 1 keV N = 14.8+4.2 ph cm-2 s-1 keV-1 . -2 . 4 In this case the reference for the intercalibration constant is SPI, since ISGRI is saturated by the high level counts of the source. This is also shown in the low value of the intercalibration constant, that is CI S GRI = 0.21+0.01 . -0.02 The best-fit intercalibration for PICsIT single events in SI is CP S I = 0.9 ± 0.1 and for PICsIT ST is CP S T = 0.54+0.07 . -0.04 We would like to underline that these are preliminary results and studies on the instrumental response of PICsIT in ST mode are currently on going.

3.

CALIBRATION MODE

OF

SPECTRAL

TIMING

In Spectral Timing Mode, PICsIT single and multiple events are not individually treated. Therefore data acquired in this mode can be straightforwardly used to build lightcurves of the whole detector plane but spectral extraction needs a proper response matrix. To date, no RMF and ARF are available and a source dependent calibration of the Spectral Timing Mode could be attempted when there are simultaneous detections in both Spectral Timing and Spectral Imaging Mode. This occurred during the long GRB041219 ( 360 s, see Fig. 3) and we used this observation to generate a preliminary version of the spectral response for ST mode data. We perform a simultaneous fit with ISGRI and SPI data in order to better determine model parameters and to check the new ST matrix. Note that when the GRB occurred the ST was set to 4 ms time resolution and 4 energy bands (156 - 208, 208 - 260, 260 - 364, 364 - 676 keV).
3

4.

CONCLUSIONS AND SUMMARY

http://isdc.unige.ch/index.cgi?Data+browse

In this work we report the status of the IBIS/PICsIT instrument on board of the INTEGRAL satellite. After the launchof the satellite, a contiunuous monitoring of PICsIT was activated. Results obtained to date (e.g. Fig. 5)


Figure 5. PICsIT background level for single (upper panel) and multiple (lower panel) events, from Revolution 36 to 505 . confirm the functional stability of instrument hardware. The number of dead pixels remained constant since the very beginning of the mission, for a total of 52 killed pixels. The average gain is in agreement with the value of 7.1 keV/ch, obtained from in-flight calibrations ([8], [9]). The background level shows a low but continuous increase, likely to be due to solar activity (see Fig. 5). PICsIT spectral capabilities have been verified using all the available observations of the Crab. The results of a joint fit of PICsIT and ISGRI data are in reasonably good agreement with the expected values. We focused on the possibility of full range analysis with long exposure data set and the need of future more detailed investigation of the instrument response. We present the first spectral analysis of PICsIT Spectral Timing data for long GRB041219, that was detected in both acquisition modes. Up to date PICsIT has revealed four compact object: two pulsars (Crab and PSR B1509-58) and two galactic black holes (Cygnus X-1 and XTE J1550-5644 ). Moreover, since the Spectral Timing mode is particularly effective in detecting powerful impulsive emissions, the list of GRBs is continuously updated and now contains 47 events. An updated PICsIT source catalogue can be found in the instrument web page5 . REFERENCES 1. Di Cocco G., Caroli E., Celesti E., et al. 2003, A&A, 411, L189 2. Bird A. J., Barlow E. J, Bazzano A. et al., 2003, A&A, 411, L159 3. Goldwurm A., David P., Foschini L., et al., 2003, A&A, 411, L223 4. Foschini L., Malaguti G., Goldwurm A., et al., 2005, IBIS/PICsIT Instrument Specific Software Scientific Validation Report - Version 5.1, available at http://isdc.unige.ch/?Support +documents 5. Segreto A., Labanti C., Bazzano A., et al. 2003, A&A, 411, L215 6. Toor A., Seward F. D., 1974, AJ, 79, 995 7. Kirsch M.G.F., Briel U.G., Burrows D., et al., 2005, Proceedings of the SPIE, 5898, 22 8. Malaguti G., Bazzano A., Bird A. J. et al. 2003, A&A, 411, L173 9. Di Cocco G., Malaguti G., Foschini L., Vitale V., Schiavone F., 2005, Internal Report IASF/BO, n.437/2005 10. Bianchin V., Foschini L., Sambruna R.M., et al., 2006, Proceedings of the VI Microquasar Workshop, PoS(MQW6)072 available at http://pos.sis sa.it/cgi-bin/reader/conf.cgi?confid= 33#session-13

4 A recent study of the 2003 outburst of this Galactic Black Hole, including PICsIT data, has been presented in [10]. 5 http://www.iasfbo.inaf.it/index.php?option= com content&task=view&id=42&Itemid=49