Development of infrared focal plane arrays for space - Astro Pas ...

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TABLE VII. Dark signal (e ) vs integration time s at 400 mV bias.Integrationtime s Dark signal at 14.7 K (e ) Dark signal at 28.5 K (e )10 6.2 7.3 9.2 9.250 15.4 8.5 12.310.8100 8.5 9.2 4.611.6200 0.810.0 13.913.1400 3.913.1 30.814.6FIG. 12. QE % at 28.5 K for FPA CRC744-40716.FIG. 15. Difference of dark images of FPA CRC744-40716 with 400 and 10s integration times at 14.7 K Unit: e .FIG. 13. QE % histogram at 28.5 K for FPA CRC744-40716. All pixelsare included.FIG. 14. QE of the central 2525 box of FPA CRC744-40716 as the Dewarwarmed up and when the fanout board was stabilized at 14.6 and 28.5 K.Also included are the average QE for the whole array when the fanout boardwas stabilized at 14.6 and 28.5 K.FIG. 16. Histogram of Fig. 15 Unit: e . All pixels are included.3574 Rev. Sci. Instrum., Vol. 68, No. 9, September 1997 IR focal plane arraysDownloaded 21 Jun 2012 to 128.151.144.191. Redistribution subject to AIP license or copyright; see http://rsi.aip.org/about/rights_and_permissions
FIG. 17. Difference of dark images of FPA CRC744-40716 with 400 and 10s integration times at 28.5 K Unit: e .uniform throughout the whole array and there are only a fewhot pixels the pixels with large dark current. The actual hotpixels are fewer than the large current pixels which can beseen in Figs. 15–18. Some large current pixels in Figs.15–18 were caused by the remnant radiation from our Dewarwhich had been used in a proton radiation test five monthsago. The 28.5 K histogram indicates that a real dark chargeof 20 e may be present; which would correspond to adark current of 0.05 e /s.E. NoiseThe read noise data were taken at 14.5 and 28.5 K withintegration times of 6 s for 1–32 pairs of Fowler samples, 12s for 64 pairs, and also 200 s for 1–32 pairs. Figure 19 showsthe noise versus number of Fowler pairs at 14.5 K. The noiseimproves with increasing numbers of Fowler pairs up to themaximum of 64 pairs. This was true at 14.5 K as well as 28.5K. Table VIII lists the noise obtained for 32 sample pairsFIG. 19. Read noise of FPA CRC744-40716 and CRC744-41626 vs numberof Fowler sample pairs N at 14.5 K. The modeling result described in thetext is also plotted as the solid line. The 41626 FPA employs a 2 mLawrence mux.with6sofintegration time, 64 sample pairs with 12 s ofintegration time, and 32 sample pairs with 200 s of integrationtime at 14.6 and 28.5 K. At 200 s of integration time, thenoise was about 50% larger than at 6 s. The 200 s performanceis noticeably better at 14.6 K than at 28.5 K.Figure 20 shows read noise in 6 s integration time with1, 8, 32, and 64 Fowler sample pairs versus temperature. Thedata shown were obtained from a 2525 box at the center ofthe array. From 5 to 40 K, the noise with 8 and 32-samplepairs increases very gradually as the temperature rises. It canbe seen in Table VIII that the noise in the central 2525 boxfor 32 Fowler sampling pairs and 6sofintegration timestabilized at temperatures of 14.6 and 28.5 K is about 1 e TABLE VIII. Noise (e ) at 14.5 K and 28.5 K, Fowler sampling. aN samp 32,integrationtime6s (x,y)(50,50) (x,y)(128,128) (x,y)(225,225)T14.6 K 7.26.4 b 6.96.2 b 7.36.7 b T28.5 K 7.5 7.7 8.4N samp 64,integrationtime12 sT14.6 K 6.75.3 b 5.85.2 b 6.65.6 b T28.5 K 6.9 7.3 7.9N samp 32,integrationtime200 sT14.6 K 9.2 9.4 10.3T28.5 K 12.7 14.2 14.3FIG. 18. Histogram of Fig. 17 Unit: e . All pixels are included.a Statistical uncertainty: 2%.b After fixing a small problem in our preamp board.Rev. Sci. Instrum., Vol. 68, No. 9, September 1997IR focal plane arrays3575Downloaded 21 Jun 2012 to 128.151.144.191. Redistribution subject to AIP license or copyright; see http://rsi.aip.org/about/rights_and_permissions
Page 1 and 2: Development of infrared focal plane
Page 3 and 4: FIG. 1. Read noise for SBRC astrono
Page 5 and 6: TABLE III. Bias setting.Biases Volt
Page 7 and 8: FIG. 7. The reset voltage measured
Page 9: TABLE V. Well depth W.D. and zero b
Page 13 and 14: FIG. 22. Load driving measurements.

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