Leonardo spaceborne infrared payloads for Earth observation: SLSTRs for Copernicus Sentinel 3 and PRISMA hyperspectral camera for PRISMA satellite

Peter Coppo; Fabio Brandani; Marco Faraci; Francesco Sarti; Michele Dami; Leandro Chiarantini; Beatrice Ponticelli; Lorenzo Giunti; Enrico Fossati; Massimo Cosi

doi:10.1364/AO.389485

Applied Optics
Vol. 59,
Issue 23,
pp. 6888-6901
(2020)
•https://doi.org/10.1364/AO.389485

Leonardo spaceborne infrared payloads for Earth observation: SLSTRs for Copernicus Sentinel 3 and PRISMA hyperspectral camera for PRISMA satellite

Peter Coppo, Fabio Brandani, Marco Faraci, Francesco Sarti, Michele Dami, Leandro Chiarantini, Beatrice Ponticelli, Lorenzo Giunti, Enrico Fossati, and Massimo Cosi

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Peter Coppo, Fabio Brandani, Marco Faraci, Francesco Sarti, Michele Dami, Leandro Chiarantini, Beatrice Ponticelli, Lorenzo Giunti, Enrico Fossati, and Massimo Cosi, "Leonardo spaceborne infrared payloads for Earth observation: SLSTRs for Copernicus Sentinel 3 and PRISMA hyperspectral camera for PRISMA satellite," Appl. Opt. 59, 6888-6901 (2020)

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Abstract

Leonardo has been involved in the realization of several infrared payloads for Earth observation since 1990. Among the currently in-orbit operative instruments are the two Sea and Land Surface Temperature Radiometers (SLSTRs) and PRISMA (PRecursore IperSpettrale della Missione Applicativa, meaning Hyperspectral Italian Pre-cursor of Operational mission). The SLSTRs are high-accuracy radiometers that provide sea surface temperature data continuity with respect to previous (A)ATSRs in order to serve climatology over the next 20 years, and exist within the framework of the European Space Agency Sentinel-3 mission, which is part of the Copernicus program. The PRISMA program is the first Agenzia Spaziale Italiana optical hyperspectral mission for Earth observation. It is based on a high spectral resolution spectrometer operating in the visible-short wave infrared channels optically integrated with a panchromatic camera.

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	S3A	S3A	S3B	S3B	Mathematical Model BOL-EOL		EOL Requirement Goal-Threshold
Tscene	267 K	304 K	267 K	304 K	270 K (F1 = 350 K, F2 = 330 K)	300 K	270 K
S7	47 mK	17 mK	42 mK	16 mK	51–56 mK	22–24 mK	50–80 mK
S8	14 mK	11 mK	17 mK	13 mK	19–21 mK	15–16 mK	30–50 mK
S9	22 mK	18 mK	18 mK	14 mK	20–24 mK	17–19 mK	30–50 mK
F1	1.1 K	0.266 K	1.5 K	0.364 K	85–95 mK	0.377–0.42 K	1 K (350–500 K)
F2	28 mK	36 mK	31 mK	30 mK	30–33 mK	35–38 mK	0.5 K (330–400 K)

	Sun Radiance ( $mW / m^{2} / Sr / nm$ )	S3A Flight		S3B Flight		Model BOL-EOL	EOL Requirements		Performance BOL-EOL
	$L_{SUN}$	SNR	$ρ_{VISCAL}$	SNR	$ρ_{VISCAL}$	SNR at $ρ_{VISCAL}$	$ρ_{TOA}$	SNR	SNR at $ρ_{TOA}$
S1	585	242	19%	235	18%	270–215	0.5%	6^b	8–6
S2	475	247	19%	224	19%	270–225	0.5%	6^b	8–7
S3	295	240	19%	239	19%	306–270	0.5%	7^b	9–8
S4	113.1	240	19%	188	19%	380–310	0.5%	9^b	13–10
S5	74	404	19%	346	18%	680–560	0.5%	20	29–23
S6	24.3	259	17.5%	230	16%	300–260	0.5%	11^b	13–11

	Requirement	VNIR	SWIR	PAN	V
Swath	$\geq 30 Km$	31 km	31 km	31 km	F
Ground sampling distance (GSD)	$\leq 31 m$ (VNIR-SWIR)^a	31 m	31 m	5.1 m	F
Ground sampling distance (GSD)	$\leq 5.1 m$ (PAN)^a	31 m	31 m	5.1 m	F
Spectral range	400–2500 nm	400–1010 nm	920–2505 nm	400–700 nm	–
Number of bands	–	66	174	1	–
Spectral co-registration (SSI = 30 µm)	$\leq \pm 0 . 1 SSI$	0.08 SSI	0.05 SSI	–	F
Image quality MTF	$\geq 0.3$ (VNIR-SWIR)	0.30	0.32	0.25	F
Image quality MTF	$\geq 0.2$ (PAN) ( $\times 2$ bin)^a	0.30	0.32	0.25	F
Spatial co-registration (GSD = 30 m)	$\leq 0.1 GSD$	0.04 GSD	0.04 GSD	0.06 GSD	F
Spectral sampling interval (SSI)	$\leq 11 nm$ ^a	7.2–11 nm	6.5–11 nm	–	G
Spectral resolution	$\leq 15 nm$ ^a	9–13 nm	9–14.5 nm	–	G
SNR	$\geq 160 - 200$ (400–450 nm)^a	161–209 (400–450 nm)	–	–	G
	$\geq 200$ (450–1000 nm)^a	200–450 (450–1000 nm)
	(930–970 nm NA)	200–450 (450–1000 nm)
	$\geq 200$ (1000–1750 nm)	–	300–800 (1000–1300 nm)	–	G
	$\geq 100$ (1950–2350 nm)	–	200–400 (1500–1750 nm)
	(NA in absorption bands)		100–200 (1950–2350 nm)
	$\geq 190$ (PAN)^a	–	–	191	G
Spectral centroid knowledge accuracy	$\leq \pm 0 . 1 nm$	$\pm 0 . 1 nm$	$\pm 0 . 1 nm$	–	G
Absolute radiometric Accuracy	$\leq 5 %$	( $Stability \leq \pm 1 %$ )^b	( $Stability \leq \pm 1 %$ )^b	–	F

	S3A	S3A	S3B	S3B	Mathematical Model BOL-EOL		EOL Requirement Goal-Threshold
Tscene	267 K	304 K	267 K	304 K	270 K (F1 = 350 K, F2 = 330 K)	300 K	270 K
S7	47 mK	17 mK	42 mK	16 mK	51–56 mK	22–24 mK	50–80 mK
S8	14 mK	11 mK	17 mK	13 mK	19–21 mK	15–16 mK	30–50 mK
S9	22 mK	18 mK	18 mK	14 mK	20–24 mK	17–19 mK	30–50 mK
F1	1.1 K	0.266 K	1.5 K	0.364 K	85–95 mK	0.377–0.42 K	1 K (350–500 K)
F2	28 mK	36 mK	31 mK	30 mK	30–33 mK	35–38 mK	0.5 K (330–400 K)

	Sun Radiance ( $mW / m^{2} / Sr / nm$ )	S3A Flight		S3B Flight		Model BOL-EOL	EOL Requirements		Performance BOL-EOL
	$L_{SUN}$	SNR	$ρ_{VISCAL}$	SNR	$ρ_{VISCAL}$	SNR at $ρ_{VISCAL}$	$ρ_{TOA}$	SNR	SNR at $ρ_{TOA}$
S1	585	242	19%	235	18%	270–215	0.5%	6^b	8–6
S2	475	247	19%	224	19%	270–225	0.5%	6^b	8–7
S3	295	240	19%	239	19%	306–270	0.5%	7^b	9–8
S4	113.1	240	19%	188	19%	380–310	0.5%	9^b	13–10
S5	74	404	19%	346	18%	680–560	0.5%	20	29–23
S6	24.3	259	17.5%	230	16%	300–260	0.5%	11^b	13–11

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Applied Optics