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ACSPO v1.40 (GAC & FRAC) Effective Date: 7 December 2010

ACSPO v1.40 (GAC & FRAC) Effective Date: 7 December 2010. XingMing Liang, Sasha Ignatov, John Stroup, Yury Kihai and Boris Petrenko NOAA/NESDIS/STAR John Sapper and Denise Frey NOAA/NESDIS/OSDPD. Significant Upgrades in ACSPO v1.40 (1). CRTM Version 2.02 used instead of v1.2

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ACSPO v1.40 (GAC & FRAC) Effective Date: 7 December 2010

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  1. ACSPO v1.40 (GAC & FRAC)Effective Date: 7 December 2010 XingMing Liang, Sasha Ignatov, John Stroup, Yury Kihai and Boris Petrenko NOAA/NESDIS/STAR John Sapper and Denise Frey NOAA/NESDIS/OSDPD ACSPO v1.40 (GAC & FRAC)

  2. Significant Upgrades in ACSPO v1.40 (1) CRTM Version 2.02 used instead of v1.2 • Based on SST-CRTM joint analyses: Specular reflectance model replaced the quasi-Lambertian model in CRTM v1.2 for solar reflection calculations • Placeholder for new coefficient data—Optical Depth in Pressure Space (ODPS)—added in ACSPO v.140. • ODPS coefficients will be used instead of ODAS (Optical Depth in Absorber Space) once tested & optimized by CRTM Team. • Processing speed slightly improved. OSTIA SST added • Daily 0.05º OSTIA SST added as an optional reference field, in addition to daily Reynolds SST. (In v1.40, Reynolds SST continues to be used, pending implementation of OSTIA real-time data stream in OSDPD operations). ACSPO v1.40 (GAC & FRAC)

  3. Significant Upgrades in ACSPO v1.40 (2) Aerosol quality flag updated • Cloud mask flag removed from aerosol quality flag. (These two are now completely separated and independent.) • A bug in aerosol quality flag fixed. Option for CRTM Parallel processing added to ACSPO v.1.40 • ACSPO CRTM module changed to be ready for parallel processing. • Will be implemented in ACSPO v2.0 pending complete testing and implementation of parallel processing in CRTM by CRTM team ACSPO code restructured towards v2.0 • ACSPO code (which heavily draws from CLAVR-x) partly restructured, to facilitate transition to ACSPO v2.0. ACSPO v1.40 (GAC & FRAC)

  4. Daytime M-O Bias in ACSPO v1.30 In ACSPO v1.30: An unrealistic cold M-O bias (~ -20K) in Ch3b found in sun glint area and a warm bias (~ +5K) elsewhere, due to inaccurate surface model (quasi-Lambertian) used in CRTM 1.2. ACSPO v1.40 (GAC & FRAC)

  5. Daytime M-O Bias in ACSPO v1.40 In ACSPO v1.40: Specular model adopted in CRTM 2.02 instead of quasi-Lambertian significantly reduces daytime M-O biases in Ch3b, due to improved CRTM performance. ams.confex.com/ams/pdfpapers/170593.pdf ACSPO v1.40 (GAC & FRAC)

  6. Re-definition of Aerosol Quality Flag (QF) in ACSPO v1.40 QF <= 2 in ACSPO v1.30: • Clear-Sky AND • Glint angle >= 40° QF <= 2 in ACSPO v1.40: • Glint angle >= 40° Aerosol QF in ACSPO v1.40 redefined: clear-sky condition removed from the definition. ACSPO v1.40 (GAC & FRAC)

  7. Aerosol Quality Flag (QF) Bug in ACSPO v1.30 In ACPSO v1.30 all pixels with SenZA > 60° were not flagged out in QF=2. ACSPO v1.40 (GAC & FRAC)

  8. Bug Fixed in ACSPO v1.40 This bug was fixed in ACSPO v1.40. ACSPO v1.40 (GAC & FRAC)

  9. Ongoing ACSPO Improvements • OSTIA will be tested as a first-guess SST field instead of Reynolds • ODPS coefficients are currently being tested by CRTM Team. Once validated, they will be used in ACSPO v2.0 instead of ODAS coefficients. ACSPO infrastructure is in place. • Implementation of CRTM parallel processing is underway. Once tested, it will be implemented in ACSPO v2.0 to speed up processing. ACSPO infrastructure is in place. • Thresholds in glint, view, and solar zenith angles in aerosol QF will be fine-tuned based on analyses in the aerosol quality monitor (AQUAM), currently being developed. • Restructured ACSPO v2.0 is under development/testing. It is a completely restructured ACSPO v1.** code (which draws heavily on CALVR-x structure), fully compliant with FORTRAN 95 and up, parallelized for faster processing, and hard-coding removed. ACSPO v1.40 (GAC & FRAC)

  10. Back-Up: Why OSTIA (coming in ACSPO v.2) • Why OSTIA was added in ACSPO v1.40? • More accurate first guess field has potential to improve accuracy of SST & M-O biases • Not implemented in ACSPO v1.40, pending implementation of real-time OSTIA access in OSDPD • Will be fully tested and implemented in ACSPO v2.0 ACSPO v1.40 (GAC & FRAC)

  11. Improvements resulting from OSTIA SST as CRTM Input compared to Reynolds SST Reynolds SST OSTIA SST • Standard deviation of M-O bias in the case of OSTIA SST as CRTM input is much smaller than from Reynolds. • Amount of clear pixels slightly increases. (OSTIA to be implemented in ACSPO v2, pending implementation of operational access in OSDPD) ACSPO v1.40 (GAC & FRAC)

  12. Stability of Reynolds SST (ACSPO v1.30) Reynolds SST as CRTM input in ACSPO v1.30 Significant unexplained short and long term M-O variations take place in M-O bias in all AVHRR thermal bands if Reynolds SST is used as CRTM input. ACSPO v1.40 (GAC & FRAC)

  13. Stability of OSTIA SST (ACSPO v1.40) OSTIA SST as CRTM input in ACSPO v1.40 The M-O variations are reduced if OSTIA SST is used as CRTM input instead of Reynolds daily SST. (OSTIA SST will be implemented in ACSPO v2.0) ACSPO v1.40 (GAC & FRAC)

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