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GOES X-Ray Sensor (XRS) GOES X-ray Sensor (XRS) Measurements Janet Machol, NOAA National Centers for Environmental Information (NCEI) and University of Colorado, Cooperative Institute for Research in Environmental Science (CIRES) Rodney Viereck, NOAA Space Weather Prediction Center (SWPC) 10 June 2016, Version 1.4.1 Important notes for users Scaling factors: For GOES 8-15, the archived fluxes have had SWPC scaling factors applied. To get true fluxes, these factors must be removed. To get true fluxes from the archived data, users must divide short channel fluxes by 0.85 and divide the long channel fluxes by 0.7. Similarly, to get true fluxes for pre-GOES-8 data, users should divide the archived fluxes by the scale factors. No adjustments are needed to use the GOES 8-15 fluxes to get the traditional C, M, and X alert levels. (See Section 2.) Time stamps: The raw data time stamps are offset 1.024 s after the integration periods. The timestamps for averaged data have a 1-3 s offset from the start of the data. (See Section 3.) Version Date Description of major changes author 1.4.1 9 June 2016 3 s data for GOES 8-12 added to archive. Revised table of Machol chronology of primary and secondary satellites. Added references and discussion of digitization. 1.4 4 March 2015 original Machol Contents 1. GOES X-ray Sensor (XRS) ........................................................................................................................... 3 2. Data issues ................................................................................................................................................ 4 2.1 Scaling factors and calibration ............................................................................................................ 4 2.2. Time stamps ....................................................................................................................................... 5 2.3 Digitization .......................................................................................................................................... 6 2.4 Contamination .................................................................................................................................... 6 2.5. Saturation ........................................................................................................................................... 6 3. Data Access ............................................................................................................................................... 7 4. Dates of GOES satellites with XRS sensors ................................................................................................ 7 5. Contacts .................................................................................................................................................... 9 6. Status flags for GOES 8-12 ...................................................................................................................... 10 7. Calibration tables for GOES 13-15 .......................................................................................................... 11 References .................................................................................................................................................. 14 Acknowledgements ..................................................................................................................................... 14 1. GOES X-ray Sensor (XRS) On each GOES satellite there are two X-ray Sensors (XRS) which provide solar X-ray fluxes for the wavelength bands of 0.5 to 4 Å (short channel) and 1 to 8 Å (long channel). Measurements in these bands have been made by NOAA satellites since 1974 and the design has changed little during that time period [Garcia, 1994]. The data comes from the NOAA Space Weather Prediction Center (SWPC) and is archived at the NOAA National Center for Environmental Information (NCEI) which was formerly the National Geophysical Data Center (NGDC). Figure 1 shows primary and secondary GOES satellites for XRS data since 1986. Figure 1. Primary (thick lines) and secondary (thin lines) GOES satellites for XRS data since 1986. GOES-13 measurements were unstable for many years, but have been been stable since 2014. However GOES 13 is not considered a primary or secondary satellite at this time. XRS data goes back to 1974, but the designation of primary and secondary satellites prior to 1986 is not known. The measurements are obtained from two gas-filled ion chambers, one for each band. Sweeper magnets deflect incoming electrons away from the assemblies so that only x rays are measured. The instruments are not thought to degrade. GOES 8-12 (GOES I-M series) and 13-15 (GOES NOP series) have ion cell detectors and the detector/filter combinations that make the spectral bandpasses nearly identical between both satellite series (and to earlier XRS detectors). A description of the GOES-8 instrument is given by Hanser and Sellers [1996]. Although electronics are very different for the two series, the measurements agree across the full dynamic ranges except at the very lowest signal levels. For each sensor, the short wavelength cutoff is defined by the ion cell, while the long wavelength cutoff is defined by the thickness of the beryllium (Be) filter. Figure 2 shows the normalized detector responses for the short and long wavelength bands. The relative spectral contributions measured by the detectors are shown in Figure 3. Figure 2. XRS detector responses. Figure 3. Relative spectral contributions for the XRS (a) short and (b) long channels. These are the detector responses multiplied by smoothed solar spectra for solar minimum, maximum, and flare conditions obtained from CHIANTI. 2. Data issues 2.1 Scaling factors and calibration The archived XRS fluxes include scaling factors that were initially implemented by SWPC to get GOES-8 to agree with GOES-7. GOES 7 was the last of the spinning GOES satellites while GOES 8 was the first of the 3-axis-stabilized satellites. The scaling factors were retained by SWPC so that flare warning levels correspond to consistent flux values; e.g., an M5 X-ray alert from SWPC is based on a flux level of 5x10-5 W/m2 for all satellites. Some rocket launches have confirmed that the new sensors are accurate and that the use of scaling factors to match the old spinner satellites is not correct. SWPC has not removed the scaling factors from the data, however, because (1) there has been no actual calibration, (2) the XRS is operational, and (3) there are many procedures and customers that require consistency more than accuracy. The next generation of satellites, GOES-R (to launch in 2016) will have well calibrated detectors and will provide the confirmation needed to finally remove the scaling factors. To get true fluxes for GOES 8-15 XRS, users must remove the SWPC scaling factors from the data. To get the true fluxes, divide the short band flux by 0.85 and divide the long band flux by 0.7. Similarly, to get true fluxes for pre-GOES-8 data, users should divide the archived fluxes by the scale factors. No adjustments are needed to use the GOES 8-15 fluxes to get the traditional C, M, and X alert levels. Calibration issues are discussed by Neupert [2011]. A comparison of XRS data with Thermosphere Ionosphere Mesosphere Energetics Dynamics– Solar Extreme Ultraviolet Experiment (TIMED-SEE) measurements is given by Rodgers et al. [2006]. 2.2. Time stamps For GOES XRS, the data sampling rate depends on the satellite generation. For GOES 13-15, the data accumulation time is 2.048 s, and both the A and B channels take data simultaneously [Data and calibration handbook, 2009, Section 9.3]. The location of the time stamps is offset relative to the integration periods. As can be seen in Figure 4, for the raw data, the time stamps are 1.024 s after the end of the integration period. Figure 4. Sketch of XRS data integration and readout from the instrument. Telemetry minor frames are 1.024 s. As an example, the relative times for integration period '3' and its delayed timestamp are indicated. For GOES 13-15, one minute averages are created by including all raw data with time stamps within a 1 minute window. The time stamp is set to the beginning of the 1 minute window. Five minute averages are created from averages of 1-min averages, and time stamped at the beginning of the average. Because the raw data time stamps are offset after the data, the time stamps for the averaged data are 1.024-3.072 s after the start of the included data. This is sketched in Figure 5. Figure 5. Sketch shows that timestamp for averaged data is offset 1.024-3.072 s after the start of the included data. For satellites prior to GOES-13, the data accumulation time was 3 s. The time stamps are <3 s after the end of the accumulation period; the offset is not defined exactly because there was no on-board satellite clock. The actual sampling rate is 0.512 according to the GOES I-M DataBook [1996], but this raw data is only available by reprocessing the raw telemetry . The averages are created in the same way as for GOES 13-15. 2.3 Digitization As described by Simões et al. [2015], the digitization of the GOES XRS data is larger than the Poisson noise from photon counting statistics. This can be problematic when differencing or taking derivatives of the flux data. GOES 8-12 had three different gain ranges and the digitization is apparent at the edges of these ranges. For GOES 10, the contractor changed the electronics to reduce the noise level of the XRS. This
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