Oco path program

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While the ABI cryocooler has similar capacity to the TES flight spare used on the original OCO instrument, it is much smaller and has a different set of electronics used to operate it.

To handle this, a small electronics board, i. The second challenge is that the command and telemetry formats are completely different. This approach will avoid the need to either the spacecraft or instrument electronics or flight software — allowing OCO-2 to use the same designs that were qualified for the original mission. Removing these anomalies from the instrument will greatly simplify the complexity of the ground data processing and improve the final quality of the science data.

These had identical readout to the Hawaii-1RG mercury-cadmium-telluride HgCdTe detectors used in the CO 2 bands — allowing a common design for the OCO electronics to provide the bias, timing and readout. To save power, the O 2 A-band detector was only cooled to K as the silicon dark current is much less than the HgCdTe detectors. One lot of parts was procured and initial testing looks likely that these parts will meet the OCO-2 needs.

This created a situation where energy was stored in the bolts to be released during the vibration testing. For OCO-2, the installation order of these bolts will be corrected to avoid storing any energy.

This will allow validation of this approach to correct the slit misalignment before the instrument level vibration testing. The focal plane test bed mentioned above has been used to recreate the stray light problem in spare HgCdTe detectors from OCO, while the silicon detectors do not exhibit the problem.

When the first substrate-removed HgCdTe detectors are tested expected in mid-September , it is expected that they will not exhibit the stray light problems. Table 3 : Changes planned for the OCO-2 instrument. The 3 spectrometers use similar optical designs and are integrated into a common structure to improve system rigidity and thermal stability.

They share a common housing and a common Cassegrain telescope Ref. The telescope consists of an 11 cm aperture, as well as a primary and a secondary mirror.

The relay optics assembly includes fold mirrors, dichroic beam splitters, band isolation filters and re-imaging mirrors. Each spectrometer consists of a slit, a two-lens collimator, a grating, and a two-lens camera.

Each of the three spectrometers has essentially an identical layout. Minor differences among the spectrometers, such as the coatings, the lenses and the gratings, account for the different bandpasses that are characteristic of each channel.

To implement an optically fast, high-spectral-resolution measurement system, the OCO-2 instrument combines refractive and reflective optical techniques. Since the light in the common telescope and relay optics assembly will not separate into the three distinct wavelength bands, these instrument subsystems use primarily reflective optics. On the other hand, the extremely narrow channel bandpasses make potential chromatic aberrations in the spectrometers negligible, which enable the use of refractive optics.

The light path is illustrated in Figures 5 and 6. Light entering the telescope is focused at a field stop and then re-collimated before entering a relay optics assembly. There, it is directed to one of the three spectrometers by a dichroic beam splitter, and then transmitted through a narrowband pre-disperser filter. The light is then refocused on the spectrometer slits by a reverse Newtonian telescope. Because the diffraction gratings efficiently disperse only the light that is polarized in the direction parallel to the slit, a polarizer was included in front of the slit to reject the unwanted polarization before it enters the spectrometer, where it could contribute to the scattered light background.

Once the light traverses a spectrometer slit, it is collimated by a 2-element refractive collimator, dispersed by a gold-coated, reflective planar holographic diffraction grating, and then focused by a 2-element camera lens on a 2-dimensional FPA Focal Plane Array , after traversing a second, narrowband filter.

Following the OCO design, the spectral range and resolving power of each channel includes the complete molecular absorption band as well as some nearby continuum to provide constraints on the optical properties of the surface and aerosols as well as absorbing gases.

To meet these requirements, the O 2 A-band channel covers 0. The grating disperses the pixel wide spectrum in the direction perpendicular to the long axis of the slit. For normal science operations, the FPAs are continuously read out at 3 Hz. The angular width of the narrow dimension of the slit is only 0. In addition to the 8 spatially-binned, element spectra, each spectrometer also returns 4 to 20 spectral samples without on-board spatial binning to provide the full along-slit spatial resolution.

These full-spatial-resolution color stripes are used to detect spatial variability within each of the spatially summed super pixels and to quantify the thermal emission and scattered light within the instrument. For the OCO instrument, the entrance slits for the 3 spectrometers were carefully co-aligned during the optical bench assembly to ensure that all 3 spectrometers would share a common bore site.

After the instrument vibration test, an optical component in the 1. The root cause of the misalignment was traced to a specific step in the optical bench assembly process.

While it was not possible to correct this misalignment for the OCO instrument, a second vibration test was performed to ensure that no further movement would occur, and the science algorithms were modified to accommodate the pointing offset. For the OCO-2 instrument, the optical bench assembly process has been modified to avoid this problem. They also have slightly lower read noise than those used for the OCO instrument.

A different cryocooler was therefore needed for the OCO-2 instrument. This cryocooler, referred to as CSS Cryogenic Subsystem , is slightly smaller and more efficient than the one used by the OCO instrument, but did require changes in the cryocooler electronics and the heat pipes. For normal science operations, the spacecraft bus orients the instrument to collect science data in Nadir, Glint, and Target modes.

The varies modes optimize the sensitivity and accuracy of the observations for specific applications.