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Advanced Multiplexed TES Arrays Project

X-ray measurements are critical for the understanding of cycles of matter and energy in the Universe, for understanding the nature of dark matter and dark energy, and for probing gravity in the extreme limit of matter accretion onto a black hole. We propose a program to mature the current x-ray microcalorimeter technology, while developing transformational technology that will enable megapixel arrays. X-ray calorimeters based on superconducting transition-edge sensors achieve the highest energy resolution of any non-dispersive detector technology. The performance of single x-ray calorimeter pixels has reached that required for many possible future missions such as IXO, RAM, and Generation-X, but further optimization is still useful. In the last years, we have made progress in developing techniques to control and engineer the properties of the superconducting transition. We propose to continue this single-pixel optimization, and to improve both the practical and theoretical understanding of the correlation between alpha, beta, and noise to identify favorable regions of parameter space for different instruments. A greater challenge is the development of mature TES x-ray calorimeter arrays with a very large number of pixels. Advances in the last several years have been significant. We have developed modestly large (256 pixel) x-ray calorimeter arrays with time-division SQUID multiplexing, and demonstrated Walsh code-division SQUID multiplexing, which has the potential to allow scaling to much larger arrays. Here we propose to extend this work, and also to introduce a new code-division SQUID multiplexing circuit with extremely compact, low-power elements. Using this approach, it is possible for the first time to fit all of the detector biasing and multiplexing elements underneath an x-ray absorber, allowing in-focal-plane multiplexing. This approach eliminates the requirement to bring leads from each pixel out of the focal plane, while reducing the power dissipati

GOES-R PLT West Texas Lightning Mapping Array (LMA) V1

The GOES-R PLT West Texas Lightning Mapping Array (LMA) dataset consists of total lightning data measured from the West Texas LMA (WTXLMA) network during the GOES-R Post Launch Test (PLT) airborne science field campaign. The GOES-R PLT airborne science field campaign took place in support of the post-launch product validation of the Advanced Baseline Imager (ABI) and the Geostationary Lightning Mapper (GLM). The LMA measures the arrival time of radiation from a lightning discharge at multiple stations and locates the sources of radiation to produce a three-dimensional map of total lightning activity. These data files are available in compressed ASCII files and are available from March 1, 2017 through June 1, 2017.

Advancement and New Optimizations of Microcalorimeter Arrays for High-Resolution Imaging X-ray Spectroscopy Project

"We propose to continue our successful research program in developing x-ray microcalorimeter arrays for astrophysics. This development will directly benefit not only the International X-ray Observatory (IXO), but also other possible mission concepts. We will investigate various array and pixel optimizations such as would be needed for large arrays for surveys, or arrays of fast pixels optimized for neutron star burst spectroscopy. The main emphasis of our research will be the further development of arrays of superconducting transition-edge sensors (TES) for imaging x-ray spectroscopy. We have developed a TES pixel that achieves better than 2.5-eV resolution at 6 keV, and arrays of such pixels that are sufficiently uniform in characteristics as to permit common biasing without significant compromises in the operation of any pixel. We are also making arrays of position sensitive TES pixels that show promise for use on IXO. We propose to advance both the single-pixel and position-sensitive arrays so that we can produce arrays suitable for subsystem-level read-out demonstrations of the IXO X-ray Microcalorimeter Spectrometer focal plane. Additionally, we propose to re-evaluate out successful pixel design which, while certainly suitable for use in developing the architecture of arrays and addressing detector systems issues, is not necessarily the final optimization. The performance of a TES depends on the functional form of the current, temperature, and magnetic-field dependence of the resistive transition, and also on the noise at each point on this transition surface. The parameters that describe this transition surface occupy a large phase space, and we have only probed a small portion of it. We propose to fabricate a series of test devices to explore other parts of the phase space and to learn how to engineer the superconducting transition. Recently, our understanding of the physical effects governing the observed resistive transitions has improved, th

SBU X-band Phased Array Radar (SKYLER) IMPACTS

The SBU X-band Phased Array Radar (SKYLER) IMPACTS dataset consists of polarimetric radar data collected by the Stony Brook University (SBU) X-band Phased Array Radar (SKYLER) during the Investigation of Microphysics and Precipitation for Atlantic Coast-Threatening Snowstorms (IMPACTS) field campaign. IMPACTS was a three-year sequence of winter season deployments conducted to study snowstorms over the U.S. Atlantic Coast (2020-2023). The campaign aimed to (1) Provide observations critical to understanding the mechanisms of snowband formation, organization, and evolution; (2) Examine how the microphysical characteristics and likely growth mechanisms of snow particles vary across snowbands; and (3) Improve snowfall remote sensing interpretation and modeling to significantly advance prediction capabilities. SKYLER provided detailed observations of cloud and precipitation microphysics, specifically ice and snow processes. These data include reflectivity, mean velocity, spectrum width, linear depolarization ratio, differential reflectivity, differential phase, specific differential phase, co-polarized correlation coefficient, and signal-to-noise ratio. The dataset files are available from January 17, 2022, through February 28, 2023, in netCDF-4 format.

GOES-R PLT Southern Ontario Lightning Mapping Array (LMA) V1

The GOES-R PLT Southern Ontario Lightning Mapping Array (LMA) dataset consists of total lightning data measured from the Southern Ontario LMA (SOLMA) network during the GOES-R Post Launch Test (PLT) airborne science field campaign. The GOES-R PLT airborne science field campaign took place in support of the post-launch product validation of the Advanced Baseline Imager (ABI) and the Geostationary Lightning Mapper (GLM). The LMA measures the arrival time of radiation from a lightning discharge at multiple stations and locates the sources of radiation to produce a three-dimensional map of total lightning activity. These data files are available in compressed ASCII files and are available from April 1, 2017 through June 1, 2017.

UARS Cryogenic Limb Array Etalon Spectrometer (CLAES) Level 3AL V009 (UARCL3AL) at GES DISC

The Cryogenic Limb Array Etalon Spectrometer (CLAES) Level 3AL data product consists of daily, 4 degree increment latitude-ordered vertical profiles of temperature and concentrations of O3, H2O, CH4, N2O, NO, NO2, N2O5, HNO3, ClONO2, HCl, CF2Cl2 (CFC-12), CFCl3 (CFC-11), and aerosol absorption coefficients. The instrument measured infrared thermal emissions at wavelengths from 3.5 to 12.7 microns. CLAES was flown on NASA's Upper Atmosphere Research Satellite (UARS) and designed to measure the chemical composition of the stratosphere and mesosphere, and also investigated the depletion of stratospheric ozone and ozone chemistry. Limb measurements were made in the altitude range between 10 and 60 km at about 2.5 km resolution. Data were collected between latitude 34S and 80N and 80S and 34N, alternating each satellite yaw cycle of about 36 days. The CLAES Level 3AL data were processed with the version 9 algorithm, except H2O which is version 7. The CLAES level 3AL product consists of 20 granules per day. A data granule is one CLAES species or subtype per day. Data are on the UARS standard pressure levels (in mbars) given by: P(i) = 1000 * 10**(-i/6) for i = 0, 1, 2, ... The data files are available in a binary record oriented format.

Magnetically-coupled microcalorimeter arrays for x-ray astrophysics with sub-eV spectral resolution and large format capability Project

"We propose to develop a revolutionary x-ray camera for astrophysical imaging spectroscopy. High-resolution x-ray spectroscopy is a powerful tool for studying the evolving universe. Emission line ratios (e.g. within the He-like triplet) provide density and temperature diagnostics. Emission and absorption line energies identify ions and determine their velocities, and the shape of the lines can be used to study turbulence or the relativistic effects of a supermassive black hole. The grating spectrometers on the XMM and Chandra satellites demonstrated the power of high-resolution x-ray spectroscopy for astrophysics, but there remains a need for instrumentation that can provide higher spectral resolution with high throughput in the Fe-K band and that can enable spatial/spectral investigations of extended sources, such as supernova remnants and galaxy clusters. The instrumentation needed is a broad-band imaging spectrometer - basically an x-ray camera that can precisely resolve x-ray energies and fluxes over a large field-of-view. While we do not claim that in 3 years we will have developed such detectors, we advocate developing the technology that has the greatest potential for achieving this. Theoretically, magnetically-coupled microcalorimeters are best equipped to achieve sub-eV energy resolution in very large formats. We propose to build upon the work carried out by our group on metallic magnetic calorimeters (MMC) in the antecedent program. The great promise of MMCs for sub-eV energy resolution has been recognized for years. During our current research program, an accident in detector fabrication produced devices that derived their sensitivity from a different operating principle - the temperature dependence of a superconduc

Silicon Micromachined Heterodyne Array Receiver at 1.9 THz Project

"We are proposing a new concept of integrated component development technology at submillimeter wavelengths that will dramatically simplify the fabrication, assembly, and integration of large focal plane arrays and imagers. This technology has the potential to significantly increase the pixel count of detector arrays and reduce the mass, volume, and complexity of array receivers for a broad range of applications in astrophysics and earth sciences. We will develop and demonstrate a highly integrated silicon-micromachined array receiver at 1.9 THz based on advanced dual-polarized, sideband-separating, balanced heterodyne mixers. The receiver front-end will be integrated with a novel micro-lens antenna array. We will design full-waveguide-band 90-degree quadrature hybrids, orthomode transducers (OMT), polarization twists, in-phase power splitters, and directional couplers at 1.9 THz; fabricate them using deep reactive ion etching (DRIE) based silicon micromachining, integrate them with existing HEB mixers at 1.9 THz; and test and fully characterize them in our laboratory. The scientific importance of high-resolution spectroscopic observations at submillimeter wavelengths is underscored by the key role of heterodyne spectrometers in the ESA cornerstone Herschel Space Observatory as well as the ground-based ALMA and airborne SOFIA. Star formation and key phases of galaxy evolution occur in region enshrouded by dust that obscures them at infrared and optical wavelengths, while the temperature range of the interstellar medium of ten to a few thousand Kelvin in these regions excites a wealth of submillimeter-wave spectral lines. With high-resolution spectroscopy, resolved line profiles reveal the dynamics of star formation, directly revealing details of turbulence, outflows, and core collapse. Observations of emission from ionized species such as C+ at 1900.53690 GHz (158 um), allow one to directly measure the cooling of the diffuse component of the interstellar m

GOES-R PLT Washington D.C. Lightning Mapping Array (LMA) V1

The GOES-R PLT Washington D.C. Lightning Mapping Array (LMA) dataset consists of total lightning data measured from the Washington D.C. LMA (DCLMA) network during the GOES-R Post Launch Test (PLT) airborne science field campaign. The GOES-R PLT airborne science field campaign took place in support of the post-launch product validation of the Advanced Baseline Imager (ABI) and the Geostationary Lightning Mapper (GLM). The LMA measures the arrival time of radiation from a lightning discharge at multiple stations and locates the sources of radiation to produce a three-dimensional map of total lightning activity. These data files are available in compressed ASCII files and are available from April 6, 2017 through June 1, 2017.

Permafrost Temperature Data from a Deep Borehole Array on the Arctic Slope of Alaska, 1973 - 2014, Version 1

These data consist of fully processed permafrost temperature data from borehole logs acquired by the U.S. Geological Survey (USGS) from the 24-element US Department of the Interior (DOI) Global Terrestrial Network for Permafrost (GTN-P) Deep Borehole Array in arctic Alaska beginning in 1973 and ending in 2014. The data represent the true temperatures in the wellbores and surrounding rocks at the time of the measurements.

GOES-R PLT Kennedy Space Center Lightning Mapping Array (LMA)

The GOES-R PLT Kennedy Space Center Lightning Mapping Array (LMA) dataset consists of total lightning data measured from the Kennedy Space Center LMA (KSCLMA) network during the GOES-R Post Launch Test (PLT) airborne science field campaign. The GOES-R PLT airborne science field campaign took place in support of the post-launch product validation of the Advanced Baseline Imager (ABI) and the Geostationary Lightning Mapper (GLM). The LMA measures the arrival time of radiation from a lightning discharge at multiple stations and locates the sources of radiation to produce a three-dimensional map of total lightning activity. These data files are available in compressed ASCII files and are available from March 1, 2017 through June 1, 2017.

GOES-R PLT Oklahoma Lightning Mapping Array (LMA) V1

The GOES-R PLT Oklahoma Lightning Mapping Array (LMA) dataset consists of total lightning data measured from the Oklahoma LMA (OKLMA) network during the GOES-R Post Launch Test (PLT) airborne science field campaign. The GOES-R PLT airborne science field campaign took place in support of the post-launch product validation of the Advanced Baseline Imager (ABI) and the Geostationary Lightning Mapper (GLM). The LMA measures the arrival time of radiation from a lightning discharge at multiple stations and locates the sources of radiation to produce a three-dimensional map of total lightning activity. These data files are available in compressed ASCII files and are available from March 1, 2017 through June 1, 2017.

Next Generation Microshutter Arrays Project

We propose to develop the next generation MicroShutter Array (MSA) as a multi-object field selector for missions anticipated in the next two decades. For many applications, this field selector improves instrument efficiency proportionally to the number of shutters opened simultaneously. We have successfully developed and built the JWST microshutter array system, which increases the observing efficiency of the Near Infrared Spectrometer by two orders of magnitude. As a result of this development, there is a significant scientific demand for these devices for space-based and ground based applications. The availability of large format microshutters can significantly increase the scientific reach of spectroscopic survey instrument such as WFIRST and future missions such as ATLAST. The basic design of the JWST MSA cannot be extended to such a large scales due to the design limitations set by the required magnetic actuation. We have recently demonstrated shutter operation using DC plus AC resonant pumping. The breakthrough demonstrates that we are able to eliminate bulky permanent magnets used for JWST MSA actuation, thus opening an avenue to create a very large focal plane field selector that can be built at much lower cost. in this program, we will fabricate electrostatically actuated microshutter arrays and demonstrate their performance for use as UV, visible, and infrared field selectors.

GOES-R PLT North Alabama Lightning Mapping Array (LMA)

The GOES-R PLT North Alabama Lightning Mapping Array (LMA) dataset consists of total lightning data measured from the North Alabama LMA (NALMA) network during the GOES-R Post Launch Test (PLT) airborne science field campaign. The GOES-R PLT airborne science field campaign took place in support of the post-launch product validation of the Advanced Baseline Imager (ABI) and the Geostationary Lightning Mapper (GLM). The LMA measures the arrival time of radiation from a lightning discharge at multiple stations and locates the sources of radiation to produce a three-dimensional map of total lightning activity. These data files are available in compressed ASCII files and are available from March 1, 2017 through June 1, 2017.

Global Ocean Biogeochemistry Array

The Global Ocean Biogeochemistry (GO-BGC) Array is a project funded by the US National Science Foundation (NSF Award 1946578 ) to build a global network of chemical and biological sensors that will monitor ocean health. This grant is being used to build and deploy 500 robotic ocean-monitoring floats around the globe as part of NSF’s Mid-scale Research Infrastructure-2 program. This network of floats is collecting data on the chemistry and the biology of the ocean from the surface to a depth of 2,000 meters, augmenting the existing Argo array that monitors ocean temperature and salinity. The GO-BGC Array is led by Director Ken Johnson and administered by the Monterey Bay Aquarium Research Institute. For questions specific to the HPLC/POC/PON data submitted to SeaBASS please contact Josh Plant at jplant@mbari.org.

Remote sensing of Electrification, Lightning, And Mesoscale/microscale Processes with Adaptive Ground Observations (RELAMPAGO) Lightning Mapping Array (LMA) V1

The Remote sensing of Electrification, Lightning, And Mesoscale/microscale Processes with Adaptive Ground Observations (RELAMPAGO) Lightning Mapping Array (LMA) was an 11-station, ground-based network located in north-central Argentina from November 2018 to April 2019 in support of the RELAMPAGO field campaign. The RELAMPAGO campaign aimed to characterize the atmospheric conditions and terrain effects that facilitate the initiation and growth of intense weather systems in this region of South America. The LMA maps Very High Frequency (VHF) emissions from lightning in three dimensions. These emissions have also been grouped, temporally and spatially, into individual flashes, and the flash characteristics analyzed to produce gridded products. The dataset was produced by NASA Marshall Space Flight Center (MSFC), via an agreement with the National Oceanic and Atmospheric Administration (NOAA), in order to serve as a validation dataset for the Geostationary Lightning Mapper (GLM). These LMA data are available from November 8, 2018 through April 20, 2019 in ASCII, HDF5, and netCDF-4 format.

GOES-R PLT Colorado Lightning Mapping Array (LMA)

The GOES-R PLT Colorado Lightning Mapping Array (LMA) dataset consists of total lightning data measured from the Colorado LMA (COLMA) network during the GOES-R Post Launch Test (PLT) airborne science field campaign. The GOES-R PLT airborne science field campaign took place in support of the post-launch product validation of the Advanced Baseline Imager (ABI) and the Geostationary Lightning Mapper (GLM). The LMA measures the arrival time of radiation from a lightning discharge at multiple stations and locates the sources of radiation to produce a three-dimensional map of total lightning activity. These data files are available in compressed ASCII files and are available from March 1, 2017 through May 31, 2017.

UARS Cryogenic Limb Array Etalon Spectrometer (CLAES) Level 3AT V009 (UARCL3AT) at GES DISC

The Cryogenic Limb Array Etalon Spectrometer (CLAES) Level 3AT data product consists of daily, 65.536 second interval time-ordered vertical profiles of temperature and concentrations of O3, H2O, CH4, N2O, NO, NO2, N2O5, HNO3, ClONO2, HCl, CF2Cl2 (CFC-12), CFCl3 (CFC-11), and aerosol absorption coefficients. The instrument measured infrared thermal emissions at wavelengths from 3.5 to 12.7 microns. CLAES was flown on NASA's Upper Atmosphere Research Satellite (UARS) and designed to measure the chemical composition of the stratosphere and mesosphere, and also investigated the depletion of stratospheric ozone and ozone chemistry. Limb measurements were made in the altitude range between 10 and 60 km at about 2.5 km resolution. Data were collected between latitude 34S and 80N and 80S and 34N, alternating each satellite yaw cycle of about 36 days. The CLAES Level 3AT data were processed with the version 9 algorithm, except H2O which is version 7. The CLAES level 3AL product consists of 20 granules per day. A data granule is one CLAES species or subtype per day. Data are on the UARS standard pressure levels (in mbars) given by: P(i) = 1000 * 10**(-i/6) for i = 0, 1, 2, ... The data files are available in a binary record oriented format.

JPSS-2 CrIS IMG_COL: Array indices for collocated VIIRS observations V3.0 (SNDRJ2CrISL1BIMGC) at GES DISC

The Cross-track Infrared Sounder (CrIS) Level 1B Full Spectral Resolution (FSR) data files contain radiance measurements along with ancillary spacecraft, instrument, and geolocation data of the CrIS instrument on the Joint Polar Satellite System-2 (JPSS-2) platform. This platform is also know as NOAA-21 (National Oceanic and Atmospheric Administration). The IMG product supplements the CrIS Level 1B (L1B) hyperspectral radiance product by providing collocated high-spatial resolution data from the Visible Infrared Imaging Radiometer Suite (VIIRS) imager located on the same platform. VIIRS radiance and cloud mask values are grouped and aggregated for every CrIS field of view (FOV) and made available in a format intended for use alongside the CrIS L1B data. The collocated VIIRS level 1 / cloud mask statistical summary (collection name SNDRJ2CrISL1BIMG) is the main product and consists of collocated CrIS field of views with the VIIRS cloud mask and radiances/reflectances. This can be thought of as a match-up between CrIS and VIIRS. The supplementary product, array indices for collocated VIIRS observations (SNDRJ2CrISL1BIMGC), product additionally makes available CrIS and VIIRS data array index values that result from the collocation process that is performed as part of producing IMG. These index values can be leveraged by end users to further augment CrIS data by extracting collocated observations from any additional VIIRS data products that aren’t already present in IMG. The FSR files have 2,223 channels (*2211 apodized channels): 637 (*633) shortwave channels from 3.9 to 4.7 microns (2555 to 2150 cm-1), 869 (*865) midwave channels from 5.7 to 8.05 microns (1752.5 to 1242.5 cm-1), and 717 (*713)longwave channels from 9.1 to 15.41 microns (1096.25 to 648.75 cm-1). Each CrIS field-of-regard (FOR) contains 9 field-of-views (FOVs) arranged in a 3X3 array. The Level 1B files contain 30 FORs in the cross track direction and 45 in the along track direction. Data products are constructed on six minute boundaries. The Visible Infrared Imaging Radiometer Suite (VIIRS) has 22 imaging and radiometric bands covering wavelengths from 0.41 to 12.5 microns. It provides the sensor data records for clouds, sea surface temperature, ocean color, and others. This IMG_COL product contains the colocation indices of the VIIRS pixels within each CrIS footprint.