{"project":{"acronym":"","projectId":94303,"title":"An Experimental Program to Achieve High Accuracy Atomic Rates for the X-ray Astrophysics Recovery Mission and Beyond","primaryTaxonomyNodes":[{"taxonomyNodeId":10741,"taxonomyRootId":8816,"parentNodeId":10740,"level":3,"code":"TX08.1.1","title":"Detectors and Focal Planes","definition":"Detectors, focal planes and readout integrated circuits provide large-format array technologies that require high quantum efficiency (QE); low noise, high resolution, uniform, and stable response; low power and cost; and high reliability. These technologies include low-noise, high-speed, low-power and radiation hardened readout integrated circuit (ROIC) electronics; superconducting sensors; spectral detectors; polarization-sensitive detectors; radiation-hardened detectors; and micro-Kelvin and sub-Kelvin high sensitivity detectors that cover the spectrum from submillimeter wave (Far-IR) to X-ray.","exampleTechnologies":"Backshort Undergrid bolometer arrays, Mercury Cadmium Telluride and Strained Superlattice Arrays, charge coupled devices, sidecar readout integrated circuits, radiometric calibration and abnormality correction algorithms (e.g. non-uniformity)","hasChildren":false,"hasInteriorContent":true}],"description":"We propose an experimental program to generate high accuracy atomic data for the Fe XXV and Fe XXVI emission diagnostics. Theoretical calculations of specific rate coefficients have estimated accuracies ranging from 5 to 30%. The individual uncertainties may translate into uncertainties on the measurement of interest, e.g. electron temperature, of 30%. EBIT measurements will test the existing theoretical calculations, both the line emission and the individual atomic rates for various processes, including excitation, recombination and ionization. We also measure the spectra of H- and He-like Ar for comparison to theory. For Ar the resonance line series will provide another benchmark for the atomic physics data. We will conduct the experiments at electron beam ion traps (EBITs) at NIST and Clemson University. We will explore in detail broad ranges in parameter space for which the accuracy of the atomic data might be low, e.g. near the threshold where resonances contribute to the collision strength. The EBIT measurements will help set priorities for future theoretical calculations. Our program will use the NIST EBIT combined with a pair of crystal spectrometers to (a) measure diagnostic line ratios over a range in parameter space; (b) conduct detailed experiments to assess the accuracy of rates for individual atomic processes; and, (c) evaluate the existing theory and determine its accuracy for input to AtomDB. We will use the EBIT at Clemson to extract and recombining ions to test recombination rates. We expect to make relatively rapid progress by regularly communicating the results from our experiments and assessments to the atomic physics and astrophysics communities. Cosmology using clusters of galaxies relies on a highly accurate measurement of the electron temperature. With current CCD spectra, the shape of the high energy continuum, dominanted by bremsstrahlung, provides the best temperature determination. The microcalorimeter on the X-ray Astrophysics Recovery Mission, as demonstrated by Hitomi, will easily determine the ratio of the fluxes of the strong allowed transitions of Fe XXV and Fe XXVI, as well as for the temperature-sensitive line ratio of the He-like Fe XXV for high signal-to-noise cluster data. Improvements to the accuracy of these diagnostics will significantly reduce the systematics from cluster cosmology. These data will also be of broad use for other sources as well. Our team will make improved atomic data available to the astronomy community in a timely manner through AtomDB.","destinations":[{"lkuCodeId":1547,"code":"OUTSIDE_SOLAR_SYSTEM","description":"Outside the Solar System","lkuCodeTypeId":526,"lkuCodeType":{"codeType":"DESTINATION_TYPE","description":"Destination Type"}}],"startYear":2018,"startMonth":1,"endYear":2020,"endMonth":12,"statusDescription":"Completed","principalInvestigators":[{"contactId":349451,"canUserEdit":false,"firstName":"Nancy","lastName":"Brickhouse","fullName":"Nancy S Brickhouse","fullNameInverted":"Brickhouse, Nancy S","middleInitial":"S","primaryEmail":"nbrickhouse@cfa.harvard.edu","publicEmail":false,"nacontact":false}],"programDirectors":[{"contactId":332808,"canUserEdit":false,"firstName":"Michael","lastName":"Garcia","fullName":"Michael A Garcia","fullNameInverted":"Garcia, Michael A","middleInitial":"A","publicEmail":false,"nacontact":false}],"programManagers":[{"contactId":123302,"canUserEdit":false,"firstName":"Dominic","lastName":"Benford","fullName":"Dominic J Benford","fullNameInverted":"Benford, Dominic J","middleInitial":"J","primaryEmail":"dominic.j.benford@nasa.gov","publicEmail":true,"nacontact":false}],"coInvestigators":[{"contactId":222431,"canUserEdit":false,"firstName":"Jill","lastName":"Robidoux","fullName":"Jill Robidoux","fullNameInverted":"Robidoux, Jill","primaryEmail":"jrobidoux@cfa.harvard.edu","publicEmail":false,"nacontact":false},{"contactId":502685,"canUserEdit":false,"firstName":"Yuri","lastName":"Ralchenko","fullName":"Yuri Ralchenko","fullNameInverted":"Ralchenko, Yuri","primaryEmail":"yuri.ralchenko@nist.gov","publicEmail":false,"nacontact":false},{"contactId":143983,"canUserEdit":false,"firstName":"Eric","lastName":"Silver","fullName":"Eric H Silver","fullNameInverted":"Silver, Eric H","middleInitial":"H","primaryEmail":"esilver@cfa.harvard.edu","publicEmail":false,"nacontact":false},{"contactId":185025,"canUserEdit":false,"firstName":"Igor","lastName":"Bray","fullName":"Igor Bray","fullNameInverted":"Bray, Igor","primaryEmail":"i.bray@curtin.edu.au","publicEmail":false,"nacontact":false},{"contactId":383115,"canUserEdit":false,"firstName":"Randall","lastName":"Smith","fullName":"Randall K Smith","fullNameInverted":"Smith, Randall K","middleInitial":"K","primaryEmail":"rsmith@cfa.harvard.edu","publicEmail":false,"nacontact":false},{"contactId":2591,"canUserEdit":false,"firstName":"Adam","lastName":"Foster","fullName":"Adam Foster","fullNameInverted":"Foster, Adam","primaryEmail":"afoster@cfa.harvard.edu","publicEmail":false,"nacontact":false},{"contactId":64347,"canUserEdit":false,"firstName":"Casey","lastName":"DeRoo","fullName":"Casey T Deroo","fullNameInverted":"DeRoo, Casey T","middleInitial":"T","primaryEmail":"casey.deroo@cfa.harvard.edu","publicEmail":false,"nacontact":false},{"contactId":416890,"canUserEdit":false,"firstName":"Ryan","lastName":"Allured","fullName":"Ryan Allured","fullNameInverted":"Allured, Ryan","primaryEmail":"rallured@cfa.harvard.edu","publicEmail":false,"nacontact":false},{"contactId":141286,"canUserEdit":false,"firstName":"Endre","lastName":"Takacs","fullName":"Endre Takacs","fullNameInverted":"Takacs, Endre","primaryEmail":"etakacs@clemson.edu","publicEmail":false,"nacontact":false}],"website":"","libraryItems":[],"transitions":[],"responsibleMd":{"acronym":"SMD","canUserEdit":false,"city":"","external":false,"linkCount":0,"organizationId":4909,"organizationName":"Science Mission Directorate","organizationType":"NASA_Mission_Directorate","naorganization":false,"organizationTypePretty":"NASA Mission Directorate"},"program":{"acronym":"APRA","active":true,"description":"
The Astrophysics Research Program competitively solicits low TRL (1-3) technology development activities of a more general nature through the Astrophysics Research and Analysis (APRA) Program element of ROSES. APRA is intended to support basic research of new technologies and feasibility demonstrations that may enable future science missions. For example, APRA seeks technology development of advanced detectors that may be proposed as instruments for future space flight experiments. APRA also supports suborbital science investigations that typically involve a significant level of technology development.
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The PCOS, COR, and EXEP programs develop and operate the Division’s strategic science missions. Thus, each of these programs conduct strategic technology development activities to enable future missions and to support early phase mission development. Each has a formal Technology Development Plan to guide its technology development activities, and maintains an annual report that documents the status of currently funded activities. Annual assessments identify future technology development needs based on the science goals of each program.
The PCOS, COR, and EXEP Programs conduct competed technology development efforts through a Research Opportunities in Space and Earth Science (ROSES) element known as Strategic Astrophysics Technology (SAT) that specifically targets technology developments that bridge the technology readiness level (TRL) 3-6 gap. SAT developed technologies are essential to enable strategic missions that specifically address the key science goals of the Astrophysics Decadal Survey recommendations. The three SAT elements for PCOS, COR, and EXEP are named Technology Development for Physics of the Cosmos (TPCOS), Technology Development for Cosmic Origins Program (TCOP), and Technology Development for Exo-Planet Missions (TDEM) respectively. In contrast to these competed efforts, each program also conducts directed technology development activities that are carried out as elements of specific strategic science missions during early development phases.
The Astrophysics Research Program competitively solicits low TRL (1-3) technology development activities of a more general nature through the Astrophysics Research and Analysis (APRA) Program element of ROSES. APRA is intended to support basic research of new technologies and feasibility demonstrations that may enable future science missions. For example, APRA seeks technology development of advanced detectors that may be proposed as instruments for future space flight experiments. APRA also supports suborbital science investigations that typically involve a significant level of technology development.
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