National Academies Press: OpenBook
« Previous: 5 Techniques to Obtain NEO Sizes
Suggested Citation:"6 The Role of Archival Data." National Academies of Sciences, Engineering, and Medicine. 2019. Finding Hazardous Asteroids Using Infrared and Visible Wavelength Telescopes. Washington, DC: The National Academies Press. doi: 10.17226/25476.
×
Page 42
Suggested Citation:"6 The Role of Archival Data." National Academies of Sciences, Engineering, and Medicine. 2019. Finding Hazardous Asteroids Using Infrared and Visible Wavelength Telescopes. Washington, DC: The National Academies Press. doi: 10.17226/25476.
×
Page 43
Suggested Citation:"6 The Role of Archival Data." National Academies of Sciences, Engineering, and Medicine. 2019. Finding Hazardous Asteroids Using Infrared and Visible Wavelength Telescopes. Washington, DC: The National Academies Press. doi: 10.17226/25476.
×
Page 44

Below is the uncorrected machine-read text of this chapter, intended to provide our own search engines and external engines with highly rich, chapter-representative searchable text of each book. Because it is UNCORRECTED material, please consider the following text as a useful but insufficient proxy for the authoritative book pages.

6 The Role of Archival Data Although the committee was not directly charged with considering archival aspects, it deemed this matter highly relevant and crucial for the success of any near Earth object (NEO) survey mission. The committee was also concerned that new ground- and space-based systems may collect such large volumes of data that they could overwhelm the archives and the systems used to access them. Observations made both from the ground and from space retain value long after they are obtained because they are valuable in providing orbit improvement and characterization information. Hence, the proper archiving and hosting of any NEO survey data is crucial for the survey’s success and its legacy value. NEO survey data include image data, source and object catalogues, as well as calibration products that are necessary to fully understand the performance of the survey system. Image archives of the sky obtained at visual and infrared wavelengths are valuable because they may contain previously unrecognized detections of NEOs discovered by the space-based survey. Positions obtained from archived images often enable a significant improvement in the accuracy of an object’s orbit after its initial discovery. For example, discovery observations of the ~500-meter-diameter, potentially hazardous, asteroid Apophis indicated a potential impact in 2029. However, shortly after the recognition of its potentially hazardous nature, archived observations taken 3 months prior to its discovery were used to better calculate its orbit and rule out the possibility of an impact. Access to such “precovery data” requires both archival and public access to these data. Finding a precovery image is not simply a matter of finding images that should have been found originally, but rather of being able to search an image to lower signal-to-noise ratio. This is made possible because if it is known that an object is within, perhaps, 10 resolution elements of a given position, then a signal-to-noise ratio of 3, or even less, is adequate to identify an object compared with the original search having to identify the object at a signal-to-noise ratio of approximately 5 among 109 resolution elements. In addition, when searching for a precovery image, one knows the direction and rate of motion of the object and so can perform a moving co-add, which significantly increases the signal-to-noise ratio. Finally, newer, more accurate star catalogs (e.g., Gaia), enable old positions to be re-measured to higher accuracy than at the time they were taken. Catalogue data, including photometric source catalogues that tabulate brightness measurements taken over time, represent a higher-level product that is generated from the image data. The publication of such catalogues enables, for instance, the derivation of absolute magnitudes, which crucially support the data provided by a mid-infrared survey system by enabling the estimation of albedos and improving diameter estimates based on thermal models. Typically, researchers put a focus on the archiving aspect, which includes the storage and backup of data. However, recent technological developments enabled the real-time browsing and search through archival image and catalogue data (e.g., the Spitzer Heritage Archive1), and the Solar System Object 1 California Institute of Technology, 2018, Spitzer Heritage Archive, https://sha.ipac.caltech.edu/applications/Spitzer/SHA/. PREPUBLICATION COPY – SUBJECT TO FURTHER EDITORIAL CORRECTION 6-1

Image Search Tool by the Canadian Astronomy Data Centre2). Such tools have been proven immensely useful in the identification of precovery data as well as additional serendipitous observations to further constrain the physical and orbital properties of asteroids. Finding: Effective archiving will facilitate improved knowledge of the distribution of NEO physical properties, leading to more appropriate model parameters and increased accuracy of derived properties, such as size. Finding: Research using archival data can play and has played an important role in future threat evaluation and NEO science by the general research and planetary defense community. Archiving all data and images to support future improved thermal modeling, searching for serendipitous precovery observations, and other types of studies not considered during the survey mission is critical to detecting and characterizing NEOs. Currently, archiving of NEO-related data is mainly accomplished through three available services in the United States: the NASA Planetary Data System (PDS),3 the International Astronomical Union Minor Planet Center (MPC),4 and the NASA Infrared Science Archive (IRSA).5 PDS is NASA’s main hub for data archival of planetary data and mainly consists of isolated archive files; the MPC is the official clearing house for solar system objects and provides large databases of small-body observations and orbital properties; IRSA includes image and catalogue data from the Spitzer and Wide-Field Infrared Survey Explorer (WISE) space telescopes. The modus operandi for accessing data from these services varies significantly and often impedes the use of the data that is stored. Common issues are that data are isolated and cannot be queried in a meaningful way. For instance, archive files from the PDS and MPC have to be downloaded and information has to be extracted and combined locally. While IRSA provides a state-of-the art user interface, NEO flux data from the Near Earth Object Wide-Field Infrared Survey Explorer (NEOWISE) have to be extracted from source tables, involving highly time-consuming queries using other services. Furthermore, most current asteroid survey programs report only astrometry and, in some cases, photometry for some select observations to the MPC, making it hard to use the existing data for further characterization efforts. The publication of additional data products would be invaluable for the physical and orbital characterization of asteroids and hence relevant to this study. To the knowledge of this committee, there is currently no uniform NASA policy in place to track whether or how NEO survey data have to be archived. Finding: The current system for archiving NEO data is not optimized for accessing data and analyzing data in an automated fashion, and there is no consistent NASA policy on archiving NEO survey data. The committee heard from experts on data archiving and was reassured that storage capacity for data will not be a problem in the future, given regular and reasonable upgrades to storage systems. However, storage alone is insufficient. In order to leverage the legacy value of NEO survey missions, it is mandatory that all data products generated by the survey are properly archived and made public in a 2 Canadian Astronomy Data Centre, 2019, Solar System Object Image Search, http://www.cadc-ccda.hia- iha.nrc-cnrc.gc.ca/en/ssois/. 3 University of Maryland, 2019, NASA Planetary Data System: Small Bodies Node, https://pds- smallbodies.astro.umd.edu/. 4 Harvard & Smithsonian Center for Astrophysics and NASA, The International Astronomical Union Minor Planet Center, https://minorplanetcenter.net. 5 California Institute of Technology, NASA/IPAC Infrared Science Archive, https://irsa.ipac.caltech.edu/frontpage/. PREPUBLICATION COPY – SUBJECT TO FURTHER EDITORIAL CORRECTION 6-2

timely manner. The publication of such data enables not only the generation of higher-level data products that are relevant to threat evaluation, but also an independent verification of the results through the scientific community. Support for such efforts should continue to be provided by NASA, as is currently being done through the Near Earth Objects Observation (NEOO) program elements of Research Opportunities in Earth and Space Sciences (ROSES). Furthermore, it is mandatory for NASA to continue support for ground-based astrometric and photometric follow-up observations to improve orbital elements and provide additional characterization information. Recommendation: All observational data, both ground- and space-based, obtained under NASA funding supporting the George E. Brown, Jr. Near Earth Object Survey Act, should be archived in a publicly available database as soon as practicable after it is obtained. NASA should continue to support the utilization of such data and provide resources to extract near Earth object detections from legacy databases and those archived in future surveys and their associated follow-up programs. PREPUBLICATION COPY – SUBJECT TO FURTHER EDITORIAL CORRECTION 6-3

Next: 7 Impact Hazards Not Explicitly Considered by the George E. Brown, Jr. Act »
Finding Hazardous Asteroids Using Infrared and Visible Wavelength Telescopes Get This Book
×
Buy Paperback | $45.00
MyNAP members save 10% online.
Login or Register to save!
Download Free PDF

Near Earth objects (NEOs) have the potential to cause significant damage on Earth. In December 2018, an asteroid exploded in the upper atmosphere over the Bering Sea (western Pacific Ocean) with the explosive force of nearly 10 times that of the Hiroshima bomb. While the frequency of NEO impacts rises in inverse proportion to their sizes, it is still critical to monitor NEO activity in order to prepare defenses for these rare but dangerous threats.

Currently, NASA funds a network of ground-based telescopes and a single, soon-to-expire space-based asset to detect and track large asteroids that could cause major damage if they struck Earth. This asset is crucial to NEO tracking as thermal-infrared detection and tracking of asteroids can only be accomplished on a space-based platform.

Finding Hazardous Asteroids Using Infrared and Visible Wavelength Telescopes explores the advantages and disadvantages of infrared (IR) technology and visible wavelength observations of NEOs. This report reviews the techniques that could be used to obtain NEO sizes from an infrared spectrum and delineate the associated errors in determining the size. It also evaluates the strengths and weaknesses of these techniques and recommends the most valid techniques that give reproducible results with quantifiable errors.

  1. ×

    Welcome to OpenBook!

    You're looking at OpenBook, NAP.edu's online reading room since 1999. Based on feedback from you, our users, we've made some improvements that make it easier than ever to read thousands of publications on our website.

    Do you want to take a quick tour of the OpenBook's features?

    No Thanks Take a Tour »
  2. ×

    Show this book's table of contents, where you can jump to any chapter by name.

    « Back Next »
  3. ×

    ...or use these buttons to go back to the previous chapter or skip to the next one.

    « Back Next »
  4. ×

    Jump up to the previous page or down to the next one. Also, you can type in a page number and press Enter to go directly to that page in the book.

    « Back Next »
  5. ×

    To search the entire text of this book, type in your search term here and press Enter.

    « Back Next »
  6. ×

    Share a link to this book page on your preferred social network or via email.

    « Back Next »
  7. ×

    View our suggested citation for this chapter.

    « Back Next »
  8. ×

    Ready to take your reading offline? Click here to buy this book in print or download it as a free PDF, if available.

    « Back Next »
Stay Connected!