Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope
Creators
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Chichura, P. M.1
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Foster, A.2
- Patel, C.3
- Ossa-Jaen, N.4
- Ade, P. A. R.5
- Ahmed, Z.6, 7
- Anderson, A. J.1, 8
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Archipley, M.3, 9
- Austermann, J. E.10, 11
- Avva, J. S.12
- Balkenhol, L.13
- Barry, P. S.1, 14
- Thakur, R. Basu1, 15
- Beall, J. A.10
- Benabed, K.16
- Bender, A. N.1, 14
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Benson, B. A.1, 8
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Bianchini, F.6, 13
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Bleem, L. E.1, 14
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Bouchet, F. R.16
- Bryant, L.1
- Byrum, K.14
- Carlstrom, J. E.1, 14
- Carter, F. W.1, 14
- Cecil, T. W.14
- Chang, C. L.1, 14
- Chaubal, P.13
- Chen, G.1
- Chiang, H. C.17, 18
- Cho, H.-M.7
- Chou, T-L.1
- Citron, R.1
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Cliche, J.-F.17
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Crawford, T. M.1
- Crites, A. T.1, 19
- Cukierman, A.6, 7
- Daley, C. M.3
- Denison, E. V.10
- Dibert, K.1
- Ding, J.14
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Dobbs, M. A.17, 20
- Dutcher, D.1
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Everett, W.11
- Feng, C.21
- Ferguson, K. R.22
- Fu, J.3
- Galli, S.16
- Gallicchio, J.1, 23
- Gambrel, A. E.1
- Gardner, R. W.1
- George, E. M.12, 24
- Goeckner-Wald, N.6
- Gualtieri, R.14
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Guns, S.12
- Gupta, N.13
- Guyser, R.3
- Haan, T. de25
- Halverson, N. W.11
- Harke-Hosemann, A. H.3, 14
- Harrington, N. L.12
- Henning, J. W.1, 14
- Hilton, G. C.10
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Hivon, E.16
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Holder, G. P.3
- Holzapfel, W. L.12
- Hood, J. C.1
- Howe, D.1
- Hrubes, J. D.1
- Huang, N.12
- Hubmayr, J.10
- Irwin, K. D.6, 7
- Jeong, O. B.12
- Jonas, M.8
- Jones, A.1
- Khaire, T. S.14
- Knox, L.26
- Kofman, A. M.27
- Korman, M.2
- Kubik, D. L.8
- Kuhlmann, S.14
- Kuo, C.-L.6, 7
- Lee, A. T.12, 28
- Leitch, E. M.1
- Li, D.7, 10
- Lowitz, A.1
- Lu, C.3
- Marrone, D. P.29
- McMahon, J. J.1
- Meyer, S. S.1
- Michalik, D.1
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Millea, M.12
- Mocanu, L. M.1, 30
- Montgomery, J.17
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Moran, C. Corbett15
- Nadolski, A.3
- Natoli, T.1
- Nguyen, H.8
- Nibarger, J. P.10
- Noble, G.17
- Novosad, V.14
- Omori, Y.6
- Padin, S.1, 15
- Pan, Z.1, 14
- Paschos, P.1
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Patil, S.13
- Pearson, J.14
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Phadke, K. A.3
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Posada, C. M.14
- Prabhu, K.26
- Pryke, C.31
- Quan, W.1
- Rahlin, A.1, 8
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Reichardt, C. L.13
- Riebel, D.1
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Riedel, B.1
- Rouble, M.17
- Ruhl, J. E.2
- Saliwanchik, B. R.2, 32
- Sayre, J. T.11
- Schaffer, K. K.1, 33
- Schiappucci, E.13
- Shirokoff, E.1
- Sievers, C.1
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Smecher, G.34
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Sobrin, J. A.1
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Springmann, A.29
- Stark, A. A.35
- Stephen, J.1
- Story, K. T.6
- Suzuki, A.28
- Tandoi, C.3
- Thompson, K. L.6, 7
- Thorne, B.26
- Tucker, C.5
- Umilta, C.3
- Vale, L. R.10
- Veach, T.36
- Vieira, J. D.3, 9
- Wang, G.14
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Whitehorn, N.22, 37
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Wu, W. L. K.1, 6, 7
- Yefremenko, V.14
- Yoon, K. W.6, 7
- Young, M. R.19
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1.
University of Chicago
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2.
Case Western Reserve University
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3.
University of Illinois Urbana-Champaign
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4.
University of Redlands
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Cardiff University
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Stanford University
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SLAC National Accelerator Laboratory
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Fermilab
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National Center for Supercomputing Applications
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National Institute of Standards and Technology
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University of Colorado Boulder
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University of California, Berkeley
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University of Melbourne
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14.
Argonne National Laboratory
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California Institute of Technology
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16.
Institut d'Astrophysique de Paris
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17.
McGill University
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18.
University of KwaZulu-Natal
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University of Toronto
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Canadian Institute for Advanced Research
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University of Science and Technology of China
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22.
University of California, Los Angeles
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Harvey Mudd College
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European Southern Observatory
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High Energy Accelerator Research Organization
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University of California, Davis
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University of Pennsylvania
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Lawrence Berkeley National Laboratory
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University of Arizona
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30.
University of Oslo
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31.
University of Minnesota
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32.
Yale University
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33.
Art Institute of Chicago
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Three-Speed Logic (Canada)
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Harvard-Smithsonian Center for Astrophysics
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Southwest Research Institute
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37.
Michigan State University
Abstract
We present the first measurements of asteroids in millimeter wavelength data from the South Pole Telescope (SPT), which is used primarily to study the cosmic microwave background (CMB). We analyze maps of two ∼270 deg² sky regions near the ecliptic plane, each observed with the SPTpol camera ∼100 times over 1 month. We subtract the mean of all maps of a given field, removing static sky signal, and then average the mean-subtracted maps at known asteroid locations. We detect three asteroids -- (324) Bamberga, (13) Egeria, and (22) Kalliope -- with signal-to-noise ratios (S/N) of 11.2, 10.4, and 6.1, respectively, at 2.0 mm (150 GHz); we also detect (324) Bamberga with an S/N of 4.1 at 3.2 mm (95 GHz). We place constraints on these asteroids' effective emissivities, brightness temperatures, and light-curve modulation amplitude. Our flux density measurements of (324) Bamberga and (13) Egeria roughly agree with predictions, while our measurements of (22) Kalliope suggest lower flux, corresponding to effective emissivities of 0.64 ± 0.11 at 2.0 and < 0.47 at 3.2 mm. We predict the asteroids detectable in other SPT data sets and find good agreement with detections of (772) Tanete and (1093) Freda in recent data from the SPT-3G camera, which has ∼10× the mapping speed of SPTpol. This work is the first focused analysis of asteroids in data from CMB surveys, and it demonstrates we can repurpose historic and future data sets for asteroid studies. Future SPT measurements can help constrain the distribution of surface properties over a larger asteroid population.
Additional Information
This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00001.CAL. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. M.A. and J.V. acknowledge support from the Center for AstroPhysical Surveys at the National Center for Supercomputing Applications in Urbana, IL. J.V. acknowledges support from the Sloan Foundation. The authors thank Jeff McMahon 55 for support in manuscript preparation through the Science Writing Practicum taught as part of U. Chicago's "Data Science in Energy and Environmental Research" NRT training program, NSF grant #DGE-1735359.Additional details
Identifiers
- Eprint ID
- 117116
- Resolver ID
- CaltechAUTHORS:20220922-931611600.14
Funding
- National Science Foundation
- OPP-1852617
Dates
- Created
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2022-09-28Created from EPrint's datestamp field
- Updated
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2022-09-28Created from EPrint's last_modified field