Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope
We present the first measurements of asteroids in millimeter wavelength (mm) data from the South Pole Telescope (SPT), which is used primarily to study the cosmic microwave background (CMB). We analyze maps of two \(\sim270\) deg\(^2\) sky regions near the ecliptic plane, each observed with the SPTp...
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| creator | Chichura, P M Foster, A Ossa-Jaen, N Ade, P A R Ahmed, Z Archipley, M Avva, J S Balkenhol, L Barry, P S R Basu Thakur Beall, J A Benabed, K Benson, B A Bianchini, F Bouchet, F R Bryant, L Byrum, K Carter, F W Cecil, T W Chang, C L Chaubal, P Chen, G Chiang, H C T-L Chou Crawford, T M Cukierman, A Denison, E V Dibert, K Dobbs, M A Dutcher, D Feng, C Ferguson, K R Gallicchio, J Gambrel, A E Gardner, R W Goeckner-Wald, N Gualtieri, R Guns, S Gupta, N Guyser, R Harke-Hosemann, A H Harrington, N L Hilton, G C Hivon, E Holzapfel, W L Hood, J C Howe, D Hrubes, J D Huang, N Irwin, K D Jeong, O B Jonas, M Jones, A Khaire, T S Kofman, A M Kubik, D L Kuhlmann, S C -L Kuo Leitch, E M Lowitz, A Marrone, D P McMahon, J J Meyer, S S Millea, M Montgomery, J C Corbett Moran Nadolski, A Natoli, T Nguyen, H Novosad, V Omori, Y Padin, S Pan, Z Pearson, J Posada, C M Prabhu, K Pryke, C Rahlin, A Reichardt, C L Riebel, D Riedel, B Rouble, M Sayre, J T Schaffer, K K Schiappucci, E Sievers, C Smecher, G Sobrin, J A Springmann, A Stephen, J Story, K T Suzuki, A Tandoi, C Thorne, B Vale, L R Veach, T Vieira, J D Whitehorn, N Wu, W L K Yefremenko, V |
| description | We present the first measurements of asteroids in millimeter wavelength (mm) data from the South Pole Telescope (SPT), which is used primarily to study the cosmic microwave background (CMB). We analyze maps of two \(\sim270\) deg\(^2\) sky regions near the ecliptic plane, each observed with the SPTpol camera \(\sim100\) times over one 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\(\text{ -- }\)(324) Bamberga, (13) Egeria, and (22) Kalliope\(\text{ -- }\)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 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 \(0.66 \pm 0.11\) at 2.0 mm and \( |
| doi_str_mv | 10.48550/arxiv.2202.01406 |
| format | Article |
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We analyze maps of two \(\sim270\) deg\(^2\) sky regions near the ecliptic plane, each observed with the SPTpol camera \(\sim100\) times over one 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\(\text{ -- }\)(324) Bamberga, (13) Egeria, and (22) Kalliope\(\text{ -- }\)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 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 \(0.66 \pm 0.11\) at 2.0 mm and \(<0.47\) at 3.2mm. We predict the asteroids detectable in other SPT datasets and find good agreement with detections of (772) Tanete and (1093) Freda in recent data from the SPT-3G camera, which has \(\sim10 \times\) 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 datasets for asteroid studies. Future SPT measurements can help constrain the distribution of surface properties over a larger asteroid population.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2202.01406</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Asteroid detection ; Asteroids ; Brightness temperature ; Cameras ; Cosmic microwave background ; Datasets ; Flux density ; Light curve ; Physics - Earth and Planetary Astrophysics ; South Pole ; Surface properties</subject><ispartof>arXiv.org, 2023-04</ispartof><rights>2023. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,777,781,882,27906</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2202.01406$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.3847/1538-4357/ac89ec$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Chichura, P M</creatorcontrib><creatorcontrib>Foster, A</creatorcontrib><creatorcontrib>Ossa-Jaen, N</creatorcontrib><creatorcontrib>Ade, P A R</creatorcontrib><creatorcontrib>Ahmed, Z</creatorcontrib><creatorcontrib>Archipley, M</creatorcontrib><creatorcontrib>Avva, J S</creatorcontrib><creatorcontrib>Balkenhol, L</creatorcontrib><creatorcontrib>Barry, P S</creatorcontrib><creatorcontrib>R Basu Thakur</creatorcontrib><creatorcontrib>Beall, J A</creatorcontrib><creatorcontrib>Benabed, K</creatorcontrib><creatorcontrib>Benson, B A</creatorcontrib><creatorcontrib>Bianchini, F</creatorcontrib><creatorcontrib>Bouchet, F R</creatorcontrib><creatorcontrib>Bryant, L</creatorcontrib><creatorcontrib>Byrum, K</creatorcontrib><creatorcontrib>Carter, F W</creatorcontrib><creatorcontrib>Cecil, T W</creatorcontrib><creatorcontrib>Chang, C L</creatorcontrib><creatorcontrib>Chaubal, P</creatorcontrib><creatorcontrib>Chen, G</creatorcontrib><creatorcontrib>Chiang, H C</creatorcontrib><creatorcontrib>T-L Chou</creatorcontrib><creatorcontrib>Crawford, T M</creatorcontrib><creatorcontrib>Cukierman, A</creatorcontrib><creatorcontrib>Denison, E V</creatorcontrib><creatorcontrib>Dibert, K</creatorcontrib><creatorcontrib>Dobbs, M A</creatorcontrib><creatorcontrib>Dutcher, D</creatorcontrib><creatorcontrib>Feng, C</creatorcontrib><creatorcontrib>Ferguson, K R</creatorcontrib><creatorcontrib>Gallicchio, J</creatorcontrib><creatorcontrib>Gambrel, A E</creatorcontrib><creatorcontrib>Gardner, R W</creatorcontrib><creatorcontrib>Goeckner-Wald, N</creatorcontrib><creatorcontrib>Gualtieri, R</creatorcontrib><creatorcontrib>Guns, S</creatorcontrib><creatorcontrib>Gupta, N</creatorcontrib><creatorcontrib>Guyser, R</creatorcontrib><creatorcontrib>Harke-Hosemann, A H</creatorcontrib><creatorcontrib>Harrington, N L</creatorcontrib><creatorcontrib>Hilton, G C</creatorcontrib><creatorcontrib>Hivon, E</creatorcontrib><creatorcontrib>Holzapfel, W L</creatorcontrib><creatorcontrib>Hood, J C</creatorcontrib><creatorcontrib>Howe, D</creatorcontrib><creatorcontrib>Hrubes, J D</creatorcontrib><creatorcontrib>Huang, N</creatorcontrib><creatorcontrib>Irwin, K D</creatorcontrib><creatorcontrib>Jeong, O B</creatorcontrib><creatorcontrib>Jonas, M</creatorcontrib><creatorcontrib>Jones, A</creatorcontrib><creatorcontrib>Khaire, T S</creatorcontrib><creatorcontrib>Kofman, A M</creatorcontrib><creatorcontrib>Kubik, D L</creatorcontrib><creatorcontrib>Kuhlmann, S</creatorcontrib><creatorcontrib>C -L Kuo</creatorcontrib><creatorcontrib>Leitch, E M</creatorcontrib><creatorcontrib>Lowitz, A</creatorcontrib><creatorcontrib>Marrone, D P</creatorcontrib><creatorcontrib>McMahon, J J</creatorcontrib><creatorcontrib>Meyer, S S</creatorcontrib><creatorcontrib>Millea, M</creatorcontrib><creatorcontrib>Montgomery, J</creatorcontrib><creatorcontrib>C Corbett Moran</creatorcontrib><creatorcontrib>Nadolski, A</creatorcontrib><creatorcontrib>Natoli, T</creatorcontrib><creatorcontrib>Nguyen, H</creatorcontrib><creatorcontrib>Novosad, V</creatorcontrib><creatorcontrib>Omori, Y</creatorcontrib><creatorcontrib>Padin, S</creatorcontrib><creatorcontrib>Pan, Z</creatorcontrib><creatorcontrib>Pearson, J</creatorcontrib><creatorcontrib>Posada, C M</creatorcontrib><creatorcontrib>Prabhu, K</creatorcontrib><creatorcontrib>Pryke, C</creatorcontrib><creatorcontrib>Rahlin, A</creatorcontrib><creatorcontrib>Reichardt, C L</creatorcontrib><creatorcontrib>Riebel, D</creatorcontrib><creatorcontrib>Riedel, B</creatorcontrib><creatorcontrib>Rouble, M</creatorcontrib><creatorcontrib>Sayre, J T</creatorcontrib><creatorcontrib>Schaffer, K K</creatorcontrib><creatorcontrib>Schiappucci, E</creatorcontrib><creatorcontrib>Sievers, C</creatorcontrib><creatorcontrib>Smecher, G</creatorcontrib><creatorcontrib>Sobrin, J A</creatorcontrib><creatorcontrib>Springmann, A</creatorcontrib><creatorcontrib>Stephen, J</creatorcontrib><creatorcontrib>Story, K T</creatorcontrib><creatorcontrib>Suzuki, A</creatorcontrib><creatorcontrib>Tandoi, C</creatorcontrib><creatorcontrib>Thorne, B</creatorcontrib><creatorcontrib>Vale, L R</creatorcontrib><creatorcontrib>Veach, T</creatorcontrib><creatorcontrib>Vieira, J D</creatorcontrib><creatorcontrib>Whitehorn, N</creatorcontrib><creatorcontrib>Wu, W L K</creatorcontrib><creatorcontrib>Yefremenko, V</creatorcontrib><title>Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope</title><title>arXiv.org</title><description>We present the first measurements of asteroids in millimeter wavelength (mm) data from the South Pole Telescope (SPT), which is used primarily to study the cosmic microwave background (CMB). We analyze maps of two \(\sim270\) deg\(^2\) sky regions near the ecliptic plane, each observed with the SPTpol camera \(\sim100\) times over one 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\(\text{ -- }\)(324) Bamberga, (13) Egeria, and (22) Kalliope\(\text{ -- }\)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 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 \(0.66 \pm 0.11\) at 2.0 mm and \(<0.47\) at 3.2mm. We predict the asteroids detectable in other SPT datasets and find good agreement with detections of (772) Tanete and (1093) Freda in recent data from the SPT-3G camera, which has \(\sim10 \times\) 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 datasets for asteroid studies. Future SPT measurements can help constrain the distribution of surface properties over a larger asteroid population.</description><subject>Asteroid detection</subject><subject>Asteroids</subject><subject>Brightness temperature</subject><subject>Cameras</subject><subject>Cosmic microwave background</subject><subject>Datasets</subject><subject>Flux density</subject><subject>Light curve</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>South Pole</subject><subject>Surface properties</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotj0tLw0AUhQdBsNT-AFcOuE6cufNIsizFFzQotOAyTJIbk5KXM5Oq_97YuricC-dwOB8hN5yFMlaK3Rv73RxDAAYh45LpC7IAIXgQS4ArsnLuwBgDHYFSYkHStfNoh6akKRo3Weyw944aT9OmbZsOZ5e-myO22H_42tGvxtfU10h3wzR_b0OLdD-7rhhGvCaXlWkdrv51SXaPD_vNc7B9fXrZrLeBSZQOhKikzrECbeKiqlDFYEyUaI66zKNICskg57EUoIsIeJlgkSNLGIvnixKxJLfn1hNqNtqmM_Yn-0POTshz4u6cGO3wOaHz2WGYbD9PykCDklwlEsQv6JJY6w</recordid><startdate>20230421</startdate><enddate>20230421</enddate><creator>Chichura, P M</creator><creator>Foster, A</creator><creator>Ossa-Jaen, N</creator><creator>Ade, P A R</creator><creator>Ahmed, Z</creator><creator>Archipley, M</creator><creator>Avva, J S</creator><creator>Balkenhol, 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arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20230421</creationdate><title>Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope</title><author>Chichura, P M ; Foster, A ; Ossa-Jaen, N ; Ade, P A R ; Ahmed, Z ; Archipley, M ; Avva, J S ; Balkenhol, L ; Barry, P S ; R Basu Thakur ; Beall, J A ; Benabed, K ; Benson, B A ; Bianchini, F ; Bouchet, F R ; Bryant, L ; Byrum, K ; Carter, F W ; Cecil, T W ; Chang, C L ; Chaubal, P ; Chen, G ; Chiang, H C ; T-L Chou ; Crawford, T M ; Cukierman, A ; Denison, E V ; Dibert, K ; Dobbs, M A ; Dutcher, D ; Feng, C ; Ferguson, K R ; Gallicchio, J ; Gambrel, A E ; Gardner, R W ; Goeckner-Wald, N ; Gualtieri, R ; Guns, S ; Gupta, N ; Guyser, R ; Harke-Hosemann, A H ; Harrington, N L ; Hilton, G C ; Hivon, E ; Holzapfel, W L ; Hood, J C ; Howe, D ; Hrubes, J D ; Huang, N ; Irwin, K D ; Jeong, O B ; Jonas, M ; Jones, A ; Khaire, T S ; Kofman, A M ; Kubik, D L ; Kuhlmann, S ; C -L Kuo ; Leitch, E M ; Lowitz, A ; Marrone, D P ; McMahon, J J ; Meyer, S S ; Millea, M ; Montgomery, J ; C Corbett Moran ; Nadolski, A ; Natoli, T ; Nguyen, H ; Novosad, V ; Omori, Y ; Padin, S ; Pan, Z ; Pearson, J ; Posada, C M ; Prabhu, K ; Pryke, C ; Rahlin, A ; Reichardt, C L ; Riebel, D ; Riedel, B ; Rouble, M ; Sayre, J T ; Schaffer, K K ; Schiappucci, E ; Sievers, C ; Smecher, G ; Sobrin, J A ; Springmann, A ; Stephen, J ; Story, K T ; Suzuki, A ; Tandoi, C ; Thorne, B ; Vale, L R ; Veach, T ; Vieira, J D ; Whitehorn, N ; Wu, W L K ; Yefremenko, V</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a956-33f46bef26a8cffe582aa7961e6db7743402b184326c721d9ecbe09008900793</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Asteroid detection</topic><topic>Asteroids</topic><topic>Brightness temperature</topic><topic>Cameras</topic><topic>Cosmic microwave background</topic><topic>Datasets</topic><topic>Flux density</topic><topic>Light curve</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>South Pole</topic><topic>Surface properties</topic><toplevel>online_resources</toplevel><creatorcontrib>Chichura, P M</creatorcontrib><creatorcontrib>Foster, A</creatorcontrib><creatorcontrib>Ossa-Jaen, N</creatorcontrib><creatorcontrib>Ade, P A R</creatorcontrib><creatorcontrib>Ahmed, Z</creatorcontrib><creatorcontrib>Archipley, M</creatorcontrib><creatorcontrib>Avva, J S</creatorcontrib><creatorcontrib>Balkenhol, L</creatorcontrib><creatorcontrib>Barry, P S</creatorcontrib><creatorcontrib>R Basu Thakur</creatorcontrib><creatorcontrib>Beall, J A</creatorcontrib><creatorcontrib>Benabed, K</creatorcontrib><creatorcontrib>Benson, B A</creatorcontrib><creatorcontrib>Bianchini, F</creatorcontrib><creatorcontrib>Bouchet, F R</creatorcontrib><creatorcontrib>Bryant, L</creatorcontrib><creatorcontrib>Byrum, K</creatorcontrib><creatorcontrib>Carter, F W</creatorcontrib><creatorcontrib>Cecil, T W</creatorcontrib><creatorcontrib>Chang, C L</creatorcontrib><creatorcontrib>Chaubal, P</creatorcontrib><creatorcontrib>Chen, G</creatorcontrib><creatorcontrib>Chiang, H C</creatorcontrib><creatorcontrib>T-L Chou</creatorcontrib><creatorcontrib>Crawford, T M</creatorcontrib><creatorcontrib>Cukierman, A</creatorcontrib><creatorcontrib>Denison, E V</creatorcontrib><creatorcontrib>Dibert, K</creatorcontrib><creatorcontrib>Dobbs, M A</creatorcontrib><creatorcontrib>Dutcher, D</creatorcontrib><creatorcontrib>Feng, 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A</creatorcontrib><creatorcontrib>Khaire, T S</creatorcontrib><creatorcontrib>Kofman, A M</creatorcontrib><creatorcontrib>Kubik, D L</creatorcontrib><creatorcontrib>Kuhlmann, S</creatorcontrib><creatorcontrib>C -L Kuo</creatorcontrib><creatorcontrib>Leitch, E M</creatorcontrib><creatorcontrib>Lowitz, A</creatorcontrib><creatorcontrib>Marrone, D P</creatorcontrib><creatorcontrib>McMahon, J J</creatorcontrib><creatorcontrib>Meyer, S S</creatorcontrib><creatorcontrib>Millea, M</creatorcontrib><creatorcontrib>Montgomery, J</creatorcontrib><creatorcontrib>C Corbett Moran</creatorcontrib><creatorcontrib>Nadolski, A</creatorcontrib><creatorcontrib>Natoli, T</creatorcontrib><creatorcontrib>Nguyen, H</creatorcontrib><creatorcontrib>Novosad, V</creatorcontrib><creatorcontrib>Omori, Y</creatorcontrib><creatorcontrib>Padin, S</creatorcontrib><creatorcontrib>Pan, Z</creatorcontrib><creatorcontrib>Pearson, J</creatorcontrib><creatorcontrib>Posada, C M</creatorcontrib><creatorcontrib>Prabhu, K</creatorcontrib><creatorcontrib>Pryke, C</creatorcontrib><creatorcontrib>Rahlin, A</creatorcontrib><creatorcontrib>Reichardt, C L</creatorcontrib><creatorcontrib>Riebel, D</creatorcontrib><creatorcontrib>Riedel, B</creatorcontrib><creatorcontrib>Rouble, M</creatorcontrib><creatorcontrib>Sayre, J T</creatorcontrib><creatorcontrib>Schaffer, K K</creatorcontrib><creatorcontrib>Schiappucci, E</creatorcontrib><creatorcontrib>Sievers, C</creatorcontrib><creatorcontrib>Smecher, G</creatorcontrib><creatorcontrib>Sobrin, J A</creatorcontrib><creatorcontrib>Springmann, A</creatorcontrib><creatorcontrib>Stephen, J</creatorcontrib><creatorcontrib>Story, K T</creatorcontrib><creatorcontrib>Suzuki, A</creatorcontrib><creatorcontrib>Tandoi, C</creatorcontrib><creatorcontrib>Thorne, B</creatorcontrib><creatorcontrib>Vale, L R</creatorcontrib><creatorcontrib>Veach, T</creatorcontrib><creatorcontrib>Vieira, J D</creatorcontrib><creatorcontrib>Whitehorn, N</creatorcontrib><creatorcontrib>Wu, W L K</creatorcontrib><creatorcontrib>Yefremenko, V</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Chichura, P M</au><au>Foster, A</au><au>Ossa-Jaen, N</au><au>Ade, P A R</au><au>Ahmed, Z</au><au>Archipley, M</au><au>Avva, J S</au><au>Balkenhol, L</au><au>Barry, P S</au><au>R Basu Thakur</au><au>Beall, J A</au><au>Benabed, K</au><au>Benson, B A</au><au>Bianchini, F</au><au>Bouchet, F R</au><au>Bryant, L</au><au>Byrum, K</au><au>Carter, F W</au><au>Cecil, T W</au><au>Chang, C L</au><au>Chaubal, P</au><au>Chen, G</au><au>Chiang, H C</au><au>T-L Chou</au><au>Crawford, T M</au><au>Cukierman, A</au><au>Denison, E V</au><au>Dibert, K</au><au>Dobbs, M A</au><au>Dutcher, D</au><au>Feng, C</au><au>Ferguson, K R</au><au>Gallicchio, J</au><au>Gambrel, A E</au><au>Gardner, R W</au><au>Goeckner-Wald, N</au><au>Gualtieri, R</au><au>Guns, S</au><au>Gupta, N</au><au>Guyser, R</au><au>Harke-Hosemann, A H</au><au>Harrington, N L</au><au>Hilton, G C</au><au>Hivon, E</au><au>Holzapfel, W L</au><au>Hood, J C</au><au>Howe, D</au><au>Hrubes, J D</au><au>Huang, N</au><au>Irwin, K D</au><au>Jeong, O B</au><au>Jonas, M</au><au>Jones, A</au><au>Khaire, T S</au><au>Kofman, A M</au><au>Kubik, D L</au><au>Kuhlmann, S</au><au>C -L Kuo</au><au>Leitch, E M</au><au>Lowitz, A</au><au>Marrone, D P</au><au>McMahon, J J</au><au>Meyer, S S</au><au>Millea, M</au><au>Montgomery, J</au><au>C Corbett Moran</au><au>Nadolski, A</au><au>Natoli, T</au><au>Nguyen, H</au><au>Novosad, V</au><au>Omori, Y</au><au>Padin, S</au><au>Pan, Z</au><au>Pearson, J</au><au>Posada, C M</au><au>Prabhu, K</au><au>Pryke, C</au><au>Rahlin, A</au><au>Reichardt, C L</au><au>Riebel, D</au><au>Riedel, B</au><au>Rouble, M</au><au>Sayre, J T</au><au>Schaffer, K K</au><au>Schiappucci, E</au><au>Sievers, C</au><au>Smecher, G</au><au>Sobrin, J A</au><au>Springmann, A</au><au>Stephen, J</au><au>Story, K T</au><au>Suzuki, A</au><au>Tandoi, C</au><au>Thorne, B</au><au>Vale, L R</au><au>Veach, T</au><au>Vieira, J D</au><au>Whitehorn, N</au><au>Wu, W L K</au><au>Yefremenko, V</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope</atitle><jtitle>arXiv.org</jtitle><date>2023-04-21</date><risdate>2023</risdate><eissn>2331-8422</eissn><abstract>We present the first measurements of asteroids in millimeter wavelength (mm) data from the South Pole Telescope (SPT), which is used primarily to study the cosmic microwave background (CMB). We analyze maps of two \(\sim270\) deg\(^2\) sky regions near the ecliptic plane, each observed with the SPTpol camera \(\sim100\) times over one 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\(\text{ -- }\)(324) Bamberga, (13) Egeria, and (22) Kalliope\(\text{ -- }\)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 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 \(0.66 \pm 0.11\) at 2.0 mm and \(<0.47\) at 3.2mm. We predict the asteroids detectable in other SPT datasets and find good agreement with detections of (772) Tanete and (1093) Freda in recent data from the SPT-3G camera, which has \(\sim10 \times\) 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 datasets for asteroid studies. Future SPT measurements can help constrain the distribution of surface properties over a larger asteroid population.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2202.01406</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2023-04 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_2202_01406 |
| source | arXiv.org; Free E- Journals |
| subjects | Asteroid detection Asteroids Brightness temperature Cameras Cosmic microwave background Datasets Flux density Light curve Physics - Earth and Planetary Astrophysics South Pole Surface properties |
| title | Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope |
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