Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope

Journal Article · 31 August 2022 · Astrophys.J.

DOI: https://doi.org/10.3847/1538-4357/ac89ec · OSTI ID:1893728

Chichura, P. M.  ^[1]; Foster, A.  ^[2]; Patel, C. ^[3]; Ossa-Jaen, N. ^[4]; Ade, P. A.R. ^[5]; Ahmed, Z. ^[6]; Anderson, A. J.  ^[7]; Archipley, M. ^[8]; Austermann, J. E. ^[9]; Avva, J. S. ^[10]; Balkenhol, L. ^[11]; Barry, P. S.  ^[12]; Basu Thakur, R. ^[13]; Beall, J. A. ^[14]; Benabed, K. ^[15]; Bender, A. N. ^[12]; Benson, B. A.  ^[16]; Bianchini, F.  ^[17]; Bleem, L. E.  ^[12]; Bouchet, F. R. ^[15] ; Bryant, L. ^[18]; Byrum, K. ^[19]; Carlstrom, J. E. ^[20]; Carter, F. W. ^[12]; Cecil, T. W.  ^[19]; Chang, C. L. ^[21]; Chaubal, P. ^[11]; Chen, G. ^[18]; Chiang, H. C. ^[22]; Cho, H.-M. ^[23]; Chou, T-L. ^[1]; Citron, R. ^[18]; Cliche, J.-F. ^[24]; Crawford, T. M.  ^[25]; Crites, A. T. ^[26]; Cukierman, A. ^[27]; Daley, C. M. ^[8]; Denison, E. V. ^[14]; Dibert, K.  ^[28]; Ding, J. ^[19]; Dobbs, M. A. ^[29]; Dutcher, D. ^[1]; Everett, W. ^[30]; Feng, C. ^[31]; Ferguson, K. R. ^[32]; Fu, J. ^[8]; Galli, S. ^[15]; Gallicchio, J. ^[33]; Gambrel, A. E. ^[34]; Gardner, R. W. ^[18]; George, E. M. ^[35]; Goeckner-Wald, N. ^[36]; Gualtieri, R. ^[19]; Guns, S. ^[10]; Gupta, N. ^[11]; Guyser, R. ^[8]; de Haan, T. ^[37]; Halverson, N. W. ^[30]; Harke-Hosemann, A. H. ^[38]; Harrington, N. L. ^[10]; Henning, J. W. ^[12]; Hilton, G. C. ^[14]; Hivon, E. ^[15]; Holder, G. P.  ^[3]; Holzapfel, W. L. ^[10]; Hood, J. C. ^[34]; Howe, D. ^[18]; Hrubes, J. D. ^[18]; Huang, N. ^[10]; Hubmayr, J.  ^[14]; Irwin, K. D. ^[39]; Jeong, O. B. ^[10]; Jonas, M. ^[40]; Jones, A. ^[18]; Khaire, T. S. ^[19]; Knox, L. ^[41]; Kofman, A. M. ^[42]; Korman, M. ^[2]; Kubik, D. L. ^[40]; Kuhlmann, S. ^[19]; Kuo, C.-L. ^[39]; Lee, A. T. ^[43]; Leitch, E. M. ^[25]; Li, D. ^[44]; Lowitz, A. ^[34]; Lu, C. ^[3]; Marrone, D. P. ^[45]; McMahon, J. J. ^[46]; Meyer, S. S. ^[46]; Michalik, D. ^[18]; Millea, M.  ^[10]; Mocanu, L. M. ^[47]; Montgomery, J.  ^[24]; Moran, C. Corbett ^[48]; Nadolski, A. ^[8]; Natoli, T. ^[25]; Nguyen, H. ^[40]; Nibarger, J. P. ^[14]; Noble, G. ^[24]; Novosad, V. ^[19]; Omori, Y. ^[49]; Padin, S. ^[13]; Pan, Z.  ^[50]; Paschos, P. ^[18]; Patil, S. ^[11]; Pearson, J. ^[19]; Phadke, K. A. ^[8]; Posada, C. M. ^[19]; Prabhu, K. ^[41]; Pryke, C. ^[51]; Quan, W. ^[1]; Rahlin, A. ^[7]; Reichardt, C. L.  ^[11]; Riebel, D. ^[18]; Riedel, B. ^[18]; Rouble, M. ^[24]; Ruhl, J. E. ^[2]; Saliwanchik, B. R. ^[52]; Sayre, J. T. ^[30]; Schaffer, K. K. ^[53]; Schiappucci, E. ^[11]; Shirokoff, E. ^[25]; Sievers, C. ^[18]; Smecher, G. ^[54]; Sobrin, J. A. ^[1]; Springmann, A. ^[55]; Stark, A. A. ^[56]; Stephen, J. ^[18]; Story, K. T. ^[49]; Suzuki, A. ^[57]; Tandoi, C. ^[8]; Thompson, K. L. ^[39]; Thorne, B. ^[41]; Tucker, C. ^[5]; Umilta, C. ^[3]; Vale, L. R. ^[14]; Veach, T. ^[58]; Vieira, J. D. ^[59]; Wang, G. ^[19]; Whitehorn, N.  ^[60]; Wu, W. L.K.  ^[61]; Yefremenko, V. ^[19]; Yoon, K. W. ^[39]; Young, M. R. ^[62]

---

1. Chicago U., EFI; Chicago U., KICP
2. Case Western Reserve U.
3. Illinois U., Urbana
4. LLNL, Livermore
5. Cardiff U.
6. KIPAC, Menlo Park; Stanford U., HEPL; SLAC
7. Fermilab; Chicago U., KICP
8. Illinois U., Urbana, Astron. Dept.
9. NIST, Boulder; Colorado U.
10. UC, Berkeley
11. Melbourne U.
12. Argonne; Chicago U., KICP
13. Chicago U., KICP; Caltech
14. NIST, Boulder
15. Paris, Inst. Astrophys.
16. Fermilab; Chicago U., KICP; Chicago U., Astron. Astrophys. Ctr.
17. KIPAC, Menlo Park; Stanford U., HEPL; Stanford U.; Melbourne U.
18. Chicago U., EFI
19. Argonne
20. Chicago U., KICP; Chicago U., EFI; Argonne; Chicago U., Astron. Astrophys. Ctr.
21. Argonne; Chicago U., KICP; Chicago U., Astron. Astrophys. Ctr.
22. McGill U.; KwaZulu Natal U.
23. SLAC
24. McGill U.
25. Chicago U., KICP; Chicago U., Astron. Astrophys. Ctr.
26. Chicago U., KICP; Chicago U., Astron. Astrophys. Ctr.; Toronto U., Astron. Dept.
27. KIPAC, Menlo Park; Stanford U., HEPL; SLAC; Stanford U.
28. Chicago U., Astron. Astrophys. Ctr.; Chicago U., KICP
29. McGill U.; Canadian Inst. Advanced Res.
30. Colorado U.
31. Hefei, CUST
32. UCLA
33. Chicago U., KICP; Harvey Mudd Coll.
34. Chicago U., KICP
35. European Southern Observ.; UC, Berkeley
36. Stanford U.; KIPAC, Menlo Park; Stanford U., HEPL
37. KEK, Tsukuba
38. Argonne; Illinois U., Urbana, Astron. Dept.
39. KIPAC, Menlo Park; Stanford U., HEPL; Stanford U.; SLAC
40. Fermilab
41. UC, Davis
42. Pennsylvania U., Dept. Math.
43. UC, Berkeley; LBNL, Berkeley
44. NIST, Boulder; SLAC
45. Arizona U., Astron. Dept. - Steward Observ.
46. Chicago U., KICP; Chicago U., EFI; Chicago U., Astron. Astrophys. Ctr.
47. Chicago U., KICP; Chicago U., Astron. Astrophys. Ctr.; Inst. Theor. Astrophys., Oslo
48. Caltech
49. KIPAC, Menlo Park; Stanford U., HEPL; Stanford U.
50. Argonne; Chicago U., KICP; Chicago U., EFI
51. Minnesota U.
52. Case Western Reserve U., CERCA; Yale U.
53. Chicago U., KICP; Chicago U., EFI; Chicago U.
54. Unlisted, CA
55. Arizona U.
56. Harvard-Smithsonian Ctr. Astrophys.
57. LBNL, Berkeley
58. Texas U., San Antonio
59. Illinois U., Urbana; Illinois U., Urbana, Astron. Dept.
60. Michigan State U.; UCLA
61. KIPAC, Menlo Park; Stanford U., HEPL; SLAC; Chicago U., KICP
62. Toronto U., Astron. Dept.

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.

• Research Organization: Paris, Inst. Astrophys.; Stanford U.; UC, Davis; Colorado U.; KwaZulu Natal U.; Stanford U., HEPL; Argonne National Laboratory (ANL), Argonne, IL (United States); Case Western Reserve U.; Canadian Inst. Advanced Res.; Minnesota U.; Yale U.; LBNL, Berkeley; Chicago U., EFI; Caltech; Toronto U., Astron. Dept.; Case Western Reserve U., CERCA; Inst. Theor. Astrophys., Oslo; SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Unlisted, CA; Cardiff U.; NIST, Boulder; Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States); Chicago U., KICP; Pennsylvania U., Dept. Math.; Harvard-Smithsonian Ctr. Astrophys.; Illinois U., Urbana, Astron. Dept.; KEK, Tsukuba; Texas U., San Antonio; Michigan State U.; Hefei, CUST; Chicago U.; Melbourne U.; Illinois U., Urbana; Arizona U., Astron. Dept. - Steward Observ.; Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Harvey Mudd Coll.; Arizona U.; European Southern Observ.; Chicago U., Astron. Astrophys. Ctr.; UCLA; UC, Berkeley; McGill U.
• Sponsoring Organization: US Department of Energy
• Grant/Contract Number: AC02-07CH11359
• OSTI ID: 1893728
• Report Number(s): FERMILAB-PUB-22-769-PPD; oai:inspirehep.net:2167221; arXiv:2202.01406
• Journal Information: Astrophys.J., Journal Name: Astrophys.J. Journal Issue: 2 Vol. 936
• Country of Publication: United States
• Language: English