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Asteroid Measurements at Millimeter Wavelengths with the South Pole Telescope

Journal Article · · Astrophys.J.
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  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.
+ Show Author Affiliations
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:
Argonne National Laboratory (ANL), Argonne, IL (United States); Arizona U.; Arizona U., Astron. Dept. - Steward Observ.; Caltech; Canadian Inst. Advanced Res.; Cardiff U.; Case Western Reserve U.; Case Western Reserve U., CERCA; Chicago U.; Chicago U., Astron. Astrophys. Ctr.; Chicago U., EFI; Chicago U., KICP; Colorado U.; European Southern Observ.; Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Harvard-Smithsonian Ctr. Astrophys.; Harvey Mudd Coll.; Hefei, CUST; Illinois U., Urbana; Illinois U., Urbana, Astron. Dept.; Inst. Theor. Astrophys., Oslo; KEK, Tsukuba; KwaZulu Natal U.; LBNL, Berkeley; Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States); McGill U.; Melbourne U.; Michigan State U.; Minnesota U.; NIST, Boulder; Paris, Inst. Astrophys.; Pennsylvania U., Dept. Math.; SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Stanford U.; Stanford U., HEPL; Texas U., San Antonio; Toronto U., Astron. Dept.; UC, Berkeley; UC, Davis; UCLA; Unlisted, CA; Yale U.
Sponsoring Organization:
US Department of Energy; USDOE Office of Science (SC), High Energy Physics (HEP)
Contributing Organization:
SPT Collaboration
Grant/Contract Number:
AC02-06CH11357; AC02-07CH11359
OSTI ID:
1893728
Alternate ID(s):
OSTI ID: 1960018
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

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79 ASTRONOMY AND ASTROPHYSICS
asteroid surfaces
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