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Dark Energy Survey: A 2.1% Measurement of the Angular Baryonic Acoustic Oscillation Scale at Redshift $$z_{\rm eff}$$=0.85 from the Final Dataset

Journal Article · · TBD
OSTI ID:2349103
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  1. Cerro-Tololo InterAmerican Obs.
  2. Illinois U., Urbana (main)
  3. LIneA, Rio de Janeiro
  4. Fermilab
  5. U. Michigan, Ann Arbor
  6. Cambridge U., Inst. of Astron.; Princeton U., Astrophys. Sci. Dept.
  7. Madrid U.
  8. Barcelona, IFAE
  9. Portsmouth U., ICG
  10. Wisconsin U., Madison
  11. UPenn, Philadelphia
  12. Paris, Inst. Astrophys.
  13. Northeastern U.
  14. Munich U.
  15. University Coll. London
  16. KIPAC, Menlo Park; SLAC
  17. Sao Paulo, IFT; LIneA, Rio de Janeiro; Brookhaven
  18. IAC, La Laguna; LIneA, Rio de Janeiro; Laguna U., Tenerife
  19. Trieste Observ.
  20. Barcelona, IEEC
  21. William-Mary Coll.
  22. Zhongshan U., Zhuhai; Hong Kong U. Sci. Tech.
  23. Chicago U., Astron. Astrophys. Ctr.; Chicago U., KICP
  24. Jodrell Bank; Nottingham U.
  25. Trieste Observ.; IFPU, Trieste
  26. Hamburg Observ.
  27. Queensland U.
  28. Madrid, CIEMAT
  29. Indian Inst. Tech., Hyderabad
  30. Carnegie Mellon U.
  31. UPenn, Philadelphia; LPSC, Grenoble
  32. Chicago U., Astron. Astrophys. Ctr.; Fermilab; Chicago U., KICP
  33. Waterloo U.
  34. Caltech, JPL
  35. Inst. Theor. Astrophys., Oslo
  36. SLAC
  37. Fermilab; Chicago U., KICP
  38. Madrid, IFT
  39. Barcelona, IEEC; Portsmouth U., ICG
  40. Barcelona, IFAE; Chicago U., KICP
  41. Illinois U., Urbana (main); Illinois U., Urbana, Astron. Dept.
  42. Geneva Observ.
  43. UC, Santa Cruz
  44. Ohio State U., CCAPP; Ohio State U.
  45. Harvard-Smithsonian Ctr. Astrophys.
  46. Australia, CSIRO, North Ryde; Lowell Observ.
  47. ARC, Canberra; Australian Natl. U., Canberra (main); Australian Natl. U., Canberra
  48. Texas A-M
  49. Ohio State U., CCAPP; Ohio State U., Dept. Astron.
  50. Madrid, CIEMAT; LPSC, Grenoble
  51. ICREA, Barcelona; Barcelona, Autonoma U.; Barcelona, IFAE
  52. Garching, Max Planck Inst., MPE; Munich U.
  53. Princeton U., Astrophys. Sci. Dept.
  54. Surrey U.
  55. Rio de Janeiro Observ.
  56. Waterloo U.; Perimeter Inst. Theor. Phys.
  57. LIneA, Rio de Janeiro; Rio de Janeiro Observ.
  58. Ruhr U., Bochum
  59. Chicago U., Astron. Astrophys. Ctr.; Nordita
  60. IJCLab, Orsay; Madrid, IFT
  61. Sussex U., Astron. Ctr.
  62. Ohio State U., CCAPP
  63. Rio Grande do Sul U.; LIneA, Rio de Janeiro
  64. Brookhaven
  65. Southampton U.
  66. ORNL, Oak Ridge (main)
  67. Duke U.
  68. Australian Natl. U., Canberra
  69. U. Michigan, Ann Arbor; LBL, Berkeley
+ Show Author Affiliations
We present the angular diameter distance measurement obtained with the Baryonic Acoustic Oscillation feature from galaxy clustering in the completed Dark Energy Survey, consisting of six years (Y6) of observations. We use the Y6 BAO galaxy sample, optimized for BAO science in the redshift range 0.6<$$z$$<1.2, with an effective redshift at $$z_{\rm eff}$$=0.85 and split into six tomographic bins. The sample has nearly 16 million galaxies over 4,273 square degrees. Our consensus measurement constrains the ratio of the angular distance to sound horizon scale to $$D_M(z_{\rm eff})/r_d$$ = 19.51$$\pm$$0.41 (at 68.3% confidence interval), resulting from comparing the BAO position in our data to that predicted by Planck $$\Lambda$$CDM via the BAO shift parameter $$\alpha=(D_M/r_d)/(D_M/r_d)_{\rm Planck}$$. To achieve this, the BAO shift is measured with three different methods, Angular Correlation Function (ACF), Angular Power Spectrum (APS), and Projected Correlation Function (PCF) obtaining $$\alpha=$$ 0.952$$\pm$$0.023, 0.962$$\pm$$0.022, and 0.955$$\pm$$0.020, respectively, which we combine to $$\alpha=$$ 0.957$$\pm$$0.020, including systematic errors. When compared with the $$\Lambda$$CDM model that best fits Planck data, this measurement is found to be 4.3% and 2.1$$\sigma$$ below the angular BAO scale predicted. To date, it represents the most precise angular BAO measurement at $$z$$>0.75 from any survey and the most precise measurement at any redshift from photometric surveys. The analysis was performed blinded to the BAO position and it is shown to be robust against analysis choices, data removal, redshift calibrations and observational systematics.
Research Organization:
SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States); Brookhaven National Laboratory (BNL), Upton, NY (United States)
Sponsoring Organization:
USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
Contributing Organization:
DES
DOE Contract Number:
AC02-07CH11359
OSTI ID:
2349103
Report Number(s):
FERMILAB-PUB-24-0027-PPD; arXiv:2402.10696; oai:inspirehep.net:2759202
Journal Information:
TBD, Journal Name: TBD
Country of Publication:
United States
Language:
English

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