Sub-percent precision in the primordial abundance of

Transcription

1 Sub-percent precision in the primordial abundance of Max Pettini Ryan Cooke

2 Deuterium is the baryometer of choice

3 Deuterium is the baryometer of choice

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5 Cen B1 III V =0.61 d = 120 pc

6 Cen B1 III V =0.61 d = 120 pc b < 0.067

7 Energy Levels *5-&"6+3) 7+8'+&.89) 15

8 Energy Levels blue-shift of 82 km/s *5-&"6+3) 7+8'+&.89) 15

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10 Quasar Image credit: ESO

11 10m Keck telescope + HIRES

12 10m Keck telescope + HIRES

13 10m Keck telescope + HIRES

14 10m Keck telescope + HIRES 10 5 D/H =2.3 ± 0.6

15 10m Keck telescope + HIRES 100 b h 2 =2.4 ± 0.6

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18 Column Density Distribution of Lya forest lines Zafar+ 2013

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21 Metallicity Distribution Rafelski et al. 2012

22 Metallicity Distribution These are the DLAs we re after Rafelski et al. 2012

23 Very Metal Poor DLAs are the choice astrophysical environments for measuring the primordial abundance of deuterium

24 Very Metal Poor DLAs are the choice astrophysical environments for measuring the primordial abundance of deuterium Low metallicities imply negligible astration of D

25 Very Metal Poor DLAs are the choice astrophysical environments for measuring the primordial abundance of deuterium Low metallicities imply negligible astration of D Narrow absorption lines make it possible to resolve the -82 km/s isotope shift between D and H

26 J Cooke+ 2015

27 J DLA at z = N(H I) = cm 2 Cooke+ 2015

28 J DLA at z = N(H I) = cm 2 Fe/H = 1/200 solar Cooke+ 2015

29 Very Metal Poor DLAs are the choice astrophysical environments for measuring the primordial abundance of deuterium Low metallicities imply negligible astration of D Narrow absorption lines make it possible to resolve the -82 km/s isotope shift between D and H High H I column densities give detectable D I lines in many transitions of the Lyman series

30 J , z= , Fe/H = 1/750 solar N(H I) = cm 2 Cooke+ 2014

31 J , z= , Fe/H = 1/750 solar Cooke+ 2014

32 30,000 s integration with UVES on VLT-2

33 Spectral analysis tailored specifically to the determination of D/H and its error Pettini & Cooke 2012

34 Spectral analysis tailored specifically to the determination of D/H and its error

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36 Percent Measure of (D/H) [Cooke et al. 2018]

37 Percent Measure of (D/H) [Cooke et al. 2018] 10 5 D/H =2.527 ± 0.030

38 100 b h 2 (BBN) = ± ± Cooke log 10 (D/H) [O/H] B,0 h 2

39 100 b h 2 (CMB) = ± Planck Coll log 10 (D/H) [O/H] B,0 h 2

40 100 b h 2 (BBN) = ± ± Cooke log 10 (D/H) [O/H] B,0 h 2

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43 Experiment Theory Broggini+ 2018

44 100 b h 2 (BBN) = ± ± Cooke log 10 (D/H) discrepancy B,0 h [O/H]

45 Joint D/H and CMB Constraints on `dark radiation N e =3.41 ± 0.45 Ne D/H CMB D/H+CMB B,0 h 2 Cooke+ 2018

46 Looking to the future...

47 Good prospects for further improvements in the near/medium term future

48 Good prospects for further improvements in the near/medium term future Three more metal-poor DLAs in the bag, bringing the total sample of high precision measures to 10 by the end of 2018.

49 Good prospects for further improvements in the near/medium term future Three more metal-poor DLAs in the bag, bringing the total sample of high precision measures to 10 by the end of Modern laboratory measurement of the cross-section for 2 H+p! 3 He + by the end of 2018.

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51 Good prospects for further improvements in the near/medium term future Three more metal-poor DLAs in the bag, bringing the total sample of high precision measures to 10 by the end of Modern laboratory measurement of the cross-section for 2 H+p! 3 He + by the end of m telescopes in mid-2020s

52 Good prospects for further improvements in the near/medium term future 30m telescopes in mid-2020s

53 Summary Herman With modern astronomical instrumentation, we can now verify experimentally the framework of Big-Bang nucleosynthesis which has its origin in ideas first put forward in the 1950s Hayashi Gamow Alpher

54 BBN CMB + = New Physics?

55 BBN CMB + = New Physics? Not yet...