Variability of the proton-to-electron mass ratio on cosmological scales
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1 Variability of the proton-to-electron mass ratio on cosmological scales Quasar absorption line spectroscopy Martin Wendt Hamburger Sternwarte Osservatorio Astronomico di Trieste, November 28th Variability of the proton-to-electron mass ratio on cosmological scales p.
2 Overview Short introduction of theory behind variation How is variation reflected in observations? Molecular Hydrogen H 2 Methods involved Analysis Summary and Outlook Variability of the proton-to-electron mass ratio on cosmological scales p.
3 Theory of shilly-shally constants Variability of the proton-to-electron mass ratio on cosmological scales p.
4 Theory of shilly-shally constants Kaluza-Klein theories Theodor Kaluza: generalisation of Einstein s GTR and the Maxwell equations in five dimensions in 1921 Variability of the proton-to-electron mass ratio on cosmological scales p.
5 Theory of shilly-shally constants Kaluza-Klein theories Theodor Kaluza: generalisation of Einstein s GTR and the Maxwell equations in five dimensions in 1921 Oscar Klein: fifth dimension possibly curled up Variability of the proton-to-electron mass ratio on cosmological scales p.
6 Theory of shilly-shally constants Kaluza-Klein theories Theodor Kaluza: generalisation of Einstein s GTR and the Maxwell equations in five dimensions in 1921 Oscar Klein: fifth dimension possibly curled up fundamental constants only constant in e.g. five-dimensional space Variability of the proton-to-electron mass ratio on cosmological scales p.
7 Theory of shilly-shally constants Kaluza-Klein theories Theodor Kaluza: generalisation of Einstein s GTR and the Maxwell equations in five dimensions in 1921 Oscar Klein: fifth dimension possibly curled up fundamental constants only constant in e.g. five-dimensional space observed constants a mere projection Variability of the proton-to-electron mass ratio on cosmological scales p.
8 Theory of shilly-shally constants Kaluza-Klein theories Theodor Kaluza: generalisation of Einstein s GTR and the Maxwell equations in five dimensions in 1921 Oscar Klein: fifth dimension possibly curled up fundamental constants only constant in e.g. five-dimensional space observed constants a mere projection another byproduct: scalar field as possible source for acceleration Variability of the proton-to-electron mass ratio on cosmological scales p.
9 How to measure variation? possible variation of the finestructure constant α = e 2 /4π c 1/137. Results under heavy debate. Variability of the proton-to-electron mass ratio on cosmological scales p.
10 How to measure variation? possible variation of the finestructure constant α = e 2 /4π c 1/137. Results under heavy debate. variation of the gravitational constant G N. Recent paper last week: Ġ N /G N yr 1. Variability of the proton-to-electron mass ratio on cosmological scales p.
11 How to measure variation? Variability of the proton-to-electron mass ratio on cosmological scales p.
12 How to measure variation? possible variation of the proton-to-electron mass ratio µ = m p m e. µ 0 = (85) (Mohr & Taylor 2000) Variability of the proton-to-electron mass ratio on cosmological scales p.
13 How to measure variation? possible variation of the proton-to-electron mass ratio µ = m p m e. µ 0 = (85) (Mohr & Taylor 2000) laboratory experiments not yet very accurate (5 years) Variability of the proton-to-electron mass ratio on cosmological scales p.
14 How to measure variation? possible variation of the proton-to-electron mass ratio µ = m p m e. µ 0 = (85) (Mohr & Taylor 2000) laboratory experiments not yet very accurate (5 years) measure possible variation on cosmological scales Variability of the proton-to-electron mass ratio on cosmological scales p.
15 How to measure variation? molecular hydrogen H 2 - energy levels E total = E electronic + E vibration + E rotation (BOA) Variability of the proton-to-electron mass ratio on cosmological scales p.
16 How to measure variation? molecular hydrogen H 2 - energy levels E total = E electronic + E vibration + E rotation (BOA) vibrational: E v = ( v + 2) 1 ωosc Variability of the proton-to-electron mass ratio on cosmological scales p.
17 How to measure variation? molecular hydrogen H 2 - energy levels E total = E electronic + E vibration + E rotation (BOA) vibrational: E v = ( v + 2) 1 ωosc with ω osc = 1 2πc k µ Variability of the proton-to-electron mass ratio on cosmological scales p.
18 How to measure variation? molecular hydrogen H 2 - energy levels E total = E electronic + E vibration + E rotation (BOA) vibrational: E v = ( v + 2) 1 ωosc with ω osc = 1 2πc k µ the classical oscillation frequency dependent on the reduced mass as µ 1 2. Variability of the proton-to-electron mass ratio on cosmological scales p.
19 How to measure variation? molecular hydrogen H 2 - energy levels rotational: I = m 1m 2 m 1 +m 2 r 2 0 = µr 2 o Variability of the proton-to-electron mass ratio on cosmological scales p.
20 How to measure variation? molecular hydrogen H 2 - energy levels rotational: I = m 1m 2 m 1 +m 2 r 2 0 = µr 2 o E J = BJ(J + 1);J = 0, 1, 2, 3,... Variability of the proton-to-electron mass ratio on cosmological scales p.
21 How to measure variation? molecular hydrogen H 2 - energy levels rotational: I = m 1m 2 m 1 +m 2 r 2 0 = µr 2 o E J = BJ(J + 1);J = 0, 1, 2, 3,... B = h 8π 2 Ic Variability of the proton-to-electron mass ratio on cosmological scales p.
22 How to measure variation? molecular hydrogen H 2 - energy levels rotational: I = m 1m 2 m 1 +m 2 r 2 0 = µr 2 o E J = BJ(J + 1);J = 0, 1, 2, 3,... B = h 8π 2 Ic rotational transitions are proportional to µ 1 Variability of the proton-to-electron mass ratio on cosmological scales p.
23 How to measure variation? homonuclear molecule - no detectable mere vibrational or rotational spectrum Variability of the proton-to-electron mass ratio on cosmological scales p.
24 How to measure variation? homonuclear molecule - no detectable mere vibrational or rotational spectrum only observable in combinations with electronic transitions (UV-Band) Variability of the proton-to-electron mass ratio on cosmological scales p.
25 How to measure variation? homonuclear molecule - no detectable mere vibrational or rotational spectrum only observable in combinations with electronic transitions (UV-Band) UV radiation is a very efficient dissociator of H 2, so any H 2 that survived would presumably be located inside very dense interstellar clouds. Variability of the proton-to-electron mass ratio on cosmological scales p.
26 How to measure variation? homonuclear molecule - no detectable mere vibrational or rotational spectrum only observable in combinations with electronic transitions (UV-Band) UV radiation is a very efficient dissociator of H 2, so any H 2 that survived would presumably be located inside very dense interstellar clouds. So far observations have borne out this supposition. Variability of the proton-to-electron mass ratio on cosmological scales p.
27 How to measure variation? molecular hydrogen H 2 Variability of the proton-to-electron mass ratio on cosmological scales p. 1
28 How to measure variation? molecular hydrogen H 2 electron-vibro-rotational transitions depend on reduced mass of molecule different dependence for different transitions Variability of the proton-to-electron mass ratio on cosmological scales p. 1
29 How to measure variation? molecular hydrogen H 2 electron-vibro-rotational transitions depend on reduced mass of molecule different dependence for different transitions distinguish cosmological redshift of a line from the shift caused by possible variation of µ Variability of the proton-to-electron mass ratio on cosmological scales p. 1
30 How to measure variation? molecular hydrogen H 2 electron-vibro-rotational transitions depend on reduced mass of molecule different dependence for different transitions distinguish cosmological redshift of a line from the shift caused by possible variation of µ λ obs = λ rest (1 + z abs )(1 + K i µ µ ) Variability of the proton-to-electron mass ratio on cosmological scales p. 1
31 How to measure variation? molecular hydrogen H 2 electron-vibro-rotational transitions depend on reduced mass of molecule different dependence for different transitions distinguish cosmological redshift of a line from the shift caused by possible variation of µ λ obs = λ rest (1 + z abs )(1 + K i µ µ ) Variability of the proton-to-electron mass ratio on cosmological scales p. 1
32 How to measure variation? molecular hydrogen H 2 electron-vibro-rotational transitions depend on reduced mass of molecule different dependence for different transitions distinguish cosmological redshift of a line from the shift caused by possible variation of µ λ obs = λ rest (1 + z abs )(1 + K i µ µ ) (Varshalovich & Levshakov 1993) Variability of the proton-to-electron mass ratio on cosmological scales p. 1
33 How to measure variation? sensitivity coefficient K i = d ln λ0 i d ln µ Variability of the proton-to-electron mass ratio on cosmological scales p. 1
34 How to measure variation? sensitivity coefficient K i = d ln λ0 i d ln µ sensitivity coefficient K i Werner Lyman restframe wavelength [Å] (Reinhold et al. 2006) Variability of the proton-to-electron mass ratio on cosmological scales p. 1
35 extragalactic H 2 local observations with UV-satellite COPERNICUS Variability of the proton-to-electron mass ratio on cosmological scales p. 1
36 extragalactic H 2 local observations with UV-satellite COPERNICUS the most abundant molecule in space Variability of the proton-to-electron mass ratio on cosmological scales p. 1
37 extragalactic H 2 local observations with UV-satellite COPERNICUS the most abundant molecule in space formation on dust grains Variability of the proton-to-electron mass ratio on cosmological scales p. 1
38 extragalactic H 2 local observations with UV-satellite COPERNICUS the most abundant molecule in space formation on dust grains shielding from UVB vs. dust obscuration Variability of the proton-to-electron mass ratio on cosmological scales p. 1
39 extragalactic H 2 local observations with UV-satellite COPERNICUS the most abundant molecule in space formation on dust grains shielding from UVB vs. dust obscuration transitions in UV (restframe) redshiftet into visual band Variability of the proton-to-electron mass ratio on cosmological scales p. 1
40 extragalactic H 2 highly inhomogeneous, clumpy distribution [1] [1] H.Hirashita, A.Ferrara, K.Wada, P.Richter,P.2003, MNRAS, 341, L18 Variability of the proton-to-electron mass ratio on cosmological scales p. 1
![extragalactic H 2 highly inhomogeneous, clumpy distribution [1] observable only in dense systems [1] H.Hirashita, A.](/docs-images/93/113048991/images/41-0.jpg "Ferrara, K.Wada, P.Richter,P.")
41 extragalactic H 2 highly inhomogeneous, clumpy distribution [1] observable only in dense systems [1] H.Hirashita, A.Ferrara, K.Wada, P.Richter,P.2003, MNRAS, 341, L18 Variability of the proton-to-electron mass ratio on cosmological scales p. 1
42 Quasar absorption line spectroscopy Variability of the proton-to-electron mass ratio on cosmological scales p. 1
43 Quasar absorption line spectroscopy rotating massive black hole hot, dense accretion disk small dense emission line clouds torus of cooler gas and dust accelerated jets of relativistic particles to large scale radio lobes Variability of the proton-to-electron mass ratio on cosmological scales p. 1
44 Quasar absorption line spectroscopy Variability of the proton-to-electron mass ratio on cosmological scales p. 1
45 Quasar absorption line spectroscopy cosmological redshift z due to expansion of space. Variability of the proton-to-electron mass ratio on cosmological scales p. 1
46 Quasar absorption line spectroscopy cosmological redshift z due to expansion of space. λ obs = λ rest (1 + z abs ) Variability of the proton-to-electron mass ratio on cosmological scales p. 1
47 Quasar absorption line spectroscopy cosmological redshift z due to expansion of space. λ obs = λ rest (1 + z abs ) Quasars as bright distant background sources against which intervening gas can be observed. Variability of the proton-to-electron mass ratio on cosmological scales p. 1
48 Quasar absorption line spectroscopy cosmological redshift z due to expansion of space. λ obs = λ rest (1 + z abs ) Quasars as bright distant background sources against which intervening gas can be observed. e.g., the Lyα transition at λ rest = Å Variability of the proton-to-electron mass ratio on cosmological scales p. 1
49 Quasar absorption line spectroscopy (Springel et. al 2006) Variability of the proton-to-electron mass ratio on cosmological scales p. 1
50 Quasar absorption line spectra - probing the universe Q a.u observed wavelength [Å] Variability of the proton-to-electron mass ratio on cosmological scales p. 1
51 Quasar absorption line spectra - probing the universe Q a.u observed wavelength [Å] L6R2 a.u. 100 a.u. 100 W3Q1 L14R1 H I Ly β observed wavelength [Å] observed wavelength [Å] Variability of the proton-to-electron mass ratio on cosmological scales p. 1
52 Quasar absorption line spectra - probing the universe Variability of the proton-to-electron mass ratio on cosmological scales p. 1
53 Quasar absorption line spectra - probing the universe H 2 lines in DLA systems Variability of the proton-to-electron mass ratio on cosmological scales p. 2
54 Quasar absorption line spectra - probing the universe H 2 lines in DLA systems contaminated continuum Variability of the proton-to-electron mass ratio on cosmological scales p. 2
55 Quasar absorption line spectra - probing the universe H 2 lines in DLA systems contaminated continuum 300 L5P1 200 L5R1 a.u observed wavelength [Å] Variability of the proton-to-electron mass ratio on cosmological scales p. 2
56 Quasar absorption line spectra - probing the universe H 2 lines in DLA systems contaminated continuum 300 L5P1 200 L5R1 a.u observed wavelength [Å] (Ivanchik et al. 2005) Variability of the proton-to-electron mass ratio on cosmological scales p. 2
57 Quasar absorption line spectra - probing the universe simulated fits to estimate accuracy Variability of the proton-to-electron mass ratio on cosmological scales p. 2
58 Quasar absorption line spectra - probing the universe simulated fits to estimate accuracy 0.35 fit of synthesized line 0.30 true positioning error [Å] synthesized H 2 line synthesized H I line + continuum 0.05 resulting error relative lineposition [Å] Variability of the proton-to-electron mass ratio on cosmological scales p. 2
59 Quasar absorption line spectra - probing the universe simulated fits to estimate accuracy 0.35 fit of synthesized line component fit line with S/N = true positioning error [Å] synthesized H 2 line synthesized H I line + continuum true positioning error [Å] resulting error relative lineposition [Å] relative lineposition [Å] Variability of the proton-to-electron mass ratio on cosmological scales p. 2
60 Variability of the proton-to-electron mass ratio on cosmological scales p. 2
61 mean error of position [Å] mean true error output from fit mean error of position [Å] mean true error relative line position [Å] relative line position [Å] Variability of the proton-to-electron mass ratio on cosmological scales p. 2
![0.20 0.20 mean error of position [Å] 0.15 0.10 0.05 mean true error output from fit mean error of position [Å] 0.15 0.10 0.05 mean true error 0.00 2.0 1.5 1.0 0.5 0.0 0.5 1.0 1.5 2.](/docs-images/93/113048991/images/62-0.jpg "0 relative line position [Å] 0.00 2.0 1.5 1.0 0.5 0.0 0.5 1.0 1.5 2.0 relative line position [Å] 0.20 0.20 0.15 0.15 net shift in position [Å] 0.10 0.05 0.00 0.05 net shift in position [Å] 0.10 0.05 0.00 0.05 0.10 0.10 0.15 2.")
62 mean error of position [Å] mean true error output from fit mean error of position [Å] mean true error relative line position [Å] relative line position [Å] net shift in position [Å] net shift in position [Å] relative line position [Å] relative line position [Å] Variability of the proton-to-electron mass ratio on cosmological scales p. 2
63 b = (1 + z abs ) µ µ Variability of the proton-to-electron mass ratio on cosmological scales p. 2
64 b = (1 + z abs ) µ µ J=1 J=2 J=3 1.5 relative redshift z i sensitivity coefficient K i corresponding to µ µ = 2.1 ± (Reinhold et al. 2006: µ µ = 2.0 ± ) Variability of the proton-to-electron mass ratio on cosmological scales p. 2
65 b = (1 + z abs ) µ µ J=1 3 J=3 redshift z i K i K i Variability of the proton-to-electron mass ratio on cosmological scales p. 2
66 b = (1 + z abs ) µ µ J=1 3 J=2 redshift z i K i K i Variability of the proton-to-electron mass ratio on cosmological scales p. 2
67 b = (1 + z abs ) µ µ J=1 3 J=1 redshift z i K i K i Variability of the proton-to-electron mass ratio on cosmological scales p. 2
68 b = (1 + z abs ) µ µ J=1 3 J=1 redshift z i K i K i Merely transitions with high vibrational quantum numbers in the first rotational level contribute to a positive result Variability of the proton-to-electron mass ratio on cosmological scales p. 2
69 News or noise? redshift z i K i Variability of the proton-to-electron mass ratio on cosmological scales p. 2
70 News or noise? redshift z i K i no detectable correlation in a 85% subset Variability of the proton-to-electron mass ratio on cosmological scales p. 2
71 News or noise? redshift z i K i no detectable correlation in a 85% subset µ/µ over the period of 11.5 Gyr Variability of the proton-to-electron mass ratio on cosmological scales p. 2
72 Outlook Variability of the proton-to-electron mass ratio on cosmological scales p. 2
73 Outlook line lists of required accuracy just available increased need for high resolution Variability of the proton-to-electron mass ratio on cosmological scales p. 2
74 Outlook line lists of required accuracy just available increased need for high resolution in general attach more importance to data reduction Variability of the proton-to-electron mass ratio on cosmological scales p. 2
75 Outlook line lists of required accuracy just available increased need for high resolution in general attach more importance to data reduction search for more quasar spectra with DLA and H 2 signatures Variability of the proton-to-electron mass ratio on cosmological scales p. 2
76 Outlook line lists of required accuracy just available increased need for high resolution in general attach more importance to data reduction search for more quasar spectra with DLA and H 2 signatures further simulations of detectability of variation Variability of the proton-to-electron mass ratio on cosmological scales p. 2
77 Outlook line lists of required accuracy just available increased need for high resolution in general attach more importance to data reduction search for more quasar spectra with DLA and H 2 signatures further simulations of detectability of variation better understanding of the nature of DLAs Variability of the proton-to-electron mass ratio on cosmological scales p. 2
78 Variability of the proton-to-electron mass ratio on cosmological scales p. 2
79 450 A1 A2 A3 a.u. of flux B1 B2 B3 a.u. of flux C1 C2 C3 COADDED a.u. of flux observed wavelength [Å] observed wavelength [Å] observed wavelength [Å] observed wavelength [Å] Nine separately observed spectra with errorbars and exemplary fit of L1R1. Variability of the proton-to-electron mass ratio on cosmological scales p. 2
80 L1P1 L3P L1R1 L4R1 A L2R1 L4P1 A L3R1 L5P1 A L5R1 L9R1 A A L7R1 L10P1 A A L8R1 W2Q radial velocity [km/s] L9P1 W3Q radial velocity [km/s] L13R radial velocity [km/s] L14R radial velocity [km/s] Variability of the proton-to-electron mass ratio on cosmological scales p. 2
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