a possible dipole in the laws of physics: how alma can help john webb, school of physics, university...
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A possible dipole in the laws of physics: How ALMA can help
John Webb, School of Physics, University of New South Wales, Australia
UNSW team:Matthew BainbridgeJulian BerengutSteve CurranVictor FlambaumJulian KingElliott KochAnant TannaMike WilcynzskaJohn WebbAngus WrightElsewhere:Bob Carswell (Cambridge)Michael Murphy (Swinburne)Wim Ubachs (Amsterdam)
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Motivation:
relies entirely on himThis: plus this
Let’s check the basic assumptions to the best of our ability
Is the cosmological principle right, or just a very good approximation?
To Earth
CIVSiIVCIISiIILyaem
Lya forest
Lyman limit Lya
NVem
SiIVem
CIVem
Lybem
Lyb SiII
quasar
Quasars: physics laboratories in the early universe
Exaggerated illustration of how transitions shift in different directions by different amounts – unique pattern
First calculated, relativisitic Hartree-Fock, 1999.Typicallly ~100<Q<1500
α 1999-2004, HIRES/KeckΔα
/α (1
0-5)
• Previous largest sample of quasar absorber constraints on Δα/α, Murphy et al (2004), from Keck/HIRES• Δα/α = ( -0.57 ± 0.11 ) x 10-5
• Obvious question: what would a different telescope find?
α 2011: Comparing new UVES/VLT data with Keck
VLT + Keck
Keck
VLT
KeckVLT
Different patterns in different directions
Lines on Earth
Redshifted lines
Looking “South”
Looking “North”
Looks pretty shifty…
4.1σ departure from α=constant (variable)
Δα/α = c + A cos(θ)
Keck & VLT dipoles independently agree, p=4%
VLT Keck Combined
Low and high redshift cuts are consistent in direction.Effect is larger at high redshift.
z > 1.6 z < 1.6 Combined
Distance dependence
∆α/α vs BrcosΘ for the model ∆α/α=BrcosΘ+m showing the gradient in α along the best-fit dipole. The best- fit direction is at right ascension 17.4 ± 0.6 hours, declination −62 ± 6 degrees, for which B = (1.1 ± 0.2) × 10−6 GLyr−1 and m = (−1.9 ± 0.8) × 10−6. This dipole+monopole model is statistically preferred over a monopole-only model also at the 4.1σ level. A cosmology with parameters (H0 , ΩM , ΩΛ ) = (70.5, 0.2736, 0.726).
Are a few high S/N outliers responsible for the signal, by chance?
• Alternative to growing error bars• Robustness check – iterative trimming• Adopt statistical-only errors and iteratively clip most deviant point• How much data do we need to discard to remove the dipole?
• c2 n = 1 reached
when ~10% clipped• Dipole significance ~5.5s at c2
n = 1 • Dipole significance stays above 3 s until ~60% of data discarded
Hints that this result might be real
Two internal consistencies:
1 Keck and VLT dipoles agree. Independent samples, different data reduction procedures, different instruments and telescopes.
2 High and low redshift dipoles also agree - different species used at low and high redshift – and different transitions respond differently to the same change in .a
Other suggestive points:
3 Scatter in data exceeds statistical-only error bars (expected). Keeping all points and growing errors is conservative. Trimming increases significance and shows signal is present in the majority or all of the data.
4 Monopole. Predominant in Keck. Mg isotopes? Early enrichment by very massive stars?
How can ALMA help?
• High-z sub-mm galaxies• Radio lines very sensitive to e.g. • Strong CI and CO and other lines• Select gravitationally lensed objects and pick out
individual massive molecular cores• Minimise radiative transfer effects, line offsets (carbon
isotopes?)• Statistical sample to randomise residual species offsets
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