photodissociation in astrochemistry leiden, 5 feb. 2015 wim ubachs vu university amsterdam molecular...
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Photodissociation in AstrochemistryPhotodissociation in AstrochemistryLeiden, 5 Feb. 2015Leiden, 5 Feb. 2015
Wim UbachsWim UbachsVU University AmsterdamVU University Amsterdam
Molecular hydrogen in the photosphere ofWhite Dwarfs
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H2 in space
Copernicus (1972-1981)
FUSE (1999-2007)
IUE (1978-1996)
1970
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Keck
VLT
Earth-based observations of H2; in high redshift quasar sightlines
Spectrum of J2123—001 at z = 2.05
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on ground March 2013
Q1441+272 ; the most distant H2 absorberzabs = 4.22 ; 1.5 Gyrs after the Big Bang
Bagdonaite et al.Phys. Rev. Lett. Feb 2015Arxiv:1501.05533
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Astroph. J. Lett. 766, L18 (2013)
Cosmic Origins Spectrograph on HST (R ~ 20,000)
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Contributions of many lines in the B-X Lyman system
T=13,000 K
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H2 laboratory wavelengths
XUV-laser excitation (1 + 1’ REMPI detection)
P(3) C-X(1,0)
R(0) B-X(9,0) line
Ubachs, Phys. Rev. Lett. (2004)Reinhold et al, Phys. Rev. Lett. (2006)
For HDIvanov et al., Phys. Rev. Lett. (2008)
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H2 laboratory wavelengths Lyman bands
FT-IR+Vis
XUV2-photondeep-UV
EF 1g+
B 1u+
X 1g+
~ (5 – 50) x 10-9
Salumbides et al. Phys. Rev. Lett. 101 (2008) 223001Bailly et al., Mol. Phys. 108 (2010) 827
Two-step excitation Two-photon laser Doppler-free
FTIR and FT-VIS
1s2s
1s2
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Determination of accurate wavelengths for Lyman bands
Baillyet al.Mol. Phys.(2010)
Experimentallevelenergies
B-state: Limited to J<13X-state: accurate calculations by Pachucki & Komasa et al.
Higher J (J>12): ab initio framework Abgrall/Roueff
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Data base for hot H2
> 1500 linesincluded tomodel thespectrum
max max
0
)(
0
exp)12)((
exp)12)(()( v
v
vJ
J
vJI
vJI
vJ
kTE
JJg
kTE
JJgTP )("""'"' TPfNI JvJJvvc o l u m ni
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ia b si
i
i Kzz
1110
EmpiricalEmpirical search for a change in search for a change in =M=Mpp/m/mee
d
dE
d
dE
EEd
dK XB
XB
ii ln
)(ln
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Varying Constants ?
Bekenstein-Barrow –Sandvik – Mageijo – Light scalar fields
1) Coupling to cosmologyVariation on cosmologicaltime scales
d
l
ceFFA
c
jLS m a t
220
24
Coupling constants are free parameters in Standard Model
2) Coupling to matterdensity -> “chameleons”Coupling to gravity(test EEP)
Jacob Bekenstein
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GD133: = (-2.7 +/- 4.7) x 10-5 z=0.0001820 (10)
GD29-38: = (-5.9 +/-3.8) x 10-5z=0.0001360 (8)
Dependence of on gravitational field
Insert fit parameters:
T and and z
Pv”,J” and Ki included
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[5] Chardonnet, PRL 100, 150801 (2008)
SF6/Cs measurement
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Thanks & Acknowledgement
Edcel Salumbides
Julija Bagdonaite
Michael Murphy
EvelyneRoueff
HerveAbgrall
SimonPreval
MartinBarstow
John Barrow
J. Bagdonaite, et al.Phys. Rev. Lett. 113, 123002 (2014)
E.J. Salumbides et al.ArXiv 1412.6920