Transcript Slide 1

Photophysical properties of
protonated aromatic hydrocarbons
Vadym Kapinus
Department of Chemistry
Blake group
PAHs in Space
• Polycyclic aromatic hydrocarbons (PAHs) are the most abundant free
organic molecules in interstellar medium (ISM), as a class.
As evidence, the Unidentified IR emission bands (UIRs) are most
likely produced by PAHs.
Sample UIR spectrum
Astronomical Spectra
PAHs and DIBs
• Diffuse interstellar bands (DIBs) – unassigned absorption bands from
diffuse interstellar clouds. Discovered in 1920s.
• PAHs are possible carriers of DIBs.
• In diffuse clouds PAHs would be ionized and may protonate easily.
• Protonated PAHs are closed shell ions and have similar to neutrals
electronic structure.
• Their electronic transitions are red-shifted with respect to neutral
PAHs. May expect even smaller molecules to absorb in DIB l range.
Importance in Chemistry and Biology
• Protonated aromatic hydrocarbons are close in structure to
intermediates in aromatic electrophilic substitution reactions.
C6H6 + E+ - > C6H6E+ - > C6H5E + H+
E = Cl, Br, NO3, SO3H, etc.
• DNA base pairs in cells form bridges through proton transfer.
UV spectroscopy of protonated aromatic molecules may shed
more light on cell radiation damage.
Goals
Tasks to perform
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Determine possible structures of protonated PAHs.
Find out how protonated PAHs interact with UV & visible radiation.
Measure electronic spectra of protonated PAHs.
Due to experimental considerations will work on photodissociation
spectra.
Main questions
Quick answers
1. Do protonated PAHs exist in interstellar medium?
2. If yes, do they produce DIBs?
Most likely, Yes
Most likely, No
Protonated Benzene Structure
Ab initio structures for protonated benzene – CH2 benzenium (1),
bridged benzonium (2) and ring (3) isomers.
C6H7+
Protonated benzene DFT structure.
Proton binds to carbon atom !
Protonated Benzene Experiments
C6H7+ UV dissociation in
FT-ICR mass spectrometer
(Freiser, Beauchamp 1976)
C6H7+ · Ar cluster
IR dissociation
(Solca, Dopfer 2002)
Calculations Details
• GAUSSIAN 98W - calculations
• GaussView
- visualization
• PC configuration : Intel Pentium 4 2.72GHz CPU,
1Gb PC1066 RDRAM, 30Gb on HD, Microsoft Windows XP SP1
• Geometries and vibrational frequencies calculated with density functional
theory
B3LYP 6-311++G(2d,2p)
- benzene
B3LYP 6-311++G(d,p)
- naphthalene
B3LYP 6-31+G(d)
- anthracene, phenanthrene, pyrene
• Excited electronic states calculated with configuration interaction singles
method
CIS 6-311++G(2d,2p)
on B3LYP 6-311++G(d,p) geometries
PC Choice for GAUSSIAN 98
• Tested with GAUSSIAN 98W, Revision-A.9
• Test systems :
– P4: Intel Pentium 4 2.66 GHz @ 2.72GHz (2.26% OC) , 1Gb RAM, HD ATA-5
(133Mb/s), Windows XP SP1
– AXP: AMD Athlon XP 2800+ @ 2.112GHz (0% OC), 1Gb RAM, HD SATA
(150Mb/s), Windows 2000 SP4
– A64: AMD Athlon 64 3000+ @ 2.1GHz (5% OC), 1Gb RAM, HD ATA-5
(133Mb/s), Windows XP SP1
P4
AXP
A64
CPU clock, MHz
2720
2112
2100
In-memory job, s
86286
106568
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High disk swap job, s
5484
7102
5665
• Conclusion – get Pentium 4 system, as fast as you can afford !
Protonated Naphthalene, Anthracene Structures
Protonated naphthalene C10H9+
Protonated anthracene C14H11+
(1)
(1)
(2)
(2)
(9)
Protonated Phenanthrene, Pyrene Structures
Protonated phenanthrene C14H11+
Protonated pyrene C16H11+
(1)
(1)
(2)
(3)
(2)
(4)
(4)
(9)
Proton Affinities
Calculated proton affinities (in kCal/mol) are in good agreement with
experimental values. Tests if the theory level and basis set are good enough.
Experimental
Calculated
H+ site
Benzene
179.3
182.59
Any
Naphthalene
191.9
196.21
1
193.32
2
204.28
1
200.89
2
213.02
9
199.04
1
199.39
2
197.85
3
200.02
4
199.85
9
212.26
1
197.98
2
201.89
4
Anthracene
Phenanthrene
Pyrene
209.7
197.3
207.7
Energy Landscape – Protonated Benzene
Energy Landscape – Protonated Naphthalene
Energy Landscape – Protonated Anthracene
Vibrational Spectrum Changes
Typical changes in IR vibrational spectrum – more IR active modes,
new CH2 modes appear at ~2780 - 2900 cm-1
Ground electronic state results
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Proton binds to carbon atoms. Bridged structures are transition states.
Protonated aromatic molecules are still planar.
Aromaticity breaks at the CH2 site. That ring looks like a cyclodiene.
C-H bond length for sp3 carbon is longer than sp2 – 1.100Å vs. 1.085Å
• C-H vibrations are around 2780-2900cm-1 for sp3, less than 10cm-1 apart.
For sp2 they are in 3000-3100cm-1 range and very weak or not IR active.
This may contribute to the long wavelength shoulder in 3.3mm UIR feature.
• Dissociation energies are in 2-3eV (400-600nm) range.
• Lowest dissociation channels are loss of H atom or H2 molecule. When
loosing 2H or H2, will again form closed shell species.
• With sufficient internal energy, can isomerize without dissociation.
• In diffuse clouds PAHs would be most definitely in protonated form,
if they can survive in the radiation field!
Benzene Molecular Orbitals
C6H6 (benzene)
C6H7+ (protonated benzene)
Excited electronic states results. S0 – S1
transition, nm
Unlike neutral PAHs, small protonated PAHs have their S0 – S1
transitions well into DIB wavelengths range.
Calc
Red Shift
f
Benzene
Calc
Red Shift
f
Phenanthrene
C6H6
262.56
C6H7+
349.50
86.94
0.0000
C14H10
341.16
0.1741
1-C14H11+
493.38
152.22
0.1984
2-C14H11+
461.04
119.88
0.3068
0.0825
3-C14H11+
498.03
156.87
0.1205
Naphthalene
0.0318
C10H8
312.30
1-C10H9+
382.53
70.22
0.40904
4-C14H11+
477.43
136.27
0.4661
2-C10H9+
438.90
126.60
0.1714
9-C14H11+
479.60
138.44
0.2854
Anthracene
Pyrene
C14H10
361.17
0.1399
C16H10
367.57
1-C14H11+
443.09
81.92
0.3459
1-C16H11+
440.54
72.97
0.3338
2-C14H11+
490.41
129.24
0.1862
2-C16H11+
566.34
198.77
0.1499
9-C14H11+
376.46
15.29
0.7120
4-C16H11+
496.65
129.08
0.1464
0.3658
DIBs and Predicted S0-S1 Transitions
• Variety of isomers increases chances of coincidence with DIBs.
• This may be used for more certain DIB assignment.
Experimental Setup – Discharge Source
Possible protonation mechanisms in H2:
H2 + e- - > H2+ + 2eH2+ + H2 - > H3+ + H
H3+ + PAH - > PAH-H+ + H2
or
PAH + e- - > PAH+ + 2ePAH+ + H2 - > PAH-H+ + H
P(H2) = 1-2 atm
Experimental Setup – Time-of-Flight Mass
Spectrometer
• Discharge plasma is guided to skimmer.
• Ions are extracted into TOF MS by pulser.
• Separated ions are intercepted by laser in
front of reflectron.
• Ions are turned around by reflectron to
reflectron detector.
• Neutrals go through reflectron to
linear detector.
Experimental Setup – Tunable Light Sources
Old BBO type II OPO
Pumped by Coherent Infinity 40-100 Nd:YAG laser
New mixed BBO type
I and II prism OPO
Pumped by SpectraPhysics GCR-16S Nd:YAG laser @ 10Hz
OPO Operational Principle
OPO conversion – phase
matching conditions
Light vectors in nonlinear crystal
wp = ws + wi
kp = ks + k i
Beam polarizations for OPO
Xtl
Pump
Signal
Idler
BBO I
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BBO II
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Mixed Cavity OPO
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Using BBO type II as bandwidth filter, BBO type I as amplifier.
Different crystal types eliminate a need for a waveplate.
Improved beam profile. Beam divergency ≤ 3 mrad.
Extended generation range to degeneracy point, with good pulse energy.
@ 2m
Data Acquisition System
• The experiment is controlled by a PC (PIII, 533MHz, 392Mb RAM,
Windows 2000 SP4) via a developed BGSpecT software package .
• TOF MS traces are acquired by GaGe CS85G oscilloscope card, laser
pulse energy is measured with pyroelectric detector via GaGe CS1450
card. Each TOF MS trace is analyzed for the presence of certain level of
ion signal. “Good” waveforms are then averaged.
• OPO crystal positions are controlled with Newport 850F microstepper
motors via Precision MicroControl DCX PC100 card.
• Time delays for lasers, pulsed valves and discharge are controlled by
Stanford Research Systems DG535 digital delay/pulse generators.
• Pulsed valves are operated at 0.91Hz (10/11) due to slow pumping speed.
Blake Group Spectroscopy Tools/Software
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Simultaneously controls multiple devices of the same kind.
Controls devices via GPIB, RS232 interfaces, PCI and ISA plug-in cards.
Simultaneously controls multiple GPIB boards.
Smart oscilloscope waveform acquisition.
Wavelength source wavelength conversions.
Master/Slave locking of delay lines from pulse delay generator.
Huge number of supported oscilloscopes.
Easy process of spectra acquisition.
Fast. Runs easily on 100MHz Pentium system.
Flexible to configure.
User friendly interface. Partial Windows XP themes support.
www.its.caltech.edu/~vadym/BGSpecT_exe.zip
Discharge Products – TOF MS Spectra
Protonation evidence
Combined for H2 discharge with
different PAHs and without
Photodissociation – TOF MS Spectra
• Photodissociation with high energy excimer laser pulses (193, 248
nm) is rather efficient.
• Main dissociation channel – loss of H2 molecule (or 2 H atoms).
• No dissociation by low pulse energy visible (415 - 600 nm) and UV
(208 – 290 nm) wavelengths .
Photodissociation – Protonated Anthracene
Dissociation is clearly multiphoton
Photodissociation – Protonated Pyrene
Similarly to protonated anthracene - multiphoton
Protonated Anthracene – Photostability Estimate
• Protonated anthracene
dissociation is 3-photon at both
193 and 248 nm.
• Need ~13-15 eV to fall it apart.
This is much higher than
predicted 2.6 eV.
• IVR is responsible for such
behavior.
Photostability of Protonated PAHs
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Protonated PAHs do not dissociate from visible photons.
Even in the UV l range dissociation is multiphoton.
Needed photon energy is much higher than predicted.
IVR is likely responsible for the photostability.
• Good news for ISM !
May absorb UV/visible photons and then within milliseconds cool off by
emitting in IR. Can cycle for long time.
• Bad news for spectroscopy.
Need to use a different method to record spectra.
Will work on cluster dissociation.
Cluster Source
• Most atoms and molecules in the
discharge turn PAH protonation
off.
• Need to mix in the third
molecule at the discharge exit.
• Use H2 as a carrier gas in both
pulsed valves.
• Clusters don’t form with rare
gases.
• Works with water.
P1(H2) = 1 atm
P2(H2) = 2.3 atm
Protonated Anthracene – Clusters with Water
• Can produce large quantities of C14H11+ · (H2O)n clusters.
• Cluster spectrum should be red-shifted by ~2 nm.
Cluster Geometry – Electrostatic Nature
• C6H6 · H2O cluster :
interaction between water
dipole and benzene quadrupole
moments.
Can bind only at the top or
bottom.
• C14H11+ · H2O cluster :
‘+’ charge - dipole interaction.
Charge makes water O atom face
protonated anthracene. Can bind
only from the side. Will bind to a
site with largest ‘+’ charge or
dipole – CH2
Cluster Photodissociation Spectrum
• The visible spectrum does
not have narrow features
• Observed two bands at
445.8 and 470.7 nm,
FWHM=19.6 nm
Implications
• Observed bands are broad. Likely, due to high vibrational density of
states, clusters being warm.
• Temperature in diffuse interstellar clouds is 100-200K. Clusters are not
hotter than clouds.
• Vibrational density of states in protonated PAHs is higher than in neutrals
and cations. Mainly, due to the ability of H atom to ‘jump’ from one C
atom to another. This feature is unique to protonated PAHs.
• Since clusters are in similar to ISM conditions and absorption bands are
much wider than DIBs, small protonated PAHs are not DIB carriers ! The
isomerization process should be present in larger protonated PAHs as
well, and so should produce broad absorption features.
Summary
• Aromatic hydrocarbons are protonated effectively.
• Ground state DFT calculations were performed for different protonated
PAHs. Loss of H atom or H2 molecule were identified as energetically
lowest dissociation channels. Isomerization is possible with enough
vibrational energy.
• CH vibrations of sp3 carbon were calculated. They may account for the
red wing in 3.3mm feature in UIRs.
• Calculated S0-S1 transitions for protonated PAHs are in the DIB
wavelengths range even for small PAHs.
• Protonated PAHs are very photostable for 1-photon absorption. This
makes them even more viable candidates for ISM.
• Direct UV/visible dissociation spectra are impossible to record.
• Visible spectra of protonated anthracene-water clusters were measured.
Spectral features are very broad. Protonated PAHs are unlikely to be DIB
contributors if this broadening is intrinsic to the protonated PAHs.
• Sources for PAH protonation and clustering with water were designed.
• Mixed BBO type I and II OPO with the prism cavity was developed.
• Flexible data collection software was designed.
Conclusions
1. Do protonated PAHs exist in interstellar medium?
Yes. Most likely.
PAHs are UIR carriers. In diffuse clouds PAHs will protonate.
Protonated PAHs are very photostable.
2. If yes, do they produce DIBs?
No.
Electronic absorption bands are wider than DIBs, although, they are
in DIB range.
Acknowlegements
• Geoffrey A. Blake
• Sheng Wu
• Blake group
• Funding
– NASA
– NSF
- adviser
- OPOs