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Interstellar PAH variants IR Spectroscopy
Amit Pathak Banaras Hindu University
Varanasi
SUBARU, TIFR
Collaborators
Mridusmita Buragohain, Itsuki Sakon, Takashi Onaka (UoTokyo) Ekant Vats (BHU) N K Gour (Tezpur University) Peter Sarre (UoNottingham)
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Polycyclic Aromatic Hydrocarbons (PAHs)
They are stable, made mostly of carbon and are everywhere.
These sooty molecules make upto 10-15% of the total carbon.
They are carcinogenic.
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Why PAHs?
Aromatic Infrared Bands
UV bump at 217.5 nm.
3.4 µm absorption feature.
The Extended Red Emission (PAH clusters).
Diffuse Interstellar Bands.
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Infrared emission at 3030, 1610, 1300, 1160 & 890 cm-1 (3.3, 6.2, 7.7, 8.6 and 11.2 µm).
Weak features (ISO, SPITZER, AKARI, etc.) point to variations in the interstellar PAH population.
(Tielens 2008)
(Joblin 1992 & Clayton 2004)
(Salama et al., Ap. J. 1999, 526 : 265)
(Witt et al., Ap. J. 2006)
Aromatic Infrared Bands
UV bump at 217.5 nm.
3.4 µm absorption feature.
The Extended Red Emission (PAH clusters).
Diffuse Interstellar Bands.
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Why PAHs?
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PAH variants
Deuterated
Aliphatics
Dehydrogenated anions
Nitrogenated
ISO Observations Peeters et al. 2004
Deuterated and Deuteronated PAHs
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Deuterated and Deuteronated PAHs
AKARI Observations Onaka et al. 2014
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Deuterium abundance
Current Deuterium (D/H) in interstellar gas is less compared to the primordial abundance (7 to 22 ppm compared to 26 ppm).
This is not explained by astration (comparison of D/H with O/H).
Large variation in D/H is present (over a few hundred pc scale) compared to O/H.
No anti-correlation between D/H and O/H observed.
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IR spectra for coronene Buragohain et al. 2015, 2016
A peak at 4.4 µm (2275 cm-1) in
deuterated coronene C-D
stretching
In deuteronated PAHs,
frequency shifts towards longer
wavelength side - larger mass
peak at 4.7 µm (2130 cm-1) in
spectrum of deuteronated PAHs –
attributed to C – D stretching
Deuterated &
Deuteronated PAHs
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splits into 2 peaks
Protonated coronene H-C-H+ symmetric stretching
Deuteronated coronene
C-H stretching
C-D stretching
Protonated & Deuteronated PAHs
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The aliphatic C-D stretch in DPAH+
DPAH+ Wavelength µm
Relative Intensity
[D/H]num [D/H]int [D/H]sc
D-Pyrene 4.78 0.14 0.1 0.52 5.2
D-Perylene 4.79 0.06 0.083 0.25 3.0
D-Coronene 4.74 0.04 0.083 0.22 2.7
D-CorD+ 4.74 0.07 0.18 0.26 1.4
D-Circumcoronene 4.70 0.003 0.06 0.008 0.1
[D/H]num – no. of D atoms / no. of H atoms
[D/H]int – intensity of C-D stretch / intensity of C-H stretch
[D/H]sc – [D/H]num / [D/H]int
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The aliphatic C-D stretch in DPAH+
DPAH+ Wavelength µm
Relative Intensity
[D/H]num [D/H]int [D/H]sc
D-Pyrene 4.78 0.14 0.1 0.52 5.2
D-Perylene 4.79 0.06 0.083 0.25 3.0
D-Coronene 4.74 0.04 0.083 0.22 2.7
D-CorD+ 4.74 0.07 0.18 0.26 1.4
D-Circumcoronene 4.70 0.003 0.06 0.008 0.1
[D/H]num – no. of D atoms / no. of H atoms
[D/H]int – intensity of C-D stretch / intensity of C-H stretch
[D/H]sc – [D/H]num / [D/H]int
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Formation of Deuterated / Deuteronated PAHs
Deuterium is restricted to grain surface reactions (mostly in dense clouds).
PAHs may be the largest reservoir of materials enriched in D by ion-
molecule reactions (i) PAHs are more stable (ii) PAHs have peripheral H atoms (for substitution by D)
D atom addition to PAHs producing aliphatic C – D bonds.
D atom substituting the existing H atom on the PAH.
In harsh radiation field interstellar environments, since the rate of
unimolecular photodissociation will increase with decreasing molecular size, smaller PAHs are more likely to get deuterated.
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Aliphatic PAHs – C-H stretch
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PAH anions may be the principal carriers of negative charge in IS clouds
Dehydrogenated PAHs may lead to formation of Fullerenes
Carbon loss followed by pentagon formation initiates the curling of the molecule.
The graphene sheet curls up, forms a bowl-like structure, and zips up into a ball.
Dehydrogenation of PAHs
In less dense
environments
Chuvilin et al., Nature Chemistry 2010
Berne & Tielens, 2011, PNAS
Dehydrogenated PAH anions
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Dehydrogenated PAH anions
Partially dehydrogenated PAH anions
may contribute to the 3.3 μm band and
intense features in the 5–10 μm region.
Duo C–H group may convert into a solo
C–H unit producing 3.4 μm feature due to
C–H stretching.
5.2 μm feature (free C–C/C–C–C stretch)
identifies dehydrogenated PAH anions.
Absence of this feature suggests that
such PAHs may be dehydrogenated up to a
certain limit.
Buragohain et al. 2018
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Nitrogenated PAHs
Important to explain the
position of the 6.2 μm band.
Surprisingly the 11.2 μm is
strong even in ionized ones.
Observations of disks around
Herbig Ae/Be objects, Planetary
Nebulae, etc. have similar
charactersitics.
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Nitrogenated PAHs
Important to explain the
position of the 6.2 μm band.
Surprisingly the 11.2 μm is
strong even in ionized ones.
Observations of disks around
Herbig Ae/Be objects, Planetary
Nebulae, etc. have similar
charactersitics.
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SUBARU and PAHs
COMICS N-band (7.5 – 13.5 μm) is appropriate for the observations of PAH bands.
Observations of MWC1080 (Herbig Ae/Be star) to estimate the ionization of PAHs.
Sakon et al. 2006
Summary
Detection of a single PAH still elusive (degeneracy is the culprit)
Dedicated observations in the mid-IR needed
COMICS fills in the gap due to unavailability of space instruments
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Acknowledgement
JSPS-DST collaboration
SERB-DST, New Delhi funding
UK India Education and Research Initiative
HPC@Nottingham
HPC@IUCAA
UGC-CSIR, New Delhi
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