shining light on pahs in interstellar ices
DESCRIPTION
Shining light on PAHs in interstellar ices. Jordy Bouwman Sackler Laboratory for Astrophysics, Leiden Observatory. IR absorption. PDR. Bauschlicher et al., ApJ 697, 311, 2009. Wealth of frozen species. CO. H 2 O stretch. H 2 O Lib. H 2 O bend. E.L. Gibb et al., ApJ 536, 347 (2000). - PowerPoint PPT PresentationTRANSCRIPT
Jordy BouwmanSackler Laboratory for Astrophysics, Leiden Observatory
Shining light on PAHs in interstellar ices
IR absorption
PDR
Bauschlicher et al., ApJ 697, 311, 2009
Wealth of frozen species
E.L. Gibb et al., ApJ 536, 347 (2000)
IR spectrum towards a high mass protostar and laboratory spectrum
H2Ostretch
H2Obend
H2OLib.
CO
Bouwman et al., A&A, 476, 995 (2007)
IR Emission bands
PDR
3.3, 6.2, 7.7, 8.6, and 11.3 m
PAHs in ices
• PAHs are likely to freeze out on cold grains and are incorporated in ices…
1.How can we study these mixtures spectroscopically?
2.How do PAHs trapped in ices behaveupon VUV irradiation?
IR spectroscopy
• Anthracene:H2O ice 1:70 mixture
Bernstein et al., ApJ, 664, 1264 (2007)
PAHs in ices
E.L. Gibb et al., ApJ 536, 347 (2000)
Bernstein et al., ApJ, 664, 1264 (2007)
Other options?
• PAHs are known to be strong UV/VIS absorbers
• Common interstellar ice constituents are transparent for > 240 nm
Near UV/VIS spectroscopy!
Sensitive Solid-State Spectrometer
J. Bouwman, D.M. Paardekooper, H.M. Cuppen, H. Linnartz, L.J. Allamandola, ApJ, in press (2009)
Pyrene:H2O ice spectrum
J. Bouwman et al., Astronomy and Astrophysics, in prep.
Assignment 400 nm band
• Not a direct photon product!
• Evidence for HCO. radicals
Time and temperature evolution
Ionization is most efficient at low temperatures
Photoproduct band growth faster at high temperatures
PyH. nm band more prominent at high temperaturesJ. Bouwman et al., Astronomy and Astrophysics, in prep.
T=11 K T=100 K
Chemical evolution• VUV irradiation while measuring spectra
every 10 s permits real time tracking
J. Bouwman et al., Astronomy and Astrophysics, in prep.
T=25 K
Reaction rates
Py = Pyrene
Py.+ = Pyrene cation
PyH. = unknownPi = Product ikjj = reaction rate jj
Reaction scheme:
Pyrene H2O ice photochemistry
• Evidence for PAH-ion mediated (photo-) chemistry
• Two different temperature regimesReaction scheme:
low T regimeHigh T regime
Py = PyrenePy+ = Pyrene cation
PyH. = unknownPi = Product iKjj = reaction rate jj
Astrochemical picture
Bernstein, Sandford, Allamandola , Sci. Am. 7, p26 (1999)
Conclusions
• The setup shows great potential for both spectroscopy and kinetics
• PAH reaction paths are temperature dependent
• PAHs in H2O ice are readily ionized• Ions are stabilized in water ice and play a
previously neglected role in ice chemistry• VLT UV/VIS observations of embedded
objects are awaiting data reduction (help)
AcknowledgementsThanks to the Sackler laboratory group:
€€€
• Harold Linnartz• Herma Cuppen• Lou Allamandola• Claire Romanzin• Arthur Bakker• Daniël Paardekooper
• Nadine Wehres• Sergio Ioppolo• Karoliina Isokoski• Karin Öberg• Edith Fayolle• Ankan Das
Trapping of cations• Irradiate to obtain maximum cation signal
J. Bouwman et al., Astronomy and Astrophysics, in prep.
T=25 K
Normalized pyrene cation decay
• Double exponential decay at 10 K
1 = 2 hrs
2 = 351 hrs
J. Bouwman et al., Astrophysical Journal, in press (2009)