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Spitzer Approved Galactic Spitzer Approved Galactic Printed_by_SSC Mar 25, 10 16:33Spitzer_Approved_Galactic Page 1/847 Mar 25, 10 16:33Spitzer_Approved_Galactic Page 2/847 Spitzer Space Telescope − Archive Research Proposal #20309 Spitzer Space Telescope − Archive Research Proposal #30144 PAH Emission Features in the 15 to 20 Micron Region: Emitting to the Beat of a Diamonds are a PAHs Best Friend Different Drummer Principal Investigator: Louis Allamandola Principal Investigator: Louis Allamandola Institution: NASA Ames Research Center Institution: NASA Ames Research Center Technical Contact: Louis Allamandola, NASA Ames Research Center Technical Contact: Louis Allamandola, NASA Ames Research Center Co−Investigators: Co−Investigators: Andrew Mattioda, SETI Andrew Mattioda, SETI Institute and NASA Ames Els Peeters, SETI Els Peeters, NASA Ames Research Center Douglas Hudgins, NASA Ames Research Center Douglas Hudgins, NASA Ames Research Center Alexander Tielens, NASA Ames Research Center Xander Tielens, Kapteyn Institute, The Netherlands Charles Bauschlicher, Jr., NASA Ames Research Center Charlie Bauschlicher, Jr., NASA Ames Research Center Science Category: ISM Science Category: ISM Dollars Approved: 56727.0 Dollars Approved: 72000.0 Abstract: Abstract: The mid−IR spectroscopic capabilities and unprecedented sensitivity of the Spitzer has added a new complex of bands near 17 um to the PAH emission band Spitzer Space Telescope has shown that the ubiquitious infrared (IR) emission family. This 17 um band complex, the second most intense of the PAH features, features can be used as probes of many galactic and extragalactic objects. carries unique information about the emitting species. Because these bands arise These features, formerly called the Unidentified Infrared (UIR) Bands, are now from drumhead vibrations of the hexagonal carbon skeleton, they carry generally attributed to the vibrational emission from polycyclic aromatic information directly related to PAH shape, size, and charge. Further, since much hydrocarbons, PAHs, and related species. However there is some difficulty in of the emission at these wavelengths originates from PAHs at the small end of reproducing all the features of the interstellar emission spectrum solely with the very small grain (vsg) population, this provides the first glimpse into PAH spectra. Because these differences have persisted as our knowledge of PAH details of the vsg population on a molecular level. Since the information spectroscopy has increased these differences point to at least one other type of contained in this band is fundamentally different from that of the mid−IR contributor to the interstellar emission spectrum. The association of these features and it probes the vsg population, the 17 um band complex is an features with objects abundant in cosmic carbon points to an additional important new tool with which to probe conditions within the Galaxy and in carbonaceous material contributing to the features. Among the possibilities extragalactic star forming regions and simultaneously gives insight into the diamonds are particularly attractive. However, until very recently, this could cosmic history of the important biogenic element, carbon. However, since little not be tested because well−characterized microdiamonds were not available for is known about PAH spectroscopic properties at wavelengths longer than about 15 study. These are now available for purchase from ChevronTexaco. We propose to um, it is impossible to utilize the 17 um band complex as a new astronomical use the matrix isolation technique to measure the 0.7 to 20 μm spectra of investigative tool. We propose a laboratory study to remedy this situation. We astrophysically relevant, cold microdiamonds. We will also develop and apply the will measure the 15 to 20 um spectra of PAHs which vary in size, shape, and computational techniques required to calculate these spectra and the spectra of ionization state. Spanning the range from C30H14 to C132H34, the PAH sample microdiamonds for which we cannot obtain samples. Given the lack of availability varies from moderately sized PAHs to the largest PAHs available anywhere. We of microdiamonds until recently, their IR spectroscopic properties are not will combine these experimental studies with quantum computations to test and known. Since microdiamonds have been long thought to be present throughout the perfect the computational approach for this new wavelength and fundamental ISM this lack of spectroscopic information prevents a complete analysis of vibration regime. The laboratory work will provide data with which one can Spitzer data, especially in the 7 to 8 μm region. These data will be made analyze the new 17 um emission band complex and will ultimately be used to available to the astronomical community. Incorporating these new data into develop computational techniques to model the longer wavelength spectra of much existing models will improve their ability to probe conditions such as radiation larger PAHs. We will make these spectra available on the web and develop field, charge state, electron and hydrogen density, and cosmochemical history of protocols for analyzing the Spitzer spectra and publish this procedure so it is the object. accessible to the community. Thursday March 25, 2010 gal_covers.txt 1/424 Printed_by_SSC Mar 25, 10 16:33Spitzer_Approved_Galactic Page 3/847 Mar 25, 10 16:33Spitzer_Approved_Galactic Page 4/847 Spitzer Space Telescope − Archive Research Proposal #40131 Spitzer Space Telescope − Archive Research Proposal #40364 PAH Spectra for Everyone IR Spectroscopy of PAHs in Dense Clouds Principal Investigator: Louis Allamandola Principal Investigator: Louis Allamandola Institution: NASA Ames Research Center Institution: NASA Ames Research Center Technical Contact: Louis Allamandola, NASA Ames Research Center Technical Contact: Louis Allamandola, NASA Ames Research Center Co−Investigators: Co−Investigators: Charlie Bauschlicher, Jr., NASA Ames Research Center Andrew Mattioda, SETI/NASA Ames Andrew Mattioda, NASA Ames Research Center Scott Sandford, NASA Ames Reserach Center Max Bernstein, NASA Ames Research Center Science Category: ISM Dollars Approved: 40000.0 Science Category: ISM Dollars Approved: 63016.0 Abstract: The Ames Astrochemistry Laboratory now has PAH IR spectra of more than 220 Abstract: laboratory measured and over 600 theoretically calculated IR spectra of Interstellar PAHs are likely to be a component of the ice mantles that form on polycyclic aromatic hydrocarbons (PAHs) in a multitude of forms. The vast dust grains in dense molecular clouds. PAHs frozen in grain mantles will produce majority of these spectra are not readily accessible to the public. We propose IR absorption bands, not IR emission features. A couple of very weak absorption to make the full collection of the Ames experimental and computational features in ground based spectra of a few objects embedded in dense clouds may collection of PAH IR spectra available to the entire Spitzer community and be due to PAHs. Additionally spaceborne observations in the 5 to 8 ?m region, accessible via the World Wide Web (WWW). The laboratory measured mid−IR spectral the region in which PAH spectroscopy is rich, reveal unidentified new bands and collection includes over 220 neutral, cationic, and anionic PAHs, PAHs with significant variation from object to object. It has not been possible to deuterium in place of hydrogen, PAHs containing oxygen, and PAHs containing properly evaluate the contribution of PAH bands to these IR observations because nitrogen (PANHs). The formulae of the PAHs in the experimental data collection the laboratory absorption spectra of PAHs condensed in realistic interstellar range from C10H8 to C50H22. Unfortunately, it is not possible to obtain physical mixed−molecular ice analogs is lacking. This experimental data is necessary to samples of all of the types of PAHs that are of astrophysical interest for interpret observations because, in ice mantles, the interaction of PAHs with the experimental study. We also have an extensive collection of accurate surrounding molecules effects PAH IR band positions, widths, profiles, and computational spectra to fill in gaps in the experimentally available spectra. intrinsic strengths. Furthermore, PAHs are readily ionized in pure H2O ice, Our theoretical PAH spectral collection includes very large PAHs, PAHs further altering the PAH spectrum. This laboratory proposal aims to remedy the containing 40 to 132 carbon atoms which are comparable to the size of the PAHs situation by studying the IR spectroscopy of PAHs frozen in laboratory ice thought to dominate the interstellar emission spectrum. Large PAHs might be analogs that realistically reflect the composition of the interstellar ices multiply charged and these are also represented in the theoretical database. observed in dense clouds. The purpose is to provide laboratory spectra which can There is also observational evidence for PAH cations with nitrogen in the inner be used to interpret IR observations. We will measure the spectra of these mixed rings (PANHs) and interest in the spectroscopy of aromatic species containing molecular ices containing PAHs before and after ionization and determine the oxygen and deuterium as well as PAH metal clusters. All of these types of PAHs intrinsic band strengths of neutral and ionized PAHs in these ice analogs. This are represented in the Ames computational PAH IR spectroscopic collection. If will enable a quantitative assessment of the role that PAHs can play in funded,
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