Quasar 3C 298: A test-case for meteoritic nanodiamond 3.5 μm emission
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Quasar 3C 298 : A test-case for meteoritic nanodiamond 3.5 μm emission. / De Diego, J. A.; Binette, L.; Ogle, P.; Andersen, A. C.; Haro-Corzo, S.; Wold, M.
In: Astronomy and Astrophysics, Vol. 467, No. 1, 01.05.2007, p. L7-L10.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - Quasar 3C 298
T2 - A test-case for meteoritic nanodiamond 3.5 μm emission
AU - De Diego, J. A.
AU - Binette, L.
AU - Ogle, P.
AU - Andersen, A. C.
AU - Haro-Corzo, S.
AU - Wold, M.
PY - 2007/5/1
Y1 - 2007/5/1
N2 - Aims. We calculate the dust emission expected at 3.43 and 3.53 μm if meteoritic (i.e. hydrogenated) nanodiamonds are responsible for most of the far-UV break observed in quasars. Methods. We integrate the UV flux that hydrogenated nanodiamonds must absorb to reproduce the far-UV break. Based on laboratory spectra of H-terminated diamond surfaces, we analyse the radiative energy budget and derive theoretically the IR emission profiles expected for possible C-H surface stretch modes of the diamonds. Results. Using as test case a spectrum of 3C 298 provided by the Spitzer Observatory, we do not find evidence of these emission bands. Conclusions. While diamonds without surface adsorbates remain a viable candidate for explaining the far-UV break observed in quasars, hydrogenated nanodiamonds appear to be ruled out, as they would give rise to IR emission bands, which have not been observed so far.
AB - Aims. We calculate the dust emission expected at 3.43 and 3.53 μm if meteoritic (i.e. hydrogenated) nanodiamonds are responsible for most of the far-UV break observed in quasars. Methods. We integrate the UV flux that hydrogenated nanodiamonds must absorb to reproduce the far-UV break. Based on laboratory spectra of H-terminated diamond surfaces, we analyse the radiative energy budget and derive theoretically the IR emission profiles expected for possible C-H surface stretch modes of the diamonds. Results. Using as test case a spectrum of 3C 298 provided by the Spitzer Observatory, we do not find evidence of these emission bands. Conclusions. While diamonds without surface adsorbates remain a viable candidate for explaining the far-UV break observed in quasars, hydrogenated nanodiamonds appear to be ruled out, as they would give rise to IR emission bands, which have not been observed so far.
KW - Galaxies: active
KW - Infrared: galaxies
KW - ISM: dust, extinction
KW - Quasars: individual: 3C 298
KW - Ultraviolet: galaxies
UR - http://www.scopus.com/inward/record.url?scp=34249293030&partnerID=8YFLogxK
U2 - 10.1051/0004-6361:20077081
DO - 10.1051/0004-6361:20077081
M3 - Journal article
AN - SCOPUS:34249293030
VL - 467
SP - L7-L10
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
SN - 0004-6361
IS - 1
ER -
ID: 232622504