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 journalJournal articlepeer-review

Harvard

De Diego, JA, Binette, L, Ogle, P, Andersen, AC, Haro-Corzo, S & Wold, M 2007, 'Quasar 3C 298: A test-case for meteoritic nanodiamond 3.5 μm emission', Astronomy and Astrophysics, vol. 467, no. 1, pp. L7-L10. https://doi.org/10.1051/0004-6361:20077081

APA

De Diego, J. A., Binette, L., Ogle, P., Andersen, A. C., Haro-Corzo, S., & Wold, M. (2007). Quasar 3C 298: A test-case for meteoritic nanodiamond 3.5 μm emission. Astronomy and Astrophysics, 467(1), L7-L10. https://doi.org/10.1051/0004-6361:20077081

Vancouver

De Diego JA, Binette L, Ogle P, Andersen AC, Haro-Corzo S, Wold M. Quasar 3C 298: A test-case for meteoritic nanodiamond 3.5 μm emission. Astronomy and Astrophysics. 2007 May 1;467(1):L7-L10. https://doi.org/10.1051/0004-6361:20077081

Author

De Diego, J. A. ; Binette, L. ; Ogle, P. ; Andersen, A. C. ; Haro-Corzo, S. ; Wold, M. / Quasar 3C 298 : A test-case for meteoritic nanodiamond 3.5 μm emission. In: Astronomy and Astrophysics. 2007 ; Vol. 467, No. 1. pp. L7-L10.

Bibtex

@article{374a8bc53b52463298a1abe466013e78,
title = "Quasar 3C 298: A test-case for meteoritic nanodiamond 3.5 μm emission",
abstract = "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.",
keywords = "Galaxies: active, Infrared: galaxies, ISM: dust, extinction, Quasars: individual: 3C 298, Ultraviolet: galaxies",
author = "{De Diego}, {J. A.} and L. Binette and P. Ogle and Andersen, {A. C.} and S. Haro-Corzo and M. Wold",
year = "2007",
month = may,
day = "1",
doi = "10.1051/0004-6361:20077081",
language = "English",
volume = "467",
pages = "L7--L10",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "E D P Sciences",
number = "1",

}

RIS

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