Herschel-SPIRE spectroscopy of G29.96-0.02: Fitting the full SED
- Creators
- Kirk, J. M.
- Polehampton, E.
- Anderson, L. D.
- Baluteau, J. -P.
- Bontemps, S.
- Joblin, C.
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Jones, S. C.
- Naylor, D. A.
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Ward-Thompson, D.
- White, G. J.
- Abergel, A.
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Ade, P.
- André, P.
- Arab, H.
- Bernard, J. -P.
- Blagrave, K.
- Boulanger, F.
- Cohen, M.
- Compiegne, M.
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Cox, P.
- Dartois, E.
- Davis, G.
- Emery, R.
- Fulton, T.
- Gry, C.
- Habart, E.
- Huang, M.
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Lagache, G.
- Lim, T.
- Madden, S.
- Makiwa, G.
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Martin, P.
- Miville-Deschênes, M.-A.
- Molinari, S.
- Moseley, H.
- Motte, F.
- Okumura, K.
- Pinheiro Goncalves, D.
- Rodon, J. A.
- Russeil, D.
- Saraceno, P.
- Sidher, S.
- Spencer, L.
- Swinyard, B.
- Zavagno, A.
Abstract
We use the SPIRE Fourier-transform spectrometer (FTS) on-board the ESA Herschel Space Observatory to analyse the submillimetre spectrum of the Ultra-compact HII region G29.96-0.02. Spectral lines from species including (CO)-C-13, CO, [CI], and [NII] are detected. A sparse map of the [NII] emission shows at least one other HII region neighbouring the clump containing the UCHII. The FTS spectra are combined with ISO SWS and LWS spectra and fluxes from the literature to present a detailed spectrum of the source spanning three orders of magnitude in wavelength. The quality of the spectrum longwards of 100 mu m allows us to fit a single temperature greybody with temperature 80.3 +/- 0.6 K and dust emissivity index 1.73 +/- 0.02, an accuracy rarely obtained with previous instruments. We estimate a mass of 1500 M-circle dot for the clump containing the HII region. The clump's bolometeric luminosity of 4 x 10(6) L-circle dot is comparable to, or slightly greater than, the known O-star powering the UCHII region.
Additional Information
© 2010 ESO. Received 31 March 2010. Accepted 10 May 2010. Published online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. We thank D. Neufeld for identifying the 1.2 THz HF absorption feature. J.M.K. acknowledges STFC funding, while this work was carried out, under the auspices of the Cardiff Astronomy Rolling Grant. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA).Attached Files
Published - Kirk2010p11894Astron_Astrophys.pdf
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Additional details
- Eprint ID
- 23187
- Resolver ID
- CaltechAUTHORS:20110331-095317951
- Science and Technology Facilities Council (STFC)
- Created
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2011-05-25Created from EPrint's datestamp field
- Updated
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2021-11-09Created from EPrint's last_modified field