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Determining dust temperatures and masses in the Herschel era: The importance of observations longward of 200 micron

Gordon, K. D. and Reach, W. T. (2010) Determining dust temperatures and masses in the Herschel era: The importance of observations longward of 200 micron. Astronomy and Astrophysics, 518 . Art. No. L89. ISSN 0004-6361.

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Context. The properties of the dust grains (e.g., temperature and mass) can be derived from fitting far-IR SEDs (≥100 μm). Only with SPIRE on Herschel has it been possible to get high spatial resolution at 200 to 500 μm that is beyond the peak (~160 μm) of dust emission in most galaxies. Aims. We investigate the differences in the fitted dust temperatures and masses determined using only <200 μm data and then also including >200 μm data (new SPIRE observations) to determine how important having >200 μm data is for deriving these dust properties. Methods. We fit the 100 to 350 μm observations of the Large Magellanic Cloud (LMC) point-by-point with a model that consists of a single temperature and fixed emissivity law. The data used are existing observations at 100 and 160 μm (from IRAS and Spitzer) and new SPIRE observations of 1/4 of the LMC observed for the HERITAGE key project as part of the Herschel science demonstration phase. Results. The dust temperatures and masses computed using only 100 and 160 μm data can differ by up to 10% and 36%, respectively, from those that also include the SPIRE 250 & 350 μm data. We find that an emissivity law proportional to λ^(−1.5) minimizes the 100–350 μm fractional residuals. We find that the emission at 500 μm is ~10% higher than expected from extrapolating the fits made at shorter wavelengths. We find the fractional 500 μm excess is weakly anti-correlated with MIPS 24 μm flux and the total gas surface density. This argues against a flux calibration error as the origin of the 500 μm excess. Our results do not allow us to distinguish between a systematic variation in the wavelength dependent emissivity law or a population of very cold dust only detectable at λ ≥ 500 μm for the origin of the 500 μm excess.

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Reach, W. T.0000-0001-8362-4094
Additional Information:© 2010 ESO. Received 30 March 2010, Accepted 1 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 acknowledge financial support from the NASA Herschel Science Center, J.P.L. contracts # 1381522 & 1381650. M.R. is supported by FONDECYT No1080335 and FONDAP No15010003. We thank the contributions and support from the European Space Agency (ESA), the PACS and SPIRE teams, the Herschel Science Center and the NASA Herschel Science Center (esp. A. Barbar and K. Xu) and the PACS and SPIRE data center at CEASaclay, without which none of this work would be possible.We thank the referee, Thomas Henning, for suggestions that improved the clarity of this paper.
Funding AgencyGrant Number
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT) (Chile)1080335
Fondo de Financiamiento de Centros de Excelencia en Investigación (FONDAP) (Chile)15010003
European Space Agency (ESA)UNSPECIFIED
Spectral and Photometric Imaging Receiver (SPIRE)UNSPECIFIED
Herschel Science CenterUNSPECIFIED
Subject Keywords:ISM: general, galaxies: individual: LMC, Magellanic Clouds, infrared: ISM
Record Number:CaltechAUTHORS:20101202-092436316
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Official Citation:Determining dust temperatures and masses in the Herschel era: The importance of observations longward of 200 micron K. D. Gordon, F. Galliano, S. Hony, J.-P. Bernard, A. Bolatto, C. Bot, C. Engelbracht, A. Hughes, F. P. Israel, F. Kemper, S. Kim, A. Li, S. C. Madden, M. Matsuura, M. Meixner, K. Misselt, K. Okumura, P. Panuzzo, M. Rubio, W. T. Reach, J. Roman-Duval, M. Sauvage, R. Skibba and A. G. G. M. Tielens A&A 518 L89 (2010) DOI: 10.1051/0004-6361/201014541
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21111
Deposited By: Benjamin Perez
Deposited On:02 Dec 2010 19:31
Last Modified:03 Oct 2019 02:19

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