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HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dust

Meixner, M. and Paradis, D. and Reach, W. T. (2010) HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dust. Astronomy and Astrophysics, 518 . Art. No. L71. ISSN 0004-6361.

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The HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) of the Magellanic Clouds will use dust emission to investigate the life cycle of matter in both the Large and Small Magellanic Clouds (LMC and SMC). Using the Herschel Space Observatory’s PACS and SPIRE photometry cameras, we imaged a 2° × 8° strip through the LMC, at a position angle of ~22.5° as part of the science demonstration phase of the Herschel mission. We present the data in all 5 Herschel bands: PACS 100 and 160 μm and SPIRE 250, 350 and 500 μm. We present two dust models that both adequately fit the spectral energy distribution for the entire strip and both reveal that the SPIRE 500 μm emission is in excess of the models by ~6 to 17%. The SPIRE emission follows the distribution of the dust mass, which is derived from the model. The PAH-to-dust mass (f_(PAH)) image of the strip reveals a possible enhancement in the LMC bar in agreement with previous work. We compare the gas mass distribution derived from the HI 21 cm and CO J = 1−0 line emission maps to the dust mass map from the models and derive gas-to-dust mass ratios (GDRs). The dust model, which uses the standard graphite and silicate optical properties for Galactic dust, has a very low GDR = 65^(+15) _(−18) making it an unrealistic dust model for the LMC. Our second dust model, which uses amorphous carbon instead of graphite, has a flatter emissivity index in the submillimeter and results in a GDR = 287^_(+25)_(−42) that is more consistent with a GDR inferred from extinction.

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Reach, W. T.0000-0001-8362-4094
Additional Information:© 2010 ESO. Received 31 March 2010, Accepted 14 April 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, JPL contracts # 1381522 & 1381650. M.R. is supported by FONDECYT No. 1080335 and FONDAP No. 15010003. 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 instrument control centers, without which none of this work would be possible.
Funding AgencyGrant Number
NASA Herschel Science Center1381522
NASA Herschel Science Center1381650
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) (UK)UNSPECIFIED
PACS/SPIRE instrument control centersUNSPECIFIED
Subject Keywords:Magellanic Clouds, dust, extinction, submillimeter: galaxies, submillimeter: ISM
Record Number:CaltechAUTHORS:20101202-140057337
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Official Citation:HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dust M. Meixner, F. Galliano, S. Hony, J. Roman-Duval, T. Robitaille, P. Panuzzo, M. Sauvage, K. Gordon, C. Engelbracht, K. Misselt, K. Okumura, T. Beck, J.-P. Bernard, A. Bolatto, C. Bot, M. Boyer, S. Bracker, L. R. Carlson, G. C. Clayton, C.-H. R. Chen, E. Churchwell, Y. Fukui, M. Galametz, J. L. Hora, A. Hughes, R. Indebetouw, F. P. Israel, A. Kawamura, F. Kemper, S. Kim, E. Kwon, B. Lawton, A. Li, K. S. Long, M. Marengo, S. C. Madden, M. Matsuura, J. M. Oliveira, T. Onishi, M. Otsuka, D. Paradis, A. Poglitsch, D. Riebel, W. T. Reach, M. Rubio, B. Sargent, M. Sewiło, J. D. Simon, R. Skibba, L. J. Smith, S. Srinivasan, A. G. G. M. Tielens, J. Th. van Loon, B. Whitney and P. M. Woods A&A 518 L71 (2010) DOI: 10.1051/0004-6361/201014662
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21130
Deposited By: Benjamin Perez
Deposited On:02 Dec 2010 22:58
Last Modified:03 Oct 2019 02:20

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