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

Authordc.contributor.authorMeixner, M. 
Authordc.contributor.authorGalliano, F. es_CL
Authordc.contributor.authorHony, S. es_CL
Authordc.contributor.authorRoman-Duval, J. es_CL
Authordc.contributor.authorRobitaille, T. es_CL
Authordc.contributor.authorPanuzzo, P. es_CL
Authordc.contributor.authorSauvage, M. es_CL
Authordc.contributor.authorGordon, K. es_CL
Authordc.contributor.authorEngelbracht, C. es_CL
Authordc.contributor.authorMisselt, K. es_CL
Authordc.contributor.authorOkumura, K. es_CL
Authordc.contributor.authorBeck, T. es_CL
Authordc.contributor.authorBernard, J. P. es_CL
Authordc.contributor.authorBolatto, Alberto es_CL
Authordc.contributor.authorBot, Caroline es_CL
Authordc.contributor.authorBoyer, M. es_CL
Authordc.contributor.authorBracker, S. es_CL
Authordc.contributor.authorCarlson, L. R. es_CL
Authordc.contributor.authorClayton, G. C. es_CL
Authordc.contributor.authorChen, C.-H. R. es_CL
Authordc.contributor.authorChurchwell, E. es_CL
Authordc.contributor.authorFukui, Y. es_CL
Authordc.contributor.authorGalametz, M. es_CL
Authordc.contributor.authorHora, J. L. es_CL
Authordc.contributor.authorHughes, A. es_CL
Authordc.contributor.authorIndebetouw, R. es_CL
Authordc.contributor.authorIsrael, F. P. es_CL
Authordc.contributor.authorKawamura, A. es_CL
Authordc.contributor.authorKemper, F. es_CL
Authordc.contributor.authorKim, S. es_CL
Authordc.contributor.authorKwon, E. es_CL
Authordc.contributor.authorLawton, B. es_CL
Authordc.contributor.authorLi, A. es_CL
Authordc.contributor.authorLong, K. S. es_CL
Authordc.contributor.authorMarengo, M. es_CL
Authordc.contributor.authorMadden, S. C. es_CL
Authordc.contributor.authorMatsuura, M. es_CL
Authordc.contributor.authorOliveira, J. M. es_CL
Authordc.contributor.authorOnishi, T. es_CL
Authordc.contributor.authorOtsuka, M. es_CL
Authordc.contributor.authorParadis, D. es_CL
Authordc.contributor.authorPoglitsch, A. es_CL
Authordc.contributor.authorRiebel, D. es_CL
Authordc.contributor.authorReach, W. T. es_CL
Authordc.contributor.authorRubio López, Mónica es_CL
Authordc.contributor.authorSargent, B. es_CL
Authordc.contributor.authorSewiło, M. es_CL
Authordc.contributor.authorSimon, J. D. es_CL
Authordc.contributor.authorSkibba, R. es_CL
Authordc.contributor.authorSmith, L. J. es_CL
Authordc.contributor.authorSrinivasan, S. es_CL
Authordc.contributor.authorTielens, A. G. G. M. es_CL
Authordc.contributor.authorvan Loon, J. Th. es_CL
Authordc.contributor.authorWhitney, B. es_CL
Authordc.contributor.authorWoods, P. M. es_CL
Cita de ítemdc.identifier.citationA&A 518, L71 (2010)en_US
Identifierdc.identifier.otherDOI: 10.1051/0004-6361/201014662
General notedc.descriptionArtículo de publicación ISIen_US
Abstractdc.description.abstractThe 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 ( fPAH) 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.en_US
Patrocinadordc.description.sponsorshipfinancial 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.en_US
Publisherdc.publisherEDP SCIENCES S A.en_US
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 Chile*
Link to Licensedc.rights.uri*
Keywordsdc.subjectINTERSTELLAR DUSTen_US
Títulodc.titleHERschel Inventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dusten_US
Document typedc.typeArtículo de revistaen_US

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Except where otherwise noted, this item's license is described as Attribution-NonCommercial-NoDerivs 3.0 Chile