2010A&A...518L..89G


Query : 2010A&A...518L..89G

2010A&A...518L..89G - Astronomy and Astrophysics, volume 518, L89-89 (2010/7-2)

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

GORDON K.D., GALLIANO F., HONY S., BERNARD J.-P., BOLATTO A., BOT C., ENGELBRACHT C., HUGHES A., ISRAEL F.P., KEMPER F., KIM S., LI A., MADDEN S.C., MATSUURA M., MEIXNER M., MISSELT K., OKUMURA K., PANUZZO P., RUBIO M., REACH W.T., ROMAN-DUVAL J., SAUVAGE M., SKIBBA R. and TIELENS A.G.G.M.

Abstract (from CDS):

The properties of the dust grains (e.g., temperature and mass) can be derived from fitting far-IR SEDs (≥100µm). Only with SPIRE on Herschel has it been possible to get high spatial resolution at 200 to 500µm that is beyond the peak (∼160µm) of dust emission in most galaxies. We investigate the differences in the fitted dust temperatures and masses determined using only <200µm data and then also including >200µm data (new SPIRE observations) to determine how important having >200µm data is for deriving these dust properties. We fit the 100 to 350µm 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 160µm (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. The dust temperatures and masses computed using only 100 and 160µm data can differ by up to 10% and 36%, respectively, from those that also include the SPIRE 250 & 350µm data. We find that an emissivity law proportional to λ–1.5 minimizes the 100-350µm fractional residuals. We find that the emission at 500µm is ∼10% higher than expected from extrapolating the fits made at shorter wavelengths. We find the fractional 500µm excess is weakly anti-correlated with MIPS 24µm flux and the total gas surface density. This argues against a flux calibration error as the origin of the 500µm 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≥500µm for the origin of the 500µm excess.

Abstract Copyright:

Journal keyword(s): ISM: general - galaxies: individual: LMC - Magellanic Clouds - infrared: ISM

Simbad objects: 3

goto Full paper

goto View the references in ADS

Number of rows : 3
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10530 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6555 1
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16509 1

To bookmark this query, right click on this link: simbad:objects in 2010A&A...518L..89G and select 'bookmark this link' or equivalent in the popup menu


2023.01.30-23:19:36

© Université de Strasbourg/CNRS

    • Contact