000002118 001__ 2118
000002118 005__ 20160706150424.0
000002118 0247_ $$2DOI$$a10.1051/0004-6361/201424189
000002118 037__ $$aASTROimport-275
000002118 100__ $$aVan de Steene, G. C.
000002118 245__ $$aHerschel imaging of the dust in the Helix nebula (NGC 7293)
000002118 260__ $$c2015
000002118 520__ $$aAims: In our series of papers presenting the Herschel imaging of evolved planetary nebulae, we present images of the dust distribution in the Helix nebula (NGC 7293).  Methods: Images at 70, 160, 250, 350, and 500 µm were obtained with the PACS and SPIRE instruments on board the Herschel satellite.  Results: The broadband maps show the dust distribution over the main Helix nebula to be clumpy and predominantly present in the barrel wall. We determined the spectral energy distribution of the main nebula in a consistent way using Herschel, IRAS, and Planck flux values. The emissivity index of ß = 0.99 ± 0.09, in combination with the carbon rich molecular chemistry of the nebula, indicates that the dust consists mainly of amorphous carbon. The dust excess emission from the central star disk is detected at 70 µm and the flux measurement agrees with previous measurement. We present the temperature and dust column density maps. The total dust mass across the Helix nebula (without its halo) is determined to be 3.5 × 10-3 M? at a distance of 216 pc. The temperature map shows dust temperatures between 22 K and 42 K, which is similar to the kinetic temperature of the molecular gas, confirming that the dust and gas co-exist in high density clumps. Archived images are used to compare the location of the dust emission in the far infrared (Herschel) with the ionized (GALEX and Hß) and molecular (H2) component. The different emission components are consistent with the Helix consisting of a thick walled barrel-like structure inclined to the line of sight. The radiation field decreases rapidly through the barrel wall. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
000002118 700__ $$avan Hoof, P. A. M.
000002118 700__ $$aExter, K. M.
000002118 700__ $$aBarlow, M. J.
000002118 700__ $$aCernicharo, J.
000002118 700__ $$aEtxaluze, M.
000002118 700__ $$aGear, W. K.
000002118 700__ $$aGoicoechea, J. R.
000002118 700__ $$aGomez, H. L.
000002118 700__ $$aGroenewegen, M. A. T.
000002118 700__ $$aHargrave, P. C.
000002118 700__ $$aIvison, R. J.
000002118 700__ $$aLeeks, S. J.
000002118 700__ $$aLim, T. L.
000002118 700__ $$aMatsuura, M.
000002118 700__ $$aOlofsson, G.
000002118 700__ $$aPolehampton, E. T.
000002118 700__ $$aSwinyard, B. M.
000002118 700__ $$aUeta, T.
000002118 700__ $$aVan Winckel, H.
000002118 700__ $$aWaelkens, C.
000002118 700__ $$aWesson, R.
000002118 773__ $$cA134$$pAstronomy and Astrophysics$$v574$$y2015
000002118 85642 $$ahttp://esoads.eso.org/abs/2015A%26A...574A.134V
000002118 905__ $$apublished in
000002118 980__ $$aREFERD