Left: intensity of thermal dust emission (MJy sr^-1) at the wavelength λ = 250μm in a region of 5′ × 5′ region around Cha-MMS1. The map is centred at the Spitzer 24 μm peak indicated with a red triangle. The red circle in the top right corner corresponds to the average Herschel beamsize (FWHM, 18″) at 250 μm. The small white ellipse shows the synthesised ATCA beam (~7″). Middle: dust temperature, T_dust (K), in the same region. The red circle in the top right corner represents the resolution of the calculated T_dust and H₂ column density maps (40″). Right: H₂ column density, N(H₂) (10²² cm^-2) derived from the 250 μm optical thickness, τ_{250 μm}. The dust temperature and column density maps are derived by fitting a modified blackbody function to the Herschel intensity maps at 500, 350, 250, and 160 μm assuming an emissivity index of β = 2.0 (see text). The locations of three prominent young stellar objects (YSOs), Ced110 IRS2 (right), IRS4 (middle), and IRS6 (left), are indicated with asterisks. The plus sign indicates the location of the millimetre source Cha-MMS1a (Reipurth et al. 1996). The white contour shows the integrated intensity level 5 K km s^-1 of the NH₃(1,1) satellites as observed with ATCA. The yellow contours in the right panel shows the integrated intensity () of the NH₃(1,1) line emission (K km s^-1) observed at Parkes. The Parkes beam is shown with the large yellow circle in the top right corner.