Multi-scale view of the magnetic field around Ser-emb 8 (﹩{\alpha }_{{\rm{J}}2000}﹩ = 18:29:48.089, ﹩{\delta }_{{\rm{J}}2000}﹩ = +1:16:43.32). Line segments represent the magnetic field orientation, rotated by ﹩90^\circ ﹩ from the dust polarization (the length of each segment is identical and does not represent any other quantity). Grayscale is total intensity (Stokes I) thermal dust emission. Panel (a) shows 870 μm JCMT observations (Matthews et al. 2009), (b) shows 1.3 mm CARMA observations (Hull et al. 2014), and (c) shows 870 μm ALMA observations, revealing the magnetic field morphology with ∼10,000, 1000, and 140 au resolution, respectively. For the ALMA data, line segments are plotted where the polarized intensity ﹩P\gt 3{\sigma }_{P};﹩ the rms noise in the polarized intensity map ﹩{\sigma }_{P}=25﹩ μJy beam⁻¹. The dust emission is shown starting at 3 × σ_I, where the rms noise in the Stokes I map σ_I = 50 μJy beam⁻¹. The peak polarized and total intensities in the ALMA data are 0.693 mJy beam⁻¹ and 102 mJy beam⁻¹, respectively (the two peaks do not coincide exactly). The red and blue arrows indicate the redshifted and blueshifted lobes of the bipolar outflow (Hull et al. 2014). The text below each of the panels indicates the physical size of the image at the 436 pc distance to the Serpens Main region (Ortiz-León et al. 2017; see earlier results by Dzib et al. 2010, 2011). The black ellipses in the lower left corners of the ALMA and CARMA maps represent the synthesized beams (resolution elements). The ALMA beam measures ﹩0\buildrel{\prime\prime}\over{.} 35\times 0\buildrel{\prime\prime}\over{.} 32﹩ at a position angle of −63°; the CARMA beam measures ﹩2\buildrel{\prime\prime}\over{.} 89\times 2\buildrel{\prime\prime}\over{.} 43﹩ at a position angle of ﹩13^\circ ﹩. The JCMT data have a resolution of ﹩20^{\prime\prime} ﹩.

(The data used to create this figure are available.)