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Abstract Due to dust grain alignment with magnetic fields, dust polarization observations of far-infrared emission from cold molecular clouds are often used to trace magnetic fields, allowing a probe of the effects of magnetic fields on the star formation process. We present inferred magnetic field maps of the Pillars of Creation region within the larger M16 emission nebula, derived from dust polarization data in the 89 and 154μm continuum using the Stratospheric Observatory For Infrared Astronomy/High-resolution Airborne Wideband Camera. We derive magnetic field strength estimates using the Davis–Chandrasekhar–Fermi method. We compare the polarization and magnetic field strengths to column densities and dust continuum intensities across the region to build a coherent picture of the relationship between star-forming activity and magnetic fields in the region. The projected magnetic field strengths derived are in the range of ∼50–130μG, which is typical for clouds of similarn(H₂), i.e., molecular hydrogen volume density on the order of 10⁴–10⁵cm⁻³. We conclude that star formation occurs in the finger tips when the magnetic fields are too weak to prevent radial collapse due to gravity but strong enough to oppose OB stellar radiation pressure, while in the base of the fingers the magnetic fields hinder mass accretion and consequently star formation. We also support an initial weak-field model (<50μG) with subsequent strengthening through realignment and compression, resulting in a dynamically important magnetic field. 

With the goal of adding Science Ready Data Products to the archive of the Large Millimeter Telescope (LMT), we have developed a toolkit that allows automated pipeline processing of LMT single dish spectral line data. The data products include automatic source detection and spectral line detection using the ALMA Data Mining Toolkit (ADMIT). Adopting SDFITS as the interchange format, we aim that other observatories can use our toolkit and that LMT data can be analyzed by other packages. Interoperability tests are planned for this. In addition to the on-site Quick Look products, we now produce Timely Analysis Products (TAP) within 15 minutes after the observation has ended for an on-the-fly map, and much faster for pointed observations. These provide the scientist with rapid feedback on the scientific content.