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tokens: We thank the anonymous referee for a very thorough report, which led to numerous improvements in this manuscript. GCS was supported by NASA through Contract Number 1257184 issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407 and the NSF through Award 1108645. We thank Jean-Baptiste Marquette (IAP) for providing some EROS2 photometric data, Alistair Glasse (UKATC) for providing the JWST/MIRI filter response curves, and Sara Bladh (Padova University) for providing the results for her M-star models, including the gas-to-dust ratios. This publication is partly based on the OGLE observations obtained with the Warsaw Telescope at the Las Campanas Observatory, Chile, operated by the Carnegie Institution of Washington. This paper utilizes public domain data originally obtained by the MACHO Project, whose work was performed under the joint auspices of the U.S. Department of Energy, National Nuclear Security Administration by the University of California, Lawrence Livermore National Laboratory under contract No. W-7405-Eng-48, the National Science Foundation through the Center for Particle Astrophysics of the University of California under cooperative agreement AST-8809616, and the Mount Stromlo and Siding Spring Observatory, part of the Australian National University. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France. This publication makes use of data products from WISE and NEOWISE, which a joint projects of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Based on data from the OMC Archive at CAB (INTA-CSIC), pre-processed by ISDC. The CSS survey is funded by the National Aeronautics and Space Administration under Grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the U.S. National Science Foundation under grants AST-0909182. Based on observations made with VISTA at ESO under programme ID 179.B-2003.