tokens: We thank the anonymous referee for constructive comments that improve the paper significantly. We also thank Katelyn Allers for insightful comments on this work and Annie Robin for discussions about the Besançon Galactic models. We thank Kevin Luhman for providing his SpeX spectra of previously known Taurus members. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, and the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. UKIRT is owned by the University of Hawaii (UH) and operated by the UH Institute for Astronomy; operations are enabled through the cooperation of the East Asian Observatory. When (some of) the data reported here were acquired, UKIRT was operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK. This research has made use of the SIMBAD database, the VizieR catalog access tool, and “Aladin sky atlas” developed and operated at CDS, Strasbourg, France; the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; NASA’s Astrophysics Data System; the SpeX Prism Library, maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism ; and the catalog of photometry and proper motions of M, L, and T dwarfs from the PS1 3 π survey, maintained by William Best at http://www.ifa.hawaii.edu/wbest/Will_Best/PS1_MLT_Dwarfs.html . This work was greatly facilitated by many features of the TOPCAT software written by Mark Taylor ( http://www.starlink.ac.uk/topcat/ ). Finally, the authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Facilities: PS1 , IRTF (SpeX) , UKIRT (WFCAM) . Software: IPython (Pérez Granger 2007 ), Numpy and Scipy (van Der Walt et al. 2011 ), Astropy (Astropy Collaboration et al. 2013 ), Matplotlib (Hunter 2007 ).
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