A Novel Survey for Young Substellar Objects with the W-band Filter. I. Filter Design and New Discoveries in Ophiuchus and Perseus

We present the design and implementation of a medium-band near-IR filter tailored for detecting low-mass stars and brown dwarfs from the summit of Maunakea. The W -band filter is centered at 1.45 μ m with a bandpass width of 6%, designed to measure the depth of the H 2 O water absorption prominent in objects with spectral types of M6 and later. When combined with standard J and H photometry, the W -band filter is designed to determine spectral types to ≈1.4 subtypes for late-M and L dwarfs, largely independent of surface gravity and reddening. This filter’s primary application is completing the census of young substellar objects in star-forming regions, using W -band selection to greatly reduce contamination by reddened background stars that impede broad-band imaging surveys. We deployed the filter on the UH 88 inch telescope to survey ∼3 degree 2 of the NGC 1333, IC 348, and ρ Ophiuchus star-forming regions. Our spectroscopic followup of W -band selected candidates resulted in the confirmation of 48 ultracool dwarfs with a success rate of 89%, demonstrating the efficacy of this new filter and selection method.