English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Multiplicity is a key statistic for understanding the formation of very lowmass (VLM) stars and brown dwarfs. Currently, the separation distribution ofVLM binaries remains poorly constrained at small separations ($\leq$ 1 AU),leading to uncertainty in the overall binary fraction. We approach this problemby searching for late-M/early-L plus T dwarf spectral binaries whose combinedlight spectra exhibit distinct peculiarities, allowing forseparation-independent identification. We define a set of spectral indicesdesigned to identify these systems, and use a spectral template fitting methodto confirm and characterize spectral binary (SB) candidates from a library of815 spectra from the SpeX Prism Spectral Libraries. We present eleven newbinary candidates, confirm three previously reported candidates and rule outtwo previously identified candidates, all with primary and secondary spectraltypes between M7-L7 and T1-T8, respectively. We find that subdwarfs and blue Ldwarfs are the primary contaminants in our sample and propose a method forsegregating these sources. If confirmed by follow-up observations, thesesystems may add to the growing list of tight separation binaries, whose orbitalproperties may yield further insight into brown dwarf formation scenarios.

SpeX Spectroscopy of Unresolved Very Low Mass Binaries. II. Identification of Fourteen Candidate Binaries with Late-M/Early-L and T Dwarf Components