A Survey for New Members of Taurus from Stellar to Planetary Masses
AffiliationUniv Arizona, Steward Observ
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationEsplin, T. L., & Luhman, K. L. (2019). A Survey for New Members of Taurus from Stellar to Planetary Masses. The Astronomical Journal, 158(2), 54.
JournalThe Astronomical Journal
RightsCopyright © 2019. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractWe present a large sample of new members of the Taurus star-forming region that extend from stellar to planetary masses. To identify candidate members at substellar masses, we have used color-magnitude diagrams and proper motions measured with several wide-field optical and infrared (IR) surveys. At stellar masses, we have considered the candidate members that were found in a recent analysis of high-precision astrometry from the Gaia mission. Using new and archival spectra, we have measured spectral types and assessed membership for these 161 candidates, 79 of which are classified as new members. Our updated census of Taurus now contains 519 known members. According to Gaia data, this census should be nearly complete for spectral types earlier than M6-M7 at A(J) < 1. For a large field encompassing similar to 72% of the known members, the census should be complete for K < 15.7 at A(J) < 1.5, which corresponds to similar to 5-13. M-Jup for ages of 1-10. Myr based on theoretical evolutionary models. Our survey has doubled the number of known members at >= M9 and has uncovered the faintest known member in M-K, which should have a mass of similar to 3-10 M-Jup for ages of 1-10 Myr. We have used mid-IR photometry from the Spitzer Space Telescope and the Wide-field Infrared Survey Explorer to determine whether the new members exhibit excess emission that would indicate the presence of circumstellar disks. The updated disk fraction for Taurus is similar to 0.7 at <= M3.5 and similar to 0.4 at > M3.5.
VersionFinal published version
SponsorsNASA [80NSSC18 K0444, NNH14CK55B]; NASA; University of Texas at Austin McDonald Observatory; Pennsylvania State University; Department of Astronomy; National Development and Reform Commission; NSF; Alfred P. Sloan Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences; Los Alamos National Laboratory; Max-Planck-Institute for Astronomy; Max-Planck-Institute for Astrophysics; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; National Aeronautics and Space Administration [NNX08AR22G]; NSF [AST-1238877]; Eberly College of Science; Pennsylvania Space Grant Consortium; New Mexico State University; [U/17B/UA05]; [GN-2017B-Q-8]; [GN-2018B-Q-114]; [GN-2018B-FT-205]; [GN-2018B-FT-207]