TY - JOUR
T1 - The Hawaii Infrared Parallax Program. VI. The Fundamental Properties of 1000+ Ultracool Dwarfs and Planetary-mass Objects Using Optical to Mid-infrared Spectral Energy Distributions and Comparison to BT-Settl and ATMO 2020 Model Atmospheres
AU - Sanghi, Aniket
AU - Liu, Michael C.
AU - Best, William M.J.
AU - Dupuy, Trent J.
AU - Siverd, Robert J.
AU - Zhang, Zhoujian
AU - Hurt, Spencer A.
AU - Magnier, Eugene A.
AU - Aller, Kimberly M.
AU - Deacon, Niall R.
N1 - Funding Information:
The authors would like to thank the anonymous referee for many helpful comments, which improved the manuscript. We also thank August (Gus) Muench, AAS Data Editor, for helpful suggestions, which improved the presentation and accessibility of data products associated with this work, and Aaron Meisner and Adam Schneider for helpful discussions on cross-matching ALLWISE sources with CatWISE2020 sources. This work has benefitted from The UltracoolSheet, maintained by Will Best, Trent Dupuy, Michael Liu, Aniket Sanghi, Rob Siverd, and Zhoujian Zhang, and developed from compilations by Dupuy & Liu (2012), Dupuy & Kraus (2013), Liu et al. (2016), Best et al. (2018, 2020), and Schneider et al. (2023). The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA). The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. 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.
Funding Information:
This publication makes use of data products from the following: the Two Micron All Sky Survey (2MASS), 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; the UKIRT Infrared Deep Sky Survey (UKIDSS) project, which is defined in Lawrence et al. (), uses the UKIRT Wide Field Camera (WFCAM; Casali et al. ) and a photometric system described in Hewett et al. (), and the pipeline and science archives described in Irwin (), Hambly et al. (); the Wide-field Infrared Survey Explorer (WISE), 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; the SIMBAD database, Aladin, and Vizier, operated at the Strasbourg astronomical Data Center (CDS), Strasbourg, France; the SpeX prism Spectral Libraries, maintained by Adam Burgasser; the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; the Spanish Virtual Observatory ( https://svo.cab.inta-csic.es ) project funded by MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00.
Funding Information:
A.S. acknowledges support from Research Experience for Undergraduate program at the Institute for Astronomy, University of Hawaii-Manoa funded through National Science Foundation (NSF) grant No. 2050710. A.S. would like to thank the Institute for Astronomy for their hospitality during the course of this project. This research was funded in part by the Gordon and Betty Moore Foundation through grant GBMF8550 to M.C.L. W.M.J.B. acknowledges support from grant HST-GO-15238 provided by STScI and AURA. T.J.D. acknowledges support from UKRI STFC Astronomy Grants Panel (AGP) grant ST/W001209/1. For the purpose of open access, the author has applied a Creative Commons Attribution (CC BY) licence to any author accepted manuscript version arising from this submission.
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/12/6
Y1 - 2023/12/6
N2 - We derive the bolometric luminosities (L bol) of 865 field-age and 189 young ultracool dwarfs (spectral types M6-T9, including 40 new discoveries presented here) by directly integrating flux-calibrated optical to mid-infrared (MIR) spectral energy distributions (SEDs). The SEDs consist of low-resolution (R ∼ 150) near-infrared (NIR; 0.8-2.5μm) spectra (including new spectra for 97 objects), optical photometry from the Pan-STARRS1 survey, and MIR photometry from the CatWISE2020 survey and Spitzer/IRAC. Our L bol calculations benefit from recent advances in parallaxes from Gaia, Spitzer, and UKIRT, as well as new parallaxes for 19 objects from CFHT and Pan-STARRS1 presented here. Coupling our L bol measurements with a new uniform age analysis for all objects, we estimate substellar masses, radii, surface gravities, and effective temperatures (T eff) using evolutionary models. We construct empirical relationships for L bol and T eff as functions of spectral type and absolute magnitude, determine bolometric corrections in optical and infrared bandpasses, and study the correlation between evolutionary model-derived surface gravities and NIR gravity classes. Our sample enables a detailed characterization of BT-Settl and ATMO 2020 atmospheric model systematics as a function of spectral type and position in the NIR color-magnitude diagram. We find the greatest discrepancies between atmospheric and evolutionary model-derived T eff (up to 800 K) and radii (up to 2.0 R Jup) at the M/L spectral type transition boundary. With 1054 objects, this work constitutes the largest sample to date of ultracool dwarfs with determinations of their fundamental parameters.
AB - We derive the bolometric luminosities (L bol) of 865 field-age and 189 young ultracool dwarfs (spectral types M6-T9, including 40 new discoveries presented here) by directly integrating flux-calibrated optical to mid-infrared (MIR) spectral energy distributions (SEDs). The SEDs consist of low-resolution (R ∼ 150) near-infrared (NIR; 0.8-2.5μm) spectra (including new spectra for 97 objects), optical photometry from the Pan-STARRS1 survey, and MIR photometry from the CatWISE2020 survey and Spitzer/IRAC. Our L bol calculations benefit from recent advances in parallaxes from Gaia, Spitzer, and UKIRT, as well as new parallaxes for 19 objects from CFHT and Pan-STARRS1 presented here. Coupling our L bol measurements with a new uniform age analysis for all objects, we estimate substellar masses, radii, surface gravities, and effective temperatures (T eff) using evolutionary models. We construct empirical relationships for L bol and T eff as functions of spectral type and absolute magnitude, determine bolometric corrections in optical and infrared bandpasses, and study the correlation between evolutionary model-derived surface gravities and NIR gravity classes. Our sample enables a detailed characterization of BT-Settl and ATMO 2020 atmospheric model systematics as a function of spectral type and position in the NIR color-magnitude diagram. We find the greatest discrepancies between atmospheric and evolutionary model-derived T eff (up to 800 K) and radii (up to 2.0 R Jup) at the M/L spectral type transition boundary. With 1054 objects, this work constitutes the largest sample to date of ultracool dwarfs with determinations of their fundamental parameters.
UR - http://www.scopus.com/inward/record.url?scp=85180105433&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/acff66
DO - 10.3847/1538-4357/acff66
M3 - Article
AN - SCOPUS:85180105433
SN - 0004-637X
VL - 959
SP - 1
EP - 41
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 63
ER -