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Population Properties of Brown Dwarf Analogs to Exoplanets Jacqueline K

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Population Properties of Brown Dwarf Analogs to Exoplanets Jacqueline K Dartmouth College Dartmouth Digital Commons Open Dartmouth: Faculty Open Access Articles 7-2016 Population Properties of Brown Dwarf Analogs to Exoplanets Jacqueline K. FahertY American Museum of Natural History Adric R. Riedel American Museum of Natural History Kelle L. Cruz American Museum of Natural History Jonathan Gagne Carnegie Institution of Washington Joseph C. Filippazzo American Museum of Natural History See next page for additional authors Follow this and additional works at: https://digitalcommons.dartmouth.edu/facoa Part of the Stars, Interstellar Medium and the Galaxy Commons Recommended Citation FahertY, Jacqueline K.; Riedel, Adric R.; Cruz, Kelle L.; Gagne, Jonathan; Filippazzo, Joseph C.; Lambrides, Erini; Fica, Haley; Weinberger, Alycia; and Thorstensen, John R., "Population Properties of Brown Dwarf Analogs to Exoplanets" (2016). Open Dartmouth: Faculty Open Access Articles. 2297. https://digitalcommons.dartmouth.edu/facoa/2297 This Article is brought to you for free and open access by Dartmouth Digital Commons. It has been accepted for inclusion in Open Dartmouth: Faculty Open Access Articles by an authorized administrator of Dartmouth Digital Commons. For more information, please contact [email protected]. Authors Jacqueline K. FahertY, Adric R. Riedel, Kelle L. Cruz, Jonathan Gagne, Joseph C. Filippazzo, Erini Lambrides, Haley Fica, Alycia Weinberger, and John R. Thorstensen This article is available at Dartmouth Digital Commons: https://digitalcommons.dartmouth.edu/facoa/2297 The Astrophysical Journal Supplement Series, 225:10 (57pp), 2016 July doi:10.3847/0067-0049/225/1/10 © 2016. The American Astronomical Society. All rights reserved. POPULATION PROPERTIES OF BROWN DWARF ANALOGS TO EXOPLANETS* Jacqueline K. Faherty1,2,11, Adric R. Riedel2,3, Kelle L. Cruz2,3,4, Jonathan Gagne1,12, Joseph C. Filippazzo2,4,5, Erini Lambrides2, Haley Fica2, Alycia Weinberger1, John R. Thorstensen6, C. G. Tinney7,8, Vivienne Baldassare2,9, Emily Lemonier2,10, and Emily L. Rice2,4,5 1 Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA; [email protected] 2 Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10034, USA; [email protected] 3 Department of Physics & Astronomy, Hunter College, 695 Park Avenue, New York, NY 10065, USA 4 Physics Program, The Graduate Center, City University of New York, New York, NY 10016, USA 5 Department of Engineering Science & Physics, College of Staten Island, 2800 Victory Boulevard, Staten Island, NY 10301, USA 6 Department of Physics and Astronomy, Dartmouth College, Hanover NH 03755, USA 7 School of Physics,UNSW Australia, 2052, Australia 8 Australian Centre for Astrobiology, UNSW Australia, 2052, Australia 9 Department of Astronomy, University of Michigan, 1085 S. University, Ann Arbor, MI 48109, USA 10 Department of Physics & Astronomy, Columbia University, Broadway and 116th Street, New York, NY 10027, USA Received 2016 February 1; revised 2016 May 4; accepted 2016 May 6; published 2016 July 22 ABSTRACT We present a kinematic analysis of 152 low surface gravity M7-L8 dwarfs by adding 18 new parallaxes (including 10 for comparative field objects), 38 new radial velocities, and 19 new proper motions. We also add low- or moderate- resolution near-infrared spectra for 43 sources confirming their low surface gravity features. Among the full sample, we find 39 objects to be high-likelihood or new bona fide members of nearby moving groups, 92 objects to be ambiguous members and 21 objects that are non-members. Using this age-calibrated sample, we investigate trends in gravity classification, photometric color, absolute magnitude, color–magnitude, luminosity, and effective temperature. We find that gravity classification and photometric color clearly separate 5–130 Myr sources from >3Gyrfield objects, but they do not correlate one to one with the narrower 5–130 Myr age range. Sources with the same spectral subtype in the same group have systematically redder colors, but they are distributed between 1 and 4σ from the field sequences and the most extreme outlier switches between intermediate- and low-gravity sources either confirmed in a group or not. The absolute magnitudes of low-gravity sources from the J band through W3showaflux redistribution when compared to equivalently typed field brown dwarfs that is correlated with spectral subtype. Low-gravity, late-type L dwarfs are fainter at J than the field sequence but brighter by W3. Low-gravity M dwarfs are >1 mag brighter than field dwarfs in all bands from J through W3. Clouds, which are a far more dominant opacity source for L dwarfs, are the likely cause. On color–magnitude diagrams, the latest-type, low-gravity L dwarfs drive the elbow of the L/T transition up to 1 mag redder and 1 mag fainter than field dwarfs at MJ but are consistent with or brighter than the elbow at MW1 and MW2.We conclude that low-gravity dwarfs carry an extreme version of the cloud conditions of field objects to lower temperatures, which logically extends into the lowest-mass, directly imaged exoplanets. Furthermore, there is an indication on color- magnitude diagrams (CMDs; such as MJ versus ( J–W2)) of increasingly redder sequences separated by gravity classification, although it is not consistent across all CMD combinations. Examining bolometric luminosities for planets and low-gravity objects, we confirm that (in general) young M dwarfs are overluminous while young L dwarfs are normal compared to the field. Using model extracted radii, this translates into normal to slightly warmer M dwarf temperatures compared to the field sequence and lower temperatures for L dwarfs with no obvious correlation with the assigned moving group. Key words: astrometry – brown dwarfs – stars: low-mass 1. INTRODUCTION Objects with masses 75 MJup cool through their lives with spectral energy distributions evolving as their atmospheric At masses 75 MJup,thatis,theH-burning mass limit, the fi chemistry changes with decreasing temperatures. The spectral interior of a source changes signi cantly. Below this mass limit, fi ( > > ) fi classi cation for sources in the range 3000 K Teff 250 K electron degeneracy pressure suf ciently slows contraction that fi the core of a given object is prevented from ever reaching the corresponds to late-type M, L, T, and Y with each class de ned ( by the effects of changing molecular species available in the temperatures required for nuclear fusion Hayashi & Nakano ( 1963;Kumar1963). As a consequence, the evolution of photosphere Kirkpatrick 2005; Burgasser et al. 2002a; Cush- ing et al. 2011). At the warmest temperatures, the atmosphere is substellar-mass objects produces a temperature, age, and mass ( degeneracy that leads to an important, and at times completely too hot for the condensation of solids Allard & Hauschildt 1995; Lodders 1999). However, as Teff falls below indistinguishable, overlap in the physical properties of the lowest- ( ) ( ) mass stars, brown dwarfs, and planets. 2500 K, both liquid e.g., Fe and solid e.g., CaTiO3,VO mineral and metal condensates settle into discrete cloud layers (Tsuji et al. 1996a, 1996b; Ackerman & Marley 2001; Allard * This paper includes data gathered with the 6.5 m Magellan Telescopes ) located at Las Campanas Observatory, Chile. et al. 2001; Woitke & Helling 2004 . 11 Hubble Fellow. As temperatures cool further, cloud layers form at such deep 12 Sagan Fellow. levels in the photosphere that they have little or no impact on 1 The Astrophysical Journal Supplement Series, 225:10 (57pp), 2016 July Faherty et al. the emergent spectrum. This transition between “cloudy” to planetary-mass companions (e.g., PSO318, SDSS1110, 0047 “cloudless” objects occurs rapidly over a narrow temperature +6803; Gizis et al. 2012, 2015; Liu et al. 2013; Gagné et al. range (1200–1400 K, corresponding to the transition between 2015c). Studies of these two populations in concert may L-type and T-type spectra) and drives extreme photometric, resolve questions of the formation of companions versus spectroscopic, and luminosity changes (Burgasser et al. 2002b; isolated equivalents and help to untangle atmosphere, temper- Tinney et al. 2003; Artigau et al. 2009; Dupuy & Liu 2012; ature, age, and metallicity effects on the observables. Faherty et al. 2012, 2014a; Radigan et al. 2012). Violent storms In this work, we examine this new population of suspected (like those seen on Jupiter), along with magnetic-activity- young, low surface gravity sources that are excellent exoplanet inducing aurorae, have been noted as environmental conditions analogs. In Section 2, we explain the sample examined in this likely to be present at the L-T transition (Radigan et al. 2012; work and in Section 3 we describe the imaging and spectral Apai et al. 2013; Gillon et al. 2013; Buenzli et al. 2014, 2015; data acquired. In Section 4, we review new near-infrared Burgasser et al. 2014; Faherty et al. 2014a; Hallinan et al. spectral types designated in this work and in Section 5 we 2015; Metchev et al. 2015). discuss how we measured new radial velocities. In Section 6, Confounding our understanding of cloud formation in low- we assess the likelihood of membership in nearby moving temperature atmospheres is the mounting evidence for a groups such as β Pictoris, AB Doradus, Argus, Columba, TW correlation between cloud properties and youth. Low surface Hydrae, and Tucana Horologium. In Section 7, we review the gravity brown dwarfs, which are thought to be young, have diversity of the whole sample in spectral features, infrared unusually red near- to mid-infrared colors and a fainter absolute colors, absolute magnitudes, bolometric luminosities, and magnitude through ∼2.5 μm when compared to their older effective temperatures. In Section 8, we place the young brown spectral counterparts with field surface gravities (Faherty dwarf sample in context with directly imaged planetary-mass et al. 2012, 2013; Liu et al. 2013; Gagné et al. 2015b; companions. Conclusions are presented in Section 9. Filippazzo et al. 2015). Metchev & Hillenbrand (2006) made the first connection between age and cloudiness in their study 2.
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