Meeting the Cool Neighbors. X. Ultracool Dwarfs From the 2mass All-Sky Data Release

Reid, I. Neill; Cruz, Kelle L.; Kirkpatrick, J. Davy; Allen, Peter; Mungall, F.; Liebert, James; Lowrance, P.; Sweet, Anne

doi:10.1088/0004-6256/136/3/1290

Cited by 208 publications

(16 citation statements)

References 107 publications

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“…J1048−3956 was discovered and optically spectral typed as an M9 by Montes et al (2001). J1048−3956 was discovered by Reid et al (2008) and optically spectral typed as a L0 γ by Cruz et al (2009). As reported in Faherty et al (2016), J0223−5815 is a member of the Tucana-Horlogium moving group with an age ranging from 41 − 49 Myr (Bell et al 2015).…”

Section: Sample Selection and Propertiesmentioning

confidence: 65%

Understanding Fundamental Properties and Atmospheric Features of Subdwarfs via a Case Study of SDSS J125637.13–022452.4^∗

Gonzales¹,

Faherty²,

Gagné³

et al. 2018

ApJ

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We present the distance-calibrated spectral energy distribution (SED) of the sdL3.5 subdwarf SDSS J125637.13−022452.4 (J1256−0224) using its Gaia parallax and its resultant bolometric luminosity and semi-empirical fundamental parameters, as well as updated UVW velocities. The SED of J1256−0224 is compared to field-age and low-gravity dwarfs of the same effective temperature (T eff ) and bolometric luminosity. In the former comparison, we find that the SED of J1256−0224 is brighter than the field source in the optical, but dims in comparison beyond the J-band, where it becomes fainter than the field from the H through W2 bands. Compared to the young source, its fainter at all wavelengths. We conclude that J1256−0224 is depleted of condensates compared to both objects. A near infrared band-by-band analysis of the spectral features of J1256−0224 is done and is compared to the equivalent T eff sample. From this analysis, we find a peculiar behavior of the J-band K I doublets whereby the 1.17 µm doublet is stronger than the field or young source as expected, while the 1.25 µm doublet shows indications of low gravity. In examining a sample of 4 other subdwarfs with comparable data we confirm this trend across different subtypes indicating that the 1.25 µm doublet is a poor indicator of gravity for low metallicity objects. In the K-band analysis of J1256−0224 we detect the 2.29 µm CO line of J1256−0224, previously unseen in the low-resolution SpeX data. We also present fundamental parameters using Gaia parallaxes for 9 additional subdwarfs with spectral types M7 -L7 for comparison. The 10 subdwarfs are placed in a temperature sequence and we find a poor linear correlation with spectral type. We present polynomial relations for absolute magnitude in JHKW1W2, effective temperature, and bolometric luminosity versus spectral type for subdwarfs.

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Section: Sample Selection and Propertiesmentioning

confidence: 65%

Understanding Fundamental Properties and Atmospheric Features of Subdwarfs via a Case Study of SDSS J125637.13–022452.4^∗

Gonzales¹,

Faherty²,

Gagné³

et al. 2018

ApJ

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“…The UVW velocities are displayed in a Toomre diagram ( Figure 16) along with γ sources from Faherty et al (2016), Teegarden's Star, and LHS 132. For objects in this work labeled as "not in group" or "non-members", these are References-(1) Gizis et al (2000), (2) Reid et al (2008) sources from Faherty et al (2016) that could be ambiguous members, candidate members, or true non-members of any currently known group, thus objects that are not bonafide members.…”

Section: Uvwmentioning

confidence: 99%

A Reanalysis of the Fundamental Parameters and Age of TRAPPIST-1*

Gonzales

Faherty

Gagné

et al. 2019

ApJ

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We present the distance-calibrated spectral energy distribution (SED) of TRAPPIST-1 using a new medium resolution (R∼6000) near-infrared FIRE spectrum and its Gaia parallax. We report an updated bolometric luminosity (L bol ) of −3.216 ± 0.016, along with semi-empirical fundamental parameters: effective temperature T eff = 2628 ± 42 K, mass=90 ± 8 M Jup , radius=1.16 ± 0.03 R Jup , and log g=5.21 ± 0.06 dex. It's kinematics point toward an older age while spectral indices indicate youth therefore, we compare the overall SED and nearinfrared bands of TRAPPIST-1 to field-age, low-gravity, and low-metallicity dwarfs of similar T eff and L bol . We find field dwarfs of similar T eff and L bol best fit the overall and band-by-band features of TRAPPIST-1. Additionally, we present new Allers & Liu (2013) spectral indices for the SpeX SXD and FIRE spectra of TRAPPIST-1, both classifying it as intermediate gravity. Examining T eff , L bol , and absolute JHKW 1W 2 magnitudes versus optical spectral type places TRAPPIST-1 in an ambiguous location containing both field-and intermediategravity sources. Kinematics place TRAPPIST-1 within a subpopulation of intermediate-gravity sources lacking bonafide membership in a moving group with higher tangential and UVW velocities. We conclude that TRAPPIST-1 is a field-age source with subtle spectral features reminiscent of a low surface gravity object. To resolve the cause of TRAPPIST-1's intermediate gravity indicators we speculate two avenues which might be correlated to inflate the radius: (1) magnetic activity or (2) tidal interactions from planets. We find the M8 dwarf LHS 132 is an excellent match to TRAPPIST-1's spectral peculiarities along with the M9 β dwarf 2MASS J10220489+0200477, the L1 β 2MASS J10224821+5825453, and the L0 β 2MASS J23224684−3133231 which have distinct kinematics making all three intriguing targets for future exoplanet studies.

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“…The primary and the secondary are scaled based on their flux contribution according to the M K -spectral-type relation of Burgasser (2007a), with the source and light combined spectra being normalized to the J band. Figure 9 shows the best fit composite spectrum for W0404+4127, an L2 primary and an Kirkpatrick et al (2010) is an L o 1.5/L n 1 (Kirkpatrick et al , 2010, Kelu-1 is an L o 2/L n 2, 2MASSW J1506544+132106 is an L o 3/L n 3, 2MASS J08234818+2428577 observed by Burgasser et al (2010) is an L o 3 (Reid et al 2008), 2MASS J21580457−1550098 observed by Kirkpatrick et al (2010) is an L o 4:/L n 4 (Kirkpatrick et al , 2010, and SDSS J083506.16+195304.4 observed by Chiu et al (2006) is an L n 5 (Kirkpatrick et al 2010). The L2 standard (χ 2 = 0.22) is the best statistical fit.…”

Section: Unresolved Binary?mentioning

confidence: 99%

DISCOVERY OF FOUR HIGH PROPER MOTION L DWARFS, INCLUDING A 10 pc L DWARF AT THE L/T TRANSITION^,

Castro¹,

Gizis²,

Harris³

et al. 2013

ApJ

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We discover four high proper motion L dwarfs by comparing the Wide-field Infrared Survey Explorer (WISE) to the Two Micron All Sky Survey. WISE J140533.32+835030.5 is an L dwarf at the L/T transition with a proper motion of 0.85 ± 0. 02 yr −1 , previously overlooked due to its proximity to a bright star (V ≈ 12 mag). From optical spectroscopy we find a spectral type of L8, and from moderate-resolution J band spectroscopy we find a near-infrared spectral type of L9. We find WISE J140533.32+835030.5 to have a distance of 9.7 ± 1.7 pc, bringing the number of L dwarfs at the L/T transition within 10 pc from six to seven. WISE J040137.21+284951.7, WISE J040418.01+412735.6, and WISE J062442.37+662625.6 are all early L dwarfs within 25 pc, and were classified using optical and low-resolution near-infrared spectra. WISE J040418.01+412735.6 is an L2 pec (red) dwarf, a member of the class of unusually red L dwarfs. We use follow-up optical and low-resolution near-infrared spectroscopy to classify a previously discovered fifth object WISEP J060738.65+242953.4 as an (L8 Opt/L9 NIR), confirming it as an L dwarf at the L/T transition within 10 pc. WISEP J060738.65+242953.4 shows tentative CH 4 in the H band, possibly the result of unresolved binarity with an early T dwarf, a scenario not supported by binary spectral template fitting. If WISEP J060738.65+242953.4 is a single object, it represents the earliest onset of CH 4 in the H band of an L/T transition dwarf in the SpeX Library. As very late L dwarfs within 10 pc, WISE J140533.32+835030.5 and WISEP J060738.65+242953.4 will play a vital role in resolving outstanding issues at the L/T transition.

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Meeting the Cool Neighbors. X. Ultracool Dwarfs From the 2mass All-Sky Data Release

Cited by 208 publications

References 107 publications

Understanding Fundamental Properties and Atmospheric Features of Subdwarfs via a Case Study of SDSS J125637.13–022452.4^∗

Understanding Fundamental Properties and Atmospheric Features of Subdwarfs via a Case Study of SDSS J125637.13–022452.4^∗

A Reanalysis of the Fundamental Parameters and Age of TRAPPIST-1*

DISCOVERY OF FOUR HIGH PROPER MOTION L DWARFS, INCLUDING A 10 pc L DWARF AT THE L/T TRANSITION^,

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Meeting the Cool Neighbors. X. Ultracool Dwarfs From the 2mass All-Sky Data Release

Cited by 208 publications

References 107 publications

Understanding Fundamental Properties and Atmospheric Features of Subdwarfs via a Case Study of SDSS J125637.13–022452.4∗

Understanding Fundamental Properties and Atmospheric Features of Subdwarfs via a Case Study of SDSS J125637.13–022452.4∗

A Reanalysis of the Fundamental Parameters and Age of TRAPPIST-1*

DISCOVERY OF FOUR HIGH PROPER MOTION L DWARFS, INCLUDING A 10 pc L DWARF AT THE L/T TRANSITION,

Contact Info

Product

Resources

About

Understanding Fundamental Properties and Atmospheric Features of Subdwarfs via a Case Study of SDSS J125637.13–022452.4^∗

Understanding Fundamental Properties and Atmospheric Features of Subdwarfs via a Case Study of SDSS J125637.13–022452.4^∗

DISCOVERY OF FOUR HIGH PROPER MOTION L DWARFS, INCLUDING A 10 pc L DWARF AT THE L/T TRANSITION^,