Discovery of the benchmark metal-poor T8 dwarf BD +01° 2920B

Pinfield, D. J.; Burningham, B.; Lodieu, N.; Leggett, S. K.; Tinney, C. G.; Spaandonk, L. van; Marocco, F.; Smart, R. L.; Gomes, Jorge; Smith, Leigh C.; Lucas, P. W.; Day-Jones, A. C.; Murray, D. N.; Katsiyannis, A. C.; Catalán, S.; Cardoso, C.; Clarke, J. R. A.; Folkes, S. L.; Galvez-Ortiz, M. C.; Homeier, D.; Jenkins, James S.; Jones, H. R. A.; Zhang, ZH

doi:10.1111/j.1365-2966.2012.20549.x

Cited by 64 publications

(73 citation statements)

References 115 publications

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“…9 of Pavlenko et al (2015). Objects with T eff > 3500 K (yellow, red, blue and black crosses are for dM, sdM, esdM, and usdM, respectively) are from Woolf & Wallerstein (2006) and Woolf, Lépine, & Wallerstein (2009 Pinfield et al 2012). The remaining T eff < 3000 K objects are provided in Table 7.…”

Section: Metallicity Ranges Of the Subclasses Of M And L Subdwarfsmentioning

confidence: 99%

Primeval very low-mass stars and brown dwarfs – I. Six new L subdwarfs, classification and atmospheric properties

Zhang

Pinfield

Galvez-Ortiz

et al. 2016

Mon. Not. R. Astron. Soc.

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We have conducted a search for L subdwarf candidates within the photometric catalogues of the UKIRT Infrared Deep Sky Survey and Sloan Digital Sky Survey. Six of our candidates are confirmed as L subdwarfs spectroscopically at optical and/or nearinfrared wavelengths. We also present new optical spectra of three previously known L subdwarfs (WISEA J001450.17-083823.4, 2MASS J00412179+3547133 and ULAS J124425.75+102439.3). We examined the spectral type and metallicity classification of subclasses of known L subdwarfs. We summarized the spectroscopic properties of L subdwarfs with different spectral types and subclasses. We classify these new L subdwarfs by comparing their spectra to known L subdwarfs and L dwarf standards. We estimate temperatures and metallicities of 22 late-type M and L subdwarfs by comparing their spectra to BT-Settl models. We find that L subdwarfs have temperatures between 1500 and 2700 K, which are higher than similar-typed L dwarfs by around 100-400 K depending on different subclasses and subtypes. We constrained the metallicity ranges of subclasses of M, L, and T subdwarfs. We also discussed the spectral-type and absolute magnitude relationships for L and T subdwarfs.

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Section: Metallicity Ranges Of the Subclasses Of M And L Subdwarfsmentioning

confidence: 99%

Primeval very low-mass stars and brown dwarfs – I. Six new L subdwarfs, classification and atmospheric properties

Zhang

Pinfield

Galvez-Ortiz

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The top panels of the figure show the T0, T2, T4, T6, and T8 spectral standards of Burgasser et al (2006a) 7 and the Y0 standard (WISEP J173835.52+273258.9) defined by Cushing et al (2011). The middle row compares our observed spectra to the T5.5 dwarf 2MASS J23565477−1553111 8 (Burgasser et al 2002(Burgasser et al , 2006a and the peculiar T8 dwarf WISE J142320.84+011638.0 (BD +01 • 2920B; Pinfield et al 2012;Mace et al 2013). The 2MASS 2356−1553 spectra were published by McLean et al (2003) and represent the mid-type T dwarf classification that some of our photometry imply.…”

Section: Comparing Wise 2005+5424 To Observed and Synthetic Spectramentioning

confidence: 99%

“…WISE 1423+0116 is the closest object of similar type to WISE 2005+5424 in the literature and the Magellan/FIRE spectrum from Mace et al (2013) is used here for comparison. Discovered by Pinfield et al (2012), WISE 1423+0116 is a companion to a G1 dwarf at ∼17.2 pc, which provides an inferred [Fe/H] = −0.36 ± 0.06 dex. Based on comparison to the model isochrones of Baraffe et al (2003) they estimate T eff = 680 ± 55 K and log(g) = 5.0 ± 0.3 dex for WISE 1423+0116.…”

Section: Comparing Wise 2005+5424 To Observed and Synthetic Spectramentioning

confidence: 99%

“…These include the young T8.5 dwarf Ross 458C (J − H = −0.36 ± 0.03; Goldman et al 2010;Burningham et al 2011) and the old T8 dwarf WISE J142320.84+011638.0 (J − H = −0.41 ± 0.08; Mace et al 2013;Pinfield et al 2012) that we use for spectral comparison in Section 4.2. The addition of WISE 2005+5424, which has an inferred metallically of [Fe/H] = −0.64 ± 0.17, to the group of red J − H outliers makes a compelling argument that this group at least partially represents the low-metallically T dwarf population.…”

Section: Identifying T Dwarfs With Color Indices Similar To Wise 2005mentioning

confidence: 99%

“…Constraining physical properties like mass, age, and metallicity for isolated field brown dwarfs discovered by such surveys inevitably requires comparison to models. These models are improved by employing wide-separation T dwarf companions to well studied stars as benchmarks for our analysis of the larger solivagant population (Burgasser et al 2000Wilson et al 2001;Scholz et al 2003;McCaughrean et al 2004;Mugrauer et al 2006;Liu et al 2007;Luhman et al 2007;Pinfield et al 2006Pinfield et al , 2008Pinfield et al , 2012Burningham et al 2009Burningham et al , 2013Goldman et al 2010;Albert et al 2011;Day-Jones et al 2011;Luhman et al 2011;Murray et al 2011;Deacon et al 2012aDeacon et al , 2012bDupuy & Liu 2012;Wright et al 2013). WISE J200520.38+542433.9 (WISE 2005+5424 hereafter) is a faint (J ∼ 19.6 mag), late-type T dwarf located 188.…”

Section: Introductionmentioning

confidence: 99%

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The Exemplar T8 Subdwarf Companion of Wolf 1130

Mace

Kirkpatrick

Cushing

et al. 2013

ApJ

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We have discovered a wide separation (188. 5) T8 subdwarf companion to the sdM1.5+WD binary Wolf 1130. Companionship of WISE J200520.38+542433.9 is verified through common proper motion over a ∼3 yr baseline. Wolf 1130 is located 15.83 ± 0.96 pc from the Sun, placing the brown dwarf at a projected separation of ∼3000 AU. Near-infrared colors and medium resolution (R ≈ 2000-4000) spectroscopy establish the uniqueness of this system as a high-gravity, low-metallicity benchmark. Although there are a number of low-metallicity T dwarfs in the literature, WISE J200520.38+542433.9 has the most extreme inferred metallicity to date with [Fe/H] = −0.64 ± 0.17 based on Wolf 1130. Model comparisons to this exemplar late-type subdwarf support it having an old age, a low metallicity, and a small radius. However, the spectroscopic peculiarities of WISE J200520.38+542433.9 underscore the importance of developing the low-metallicity parameter space of the most current atmospheric models.

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The kinematics of very low mass dwarfs: Splinter session summary

et al. 2013

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Kinematic investigations are being increasingly deployed in studies of the lowest mass stars and brown dwarfs to investigate their origins, characterize their atmospheres, and examine the evolution of their physical parameters. This article summarizes the contributions made at the "Kinematics of Very Low Mass Dwarfs" splinter session. Results discussed include analysis of kinematic distributions of M, L, and T dwarfs; theoretical tools for interpreting these distributions; identifications of very low mass halo dwarfs and wide companions to nearby stars; radial velocity variability among young and very cool brown dwarfs; and the search and identification of M dwarfs in young moving groups. A summary of discussion points at the conclusion of the splinter sesseion is also presented.

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Discovery of the benchmark metal-poor T8 dwarf BD +01° 2920B

Cited by 64 publications

References 115 publications

Primeval very low-mass stars and brown dwarfs – I. Six new L subdwarfs, classification and atmospheric properties

Primeval very low-mass stars and brown dwarfs – I. Six new L subdwarfs, classification and atmospheric properties

The Exemplar T8 Subdwarf Companion of Wolf 1130

The kinematics of very low mass dwarfs: Splinter session summary

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