A Proper Motion Survey Using the First Sky Pass of Neowise-Reactivation Data

Schneider, Adam C.; Greco, Jennifer J.; Cushing, Michael C.; Kirkpatrick, J. Davy; Mainzer, Amy; Gelino, Christopher R.; Fajardo-Acosta, S. B.; Bauer, J. M.

doi:10.3847/0004-637x/817/2/112

Cited by 59 publications

(76 citation statements)

References 62 publications

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“…12. of Schneider et al (2016) compare well with LSR1826, and we thus classify them as sdL0. Table 4 shows a list of currently known L subdwarfs with updated spectral types.…”

Section: Subclass Spectral Characterizticsmentioning

confidence: 95%

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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“…12. of Schneider et al (2016) compare well with LSR1826, and we thus classify them as sdL0. Table 4 shows a list of currently known L subdwarfs with updated spectral types.…”

Section: Subclass Spectral Characterizticsmentioning

confidence: 95%

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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“…Additionally, their astrometric precision reaches 0.5 /h, whereas candidate Planet 9 instead has a movement of around 0.3 /h . A search in the IR domain was performed by Luhman (2014), who inspected the WISE data for a distant companion to the Sun (see also Schneider et al 2016). The WISE satellite mapped the whole sky twice and started mapping it a third time.…”

Section: Discussionmentioning

confidence: 99%

Evolution and magnitudes of candidate Planet Nine

Linder

Mordasini

2016

A&A

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Context. The recently renewed interest in a possible additional major body in the outer solar system prompted us to study the thermodynamic evolution of such an object. We assumed that it is a smaller version of Uranus and Neptune. Aims. We modeled the temporal evolution of the radius, temperature, intrinsic luminosity, and the blackbody spectrum of distant ice giant planets. The aim is also to provide estimates of the magnitudes in different bands to assess whether the object might be detectable. Methods. Simulations of the cooling and contraction were conducted for ice giants with masses of 5, 10, 20, and 50 M ⊕ that are located at 280, 700, and 1120 AU from the Sun. The core composition, the fraction of H/He, the efficiency of energy transport, and the initial luminosity were varied. The atmospheric opacity was set to 1, 50, and 100 times solar metallicity. Results. We find for a nominal 10 M ⊕ planet at 700 AU at the current age of the solar system an effective temperature of 47 K, much higher than the equilibrium temperature of about 10 K, a radius of 3.7 R ⊕ , and an intrinsic luminosity of 0.006 L . It has estimated apparent magnitudes of Johnson V, R, I, L, N, Q of 21.7, 21.4, 21.0, 20.1, 19.9, and 10.7, and WISE W1-W4 magnitudes of 20.1, 20.1, 18.6, and 10.2. The Q and W4 band and other observations longward of about 13 µm pick up the intrinsic flux. Conclusions. If candidate Planet 9 has a significant H/He layer and an efficient energy transport in the interior, then its luminosity is dominated by the intrinsic contribution, making it a self-luminous planet. At a likely position on its orbit near aphelion, we estimate for a mass of 5, 10, 20, and 50 M ⊕ a V magnitude from the reflected light of 24.3, 23.7, 23.3, and 22.6 and a Q magnitude from the intrinsic radiation of 14.6, 11.7, 9.2, and 5.8. The latter would probably have been detected by past surveys.

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“…We then scrutinized each candidate individually by creating and inspecting a finder chart for each source using available optical Digitized Sky Survey (DSS), nearinfrared (2MASS), and mid-infrared (AllWISE) images (see e.g., Schneider et al 2016a) to ensure each candidate is a point source (i.e., not extended or blended) and has noticeable proper motion.…”

Section: Identifying Young Late-type L Dwarfsmentioning

confidence: 99%

A 2MASS/AllWISE Search for Extremely Red L Dwarfs: The Discovery of Several Likely L Type Members of β Pic, AB Dor, Tuc-Hor, Argus, and the Hyades

Schneider

Windsor

Cushing

et al. 2017

Self Cite

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Young brown dwarfs share many properties with directly imaged giant extrasolar planets. They therefore provide unique laboratories for investigating the full range of temperature and mass encompasses by the growing collection of planets discovered outside our Solar System. Furthermore, if they can be tied to a particular group of coeval stars, they also provide vital anchor points for low-mass empirical isochrones. We have developed a novel procedure for identifying such objects based on their unique 2MASS and AllWISE colors. Using our search criteria, we have identified 50 new, late-type L dwarf candidates, 47 of which are spectroscopically confirmed as L dwarfs with follow-up near-infrared spectroscopy. We evaluate the potential membership of these objects in nearby, young moving groups using their proper motions, photometric distance estimates, and spectroscopic indicators of youth, and find seven likely L-type members belonging to the β Pictoris moving group, the AB Doradus moving group, the Tucana-Horologium association, or the Argus association, in addition to several lower probability members. Also found are two late-type (L5 and L6) potential members of the nearby Hyades cluster (WISEA J043642.75+190134.8 and WISEA J044105.56+213001.5).

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A Proper Motion Survey Using the First Sky Pass of Neowise-Reactivation Data

Cited by 59 publications

References 62 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

Evolution and magnitudes of candidate Planet Nine

A 2MASS/AllWISE Search for Extremely Red L Dwarfs: The Discovery of Several Likely L Type Members of β Pic, AB Dor, Tuc-Hor, Argus, and the Hyades

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