Wisea J114724.10-204021.3: A Free-Floating Planetary Mass Member of the Tw Hya Association

Schneider, Adam C.; Windsor, James; Cushing, Michael C.; Kirkpatrick, J. Davy; Wright, E. L.

doi:10.3847/2041-8205/822/1/l1

Cited by 72 publications

(66 citation statements)

References 48 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…BASS-UC 56 (2MASS J11472421-2040204) has been independently discovered by Schneider et al (2016a) as a young L7 candidate member of TWA. The similarities between this object and 2MASS J11193254-1137466 are remarkable, with their similar spectral types, distances (31-33 pc) and estimated masses (6-13 M Jup ).…”

Section: Bass-ultracoolmentioning

confidence: 99%

“…2MASS J11193254-1137466 (Kellogg et al 2015J11193254-1137466 (Kellogg et al , 2016 and 2MASS J11472421-2040204 (Schneider et al 2016a) are both candidate members of TWA with spectral types L7 that display signs of youth, and with estimated masses as low as 5-7 M Jup . Their close distances to the Sun (29-33 pc) place them at the nearer side of the TWA spatial distribution.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

Gagné

Faherty

Mamajek

et al. 2017

ApJS

103

106

View full text Add to dashboard Cite

A determination of the initial mass function (IMF) of the current, incomplete census of the 10 Myrold TW Hya association (TWA) is presented. This census is built from a literature compilation supplemented with new spectra and 17 new radial velocities from on-going membership surveys, as well as a re-analysis of Hipparcos data that confirmed HR 4334 (A2 Vn) as a member. Though the dominant uncertainty in the IMF remains census incompleteness, a detailed statistical treatment is carried out to make the IMF determination independent of binning, while accounting for small number statistics. The currently known high-likelihood members are fitted by a log-normal distribution with a central mass of 0.21−0.06 M and a characteristic width of 0.8 +0.2 −0.1 dex in the 12 M Jup -2 M range, whereas a Salpeter power law with α = 2.2 +1.1 −0.5 best describes the IMF slope in the 0.1-2 M range. This characteristic width is higher than other young associations, which may be due to incompleteness in the current census of low-mass TWA stars. A tentative overpopulation of isolated planetary-mass members similar to 2MASS J11472421-2040204 and 2MASS J11193254-1137466 is identified: this indicates that there might be as many as 10 +13 −5 similar members of TWA with hot-start modeldependent masses estimated at ∼ 5-7 M Jup , most of which would be too faint to be detected in 2MASS . Our new radial velocity measurements corroborate the membership of 2MASS J11472421-2040204, and secure TWA 28 (M8.5 γ), TWA 29 (M9.5 γ) and TWA 33 (M4.5 e) as members. The discovery of 2MASS J09553336-0208403, a young L7-type interloper unrelated to TWA, is also presented.

show abstract

Section: Bass-ultracoolmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

Gagné

Faherty

Mamajek

et al. 2017

ApJS

103

106

View full text Add to dashboard Cite

show abstract

“…Some of these objects include the young companions HD 203030B (L7.5, 130-400 Myr; Metchev & Hillenbrand 2006), HN PegB (T2.5, 100-500 Myr; Luhman et al 2007), LP 261-75B (L6, 100-200 Myr;Reid & Walkowicz 2006), GU Psc b (T3.5, 70-130 Myr;Naud et al 2014), or VHS J1256-12 (L7, 150-300 Myr; Gauza et al 2015), or the very low-mass brown dwarfs PSO J318.5-22 (L7, 23 ± 3 Myr; Liu et al 2013;Allers et al 2016), 2MASS J1119-11AB (L7, 10±3 Myr; Kellogg et al 2016;Best et al 2017) or WISEA J1147-20 (L7, 10±3 Myr; Schneider et al 2016).…”

mentioning

confidence: 99%

The Prototypical Young L/T-Transition Dwarf HD 203030B Likely Has Planetary Mass

Miles-Páez¹,

Metchev²,

Luhman³

et al. 2017

View full text Add to dashboard Cite

Upon its discovery in 2006, the young L7.5 companion to the solar analog HD 203030 was found to be unusual in being ≈200 K cooler than older late-L dwarfs. HD 203030B offered the first clear indication that the effective temperature at the L-to-T spectral type transition depends on surface gravity: now a well-known characteristic of low-gravity ultra-cool dwarfs. An initial age analysis of the G8V primary star indicated that the system was 130-400 Myr old, and so the companion between 12-31 M Jup . Using moderate resolution near-infrared spectra of HD 203030B, we now find features of very low gravity comparable to those of 10-150 Myr-old L7-L8 dwarfs. We also obtained more accurate near infrared and Spitzer/IRAC photometry, and find a (J − K) MKO color of 2.56 ± 0.13 mag-comparable to those observed in other young planetary-mass objects-and a luminosity of log(L bol /L ) = −4.75 ± 0.04 dex. We further reassess the evidence for the young age of the host star, HD 203030, with a more comprehensive analysis of the photometry and updated stellar activity measurements and age calibrations. Summarizing the age diagnostics for both components of the binary, we adopt an age of 100 Myr for HD 203030B and an age range of 30-150 Myr. Using cloudy evolutionary models, the new companion age range and luminosity result in a mass of 11 M Jup with a range of 8-15 M Jup , and an effective temperature of 1040 ± 50 K.

show abstract

“…For each spectral subtype, the field sequence has a color dispersion of typically ±0.15-0.25 mag. The 2016), and members of the TW Hydrae (TWA) moving group compiled by Chauvin et al (2004Chauvin et al ( , 2005a, Gagné et al (2015a), Kellogg et al (2015Kellogg et al ( , 2016, and Schneider et al (2016a) also have colors resembling the indices of the σ Orionis L0-L4.5 objects of this paper. Figure 11 shows the location of the σ Orionis, Upper Scorpius and TWA sequences using different symbols.…”

Section: Photometric Colorsmentioning

confidence: 98%

Optical and Near-infrared Spectra of σ Orionis Isolated Planetary-mass Objects

Osorio

Béjar

Ramírez

2017

ApJ

View full text Add to dashboard Cite

We have obtained low-resolution optical (0.7-0.98 µm) and near-infrared (1.11-1.34 µm and 0.8-2.5 µm) spectra of twelve isolated planetary-mass candidates (J = 18.2-19.9 mag) of the 3-Myr σ Orionis star cluster with a view to determining the spectroscopic properties of very young, substellar dwarfs and assembling a complete cluster mass function. We have classified our targets by visual comparison with high-and low-gravity standards and by measuring newly defined spectroscopic indices. We derived L0-L4.5 and M9-L2.5 using high-and low-gravity standards, respectively. Our targets reveal clear signposts of youth, thus corroborating their cluster membership and planetary masses (6-13 M Jup ). These observations complete the σ Orionis mass function by spectroscopically confirming the planetary-mass domain to a confidence level of ∼75 percent. The comparison of our spectra with BT-Settl solar metallicity model atmospheres yields a temperature scale of 2350-1800 K and a low surface gravity of log g ≈ 4.0 [cm s−2 ], as would be expected for young planetary-mass objects. We discuss the properties of the cluster least-massive population as a function of spectral type. We have also obtained the first optical spectrum of S Ori 70, a T dwarf in the direction of σ Orionis. Our data provide reference optical and near-infrared spectra of very young L dwarfs and a mass function that may be used as templates for future studies of low-mass substellar objects and exoplanets. The extrapolation of the σ Orionis mass function to the solar neighborhood may indicate that isolated planetarymass objects with temperatures of ∼200-300 K and masses in the interval 6-13-M Jup may be as numerous as very low-mass stars.

show abstract

Wisea J114724.10-204021.3: A Free-Floating Planetary Mass Member of the Tw Hya Association

Cited by 72 publications

References 48 publications

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

BANYAN. IX. The Initial Mass Function and Planetary-mass Object Space Density of the TW HYA Association

The Prototypical Young L/T-Transition Dwarf HD 203030B Likely Has Planetary Mass

Optical and Near-infrared Spectra of σ Orionis Isolated Planetary-mass Objects

Contact Info

Product

Resources

About