NEAR-INFRARED SPECTROSCOPY OF 2M0441+2301 AabBab: A QUADRUPLE SYSTEM SPANNING THE STELLAR TO PLANETARY MASS REGIMES

Bowler, Brendan P.; Hillenbrand, Lynne A.

doi:10.1088/2041-8205/811/2/l30

Cited by 29 publications

(22 citation statements)

References 52 publications

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“…We find that most of the Herczeg & Hillenbrand (2008), (53) Nesterov et al (1995), (54) Martín (2000), (55) Bowler & Hillenbrand (2015), (56) Briceño et al (1999), (57) Hartigan et al (1995), (58) Cohen & Kuhi (1979), (59) Boss (1937), (60) Steffen et al (2001), (61) Malfait et al (1998), (62) Briceño et al (1993). c J−H and J−K=derived from these colors assuming photospheric near-IR colors; CTTS=derived from J−H and H−K assuming intrinsic colors of classical T Tauri stars from Meyer et al (1997), opt spec=derived from an optical spectrum; SpeX=derived from a SpeX spectrum; (1)=Briceño et al (This table is available in its entirety in machine-readable form.)…”

Section: Census From Previous Studiessupporting

confidence: 48%

A Survey for New Members of the Taurus Star-Forming Region With the Sloan Digital Sky Survey*

et al. 2017

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Previous studies have found that ∼1deg2 fields surrounding the stellar aggregates in the Taurus star-forming region exhibit a surplus of solar-mass stars relative to denser clusters like IC348 and the Orion Nebula Cluster. To test whether this difference reflects mass segregation in Taurus or a variation in the initial mass function, we have performed a survey for members of Taurus across a large field (∼40 deg 2 ) that was imaged by the Sloan Digital Sky Survey (SDSS). We obtained optical and near-infrared spectra of candidate members identified with those images and the Two Micron All Sky Survey, as well as miscellaneous candidates that were selected with several other diagnostics of membership. We have classified 22 of the candidates as new members of Taurus, which includes one of the coolest known members (M9.75). Our updated census of members within the SDSS field shows a surplus of solar-mass stars relative to clusters, although it is less pronounced than in the smaller fields toward the stellar aggregates that were surveyed for previously measured mass functions in Taurus. In addition to spectra of our new members, we include in our study near-IR spectra of roughly half of the known members of Taurus, which are used to refine their spectral types and extinctions. We also present an updated set of near-IR standard spectra for classifying young stars and brown dwarfs at M and L types.

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Section: Census From Previous Studiessupporting

confidence: 48%

A Survey for New Members of the Taurus Star-Forming Region With the Sloan Digital Sky Survey*

et al. 2017

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“…Among planetary-mass companions at all separations, few have hosts with such low masses as 2MASSJ0249−0557AB, even using its combined mass (50-150 M Jup at 2σ). The two clearest examples are 2MASSJ1207−3932b (5±2 M Jup ), which orbits a 25 M Jup TWA member (Chauvin et al 2004), and 2MASSJ0441+2301Bb (10±2 M Jup ), which orbits the 19±3 M Jup tertiary component of a quadruple system in Taurus (Todorov et al 2010;Kraus et al 2011;Bowler & Hillenbrand 2015). 20 The slightly higher-mass companions FUTauB (≈16 M Jup ; Luhman et al 2009) and 2MASSJ0219 −3925B (14±1 M Jup ; Artigau et al 2015) orbit a 50 M Jup brown dwarf in Taurus and a 110 M Jup star in Tuc-Hor, respectively.…”

Section: An Unusual System Architecturementioning

confidence: 99%

The Hawaii Infrared Parallax Program. III. 2MASS J0249–0557 c: A Wide Planetary-mass Companion to a Low-mass Binary in the β Pic Moving Group* ^†

Dupuy

Liu

Allers

et al. 2018

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We have discovered a wide planetary-mass companion to the βPic moving group member 2MASSJ02495639 −0557352 (M6 VL-G) using Canada-France-Hawaii Telescope/WIRCam astrometry from the Hawaii Infrared Parallax Program. In addition, Keck laser guide star adaptive optics aperture-masking interferometry shows that the host is itself a tight binary. Altogether, 2MASSJ0249−0557ABc is a bound triple system with an 11.6 1.0 1.3-+ M Jup object separated by 1950±200 au (40″) from a relatively close (2.17±0.22 au, 0 04) pair of 48 12 13-+ M Jup and 44 11 14-+ M Jup objects. 2MASSJ0249−0557AB is one of the few ultracool binaries to be discovered in a young moving group and the first confirmed in the βPic moving group (22±6 Myr). The mass, absolute magnitudes, and spectral type of 2MASSJ0249−0557c (L2 VL-G) are remarkably similar to those of the planet βPicb (L2, 13.0 0.3 0.4-+ M Jup). We also find that the free-floating object 2MASSJ2208+2921 (L3 VL-G) is another possible βPic moving group member with colors and absolute magnitudes similar to βPicb and 2MASSJ0249−0557c. βPicb is the first directly imaged planet to have a "twin," namely an object of comparable properties in the same stellar association. Such directly imaged objects provide a unique opportunity to measure atmospheric composition, variability, and rotation across different pathways of assembling planetary-mass objects from the same natal material.

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“…Adaptive-optics-fed integral-field spectrographs (IFS) operating at medium spectral resolving power (R λ = 2000−5000) in the near-infrared such as SINFONI at the VLT, NIFS at Gemini-North, or OSIRIS at the Keck Observatory offer to partly deblend the rich set of molecular absorption that is contained in the exoplanet spectra. They have been used to gather the spectra of young low-mass companions at large distance from their host stars (>1") or in systems with moderate contrasts in the near-infrared (McElwain et al 2007;Seifahrt et al 2007;Schmidt et al 2008Schmidt et al , 2014Lavigne et al 2009;Bowler et al 2011Bowler et al , 2017Bonnefoy et al 2014;Bowler & Hillenbrand 2015;Daemgen et al 2017). More recently, high-contrast imaging techniques such as the angular differential imaging (e.g.…”

Section: Introductionmentioning

confidence: 99%

Medium-resolution spectrum of the exoplanet HIP 65426 b

Petrus

Bonnefoy

Chauvin

et al. 2021

A&A

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Medium-resolution integral-field spectrographs (IFS) coupled with adaptive-optics such as Keck/OSIRIS, VLT/MUSE, or SINFONI are appearing as a new avenue for enhancing the detection and characterization capabilities of young, gas giant exoplanets at large heliocentric distances (>5 au). We analyzed K-band VLT/SINFONI medium-resolution (Rλ ~5577) observations of the young giant exoplanet HIP 65426 b. Our dedicated IFS data analysis toolkit (TExTRIS) optimized the cube building, star registration, and allowed for the extraction of the planet spectrum. A Bayesian inference with the nested sampling algorithm coupled with the self-consistent forward atmospheric models BT-SETTL15 and Exo-REM using the ForMoSA tool yields Teff = 1560 ± 100 K, log(g) ≤ 4.40 dex, [M/H] = 0.05−0.22+0.24 dex, and an upper limit on the C/O (≤0.55). The object is also re-detected with the so-called “molecular mapping” technique. The technique yields consistent atmospheric parameters, but the loss of the planet pseudo-continuum in the process degrades or modifies the constraints on these parameters. The solar to sub-solar C/O ratio suggests an enrichment by solids at formation if the planet was formed beyond the water snowline (≥20 au) by core accretion (CA hereafter). However, a formation by gravitational instability (GI hereafter) cannot be ruled out. The metallicity is compatible with the bulk enrichment of massive Jovian planets from the Bern planet population models. Finally, we measure a radial velocity of 26 ± 15 km s−1 compatible with our revised measurement on the star. This is the fourth imaged exoplanet for which a radial velocity can be evaluated, illustrating the potential of such observations for assessing the coevolution of imaged systems belonging to star forming regions, such as HIP 65426.

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NEAR-INFRARED SPECTROSCOPY OF 2M0441+2301 AabBab: A QUADRUPLE SYSTEM SPANNING THE STELLAR TO PLANETARY MASS REGIMES

Cited by 29 publications

References 52 publications

A Survey for New Members of the Taurus Star-Forming Region With the Sloan Digital Sky Survey*

A Survey for New Members of the Taurus Star-Forming Region With the Sloan Digital Sky Survey*

The Hawaii Infrared Parallax Program. III. 2MASS J0249–0557 c: A Wide Planetary-mass Companion to a Low-mass Binary in the β Pic Moving Group* ^†

Medium-resolution spectrum of the exoplanet HIP 65426 b

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NEAR-INFRARED SPECTROSCOPY OF 2M0441+2301 AabBab: A QUADRUPLE SYSTEM SPANNING THE STELLAR TO PLANETARY MASS REGIMES

Cited by 29 publications

References 52 publications

A Survey for New Members of the Taurus Star-Forming Region With the Sloan Digital Sky Survey*

A Survey for New Members of the Taurus Star-Forming Region With the Sloan Digital Sky Survey*

The Hawaii Infrared Parallax Program. III. 2MASS J0249–0557 c: A Wide Planetary-mass Companion to a Low-mass Binary in the β Pic Moving Group* †

Medium-resolution spectrum of the exoplanet HIP 65426 b

Contact Info

Product

Resources

About

The Hawaii Infrared Parallax Program. III. 2MASS J0249–0557 c: A Wide Planetary-mass Companion to a Low-mass Binary in the β Pic Moving Group* ^†