The age of the carina young association and potential membership of HD 95086

Booth, Mark; Burgo, C. del; Hambaryan, V.

doi:10.1093/mnras/staa3631

Cited by 28 publications

(22 citation statements)

References 72 publications

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“…Thus, our empirical approach to estimate the kinematic age of an expanding (as a whole) stellar system by the analysis of the distribution of mutual distances of bona-fide member stars in the past (see, e.g. Booth et al 2021), does not show a global minimum, suggesting also on a possible non-coeval star formation in this extended Cep OB1 association as a complex star forming region unlike to a compact ones (see, e.g., Shevchenko et al 1991). Thus, the estimated ages of Cep OB1 and 4U 2206+54 already are excluding HD 235673 as a birth counterpart owing to the longer flight time (τ = 13.2 +2.0 −0.8 Myr, Sec.…”

Section: Discussionmentioning

confidence: 99%

The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790

Hambaryan,

Stoyanov,

Mugrauer

et al. 2022

Preprint

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Based on the Gaia EDR3 astrometric parameters and our new systemic radial velocity of the high-mass X-ray binary 4U 2206+54/BD+53 2790, we studied the trace back motion of the system and propose that it originated in the subgroup of the Cepheus OB1 association (Age∼4-10 Myr) with its brightest star BD+53 2820 (B0V; L∼10 4.7 L ). The kinematic age of 4U 2206+54 is about 2.8 ± 0.4 Myr, it is at a distance of 3.1-3.3 kpc and has a space velocity of 75-100 km/s with respect to this member star (BD+53 2820 ) of the Cep OB1 association. This runaway velocity indicates that the progenitor of the neutron star hosted by 4U 2206+54 lost about 4-9 M during the supernova explosion and the latter one received a kick velocity of at least 200-350 km/s . Since the high-mass X-ray binary 4U 2206+54/BD+53 2790 was born as a member of a subgroup of Cep OB1, the initially most massive star in the system terminated its evolution within < ∼ 7 − 9 Myr, corresponding to an initial mass > ∼ 32 M .

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Section: Discussionmentioning

confidence: 99%

The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790

Hambaryan,

Stoyanov,

Mugrauer

et al. 2022

Preprint

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“…Only four 4 known directly imaged planets have nominal masses comparable to or lower than 2M0437b ( 5M JUP ), and all are older: PDS 70 b and c, which orbit a 5 Myr-old star in the Scorpius-Centaurus region (Keppler et al 2018;Haffert et al 2019), 51 Eri b, which orbits a member of the ∼23 Myr-old Beta Pictoris Moving Group (Macintosh et al 2015) and HD 95086b (Rameau et al 2013), with a host star that has been recently re-assigned to the ∼13 Myr-old Carina association (Booth et al 2021). Notably, all the host stars are much more massive than 2M0437.…”

Section: Discussion and Summarymentioning

confidence: 99%

Zodiacal Exoplanets in Time (ZEIT) XII: A Directly-Imaged Planetary-Mass Companion to a Young Taurus M Dwarf Star

Gaidos,

Hirano,

Kraus

et al. 2021

Preprint

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We report the discovery of a resolved (0 .9) substellar companion to a member of the 1-5 Myr Taurus star-forming region. The host star (2M0437) is a single mid-M type (𝑇 eff ≈3100 K) dwarf with a position, space motion, and color-magnitude that support Taurus membership, and possible affiliation with a ∼2.5 Myr-old sub-group. A comparison with stellar models suggests a 2-5 Myr age and a mass of 0.15-0.18M . Although K2 detected quasi-periodic dimming from close-in circumstellar dust, the star lacks detectable excess infrared emission from a circumstellar disk and its H𝛼 emission is not commensurate with accretion. Astrometry based on three years of AO imaging shows that the companion (2M0437b) is co-moving, while photometry of two other sources at larger separation indicates they are likely heavilyreddened background stars. A comparison of the luminosity of 2M0437b with models suggests a mass of 3-5 M JUP , well below the deuterium burning limit, and an effective temperature of 1400-1500 K, characteristic of a late L spectral type. The 𝐻-𝐾 color is redder than the typical L dwarf, but comparable to other directly detected young planets, e.g. those around HR 8799. The discovery of a super-Jupiter around a very young, very low mass star challenges models of planet formation by either core accretion (which requires time) or disk instability (which requires mass). We also detected a second, co-moving, widely-separated (75 ) object that appears to be a heavily-extincted star. This is certainly a fellow member of this Taurus sub-group and statistically likely to be a bound companion.

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“…Torres et al (2008) later re-assessed AB Pic to be a member of Carina, another young moving group (YMG) with age τ ∼ 30 Myr (e.g., Bell et al 2015;Miret-Roig et al 2018). Recently, Booth et al (2021) has revised the age of Carina to be younger and only 13 Myr. Chauvin et al (2005) observed AB Pic to host a planetary-mass companion, AB Pic b, at projected separation 5.…”

Section: Ab Picmentioning

confidence: 99%

A Mid-Infrared Study of Directly-Imaged Planetary-Mass Companions using Archival Spitzer/IRAC Images

Martinez,

Kraus

2021

Preprint

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The atmospheres and accretion disks of planetary-mass and substellar companions provide an unprecedented look into planet and moon formation processes, most notably the frequency and lifetime of circumplanetary disks. In our ongoing effort to leverage the extraordinary sensitivity of the Spitzer /Infrared Array Camera (IRAC) at 3.6, 4.5, 5.8, and 8.0 µm to study wide planetary-mass and substellar companions near the diffraction limit, we present point-spread function (PSF) fitting photometry of archival Spitzer /IRAC images for nine stars (G0 to M4+M7) in nearby star-forming regions or stellar associations that host companions at separations of ρ = 1. 17 − 12. 33. We detect all system primaries in all four IRAC channels and recover eight low-mass companions in at least one IRAC channel for our sample, five of which have not been resolved previously in IRAC images. We measure non-photospheric [3.6] − [8.0] colors for four of the system companions (DH Tau B, 2M0441 B, SR 12 c, ROXs 42B b), confirming or discovering the presence of circumstellar or circum(sub)stellar disks. We detect fluxes consistent with photospheric emission for four other companions (AB Pic b, CHXR 73 b, 1RXS J1609 b, HD 203030 b) that are unlikely to host disks. Combined with past detections of accretion or disk indicators, we determine the global disk frequency of young (<15 Myr) wide companions with masses near the deuterium-burning limit to be 56% ± 12%.

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The age of the carina young association and potential membership of HD 95086

Cited by 28 publications

References 72 publications

The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790

The origin of the high-mass X-ray binary 4U 2206+54/BD +53 2790

Zodiacal Exoplanets in Time (ZEIT) XII: A Directly-Imaged Planetary-Mass Companion to a Young Taurus M Dwarf Star

A Mid-Infrared Study of Directly-Imaged Planetary-Mass Companions using Archival Spitzer/IRAC Images

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