Examining the T Tauri system with SPHERE

Csépány, G.; Ancker, M. E. van den; Ábrahám, P.; Brandner, W.; Hormuth, F.

doi:10.1051/0004-6361/201526201

Cited by 18 publications

(31 citation statements)

References 20 publications

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“…The morphology of R2 changes significantly in K-band where we can no longer detect the south-pointing line, but see a small structure of extended emission already reported by Csépány et al (2015). After a small gap of ∼150 mas without a detection of significant emission, R2 appears to pass into the more prominent structure R3 roughly half an arcsecond south of T Tauri S, which curves away toward the west, and R3 appears near the location of the H 2 feature 3 reported by Gustafsson et al (2010).…”

Section: Continuum Imagingsupporting

confidence: 51%

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New circumstellar structure in the T Tauri system

Kasper

Santhakumari

Herbst

et al. 2016

A&A

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Aims. The immediate vicinity of T Tauri was observed with the new high-contrast imaging instrument SPHERE at the VLT to resolve remaining mysteries of the system, such as the putative small edge-on disk around T Tauri Sa and the assignment of the complex outflow patterns to the individual stars. Methods. We used SPHERE IRDIS narrow-band classical imaging in Paβ, Brγ, and the ν = 1−0 S(1) line of H 2 , as well as in the nearby continua to obtain high spatial resolution and high-contrast images over the near-infrared spectral range. Line maps were created by subtracting the nearby continuum. We also reanalyzed coronagraphic data taken with SPHERE's integral field spectrograph in J-and H-band with the goal of obtaining a precise extinction estimate to T Tauri Sb, and of verifying the recently reported claim of another stellar or substellar object in the system. Results. A previously unknown coiling structure is observed southwest of the stars in reflected light, which points to the vicinity of T Tauri N. We map the circumbinary emission from T Tauri S in J-and H-band scattered light for the first time, showing a morphology that differs significantly from that observed in K-band. Molecular Hydrogen emission is found southwest of the stars, near the coiling structure. We also detect the H 2 emitting region T Tauri NW. The motion of T Tauri NW with respect to T Tauri N and S between previous images and our 2014 data provides strong evidence that the southeast-northwest outflow triggering T Tauri NW is likely to be associated with T Tauri S. We also present accurate relative photometry of the stars, which confirms that T Tauri Sa is brightening again. Our analysis rules out the presence of the recently proposed companion to T Tauri N with high confidence.

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Section: Continuum Imagingsupporting

confidence: 51%

“…The shortest wavelength at which we can still see emission from T Tauri Sa itself is at 1.425 µm. Csépány et al (2015) have reported a tentative companion candidate (CC) to T Tauri N at separation 144 mas and position angle 198…”

Section: Continuum Imagingmentioning

confidence: 99%

New circumstellar structure in the T Tauri system

Kasper

Santhakumari

Herbst

et al. 2016

A&A

View full text Add to dashboard Cite

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“…For most of these observations, T Tau N was hidden behind a coronographic mask (Csépány et al 2015). Therefore, we did not measure its position, but only the relative positions of T Tau Sa and Sb.…”

Section: Spherementioning

confidence: 99%

“…The data was analyzed independently by a different team, who presented their results in Csépány et al (2015). In addition to the SPHERE data, we also recalibrated all the available NACO data to provide a more consistent astrometric reference frame.…”

Section: Introductionmentioning

confidence: 99%

Orbits in the T Tauri triple system observed with SPHERE

Köhler

Kasper

Herbst

et al. 2016

A&A

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Aims. We present new astrometric measurements of the components in the T Tauri system and derive new orbits and masses. Methods. T Tauri was observed during the science verification time of the new extreme adaptive optics facility SPHERE at the VLT. We combine the new positions with recalibrated NACO-measurements and data from the literature. Model fits for the orbits of T Tau Sa and Sb around each other and around T Tau N yield orbital elements and individual masses of the stars Sa and Sb. Results. Our new orbit for T Tau Sa/Sb is in good agreement with other recent results, which indicates that enough of the orbit has been observed for a reliable fit. The total mass of T Tau S is 2.65 ± 0.11 M . The mass ratio M Sb :M Sa is 0.25 ± 0.03, which yields individual masses of M Sa = 2.12 ± 0.10 M and M Sb = 0.53 ± 0.06 M . If our current knowledge of the orbital motions is used to compute the position of the southern radio source in the T Tauri system, then we find no evidence of the proposed dramatic change in its path.

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“…Csépány et al 2015, for the case of the T Tauri system). This can be alleviated by observing the same systems over a long period of time to obtain data that cover a significant fraction of the orbit.…”

Section: Introductionmentioning

confidence: 99%

Multi-epoch observations with high spatial resolution of multiple T Tauri systems

Csépány

Ancker

Ábrahám

et al. 2017

A&A

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Context. In multiple pre-main-sequence systems the lifetime of circumstellar disks appears to be shorter than around single stars, and the actual dissipation process may depend on the binary parameters of the systems. Aims. We report high spatial resolution observations of multiple T Tauri systems at optical and infrared wavelengths. We determine if the components are gravitationally bound and orbital motion is visible, derive orbital parameters and investigate possible correlations between the binary parameters and disk states. Methods. We selected 18 T Tau multiple systems (16 binary and two triple systems, yielding 16 + 2 × 2 = 20 binary pairs) in the Taurus-Auriga star forming region from the survey by Leinert et al. (1993), with spectral types from K1 to M5 and separations from 0.22 (31 AU) to 5.8 (814 AU). We analysed data acquired in 2006-07 at Calar Alto using the AstraLux lucky imaging system, along with data from SPHERE and NACO at the VLT, and from the literature. Results. We found ten pairs to orbit each other, five pairs that may show orbital motion and five likely common proper motion pairs. We found no obvious correlation between the stellar parameters and binary configuration. The 10 µm infra-red excess varies between 0.1 and 7.2 magnitudes (similar to the distribution in single stars, where it is between 1.7 and 9.1), implying that the presence of the binary star does not greatly influence the emission from the inner disk. Conclusions. We have detected orbital motion in young T Tauri systems over a timescale of ≈ 20 years. Further observations with even longer temporal baseline will provide crucial information on the dynamics of these young stellar systems.

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Examining the T Tauri system with SPHERE

Cited by 18 publications

References 20 publications

New circumstellar structure in the T Tauri system

New circumstellar structure in the T Tauri system

Orbits in the T Tauri triple system observed with SPHERE

Multi-epoch observations with high spatial resolution of multiple T Tauri systems

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