PDS 144: THE FIRST CONFIRMED Herbig Ae-Herbig Ae WIDE BINARY

Hornbeck, Jeremy; Grady, C. A.; Perrin, Marshall D.; Wisniewski, John P.; Tofflemire, B. M.; Brown, Alexander; Holtzman, Jon A.; Arraki, Kenza S.; Hamaguchi, Kenji; Woodgate, B. E.; Petre, Robert; Daly, Barry; Grogin, Norman A.; Bonfield, D. G.; Williger, G. M.; Lauroesch, J. T.

doi:10.1088/0004-637x/744/1/54

Cited by 8 publications

(12 citation statements)

References 28 publications

(44 reference statements)

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“…AA Tau was observed with HST/WFPC2 on 1999 January 11. Inspection of the Hubble Legacy Archive data for both the F606W and F814W observations shows that the star dominates Wolf et al 2003;Perrin et al 2006;Hornbeck et al 2012). In addition to the WFPC2 data, which clearly show that the star was detected, both STIS observations prior to PSF subtraction ( Figure 2) show the conspicuous diffraction spikes expected for a stellar detection, suggesting that AA Tau must be viewed at i < 80 • .…”

Section: The Outer Disk Of Aa Taumentioning

confidence: 88%

Imaging the Disk and Jet of the Classical T Tauri Star Aa Tau

Cox

Grady

Hammel

et al. 2012

ApJ

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Previous studies of the classical T Tauri star AA Tau have interpreted the UX-Orionis-like photo-polarimetric variability as being due to a warp in the inner disk caused by an inclined stellar magnetic dipole field. We test that these effects are macroscopically observable in the inclination and alignment of the disk. We use Hubble Space Telescope (HST)/STIS coronagraphic imagery to measure the V magnitude of the star for both STIS coronagraphic observations, compare these data with optical photometry in the literature, and find that, unlike other classical T Tauri stars observed in the same HST program, the disk is most robustly detected in scattered light at stellar optical minimum light. We measure the outer disk radius, 1. 15 ± 0. 10, major-axis position angle, and disk inclination and find that the inner disk, as reported in the literature, is both misinclined and misaligned with respect to the outer disk. AA Tau drives a faint jet, detected in both STIS observations and in follow-on Goddard Fabry-Perot imagery, which is also misaligned with respect to the projection of the outer disk minor axis and is poorly collimated near the star, but which can be traced 21 from the star in data from 2005. The measured outer disk inclination, 71 • ± 1 • , is out of the range of inclinations suggested for stars with UX-Orionis-like variability when no grain growth has occurred in the disk. The faintness of the disk, small disk size, and detection of the star despite the high inclination all indicate that the dust disk must have experienced grain growth and settling toward the disk midplane, which we verify by comparing the observed disk with model imagery from the literature.

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Section: The Outer Disk Of Aa Taumentioning

confidence: 88%

Imaging the Disk and Jet of the Classical T Tauri Star Aa Tau

Cox

Grady

Hammel

et al. 2012

ApJ

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“…Bate (2018)). Several multiple systems with resolved circumstellar discs showing strong misalignment have indeed been observed, such as for example the HK Tau system (Stapelfeldt et al 1998;Jensen & Akeson 2014) or the PDS 144 system (Perrin et al 2006;Hornbeck et al 2012). However, CS Cha is now one of the few hierarchical triple systems in which all components show active accretion and outflows in which the inner binary has a circumbinary disc (Ginski et al 2018).…”

Section: Discussionmentioning

confidence: 99%

CS Cha B: A disc-obscured M-type star mimicking a polarised planetary companion

Haffert

Holstein

Ginski

et al. 2020

A&A

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Context. Direct imaging provides a steady flow of newly discovered giant planets and brown dwarf companions. These multi-object systems can provide information about the formation of low-mass companions in wide orbits and/or help us to speculate about possible migration scenarios. Accurate classification of companions is crucial for testing formation pathways. Aims. In this work we further characterise the recently discovered candidate for a planetary-mass companion CS Cha b and determine if it is still accreting. Methods. MUSE is a four-laser-adaptive-optics-assisted medium-resolution integral-field spectrograph in the optical part of the spectrum. We observed the CS Cha system to obtain the first spectrum of CS Cha b. The companion is characterised by modelling both the spectrum from 6300 Å to 9300 Å and the photometry using archival data from the visible to the near-infrared (NIR). Results. We find evidence of accretion and outflow signatures in Hα and OI emission. The atmospheric models with the highest likelihood indicate an effective temperature of 3450 ± 50 K with a log g of 3.6 ± 0.5 dex. Based on evolutionary models, we find that the majority of the object is obscured. We determine the mass of the faint companion with several methods to be between 0.07 M⊙ and 0.71 M⊙ with an accretion rate of Ṁ = 4 × 10−11±0.4 M⊙ yr−1. Conclusions. Our results show that CS Cha B is most likely a mid-M-type star that is obscured by a highly inclined disc, which has led to its previous classification using broadband NIR photometry as a planetary-mass companion. This shows that it is important and necessary to observe over a broad spectral range to constrain the nature of faint companions.

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“…While sub-arcsecond companions are very likely to be bound, wider candidate companions require multi-epoch proper motion confirmation (e.g, Hornbeck et al 2012). The most extensive and deepest survey to date has been conducted with adaptive optics by Thomas et al (in prep.).…”

Section: Visual Binariesmentioning

confidence: 99%

“…• (Perrin et al 2006;Hornbeck et al 2012). Necessarily, at least one of the two disks is misaligned with the (currently unknown) orbital plane.…”

Section: Circumstellar Disks In Wide Binariesmentioning

confidence: 99%

Herbig AeBe stars: multiplicity and consequences

Duchêne¹

2014

Astrophys Space Sci

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By virtue of their young age and intermediate mass, Herbig AeBe stars represent a cornerstone for our understanding of the mass-dependency of both the stellar and planetary formation processes. In this contribution, I review the current state-of-the-art multiplicity surveys of Herbig AeBe stars to assess both the overall frequency of companions and the distribution of key orbital parameters (separation, mass ratio and eccentricity). In a second part, I focus on the interplay between the multiplicity of Herbig AeBe stars and the presence and properties of their protoplanetary disks. Overall, it appears that both star and planet formation in the context of intermediate-mass stars proceeds following similar mechanisms as lower-mass stars.

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PDS 144: THE FIRST CONFIRMED Herbig Ae-Herbig Ae WIDE BINARY

Cited by 8 publications

References 28 publications

Imaging the Disk and Jet of the Classical T Tauri Star Aa Tau

Imaging the Disk and Jet of the Classical T Tauri Star Aa Tau

CS Cha B: A disc-obscured M-type star mimicking a polarised planetary companion

Herbig AeBe stars: multiplicity and consequences

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