A break in the gas and dust surface density of the disc   around
 the T Tauri star IM Lupi

Panić, Olja; Hogerheijde, M. R.; Wilner, David J.; Qi, Chunhua

doi:10.1051/0004-6361/200911883

Cited by 118 publications

(137 citation statements)

References 27 publications

Supporting

Mentioning

126

Contrasting

Order By: Relevance

“…Such a sharp drop in the radial continuum brightness and a size discrepancy between a gas line and the associated continuum, are fingerprints for transport of the larger dust grains, dominated by inward radial drift (e.g. Panić et al 2009;Andrews et al 2012). Based on the peak intensity map shown in Fig.…”

Section: Large Grains and Free-free Emission Filling In The Diskmentioning

confidence: 99%

Cavity and other radial substructures in the disk around HD 97048

Plas

Wright

Ménard

et al. 2016

A&A

View full text Add to dashboard Cite

Context. Gaps, cavities and rings in circumstellar disks are signposts of disk evolution and planet-disk interactions. We follow the recent suggestion that Herbig Ae/Be disks with a flared disk harbour a cavity, and investigate the disk around HD 97048. Aims. We aim to resolve the 34± 4 au central cavity predicted by Maaskant et al. (2013) and to investigate the structure of the disk. Methods. We image the disk around HD 97048 using ALMA at 0.85 mm and 2.94 mm, and ATCA (multiple frequencies) observations. Our observations also include the 12 CO J=1-0, 12 CO J=3-2 and HCO + J=4-3 emission lines. Results. A central cavity in the disk around HD 97048 is resolved with a 40-46 au radius. Additional radial structure present in the surface brightness profile can be accounted for either by an opacity gap at 90 au or by an extra emitting ring at 150 au. The continuum emission tracing the dust in the disk is detected out to 355 au. The 12 CO J=3-2 disk is detected 2.4 times farther out. The 12 CO emission can be traced down to ≈ 10 au scales. Non-Keplerian kinematics are detected inside the cavity via the HCO + J=4-3 velocity map. The mm spectral index measured from ATCA observations suggests that grain growth has occurred in the HD 97048 disk. Finally, we resolve a highly inclined disk out to 150 au around the nearby 0.5 M binary ISO-ChaI 126. Conclusions. The data presented here reveal a cavity in the disk of HD 97048, and prominent radial structure in the surface brightness. The cavity size varies for different continuum frequencies and gas tracers. The gas inside the cavity follows non-Keplerian kinematics seen in HCO + emission. The variable cavity size along with the kinematical signature suggests the presence of a substellar companion or massive planet inside the cavity.

show abstract

Section: Large Grains and Free-free Emission Filling In The Diskmentioning

confidence: 99%

Cavity and other radial substructures in the disk around HD 97048

Plas

Wright

Ménard

et al. 2016

A&A

View full text Add to dashboard Cite

show abstract

“…Although CO emission likely associated with the disc is detected out to ∼ 1000 AU, it is only detected in millimetre continuum out to about 313 AU so the gas disc is more extended than the dust (Lommen et al 2007;Pinte et al 2008;Panić et al 2009;Cleeves et al 2016). The disc is also very massive, with estimates of 0.1 and 0.17 M from Pinte et al (2008) and Cleeves et al (2016) respectively.…”

Section: Introductionmentioning

confidence: 99%

First evidence of external disc photoevaporation in a low mass star forming region: the case of IM Lup

Haworth

Facchini

Clarke

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

We model the radiatively driven flow from IM Lup -a large protoplanetary disc expected to be irradiated by only a weak external radiation field (at least 10 4 times lower than the UV field irradiating the Orion Nebula Cluster proplyds). We find that material at large radii (> 400 AU) in this disc is sufficiently weakly gravitationally bound that significant mass loss can be induced. Given the estimated values of the disc mass and accretion rate, the viscous timescale is long (∼ 10 Myr) so the main evolutionary behaviour for the first Myr of the disc's lifetime is truncation of the disc by photoevaporation, with only modest changes effected by viscosity. We also produce approximate synthetic observations of our models, finding substantial emission from the flow which can explain the CO halo observed about IM Lup out to ≥ 1000 AU. Solutions that are consistent with the extent of the observed CO emission generally imply that IM Lup is still in the process of having its disc outer radius truncated. We conclude that IM Lup is subject to substantial external photoevaporation, which raises the more general possibility that external irradiation of the largest discs can be of significant importance even in low mass star forming regions.

show abstract

“…Indeed, a companion of 1 M Jup could open a gap in the disk and affect its spreading. Panić et al (2009) however argue that no candidate companion at this separation is visible in the HST image of Pinte et al (2008).…”

Section: Im Lup: a Young T Tauri Star With A Massive Circumstellar Diskmentioning

confidence: 84%

“…A more recent paper by Panić et al (2009) presents Submillimeter Array (SMA) observations showing a break in the gas and dust surface density of the IM Lup disk, seen to extend much further than the 400 AU outer edge determined by Pinte et al (2008). One of the proposed explanations for the break is a companion body near the break at 400 AU.…”

Section: Im Lup: a Young T Tauri Star With A Massive Circumstellar Diskmentioning

confidence: 99%

Direct imaging of extra-solar planets in star forming regions

Mawet

Absil

Montagnier

et al. 2012

A&A

View full text Add to dashboard Cite

Context. Most exoplanet imagers consist of ground-based adaptive optics coronagraphic cameras which are currently limited in contrast, sensitivity and astrometric precision, but advantageously observe in the near-infrared window (1-5 μm). Because of these practical limitations, our current observational aim at detecting and characterizing planets puts heavy constraints on target selection, observing strategies, data reduction, and follow-up. Most surveys so far have thus targeted young systems (1-100 Myr) to catch the putative remnant thermal radiation of giant planets, which peaks in the near-infrared. They also favor systems in the solar neighborhood (d < 80 pc), which eases angular resolution requirements but also ensures a good knowledge of the distance and proper motion, which are critical to secure the planet status, and enable subsequent characterization. Aims. Because of their youth, it is very tempting to target the nearby star forming regions, which are typically twice as far as the bulk of objects usually combed for planets by direct imaging. Probing these interesting reservoirs sets additional constraints that we review in this paper by presenting the planet search that we initiated in 2008 around the disk-bearing T Tauri star IM Lup, which is part of the Lupus star forming region (140-190 pc). Methods. We show and discuss why age determination, the choice of evolutionary model for both the central star and the planet, precise knowledge of the host star proper motion, relative or absolute (between different instruments) astrometric accuracy (including plate scale calibration), and patience are the key ingredients for exoplanet searches around more distant young stars. Results. Unfortunately, most of the time, precision and perseverance are not paying off: we discovered a candidate companion around IM Lup in 2008, which we report here to be an unbound background object. We nevertheless review in details the lessons learned from our endeavor, and additionally present the best detection limits ever calculated for IM Lup. We also accessorily report on the successful use of innovative data reduction techniques, such as the damped-LOCI and iterative roll subtraction.

show abstract

A break in the gas and dust surface density of the disc around the T Tauri star IM Lupi

Cited by 118 publications

References 27 publications

Cavity and other radial substructures in the disk around HD 97048

Cavity and other radial substructures in the disk around HD 97048

First evidence of external disc photoevaporation in a low mass star forming region: the case of IM Lup

Direct imaging of extra-solar planets in star forming regions

Contact Info

Product

Resources

About