The widest H<i>α</i> survey of accreting protoplanets around nearby transition disks

Zurlo, A.; Cugno, Gabriele; Montesinos, Matías; Pérez, Sebastián; Cánovas, H.; Casassus, S.; Christiaens, Valentin; Cieza, Lucas A.; Huélamo, N.

doi:10.1051/0004-6361/201936891

Cited by 54 publications

(57 citation statements)

References 98 publications

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“…In the plots, blue triangles are measured and blue circles are unresolved. In the histograms, the red components are lower limits of α. been observed in Hα emission with sufficient contrast to redetect PDS 70b, but no planet candidates have been detected (Zurlo et al 2020). PDS 70b is located just outside the detected inner disk, which is larger (∼ 10 au) and has a lower ξ inner (∼ 10 2 ) than most other disks in the sample (Figure 13, upper left).…”

Section: Consequences For the Presence Of Companionsmentioning

confidence: 99%

Dust-depleted Inner Disks in a Large Sample of Transition Disks through Long-baseline ALMA Observations

Francis

Marel

2020

ApJ

169

146

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Transition disks with large inner dust cavities are thought to host massive companions. However, the disk structure inside the companion orbit and how material flows toward an actively accreting star remain unclear. We present a high resolution continuum study of inner disks in the cavities of 38 transition disks. Measurements of the dust mass from archival Atacama Large Millimeter/Submillimeter Array observations are combined with stellar properties and spectral energy distributions to assemble a detailed picture of the inner disk. An inner dust disk is detected in 18 of 38 disks in our sample. Of the 14 resolved disks, 8 are significantly misaligned with the outer disk. The near-infrared excess is uncorrelated with the mm dust mass of the inner disk. The size-luminosity correlation known for protoplanetary disks is recovered for the inner disks as well, consistent with radial drift. The inner disks are depleted in dust relative to the outer disk and their dust mass is uncorrelated with the accretion rates. This is interpreted as the result of radial drift and trapping by planets in a low α (∼ 10 −3 ) disk, or a failure of the α-disk model to describe angular momentum transport and accretion. The only disk in our sample with confirmed planets in the gap, PDS 70, has an inner disk with a significantly larger radius and lower inferred gas-to-dust ratio than other disks in the sample. We hypothesize that these inner disk properties and the detection of planets are due to the gap having only been opened recently by young, actively accreting planets.

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Section: Consequences For the Presence Of Companionsmentioning

confidence: 99%

Dust-depleted Inner Disks in a Large Sample of Transition Disks through Long-baseline ALMA Observations

Francis

Marel

2020

ApJ

169

146

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“…If detected, this emission constitutes the main observational signature of the ongoing formation of a substellar object (Eriksson et al 2020). Observations of PPDs with SPHERE/ZIMPOL and MUSE have so far been unable to detect planetary-mass companions around PPD hosts other than the pair around PDS 70, despite reaching potential sensitivities down to 1 M Jup (Haffert et al 2019;Zurlo et al 2020).…”

Section: Potential For Future Detectionmentioning

confidence: 99%

Perturbers: SPHERE detection limits to planetary-mass companions in protoplanetary disks

Asensio-Torres

Henning

Cantalloube

et al. 2021

A&A

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The detection of a wide range of substructures such as rings, cavities, and spirals has become a common outcome of high spatial resolution imaging of protoplanetary disks, both in the near-infrared scattered light and in the thermal millimetre continuum emission. The most frequent interpretation of their origin is the presence of planetary-mass companions perturbing the gas and dust distribution in the disk (perturbers), but so far the only bona fide detection has been the two giant planets carving the disk around PDS 70. Here, we present a sample of 15 protoplanetary disks showing substructures in SPHERE scattered-light images and a homogeneous derivation of planet detection limits in these systems. To obtain mass limits we rely on different post-formation luminosity models based on distinct formation conditions, which are critical in the first million years of evolution. We also estimate the mass of these perturbers through a Hill radius prescription and a comparison to ALMA data. Assuming that one single planet carves each substructure in scattered light, we find that more massive perturbers are needed to create gaps within cavities than rings, and that we might be close to a detection in the cavities of RX J1604.3-2130A, RX J1615.3-3255, Sz Cha, HD 135344B, and HD 34282. We reach typical mass limits in these cavities of 3–10 MJup. For planets in the gaps between rings, we find that the detection limits of SPHERE high-contrast imaging are about an order of magnitude away in mass, and that the gaps of PDS 66 and HD 97048 seem to be the most promising structures for planet searches. The proposed presence of massive planets causing spiral features in HD 135344B and HD 36112 are also within SPHERE’s reach assuming hot-start models. These results suggest that the current detection limits are able to detect hot-start planets in cavities, under the assumption that they are formed by a single perturber located at the centre of the cavity. More realistic planet mass constraints would help to clarify whether this is actually the case, which might indicate that perturbers are not the only way of creating substructures.

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“…Such enhancement in contrast is one of the drivers for the search of accretion signatures. Observations of accretion signatures in Hα has been conducted in the past few years with MagAO (Close et al 2014;Wagner et al 2018) and SPHERE (Cugno et al 2019;Zurlo et al 2020), yielding the detection of Hα emission from substellar companions.…”

Section: Introductionmentioning

confidence: 99%

Searching for proto-planets with MUSE

Xie

Haffert

Boer

et al. 2020

A&A

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Context. Protoplanetary disks contain structures such as gaps, rings, and spirals, which are thought to be produced by the interaction between the disk and embedded protoplanets. However, only a few planet candidates are found orbiting within protoplanetary disks, and most of them are being challenged as having been confused with disk features. Aims. The VLT/MUSE discovery of PDS 70 c demonstrated a powerful way of searching for still-forming protoplanets by targeting accretion signatures with medium-resolution integral field spectroscopy. We aim to discover more proto-planetary candidates with MUSE, with a secondary aim of improving the high-resolution spectral differential imaging (HRSDI) technique by analyzing the instrumental residuals of MUSE. Methods. We analyzed MUSE observations of five young stars with various apparent brightnesses and spectral types. We applied the HRSDI technique to perform high-contrast imaging. The detection limits were estimated using fake planet injections. Results. With a 30 min integration time, MUSE can reach 5σ detection limits in apparent Hα line flux down to 10−14 and 10−15 erg s−1 cm−2 at 0.075′′ and 0.25′′, respectively. In addition to PDS 70 b and c, we did not detect any clear accretion signatures in PDS 70, J1850-3147, and V1094 Sco down to 0.1′′. MUSE avoids the small sample statistics problem by measuring the noise characteristics in the spatial direction at multiple wavelengths. We detected two asymmetric atomic jets in HD 163296 with a very high spatial resolution (down to 8 au) and medium spectral resolution (R ~ 2500). Conclusions. The HRSDI technique when applied to MUSE data allows us to reach the photon noise limit at small separations (i.e., <0.5′′). With the combination of high-contrast imaging and medium spectral resolution, MUSE can achieve fainter detection limits in apparent line flux than SPHERE/ZIMPOL by a factor of ~5. MUSE has some instrumental issues that limit the contrast that appear in cases with strong point sources, which can be either a spatial point source due to high Strehl observations or a spectral point source due to a high line-to-continuum ratio. We modified the HRSDI technique to better handle the instrumental artifacts and improve the detection limits. To avoid the instrumental effects altogether, we suggest faint young stars with relatively low Hα line-to-continuum ratio to be the most suitable targets for MUSE to search for potential protoplanets.

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The widest Hα survey of accreting protoplanets around nearby transition disks

Cited by 54 publications

References 98 publications

Dust-depleted Inner Disks in a Large Sample of Transition Disks through Long-baseline ALMA Observations

Dust-depleted Inner Disks in a Large Sample of Transition Disks through Long-baseline ALMA Observations

Perturbers: SPHERE detection limits to planetary-mass companions in protoplanetary disks

Searching for proto-planets with MUSE

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