ISPY – NaCo Imaging Survey for Planets around Young stars

Cugno, Gabriele; Quanz, Sascha P.; Launhardt, R.; Barcucci, A. Musso; Brems, Stefan S.; Cheetham, A.; Godoy, N.; Kennedy, Grant M.; Henning, Th.; Müller, André; Olofsson, J.; Pepe, F.; Quirrenbach, A.; Reffert, S.; Rickman, E. L.; Ségransan, D.

doi:10.1051/0004-6361/201935142

Cited by 11 publications

(26 citation statements)

References 47 publications

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“…-While we have not yet been able to independently discover and confirm a new planet in our target sample, our observations have already contributed to the characterisation of two new planets originally discovered by SPHERE: HIP 65426 B (Chauvin et al 2017b;Cheetham et al 2019) and PDS 70 B Müller et al 2018). We discovered two new close-in low-mass stellar companions around the young PPD star R CrA (Cugno et al 2019b) and within the DEB around HD 193571 (Musso Barcucci et al 2019). Around at least two other stars (HD 72660 and HD 92536), we find and astrometrically confirm previously unmentioned close (<1 ) low-mass co-moving stellar companions.…”

Section: Discussionsupporting

confidence: 78%

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ISPY-NACO Imaging Survey for Planets around Young stars

Launhardt

Henning

Quirrenbach

et al. 2020

A&A

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Context. The occurrence rate of long-period (a 50 au) giant planets around young stars is highly uncertain since it is not only governed by the protoplanetary disc structure and planet formation process, but also reflects both dynamical re-structuring processes after planet formation as well as possible capture of planets not formed in situ. Direct imaging is currently the only feasible method to detect such wide-orbit planets and constrain their occurrence rate. Aims. We aim to detect and characterise wide-orbit giant planets during and shortly after their formation phase within protoplanetary and debris discs around nearby young stars. Methods. We carry out a large L -band high-contrast direct imaging survey for giant planets around 200 young stars with protoplanetary or debris discs using the NACO instrument at the ESO Very Large Telescope on Cerro Paranal in Chile. We use very deep angular differential imaging observations with typically >60 • field rotation, and employ a vector vortex coronagraph where feasible to achieve the best possible point source sensitivity down to an inner working angle of about 100 mas. This paper introduces the NACO Imaging Survey for Planets around Young stars (NACO-ISPY), its goals and strategy, the target list, and data reduction scheme, and presents preliminary results from the first 2.5 survey years. Results. We achieve a mean 5 σ contrast of ∆L = 6.4 ± 0.1 mag at 150 mas and a background limit of L bg = 16.5 ± 0.2 mag at >1. 5. Our detection probability is >50% for companions with 8 M Jup at semi-major axes of 80-200 au and >13 M Jup at 30-250 au. It thus compares well to the detection space of other state-of-the-art high-contrast imaging surveys. We have already contributed to the characterisation of two new planets originally discovered by VLT/SPHERE, but we have not yet independently discovered new planets around any of our target stars. We have discovered two new close-in low-mass stellar companions around R CrA and HD 193571 and report in this paper the discovery of close co-moving low-mass stellar companions around HD 72660 and HD 92536. Furthermore, we report L -band scattered light images of the discs around eleven stars, six of which have never been imaged at L -band before. Conclusions. The first 2.5 yr of the NACO-ISPY survey have already demonstrated that VLT/NACO combined with our survey strategy can achieve the anticipated sensitivity to detect giant planets and reveal new close stellar companions around our target stars.

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Section: Discussionsupporting

confidence: 78%

“…The discovery of a close (18.7 au) low-mass stellar companion to the young (1-3 Myr) PPD star R CrA was published by Cugno et al (2019b). This companion was independently and simultaneously also discovered by SPHERE (Mesa et al 2019).…”

Section: New and Confirmed Companionsmentioning

confidence: 96%

ISPY-NACO Imaging Survey for Planets around Young stars

Launhardt

Henning

Quirrenbach

et al. 2020

A&A

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“…-While we have not yet been able to independently discover and confirm a new planet in our target sample, our observations have already contributed to the characterisation of two new planets originally discovered by SPHERE: HIP 65426 B (Chauvin et al 2017b;Cheetham et al 2019) and PDS 70 B (Keppler et al 2018;Müller et al 2018). We discovered two new close-in low-mass stellar companions around the young PPD star R CrA (Cugno et al 2019b) and within the DEB around HD 193571 (Musso Barcucci et al 2019). Around at least two other stars (HD 72660 and HD 92536), we find and astrometrically confirm previously unmentioned close (< 1 ) low-mass co-moving stellar companions.…”

Section: Discussionmentioning

confidence: 94%

ISPY -- NACO Imaging Survey for Planets around Young stars: Survey description and results from the first 2.5 years of observations

Launhardt,

Henning,

Quirrenbach

et al. 2020

Preprint

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Context. The occurrence rate of long-period (a 50 au) giant planets around young stars is highly uncertain since it is not only governed by the protoplanetary disc structure and planet formation process, but also reflects both dynamical re-structuring processes after planet formation as well as possible capture of planets not formed in-situ. Direct imaging is currently the only feasible method to detect such wide-orbit planets and constrain their occurrence rate. Aims. We aim to detect and characterise wide-orbit giant planets during and shortly after their formation phase within protoplanetary and debris discs around nearby young stars. Methods. We carry out a large L -band high-contrast direct imaging survey for giant planets around 200 young stars with protoplanetary or debris discs using the NACO instrument at the ESO Very Large Telescope on Cerro Paranal in Chile. We use very deep angular differential imaging observations with typically > 60 • field rotation, and employ a vector vortex coronagraph where feasible to achieve the best possible point source sensitivity down to an inner working angle of about 100 mas. This paper introduces the NACO Imaging Survey for Planets around Young stars ("NACO-ISPY"), its goals and strategy, the target list, and data reduction scheme, and presents preliminary results from the first 2.5 survey years. Results. We achieve a mean 5 σ contrast of ∆L = 6.4 ± 0.1 mag at 150 mas and a background limit of L bg = 16.5 ± 0.2 mag at >1 . 5. Our detection probability is >50% for companions with 8 M Jup at semi-major axes of 80 -200 au and >13 M Jup at 30 -250 au. It thus compares well to the detection space of other state-of-the-art high-contrast imaging surveys. We have already contributed to the characterisation of two new planets originally discovered by VLT/SPHERE, but we have not yet independently discovered new planets around any of our target stars. We have discovered two new close-in low-mass stellar companions around R CrA and HD 193571 and report in this paper the discovery of close co-moving low-mass stellar companions around HD 72660 and HD 92536. Furthermore, we report L -band scattered light images of the discs around eleven stars, six of which have never been imaged at L -band before. Conclusions. The first 2.5 years of the NACO-ISPY survey have already demonstrated that VLT/NACO combined with our survey strategy can achieve the anticipated sensitivity to detect giant planets and reveal new close stellar companions around our target stars.

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“…A commonly used method to characterize astrometry and photometry of companions in direct imaging is the injection of negative artificial planets (e.g. Stolker et al 2019;Cugno et al 2019b). This forward modeling technique allows to measure the relative brightness and position of a companion despite selfsubtraction, which can undermine direct measurements from the final PSF-subtracted images.…”

Section: Appendix B: Wavelength-collapsed Cubesmentioning

confidence: 99%

Molecular mapping of the PDS70 system: No molecular absorption signatures from the forming planet PDS70 b

Cugno,

Patapis,

Stolker

et al. 2021

Preprint

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Context. Determining the chemical properties of the atmosphere of young forming gas giants might shed light on the location in which their formation occurred and the mechanisms involved. Aims. We aim to detect molecules in the atmosphere of the young forming companion PDS70 b by searching for atmospheric absorption features typical of substellar objects. Methods. We obtained medium-resolution (R≈5075) spectra of the PDS70 planetary system with the SINFONI integral field spectrograph at the Very Large Telescope. We applied molecular mapping, based on cross-correlation with synthetic spectra, to identify signatures of molecular species in the atmosphere of the planet. Results. Although the planet emission is clearly detected when resampling the data to lower resolution, no molecular species could be identified with the cross-correlation technique. We estimated upper limits on the abundances of H 2 O, CO and CH 4 (log(X mol ) < −4.0, −4.1 and −4.9, respectively) assuming a clear atmosphere, and we explored the impact of clouds, which increase the upper limits by a factor up to 0.7 dex. Assuming that the observations directly probe the planet's atmosphere, we found a lack of molecular species compared to other directly imaged companions or field objects. Under the assumption that the planet atmosphere presents similar characteristics to other directly imaged planets, we conclude that a dusty environment surrounds the planet, effectively obscuring any feature generated in its atmosphere. We quantify the extinction necessary to impede the detection (A V ≈ 16 − 17 mag), pointing to the possibility of higher optical thickness than previously estimated from other studies. Finally, the non-detection of molecular species conflicts with atmospheric models previously proposed to describe the forming planet. Conclusions. To unveil how giant planets form, a comprehensive approach that includes constraints from multiple techniques needs to be undertaken. Molecular mapping emerges as an alternative to more classical techniques like SED fitting. Specifically, tuned atmospheric models are likely required to describe faithfully the atmospheres of forming protoplanet, and higher spectral resolution data may reveal molecular absorption lines despite the dusty environment enshrouding PDS70 b.

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ISPY – NaCo Imaging Survey for Planets around Young stars

Cited by 11 publications

References 47 publications

ISPY-NACO Imaging Survey for Planets around Young stars

ISPY-NACO Imaging Survey for Planets around Young stars

ISPY -- NACO Imaging Survey for Planets around Young stars: Survey description and results from the first 2.5 years of observations

Molecular mapping of the PDS70 system: No molecular absorption signatures from the forming planet PDS70 b

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