Performance of the VLT Planet Finder SPHERE

Mesa, D.; Gratton, R.; Zurlo, A.; Vigan, A.; Claudi, R.; Albéri, Matteo; Antichi, J.; Baruffolo, A.; Beuzit, J. L.; Boccaletti, A.; Bonnefoy, M.; Costille, A.; Desidera, S.; Dohlen, Kjetil; Fantinel, D.; Feldt, M.; Fusco, Thierry; Giro, E.; Henning, Th.; Kasper, Markus; Langlois, M.; Maire, Anne-Lise; Martínez, P.; Moeller-Nilsson, O.; Mouillet, D.; Moutou, C.; Pavlov, A.; Puget, P.; Salasnich, Bernardo; Sauvage, J.-F.; Sissa, E.; Turatto, M.; Udry, S.; Vakili, F.; Waters, Rens; Wildi, F.

doi:10.1051/0004-6361/201423910

Cited by 123 publications

(145 citation statements)

References 33 publications

Supporting

Mentioning

145

Contrasting

Order By: Relevance

“…This error could be reduced using the adaptive secondary mirror to create several faint replica of the star at a given separation in the field of view in order to accurately derive the star center (Marois et al 2006b;Sivaramakrishnan & Oppenheimer 2006). The use of star replica for estimating the center of coronagraphic or saturated images is employed in the new high-contrast imaging instruments SPHERE (Beuzit et al 2012;Zurlo et al 2014;Mesa et al 2015) and GPI (Macintosh et al 2014). On-sky tests are foreseen in the coming months to implement this technique for the LEECH observations.…”

Section: Discussionmentioning

confidence: 99%

The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system

Maire

Skemer

Hinz

et al. 2015

A&A

Self Cite

View full text Add to dashboard Cite

Context. Astrometric monitoring of directly imaged exoplanets allows the study of their orbital parameters and system architectures. Because most directly imaged planets have long orbital periods (>20 AU), accurate astrometry is challenging when based on data acquired on timescales of a few years and usually with different instruments. The LMIRCam camera on the Large Binocular Telescope is being used for the LBT Exozodi Exoplanet Common Hunt (LEECH) survey to search for and characterize young and adolescent exoplanets in L band (3.8 µm), including their system architectures. Aims. We first aim to provide a good astrometric calibration of LMIRCam. Then, we derive new astrometry, test the predictions of the orbital model of 8:4:2:1 mean motion resonance proposed for the system, and perform new orbital fitting of the HR 8799 bcde planets. We also present deep limits on a putative fifth planet inside the known planets. Methods. We use observations of HR 8799 and the Θ 1 Ori C field obtained during the same run in October 2013. Results. We first characterize the distortion of LMIRCam. We determine a platescale and a true north orientation for the images of 10.707 ± 0.012 mas/pix and −0.430 ± 0.076 • , respectively. The errors on the platescale and true north orientation translate into astrometric accuracies at a separation of 1 of 1.1 mas and 1.3 mas, respectively. The measurements for all planets agree within 3σ with a predicted ephemeris. The orbital fitting based on the new astrometric measurements favors an architecture for the planetary system based on 8:4:2:1 mean motion resonance. The detection limits allow us to exclude a fifth planet slightly brighter or more massive than HR 8799 b at the location of the 2:1 resonance with HR 8799 e (∼9.5 AU) and about twice as bright as HR 8799 cde at the location of the 3:1 resonance with HR 8799 e (∼7.5 AU).

show abstract

Section: Discussionmentioning

confidence: 99%

The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system

Maire

Skemer

Hinz

et al. 2015

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…centering (for SPHERE data) and via rotational centering (for MagAO), described in Sections 2.1 and 2.2, respectively, which are typically accurate to 0.25 pixels (Mesa et al 2015;Morzinski et al 2015). For both data sets, the position of HD 100453B is measured by fitting a 2D Gaussian to the source.…”

Section: Astrometric Error Budgetmentioning

confidence: 99%

The Orbit of the Companion to HD 100453A: Binary-driven Spiral Arms in a Protoplanetary Disk

Wagner

Dong

Sheehan

et al. 2018

ApJ

View full text Add to dashboard Cite

HD 100453AB is a 10±2 Myr old binary whose protoplanetary disk was recently revealed to host a global twoarmed spiral structure. Given the relatively small projected separation of the binary (1 05, or ∼108 au), gravitational perturbations by the binary seemed to be a likely driving force behind the formation of the spiral arms. However, the orbit of these stars remained poorly understood, which prevented a proper treatment of the dynamical influence of the companion on the disk. We observed HD100453AB between 2015 and 2017, utilizing extreme adaptive optics systems on the Very Large Telescope and the Magellan Clay Telescope. We combined the astrometry from these observations with published data to constrain the parameters of the binary's orbit to a = 1 06±0 09, e=0.17±0.07, and i = 32°.5 ± 6°.5. We utilized publicly available ALMA 12 CO data to constrain the inclination of the disk,~ i 28 disk , which is relatively coplanar with the orbit of the companion and consistent with previous estimates from scattered light images. Finally, we input these constraints into hydrodynamic and radiative transfer simulations to model the structural evolution of the disk. We find that the spiral structure and truncation of the circumprimary disk in HD 100453 are consistent with a companion-driven origin. Furthermore, we find that the primary star's rotation, its outer disk, and the companion exhibit roughly the same direction of angular momentum, and thus the system likely formed from the same parent body of material.

show abstract

“…After this last procedure, we are left with calibrated spectral datacubes comprised of 39 monochromatic images. An additional step using custom IDL tools has been introduced for better handling of bad pixels and to implement spectral cross-talk corrections (Mesa et al 2015). After the creation of the calibrated spectral datacubes, the differential imaging part of the data reduction is performed applying different pipelines written in IDL.…”

Section: Ifs Data Reduction and Spectra Extractionmentioning

confidence: 99%

First light of the VLT planet finder SPHERE

Zurlo

Vigan

Galicher

et al. 2016

A&A

Self Cite

141

View full text Add to dashboard Cite

Context. The planetary system discovered around the young A-type HR 8799 provides a unique laboratory to: a) test planet formation theories; b) probe the diversity of system architectures at these separations, and c) perform comparative (exo)planetology. Aims. We present and exploit new near-infrared images and integral-field spectra of the four gas giants surrounding HR 8799 obtained with SPHERE, the new planet finder instrument at the Very Large Telescope, during the commissioning and science verification phase of the instrument (July-December 2014). With these new data, we contribute to completing the spectral energy distribution (SED) of these bodies in the 1.0-2.5 µm range. We also provide new astrometric data, in particular for planet e, to further constrain the orbits. Methods. We used the infrared dual-band imager and spectrograph (IRDIS) subsystem to obtain pupil-stabilized, dual-band H2H3 (1.593 µm, 1.667 µm), K1K2 (2.110 µm, 2.251 µm), and broadband J (1.245 µm) images of the four planets. IRDIS was operated in parallel with the integral field spectrograph (IFS) of SPHERE to collect low-resolution (R ∼ 30), near-infrared (0.94-1.64 µm) spectra of the two innermost planets HR 8799 d and e. The data were reduced with dedicated algorithms, such as the Karhunen-Loève image projection (KLIP), to reveal the planets. We used the so-called negative planets injection technique to extract their photometry, spectra, and measure their positions. We illustrate the astrometric performance of SPHERE through sample orbital fits compatible with SPHERE and literature data. Results. We demonstrated the ability of SPHERE to detect and characterize planets in this kind of systems, providing spectra and photometry of its components. The spectra improve upon the signal-to-noise ratio of previously obtained data and increase the spectral coverage down to the Y band. In addition, we provide the first detection of planet e in the J band. Astrometric positions for planets HR 8799 bcde are reported for the epochs of July, August, and December 2014. We measured the photometric values in J, H2H3, K1K2 bands for the four planets with a mean accuracy of 0.13 mag. We found upper limit constraints on the mass of a possible planet f of 3-7 M Jup . Our new measurements are more consistent with the two inner planets d and e being in a 2d:1e or 3d:2e resonance. The spectra of HR 8799 d and e are well matched by those of L6-8 field dwarfs. However, the SEDs of these objects are redder than field L dwarfs longward of 1.6 µm.

show abstract

Performance of the VLT Planet Finder SPHERE

Cited by 123 publications

References 33 publications

The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system

The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system

The Orbit of the Companion to HD 100453A: Binary-driven Spiral Arms in a Protoplanetary Disk

First light of the VLT planet finder SPHERE

Contact Info

Product

Resources

About