FIRST LIGHT LBT AO IMAGES OF HR 8799 bcde AT 1.6 AND 3.3 μm: NEW DISCREPANCIES BETWEEN YOUNG PLANETS AND OLD BROWN DWARFS

Skemer, Andrew J.; Hinz, Philip M.; Esposito, Simone; Burrows, Adam; Leisenring, Jarron; Skrutskie, Michael F.; Desidera, S.; Mesa, D.; Arcidiacono, Carmelo; Mannucci, F.; Rodigas, Timothy J.; Close, Laird M.; McCarthy, D. W.; Kulesa, Craig; Agapito, Guido; Apai, Dániel; Argomedo, Javier; Bailey, Vanessa P.; Boutsia, K.; Briguglio, Runa; Brusa, Guido; Busoni, Lorenzo; Claudi, R.; Eisner, J. A.; Fini, Luca; Follette, Katherine B.; Garnavich, P.; Gratton, R.; Guerra, Juan Carlos; Hill, John M.; Hoffmann, W. F.; Jones, T. J.; Krejny, M.; Males, Jared R.; Masciadri, E.; Meyer, Michael; Miller, Douglas L.; Morzinski, Katie M.; Pinna, Enrico; Puglisi, Alfio; Quanz, Sascha P.; Quirós-Pacheco, Fernando; Riccardi, Armando; Stefanini, P.; Vaitheeswaran, Vidhya; Wilson, John C.; Xompero, Marco

doi:10.1088/0004-637x/753/1/14

Cited by 162 publications

(185 citation statements)

References 47 publications

Supporting

Mentioning

174

Contrasting

Order By: Relevance

“…Given the error bars, our values agree with the values in the literature and achieve similar accuracies (Marois et al 2008(Marois et al , 2010bCurrie et al 2014). For these reasons, we did not attempt to carry out atmospheric modeling (Skemer et al 2012) using these new photometric data.…”

Section: Photometrysupporting

confidence: 85%

“…When observing a bright star in the L band, the LMIRCam PSF is very stable, so this photometric standard is more than adequate for approximating the relatively low signal-to-noise core of an exoplanet. Since the point-source self-subtraction of angular differential imaging biases the astrometric and photometric measurements, we calibrated these effects using injection of synthetic point sources (based on the measured PSF) with different brightness and insertion positions into the preprocessed data (Skemer et al 2012). More precisely, we inserted negative artificial planets (Marois et al 2010a;Bonnefoy et al 2011) at the positions of the real planets in the preprocessed data before performing the differential imaging part of the data analysis.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…LEECH complements the other current or future large imaging surveys for young ( 200 Myr) giant exoplanets by covering longer wavelengths and probing northern, nearby ( 30-55 pc), and older ( 1 Gyr) stars. The first data obtained with LBTI/LMIRCam prior to the LEECH survey allowed the multiwavelength photometric analysis in the L band (3-4 µm) of the four planets of HR 8799 (Skemer et al 2012, and the M-band detection and photometric characterization of κ And b (Bonnefoy et al 2014a).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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

Maire

Skemer

Hinz

et al. 2015

A&A

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: Photometrysupporting

confidence: 85%

Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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

Maire

Skemer

Hinz

et al. 2015

A&A

View full text Add to dashboard Cite

show abstract

“…We note that observations of planets around HR 8799 suggest that the methane absorption in the spectra of these planets is significantly weaker than predicted by theoretical models (e.g. Bowler et al 2010;Barman et al 2011;Skemer et al 2012). If this is a general feature of young giant planets it could indicate that our expected sensitivity to these planets in the ASDI mode is overly optimistic.…”

Section: Observationsmentioning

confidence: 58%

The Gemini NICI Planet-Finding Campaign: The Frequency of Giant Planets around Young B and A Stars

Nielsen

Liu

Wahhaj³

et al. 2013

Proc. IAU

View full text Add to dashboard Cite

We have carried out high contrast imaging of 70 young, nearby B and A stars to search for brown dwarf and planetary companions as part of the Gemini NICI PlanetFinding Campaign. Our survey represents the largest, deepest survey for planets around high-mass stars (≈1.5-2.5 M ⊙ ) conducted to date and includes the planet hosts β Pic and Fomalhaut. We obtained follow-up astrometry of all candidate companions within 400 AU projected separation for stars in uncrowded fields and identified new low-mass −20 M Jup and 55 +20 −19 M Jup , making this system one of the rare substellar binaries in orbit around a star. Considering the contrast limits of our NICI data and the fact that we did not detect any planets, we use high-fidelity Monte Carlo simulations to show that fewer than 20% of 2 M ⊙ stars can have giant planets greater than 4 M Jup between 59 and 460 AU at 95% confidence, and fewer than 10% of these stars can have a planet more massive than 10 M Jup between 38 and 650 AU. Overall, we find that large-separation giant planets are not common around B and A stars: fewer than 10% of B and A stars can have an analog to the HR 8799 b (7 M Jup , 68 AU) planet at 95% confidence. We also describe a new Bayesian technique for determining the ages of field B and A stars from photometry and theoretical isochrones. Our method produces more plausible ages for high-mass stars than previous age-dating techniques, which tend to underestimate stellar ages and their uncertainties.

show abstract

“…This is done by observing flux variations on the timescales of the rotation periods of brown dwarfs, or the passage of an exoplanet in front of (or behind) its host star (Winn 2010;Buenzli et al 2012). For example, the L-and L S -bands can allow the characterization of a methane bandhead in the atmospheres of either brown dwarfs or giant planets, and can help infer the presence of disequilibrium chemistry (Skemer et al 2012(Skemer et al , 2014.…”

Section: Introductionmentioning

confidence: 99%

Precision Time-series Photometry in the Thermal Infrared with a “Wall-eyed” Pointing Mode at the Large Binocular Telescope

Spalding

Hinz

Skemer

et al. 2017

PASP

View full text Add to dashboard Cite

Time-series photometry taken from ground-based facilities is improved with the use of comparison stars due to the short timescales of atmospheric-induced variability. However, the sky is bright in the thermal infrared (3-5 µm), and the correspondingly small fields-of-view of available detectors make it highly unusual to have a calibration star in the same field as a science target. Here we present a new method of obtaining differential photometry by simultaneously imaging a science target and a calibrator star, separated by 2 amin, onto a 10×10 asec 2 field-of-view detector. We do this by taking advantage of the LBT's unique binocular design to point the two co-mounted telescopes apart and simultaneously obtain both targets in three sets of observations. Results indicate that the achievable scatter in L S -band (λ c = 3.3 µm) is at the percent level for bright targets, and possibly better with heavier sampling and characterization of the systematics.

show abstract

FIRST LIGHT LBT AO IMAGES OF HR 8799 bcde AT 1.6 AND 3.3 μm: NEW DISCREPANCIES BETWEEN YOUNG PLANETS AND OLD BROWN DWARFS

Cited by 162 publications

References 47 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 Gemini NICI Planet-Finding Campaign: The Frequency of Giant Planets around Young B and A Stars

Precision Time-series Photometry in the Thermal Infrared with a “Wall-eyed” Pointing Mode at the Large Binocular Telescope

Contact Info

Product

Resources

About