A high-contrast search for variability in HR 8799bc with VLT-SPHERE

• Published in: Monthly notices of the Royal Astronomical Society Vol. 503; no. 1; pp. 743 - 767
• Main Authors: Biller, Beth A, Apai, Dániel, Bonnefoy, Mickaël, Desidera, Silvano, Gratton, Raffaele, Kasper, Markus, Kenworthy, Matthew, Lagrange, Anne-Marie, Lazzoni, Cecilia, Mesa, Dino, Vigan, Arthur, Wagner, Kevin, Vos, Johanna M, Zurlo, Alice
• Format: Journal Article
• Language: English
• Published: Oxford University Press 01.05.2021; Oxford Journals
• Subjects: Sciences of the Universe; infrared: planetary systems; planets and satellites: gaseous planets; (stars:) brown dwarfs; Astrophysics - Earth and Planetary Astrophysics; Astrophysics - Instrumentation and Methods for Astrophysics
• ISSN: 0035-8711; 1745-3933; 1365-2966
• DOI: 10.1093/mnras/stab202

ABSTRACT The planets HR8799bc display nearly identical colours and spectra as variable young exoplanet analogs such as VHS 1256-1257ABb and PSO J318.5-22, and are likely to be similarly variable. Here we present results from a 5-epoch SPHERE IRDIS broadband-H search for variability in these two planets. HR 8799b aperture photometry and HR 8799bc negative simulated planet photometry share similar trends within uncertainties. Satellite spot lightcurves share the same trends as the planet lightcurves in the August 2018 epochs, but diverge in the October 2017 epochs. We consider Δ(mag)b − Δ(mag)c to trace non-shared variations between the two planets, and rule out non-shared variability in Δ(mag)b − Δ(mag)c to the 10–20 ${{\ \rm per\ cent}}$ level over 4–5 h. To quantify our sensitivity to variability, we simulate variable lightcurves by inserting and retrieving a suite of simulated planets at similar radii from the star as HR 8799bc, but offset in position angle. For HR 8799b, for periods <10 h, we are sensitive to variability with amplitude $\gt 5{{\ \rm per\ cent}}$. For HR 8799c, our sensitivity is limited to variability $\gt 25{{\ \rm per\ cent}}$ for similar periods.