Variability in IC5070: Two Young Stars with Deep Recurring Eclipse

Dirk Froebrich (Lead / Corresponding author), Aleks Scholz, Justyn Campbell-White, James Crumpton, Emma D’Arcy, Sally V. Makin, Tarik Zegmott, Samuel J. Billington, Ricky Hibbert, Robert J. Newport, Callum R. Fisher

Research output: Contribution to journalArticle

Abstract

Investigating the structure and properties of the innermost parts of protoplanetary accretion disks on sub-AU scales is currently only possible via indirect methods. One option to map the planet-forming zone is to search for occultations of the central young stellar object (YSO) by circumstellar material, e.g., warps or clumps in the inner disks. Such disk eclipses typically last hours to days (Cody et al. 2014) and have been identified in massive HAeBe stars such as UX Ori (Herbst & Shevchenko 1999) and lower mass objects such as AA Tau (Bouvier et al. 1999). Of particular interest are quasi-periodic dimming events. They allow distance determinations of the occulting material from the central star. In such cases the actual azimuthal physical extent of the material can be determined from the duration of the dimming event relative to the period. Observations over several periods enable investigations into temporal changes in the line of sight column density distribution, and multi-wavelength data allows us to probe the dust scattering properties. Our citizen science project HOYS-CAPS (Froebrich et al. 2018) aims to identify such periodic dimming events around YSOs. We used this data-set to search for periodic signatures in light-curves from YSOs in the Pelican nebula (IC 5070). For this field we have ~200 individual observations in the V, R, and I-band filters, distributed over ~800 days. Hence, the average cadence is 4 days, but the most frequent gap (30%) between subsequent observations is 2 days. Observations are usually taken as 8 × 2 minutes integrations in all filters to achieve a consistent S/N.
Original languageEnglish
Article number61
JournalResearch Notes of the AAS
Volume2
Issue number2
DOIs
Publication statusPublished - 22 Jun 2018

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