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A Large Ground-Based Observing Campaign of the Disintegrating Planet K2-22B

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A Large Ground-Based Observing Campaign of the Disintegrating Planet K2-22B This is a repository copy of A large ground-based observing campaign of the disintegrating planet K2-22b. White Rose Research Online URL for this paper: http://eprints.whiterose.ac.uk/138580/ Version: Published Version Article: Colón, K.D., Zhou, G., Shporer, A. et al. (27 more authors) (2018) A large ground-based observing campaign of the disintegrating planet K2-22b. Astronomical Journal, 156 (5). 227. ISSN 0004-6256 https://doi.org/10.3847/1538-3881/aae31b © 2018 The American Astronomical Society. Reproduced in accordance with the publisher's self-archiving policy. Reuse Items deposited in White Rose Research Online are protected by copyright, with all rights reserved unless indicated otherwise. They may be downloaded and/or printed for private study, or other acts as permitted by national copyright laws. The publisher or other rights holders may allow further reproduction and re-use of the full text version. This is indicated by the licence information on the White Rose Research Online record for the item. Takedown If you consider content in White Rose Research Online to be in breach of UK law, please notify us by emailing [email protected] including the URL of the record and the reason for the withdrawal request. [email protected] https://eprints.whiterose.ac.uk/ The Astronomical Journal, 156:227 (11pp), 2018 November https://doi.org/10.3847/1538-3881/aae31b © 2018. The American Astronomical Society. All rights reserved. A Large Ground-based Observing Campaign of the Disintegrating Planet K2-22b Knicole D. Colón1 , George Zhou2 , Avi Shporer3 , Karen A. Collins2 , Allyson Bieryla2 , Néstor Espinoza4,5,6, Felipe Murgas7,8, Petchara Pattarakijwanich9 , Supachai Awiphan10, James D. Armstrong11, Jeremy Bailey12,13, Geert Barentsen14,15, Daniel Bayliss16 , Anurak Chakpor10, William D. Cochran17 , Vikram S. Dhillon7,18, Keith Horne19 , Michael Ireland20 , Lucyna Kedziora-Chudczer12,13 , John F. Kielkopf21, Siramas Komonjinda22,23, David W. Latham2 , Tom. R. Marsh16 , David E. Mkrtichian10, Enric Pallé7,8, David Ruffolo9 , Ramotholo Sefako24, Chris G. Tinney12,13 , Suwicha Wannawichian22, and Suraphong Yuma9 1 NASA Goddard Space Flight Center, Exoplanets and Stellar Astrophysics Laboratory (Code 667), Greenbelt, MD 20771, USA 2 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA 3 Massachusetts Institute of Technology, Cambridge, MA 02139, USA 4 Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany 5 Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile 6 Millennium Institute of Astrophysics (MAS), Av. Vicuña Mackenna 4860, 782-0436 Macul, Santiago, Chile 7 Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, Tenerife, Spain 8 Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38205 La Laguna, Tenerife, Spain 9 Department of Physics, Faculty of Science, Mahidol University, Bangkok 10400, Thailand 10 National Astronomical Research Institute of Thailand, 260 Moo 4, Donkaew, Mae Rim, Chiang Mai, 50180, Thailand 11 Institute for Astronomy, University of Hawaii, 34 Ohia Ku St., Pukalani, Maui, HI 96768, USA 12 School of Physics, University of New South Wales, Sydney, NSW 2052, Australia 13 Australian Centre for Astrobiology, University of New South Wales, Sydney, NSW 2052, Australia 14 NASA Ames Research Center, M/S 244-30, Moffett Field, CA 94035, USA 15 Bay Area Environmental Research Institute, 625 2nd St. Ste 209, Petaluma, CA 94952, USA 16 Department of Physics, University of Warwick, Coventry CV4 7AL, UK 17 McDonald Observatory and Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA 18 Department of Physics and Astronomy, University of Sheffield, Sheffield, S3 7RH, UK 19 SUPA Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK 20 Research School of Astronomy & Astrophysics, Australian National University, Canberra, ACT 2611, Australia 21 Department of Physics and Astronomy, University of Louisville, Louisville, KY 40292, USA 22 Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, 239 Huay Kaew Road, Chiang Mai, 50200, Thailand 23 Research Center in Physics and Astronomy, Faculty of Science, Chiang Mai University, 239 Huay Kaew Road, Chiang Mai, 50200, Thailand 24 South African Astronomical Observatory, P.O. Box 9, Observatory, Cape Town 7935, South Africa Received 2018 April 9; revised 2018 September 14; accepted 2018 September 18; published 2018 October 26 Abstract We present 45 ground-based photometric observations of the K2-22 system collected between 2016 December and 2017 May, which we use to investigate the evolution of the transit of the disintegrating planet K2-22b. Last observed in early 2015, in these new observations we recover the transit at multiple epochs and measure a typical depth of <1.5%. We find that the distribution of our measured transit depths is comparable to the range of depths measured in observations from 2014 and 2015. These new observations also support ongoing variability in the K2-22b transit shape and time, although the overall shallowness of the transit makes a detailed analysis of these transit parameters difficult. We find no strong evidence of wavelength-dependent transit depths for epochs where we have simultaneous coverage at multiple wavelengths, although our stacked Las Cumbres Observatory data collected over days-to-months timescales are suggestive of a deeper transit at blue wavelengths. We encourage continued high-precision photometric and spectroscopic monitoring of this system in order to further constrain the evolution timescale and to aid comparative studies with the other few known disintegrating planets. Key words: planets and satellites: detection – planets and satellites: individual (K2-22 b) – techniques: photometric Supporting material: machine-readable tables 1. Introduction intrinsically rare or have a short enough survival lifetime that ( Exoplanet surveys have yielded many surprises over the we are lucky to catch any in the act of disintegrating van years. The discovery of “disintegrating” exoplanets was one Lieshout & Rappaport 2017). such surprise. These are planets that appear to have tails of Because such objects are rare, the systems named above dusty material that produce asymmetric transit shapes. At have been under intense study so as to better understand their present, there are only three such planets known around main- formation and evolution. In particular, observations over long sequence stars: KIC 12557548b (Rappaport et al. 2012), KOI- timescales can be used to determine the rate at which the transit 2700b (Rappaport et al. 2014), and K2-22b (Sanchis-Ojeda depth evolves over time. In addition, multi-wavelength et al. 2015). The first two were discovered in NASA’s Kepler observations can provide constraints on the properties of the prime mission, while the latter was discovered in Campaign 1 grains that are present in the dust tails. For example, several of NASA’s K2 mission (Howell et al. 2014). Given that Kepler such studies have been done for WD 1145+017 (Vanderburg and K2 have observed a combined total of several hundred et al. 2015; Vanderburg & Rappaport 2018), which is a white thousand stars, this suggests that such objects are either dwarf star that has disintegrating planetesimals in orbit around 1 The Astronomical Journal, 156:227 (11pp), 2018 November Colón et al. it and is perhaps the most well-studied “disintegrating” system telescopes ranging in size from 0.5 to 10.4 m and spanning to date (e.g., Alonso et al. 2016; Gänsicke et al. 2016; Zhou optical to near-infrared wavelengths. In Section 3, we present et al. 2016; Croll et al. 2017; Hallakoun et al. 2017; Redfield our analysis and modeling of the light curves, and we describe et al. 2017; Vanderburg & Rappaport 2018; Xu et al. 2018). and discuss our findings in Sections 4 and 5. However, because this system consists of debris orbiting a post-main-sequence star, it is arguably in a different class than 2. Observations and Data Analysis the other three disintegrating planets known. The planetary companion KIC 12557548b, which orbits a In the following sections, we describe the observations of highly spotted K-dwarf star with a period of ∼16 hr, displays K2-22 performed with nine different facilities located around variable transit depths ranging from <0.2% to 1.3% within Kepler the world. The time-series photometry from each observatory is data obtained between 2009 and 2013 (e.g., Rappaport et al. presented in Figure 1 and Table 1, and a summary of the 2012). It was later observed in 2013 and 2014 to have weaker observations is given in Table 2. transits overall than seen in the Kepler data (e.g., Schlawin et al. 2016). Studies have found evidence for a correlation between the 2.1. Anglo-Australian Telescope (AAT) variability of the transit depth and the stellar rotation period Near-infrared light curves of K2-22 were obtained using the (∼23 days; Kawahara et al. 2013; Croll et al. 2015). These studies IRIS2 camera on the 3.9 m AAT (Tinney et al. 2004), located at suggest that either the activity corresponding to enhanced Siding Spring Observatory (SSO) in Australia. IRIS2 is a ultraviolet and/orX-rayradiationinturncausesincreasedmass- 1K×1K camera utilizing a HAWAII-1 HgCdTe detector, read loss and therefore increased variability in the transit depth, or the out over four quadrants in the double-read mode, achieving a − apparent changes in transit depth occur as a dust tail passes over field of view of 7 7×7 7, at a pixel scale of 0 4486 pixel 1. star spots. In addition, while simultaneous Kepler and near- Observations were obtained on UT 2017 March 15 (transit infrared observations of KIC 12557548b revealed no significant epoch=2669) and UT 2017 March 16 (transit epoch=2671) difference in transit depth with wavelength (Crolletal.2014), with IRIS2 in the Ks band, at 30 s exposure time. These evidence for a color dependence of the transit depth between g′ observations were scheduled to accompany simultaneous and z′ was later found by Bochinski et al.
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