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Investigation of a transiting planet candidate in Trumpler 37: An astro-physical false positive eclipsing spectroscopic binary star

Errmann, R. and Howard, A. W. (2014) Investigation of a transiting planet candidate in Trumpler 37: An astro-physical false positive eclipsing spectroscopic binary star. Astronomische Nachrichten, 335 (4). pp. 345-356. ISSN 0004-6337. https://resolver.caltech.edu/CaltechAUTHORS:20170621-134023360

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Abstract

We report our investigation of the first transiting planet candidate from the YETI project in the young (∼4 Myr old) open cluster Trumpler 37. The transit-like signal detected in the lightcurve of F8V star 2M21385603+5711345 repeats every 1.364894 + 0.000015 days, and has a depth of 54.5 + 0.8 mmag in R. Membership in the cluster is supported by its mean radial velocity and location in the color-magnitude diagram, while the Li diagnostic and proper motion are inconclusive in this regard. Follow-up photometric monitoring and adaptive optics imaging allow us to rule out many possible blend scenarios, but our radial-velocity measurements show it to be an eclipsing single-lined spectroscopic binary with a late-type (mid-M) stellar companion, rather than one of planetary nature. The estimated mass of the companion is 0.15–0.44 M⊙. The search for planets around very young stars such as those targeted by the YETI survey remains of critical importance to understand the early stages of planet formation and evolution.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1002/asna.201412047DOIArticle
http://onlinelibrary.wiley.com/doi/10.1002/asna.201412047/abstractPublisherArticle
https://arxiv.org/abs/1403.6020arXivDiscussion Paper
ORCID:
AuthorORCID
Howard, A. W.0000-0001-8638-0320
Additional Information:© 2014 Wiley-VCH Verlag GmbH & Co. KGaA, Weinheim. Received 2014 Feb 2, accepted 2014 Feb 21; Published online 2014 May 2. Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration (Proposal ID H215Hr). The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. Based on observations obtained with telescopes of the University Observatory Jena, which is operated by the Astrophysical Institute of the Friedrich-Schiller-University. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC, Proposal IDs H10-3.5-015 and H10-2.2-004). Some of the observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona (Proposal ID 2010c-SAO-5). All participating observatories appreciate the logistic and financial support of their institutions and in particular their technical workshops. We wish to thank the following persons for participating in the observations of Trumpler 37: E.L.N. Jensen and D.H. Cohen at the Swarthmore telescope; A. Niedzielski at the Torun telescope; E.H. Nikogossian, T. Movsessian, and H. Harutyunyan at the Byurakan telescope; and T. Roell, S. Baar, E. Schmidt, F. Gießler, H. Gilbert, I. Häusler, D. Keeley, and P. Nährlich for the observations at the Jena telescope. We are grateful to D.W. Latham for the helpful discussion and proposing observations. RN, MK, and RE would like to thank DFG for support in the Priority Programme SPP 1385 on the “First Ten Million Years of the Solar System” in project NE 515 / 34-1 and 34-2. BD, JGS, MMH, LT, TE, and RN thank DFG in SFB TR 7 in TPs C2, C7, and B9. CM and KS thank DFG in project SCHR 665 / 7-1. CG and MM thank DFG in project MU 2695 / 13-1. CA thanks DFG in project NE 515 / 35-1 and 35-2 in SPP 1385. SR and TR thanks DFG in project NE 515 / 33-1 and 33-2 in SPP 1385. NP thanks DFG in project KR 2164 / 10-1. DD acknowledges the partial financial support of the project DDVU 02/40-2010 of the Bulgarian National Science Fund. Wu, Z.Y. was supported by the Chinese National Natural Science Foundation grant No. 11373033. This work was also supported by the joint fund of Astronomy of the National Nature Science Foundation of China and the Chinese Academy of Science, under Grant U1231113. Zhou, X. was supported by the Chinese National Natural Science Foundation grants No. 11073032, and by the National Basic Research Program of China (973 Program), No. 2014CB845704, and 2013CB834902. This work has been supported by a VEGA Grant 2/0143/13 of the Slovak Academy of Sciences. We would like to acknowledge financial support from the Thuringian government (B 515-07010) for the STK CCD camera used in this project. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
Funders:
Funding AgencyGrant Number
Deutsche Forschungsgemeinschaft (DFG)SPP 1385
Deutsche Forschungsgemeinschaft (DFG)NE 515/34-1
Deutsche Forschungsgemeinschaft (DFG)NE 515/34-2
Deutsche Forschungsgemeinschaft (DFG)SFB TR 7
Deutsche Forschungsgemeinschaft (DFG)SCHR 665/7-1
Deutsche Forschungsgemeinschaft (DFG)MU 2695/13-1
Deutsche Forschungsgemeinschaft (DFG)NE 515/35-1
Deutsche Forschungsgemeinschaft (DFG)NE 515/35-2
Deutsche Forschungsgemeinschaft (DFG)NE 515/33-1
Deutsche Forschungsgemeinschaft (DFG)NE 515/33-2
Deutsche Forschungsgemeinschaft (DFG)KR 2164/10-1
Bulgarian National Science FundDDVU 02/40-2010
National Natural Science Foundation of China11373033
Chinese Academy of SciencesU1231113
National Natural Science Foundation of China11073032
National Basic Research Program of China (973 Program)2014CB845704
National Basic Research Program of China (973 Program)2013CB834902
Slovak Academy of Sciences2/0143/13
Thuringian GovernmentB 515-07010
Subject Keywords:open clusters and associations: individual (Trumpler 37); binaries: eclipsing; binaries: spectroscopic; planetary systems; stars: fundamental parameters; stars: late-type
Issue or Number:4
Record Number:CaltechAUTHORS:20170621-134023360
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170621-134023360
Official Citation:Errmann, R., Torres, G., Schmidt, T.O.B., Seeliger, M., Howard, A.W., Maciejewski, G., Neuhäuser, R., Meibom, S., Kellerer, A., Dimitrov, D.P., Dincel, B., Marka, C., Mugrauer, M., Ginski, Ch., Adam, Ch., Raetz, St., Schmidt, J.G., Hohle, M.M., Berndt, A., Kitze, M., Trepl, L., Moualla, M., Eisenbeiß, T., Fiedler, S., Dathe, A., Graefe, Ch., Pawellek, N., Schreyer, K., Kjurkchieva, D.P., Radeva, V.S., Yotov, V., Chen, W.P., Hu, S.C.-L., Wu, Z.-Y., Zhou, X., Pribulla, T., Budaj, J., Vaňko, M., Kundra, E., Hambälek, Ľ., Krushevska, V., Bukowiecki, Ł., Nowak, G., Marschall, L., Terada, H., Tomono, D., Fernandez, M., Sota, A., Takahashi, H., Oasa, Y., Briceño, C., Chini, R. and Broeg, C.H. (2014), Investigation of a transiting planet candidate in Trumpler 37: An astro-physical false positive eclipsing spectroscopic binary star *. Astron. Nachr., 335: 345–356. doi:10.1002/asna.201412047
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:78422
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:21 Jun 2017 21:15
Last Modified:03 Oct 2019 18:08

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