The Astrophysical Journal, 849:73 (2pp), 2017 November 1 https://doi.org/10.3847/1538-4357/aa8d19 © 2017. The American Astronomical Society. All rights reserved.

Erratum: “Secure TTV Mass Measurements: Ten Kepler Exoplanets between 3 and 8 M⊕ with Diverse Densities and Incident Fluxes” (2016, ApJ, 820, 39)

Daniel Jontof-Hutter1,2 , Eric B. Ford2 , Jason F. Rowe3 , Jack J. Lissauer4, Daniel C. Fabrycky5, Christa Van Laerhoven6, Eric Agol7 , Katherine M. Deck8, Tomer Holczer9 , and Tsevi Mazeh9 1 Department of Physics, University of the Pacific, Stockton, CA 95211, USA; djontofhutter@pacific.edu 2 Department of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802, USA 3 Department of Physics and Astronomy, Bishop’s University, Sherbrooke, Quebec J1M IZ7, Canada 4 Space Science and Astrobiology Division, MS 245-3, NASA Ames Research Center, Moffett Field, CA 94035, USA 5 Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA 6 Canadian Institute for Theoretical Astrophysics, 60 St. George Street, Toronto, ON M5S 3H8, Canada 7 Department of Astronomy, University of Washington, Seattle, WA 98195, USA 8 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, USA 9 School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 69978, Israel Received 2017 August 31; accepted 2017 September 12; published 2017 November 2

Some of the figures in the original manuscript showing the joint posteriors of esinw of neighboring planets are incorrect. The original figures erroneously displayed joint posteriors of ecosw. The originals and their corrections are plotted below. None of the results in the tables or the conclusions of the paper are affected by this erratum.

Figure 1. Figure 3(c), error in the left panel, corrected in the right. Joint posteriors of esinw of Kepler-26 b and c (KOI-250). 95.4% confidence intervals are in light gray, 68.3% confidence intervals are in dark gray.

Figure 2. Figure 5(c), error in the left panel, corrected in the right. Joint posteriors of esinw of Kepler-29 b and c (KOI-738). 95.4% confidence intervals are in light gray, 68.3% confidence intervals are in dark gray.

Figure 3. Figure 7(c), error in the left panel, corrected in the right. Joint posteriors of esinw of Kepler-49 b and c (KOI-248). 95.4% confidence intervals are in light gray, 68.3% confidence intervals are in dark gray. The dashed lines mark the expected correlation between eccentricity vector components from Equation(4) of the paper.

1 The Astrophysical Journal, 849:73 (2pp), 2017 November 1 Jontof-Hutter et al.

Figure 4. Figure 17(c), error in the left panel, corrected in the right. Joint posteriors of esinw of Kepler-177 b and c (KOI-523). 95.4% confidence intervals are in light gray, 68.3% confidence intervals are in dark gray. The dashed lines mark the expected correlation between eccentricity vector components from Equation(4) of the paper.

Figure 5. Figure 19(c), error in the left panel, corrected in the right. Joint posteriors of esinw of Kepler-307 b and c (KOI-1576). 95.4% confidence intervals are in light gray, 68.3% confidence intervals are in dark gray. The dashed lines mark the expected correlation between eccentricity vector components from Equation(4) of the paper.

ORCID iDs Jason F. Rowe https://orcid.org/0000-0002-5904-1865 Daniel Jontof-Hutter https://orcid.org/0000-0002-6227-7510 Eric Agol https://orcid.org/0000-0002-0802-9145 Eric B. Ford https://orcid.org/0000-0001-6545-639X Tomer Holczer https://orcid.org/0000-0003-1306-7354

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