Erratum: “The Transiting Exoplanet Survey Satellite: Simulations of Planet Detections and Astrophysical False Positives” (2015, ApJ, 809, 77)

Abstract

An error in the code used to plot Figure 3 in the original paper caused the limiting magnitudes to appear too faint. This is corrected in Figure 1 in this erratum. Although the original caption is correct, paragraphs 4 and 5 of Section 2.3 need to be changed as follows. "For the Sun-like star, a Å R 4 planet produces a transit depth of 0.13%. The limiting magnitude for transits to be detectable is about = I 11.4 C. This also corresponds to » K 10.6 s and a maximum distance of 290pc, assuming no extinction. For the M dwarf with = T 3200 eff K, we assume  =  R R 0.155 , based on the Dartmouth Stellar Evolution Database (Dotter et al. 2008) for solar metallicity and an age of 1Gyr. Since Dressing & Charbonneau (2015) found that M dwarfs very rarely have close-in planets larger than 3R ⊕ , we consider a planet of this size rather than 4R ⊕. At 3R ⊕ , and the transit depth is 3.1% and the limiting apparent magnitude for detection is = I 15.2 C. This corresponds to » K 13 s and a maximum distance of 120 pc, assuming no extinction." Paragraph 7 of Section 2.3 should also be changed as follows. Figure 1. Limiting magnitude for planet detection as a function of stellar radius for three planetary radii. Here, detection is defined as achieving a signal-to-noise ratio greater than 7.3 from 6hours of integration time during transits. The noise model includes read noise and photon-counting noise from the target star and a typical level of zodiacal light. While the TESS bandpass is similar to the I C band, the sensitivity curve is flatter in K s magnitudes.