Setting Cut-Scores: A Critical Review of the Angoff and Modified Angoff Methods

The purpose of this article is to review critically the Angoff (1971) and modified Angoff methods for setting cut-scores. The criteria used in this review were originally proposed by Berk (1986). The assumptions of the Angoff method and other current issues surrounding this method are also discussed. Recommendations are made for using the Angoff method. In addition, several issues that are relevant to cut-score setting that are not addressed by Berk’s criteria arose while reviewing the Angoff method. These issues are addressed separately.Cet article a comme objectif d’examiner, de façon éclairée, la méthode Angoff (1971) et la méthode Angoff modifiée employées pour établir les notes de passage. Cet examen reprend des critères proposés par Berk (1986). On présente les hypothèses sur lesquelles repose la méthode Angoff, discute des questions relatives à la méthode et propose des recommandations pour son utilisation. Finalement, on présente plusieurs questions qui se sont avérées pertinentes à l’établissement des notes de passage mais dont ne tiennent pas compte les critères de Berk

Establishing Performance Standards and Setting Cut-Scores

This article serves as an introduction to the following four articles in which four methods for establishing standards and setting cut-scores are presented and evaluated. The purposes, nature, and characteristics of performance standards are first reviewed. This is followed by a brief discussion of the methods for setting cut-scores. Berk’s (1986) criteria for evaluating four of these procedures are then presented and described.Cet article sert d’introduction aux quatre articles suivants dans lesquels sont présentées et évaluées quatre méthodes pour établir des normes et des seuils de passage. Dans un premier temps, les objectifs, la nature et les caractéristiques des normes de rendement sont examinés. Ensuite, on offre un survol des méthodes employées pour déterminer les seuils de passage. En dernier lieu, on présente et décrit les critères de Berk (1986) pour évaluer quatre de ces procédures

TESS Discovery of Twin Planets near 2:1 Resonance around Early M-Dwarf TOI 4342

With data from the Transiting Exoplanet Survey Satellite (TESS), we showcase improvements to the MIT Quick-Look Pipeline (QLP) through the discovery and validation of a multi-planet system around M-dwarf TOI 4342 ($T_{mag}=11.032$, $M_* = 0.63 M_\odot$, $R_* = 0.60 R_\odot$, $T_{eff} = 3900$ K, $d = 61.54$ pc). With updates to QLP, including a new multi-planet search, as well as faster cadence data from TESS' First Extended Mission, we discovered two sub-Neptunes ($R_b = 2.266_{-0.038}^{+0.038} R_\oplus$ and $R_c = 2.415_{-0.040}^{+0.043} R_\oplus$; $P_b$ = 5.538 days and $P_c$ = 10.689 days) and validated them with ground-based photometry, spectra, and speckle imaging. Both planets notably have high transmission spectroscopy metrics (TSMs) of 36 and 32, making TOI 4342 one of the best systems for comparative atmospheric studies. This system demonstrates how improvements to QLP, along with faster cadence Full-Frame Images (FFIs), can lead to the discovery of new multi-planet systems.Comment: accepted for publication in A

The TESS-Keck Survey. XI. Mass Measurements for Four Transiting sub-Neptunes orbiting K dwarf TOI-1246

Multi-planet systems are valuable arenas for investigating exoplanet architectures and comparing planetary siblings. TOI-1246 is one such system, with a moderately bright K dwarf (V=11.6, K=9.9) and four transiting sub-Neptunes identified by TESS with orbital periods of 4.31 d, 5.90 d, 18.66 d, and 37.92 d. We collected 130 radial velocity observations with Keck/HIRES and TNG/HARPS-N to measure planet masses. We refit the 14 sectors of TESS photometry to refine planet radii (2.97±0.06 R⊕,2.47±0.08 R⊕,3.46±0.09 R⊕, 3.72±0.16 R⊕), and confirm the four planets. We find that TOI-1246 e is substantially more massive than the three inner planets (8.1±1.1M⊕, 8.8±1.2M⊕, 5.3±1.7M⊕, 14.8±2.3M⊕). The two outer planets, TOI-1246 d and TOI-1246 e, lie near to the 2:1 resonance (Pe/Pd=2.03) and exhibit transit timing variations. TOI-1246 is one of the brightest four-planet systems, making it amenable for continued observations. It is one of only six systems with measured masses and radii for all four transiting planets. The planet densities range from 0.70±0.24 to 3.21±0.44g/cm3, implying a range of bulk and atmospheric compositions. We also report a fifth planet candidate found in the RV data with a minimum mass of 25.6 ± 3.6 M⊕. This planet candidate is exterior to TOI-1246 e with a candidate period of 93.8 d, and we discuss the implications if it is confirmed to be planetary in nature

A pair of Sub-Neptunes transiting the bright K-dwarf TOI-1064 characterised with CHEOPS

Funding: TGW, ACC, and KH acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1.We report the discovery and characterization of a pair of sub-Neptunes transiting the bright K-dwarf TOI-1064 (TIC 79748331), initially detected in the Transiting Exoplanet Survey Satellite (TESS) photometry. To characterize the system, we performed and retrieved the CHaracterising ExOPlanets Satellite (CHEOPS), TESS, and ground-based photometry, the High Accuracy Radial velocity Planet Searcher (HARPS) high-resolution spectroscopy, and Gemini speckle imaging. We characterize the host star and determine Teff,⋆=4734±67K⁠, R⋆=0.726±0.007R⊙⁠, and M⋆=0.748±0.032M⊙⁠. We present a novel detrending method based on point spread function shape-change modelling and demonstrate its suitability to correct flux variations in CHEOPS data. We confirm the planetary nature of both bodies and find that TOI-1064 b has an orbital period of Pb = 6.44387 ± 0.00003 d, a radius of Rb = 2.59 ± 0.04 R⊕, and a mass of Mb=13.5+1.7−1.8 M⊕, whilst TOI-1064 c has an orbital period of Pc=12.22657+0.00005−0.00004 d, a radius of Rc = 2.65 ± 0.04 R⊕, and a 3σ upper mass limit of 8.5 M⊕. From the high-precision photometry we obtain radius uncertainties of ∼1.6 per cent, allowing us to conduct internal structure and atmospheric escape modelling. TOI-1064 b is one of the densest, well-characterized sub-Neptunes, with a tenuous atmosphere that can be explained by the loss of a primordial envelope following migration through the protoplanetary disc. It is likely that TOI-1064 c has an extended atmosphere due to the tentative low density, however further radial velocities are needed to confirm this scenario and the similar radii, different masses nature of this system. The high-precision data and modelling of TOI-1064 b are important for planets in this region of mass–radius space, and it allow us to identify a trend in bulk density–stellar metallicity for massive sub-Neptunes that may hint at the formation of this population of planets.Publisher PDFPeer reviewe

Listening. Learning. Leading. ® Single-Versus Double-Scoring of Trend Responses in Trend Score Equating With Constructed-Response Tests Single-Versus Double-Scoring of Trend Responses in Trend Score Equating With Constructed-Response Tests

Abstract This study examines the differences in equating outcomes between two trend score equating designs resulting from two different scoring strategies for trend scoring when operational constructed-response (CR) items are double-scored-the single group (SG) design, where each trend CR item is double-scored, and the nonequivalent groups with anchor test (NEAT) design, where each trend CR item is single-scored during trend score equating-for varying sample sizes (n =150, 200, 250, 300, 400). Overall results suggest larger equating errors with smaller sample sizes, though errors were small regardless of sample size. The NEAT design performed about as well as the SG design with respect to conditional and summative standard errors of equating, though it did tend to produce larger bias and root mean-squared differences (RMSDs). When accounting for the total number of trend scores required to do analyses, the NEAT design performed as well or better than the SG design (e.g., when the NEAT n =150 and the SG n = 300). This result might be partially attributable to a larger operational sample size (n = 792) and a good correlation between anchor and total score for the trend sample (r = 0.73). These results suggest that under these testing conditions, the NEAT design performed about as well as the SG design, but further research is required to assess the generalizability of the results