Creative Product Problem-solving Game

Creativity is a talent that undergirds invention and innovation, making it an important skill in today’s society. Although students are often told to “be creative,” they many times do not know how and have little practice in this skill. This document presents an analysis of 33 creative products made by adult participants at a state conference for educators working with preK-12 gifted students or their teachers as a model for what teachers can do in their classrooms to allow students to practice creative thinking. During the conference presentation, Torrance’s creative strengths were reviewed with photographic examples, definitions, and suggestions printed on handouts. For the problem-solving game, each participant was given an identical set of recycled/craft materials, and about 30 minutes to create an object or scene fitting with a given theme. This presentation was delivered each of the two days of the conference with a different theme each day: “under water” was the theme the first day and “cool space” was the theme for the products on the second day. Participants each created an object that exhibited creative strengths and followed game-rules using the additional tools of scissors, glue, markers, and thread. Photographs of the final products are shown with their creative strengths identified. Most participants were successful in developing products that showed five creative strengths as required by the game rules. The most common approach to making a creative product that exhibited creative strengths was to tell an original story involving some motion that was detailed, artistically appealing, or humorous, and contained characters with emotional expressions. Because of the success and enthusiasm of participants for the game, the authors recommend it for students, clubs, and recreational activities. [7 Tables, 33 Figures, 6 References

The development of HISPEC for Keck and MODHIS for TMT: science cases and predicted sensitivities

HISPEC is a new, high-resolution near-infrared spectrograph being designed for the W.M. Keck II telescope. By offering single-shot, R=100,000 between 0.98 - 2.5 um, HISPEC will enable spectroscopy of transiting and non-transiting exoplanets in close orbits, direct high-contrast detection and spectroscopy of spatially separated substellar companions, and exoplanet dynamical mass and orbit measurements using precision radial velocity monitoring calibrated with a suite of state-of-the-art absolute and relative wavelength references. MODHIS is the counterpart to HISPEC for the Thirty Meter Telescope and is being developed in parallel with similar scientific goals. In this proceeding, we provide a brief overview of the current design of both instruments, and the requirements for the two spectrographs as guided by the scientific goals for each. We then outline the current science case for HISPEC and MODHIS, with focuses on the science enabled for exoplanet discovery and characterization. We also provide updated sensitivity curves for both instruments, in terms of both signal-to-noise ratio and predicted radial velocity precision.Comment: 25 pages, 9 figures. To appear in the Proceedings of SPIE: Techniques and Instrumentation for Detection of Exoplanets XI, vol. 12680 (2023

The development of HISPEC for Keck and MODHIS for TMT: science cases and predicted sensitivities

HISPEC is a new, high-resolution near-infrared spectrograph being designed for the W.M. Keck II telescope. By offering single-shot, R 100,000 spectroscopy between 0.98 – 2.5 µm, HISPEC will enable spectroscopy of transiting and non-transiting exoplanets in close orbits, direct high-contrast detection and spectroscopy of spatially separated substellar companions, and exoplanet dynamical mass and orbit measurements using precision radial velocity monitoring calibrated with a suite of state-of-the-art absolute and relative wavelength references. MODHIS is the counterpart to HISPEC for the Thirty Meter Telescope and is being developed in parallel with similar scientific goals. In this proceeding, we provide a brief overview of the current design of both instruments, and the requirements for the two spectrographs as guided by the scientific goals for each. We then outline the current science case for HISPEC and MODHIS, with focuses on the science enabled for exoplanet discovery and characterization. We also provide updated sensitivity curves for both instruments, in terms of both signal-to-noise ratio and predicted radial velocity precision. © 2023 SPIE.Immediate accessThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]

Detection and Bulk Properties of the HR 8799 Planets with High-resolution Spectroscopy

International audienceUsing the Keck Planet Imager and Characterizer, we obtained high-resolution (R ~ 35,000) K-band spectra of the four planets orbiting HR 8799. We clearly detected H2O and CO in the atmospheres of HR 8799 c, d, and e, and tentatively detected a combination of CO and H2O in b. These are the most challenging directly imaged exoplanets that have been observed at high spectral resolution to date when considering both their angular separations and flux ratios. We developed a forward-modeling framework that allows us to jointly fit the spectra of the planets and the diffracted starlight simultaneously in a likelihood-based approach and obtained posterior probabilities on their effective temperatures, surface gravities, radial velocities, and spins. We measured $v\sin (i)$ values of ${10.1}_{-2.7}^{+2.8}\,\mathrm{km}\,{{\rm{s}}}^{-1}$ for HR 8799 d and ${15.0}_{-2.6}^{+2.3}\,\mathrm{km}\,{{\rm{s}}}^{-1}$ for HR 8799 e, and placed an upper limit of -1 of HR 8799 c. Under two different assumptions of their obliquities, we found tentative evidence that rotation velocity is anticorrelated with companion mass, which could indicate that magnetic braking with a circumplanetary disk at early times is less efficient at spinning down lower-mass planets