188,902 research outputs found
TESS-India Baseline Report 2013: Uttar Pradesh, Madhya Pradesh and Bihar: baseline study of teacher educators, teacher trainees, head teachers, teachers and students
No full textTESS-India is a project funded by UK Aid from the Department for International Development (DFID) and led by The Open University, UK. It aims to address the urgent need to improve the classroom practices of teachers and teacher educators as this is essential for successful educational reform. TESS-India seeks to contribute significantly towards the professional development of teacher educators and teachers in the states of Uttar Pradesh, Bihar, Madhya Pradesh, Odisha, Karnataka, Assam and West Bengal.
The project's goal is to encourage student-centric, active teaching and learning pedagogies at both elementary and secondary school levels across India. TESS-India seeks to do this through use of high-quality Teacher Development Units (TDUs) and Leadership Development Units (LDUs) by teachers and school leaders in their everyday work. However, before launching the project and making the interventions it was necessary to establish a baseline to determine the status of teacher education in the states and to learn about the current situation relating to attitudes and practices of teachers and teacher educators about student-focussed participatory pedagogy and professional development in order to provide a base for comparison with similar data to be collected at different stages in the future.
This report presents the findings of the TESS-India Baseline Study conducted on a sample basis in three project states of Uttar Pradesh (UP), Bihar and Madhya Pradesh (MP) in Sep-Nov 2013
Letter from Tess [Crager?] to Hubert Creekmore (09 July 1953)
No full textTess [Crager?] writes from New Orleans, Louisiana, on Basement Book Shop and Library letterhead to Creekmore in Jackson, Mississippi, regarding his novel, The Chain in the Heart. She praises the novel, states that she will do her best to ensure its success, and discusses business matters. Includes envelope.https://egrove.olemiss.edu/creekmore/1147/thumbnail.jp
TESS first look at evolved compact pulsators. Known ZZ Ceti stars of the southern ecliptic hemisphere as seen by TESS
No full textInternational audienceContext. We present our findings on 18 previously known ZZ Ceti stars observed by the TESS space telescope in 120 s cadence mode during the survey observation of the southern ecliptic hemisphere. Aims: We focus on the frequency analysis of the space-based observations, comparing the results with findings of previous ground-based measurements. The frequencies detected by the TESS observations can serve as inputs for future asteroseismic analyses. Methods: We performed standard pre-whitening of the data sets to derive the possible pulsation frequencies of the different targets. In some cases, we fit Lorentzians to the frequency groups that emerged as the result of short-term amplitude or phase variations that occurred during the TESS observations. Results: We detected more than 40 pulsation frequencies in seven ZZ Ceti stars observed in the 120 s cadence by TESS, with precision better than 0.1 μHz. We found that HE 0532-5605 may be a new outbursting ZZ Ceti. Ten targets do not show any significant pulsation frequencies in their Fourier transforms, due to a combination of their intrinsic faintness and/or crowding on the large TESS pixels. We also detected possible amplitude or phase variations during the TESS observations in some cases. Such behaviour in these targets was not previously identified from ground-based observations
TESS Full Orbital Phase Curve of the WASP-18b System
No full textWe present a visible-light full orbital phase curve of the transiting planet WASP-18b measured by the TESS mission. The phase curve includes the transit, secondary eclipse, and sinusoidal modulations across the orbital phase shaped by the planet's atmospheric characteristics and the star-planet gravitational interaction. We measure the beaming (Doppler boosting) and tidal ellipsoidal distortion phase modulations and show that the amplitudes of both agree with theoretical expectations. We find that the light from the planet's dayside hemisphere occulted during secondary eclipse, with a relative brightness of 341-18 +17 ppm, is dominated by thermal emission, leading to an upper limit on the geometric albedo in the TESS band of 0.048 (2σ). We also detect the phase modulation due to the planet's atmosphere longitudinal brightness distribution. We find that its maximum is well aligned with the substellar point to within 2.°9 (2σ). We do not detect light from the planet's nightside hemisphere, with an upper limit of 43 ppm (2σ), which is 13% of the dayside brightness. The low albedo, lack of atmospheric phase shift, and inefficient heat distribution from the day to night hemispheres that we deduce from our analysis are consistent with theoretical expectations and similar findings for other strongly irradiated gas giant planets. This work demonstrates the potential of TESS data for studying the full orbital phase curves of transiting systems. Finally, we complement our study by looking for transit timing variations (TTVs) in the TESS data combined with previously published transit times, although we do not find a statistically significant TTV signal
Tess DO
No full textTess Do a commencé sa carrière universitaire à l'Université Griffith et à l'Université du Queensland - où elle a terminé ses études postdoctorales - avant de rejoindre le département français à l'Université de Melbourne en 2001. Elle a publié des articles et des chapitres de livres sur Linda Lê, Anna Moï, Thanh -Van Tran-Nhut, Azouz Begag, Béatrix Beck (France), Jean Vanmai (Nouvelle-Calédonie), Le Hoang (réalisateur, Vietnam). Ses recherches actuelles se concentrent sur les genres policiers ..
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The TESS-Keck Survey I: A Warm Sub-Saturn-Mass Planet and a Caution about Stray Light in TESS Cameras
No full textWe report the detection of a Saturn-size exoplanet orbiting HD 332231 (TOI 1456) in light curves from the Transiting Exoplanet Survey Satellite (TESS). HD 332231—an F8 dwarf star with a V-band magnitude of 8.56—was observed by TESS in Sectors 14 and 15. We detect a single-transit event in the Sector 15 presearch data conditioning (PDC) light curve. We obtain spectroscopic follow-up observations of HD 332231 with the Automated Planet Finder, Keck I, and SONG telescopes. The orbital period we infer from radial velocity (RV) observations leads to the discovery of another transit in Sector 14 that was masked by PDC due to scattered light contamination. A joint analysis of the transit and RV data confirms the planetary nature of HD 332231 b, a Saturn-size (0.867^(+0.027)_(−0.025) R_J), sub-Saturn-mass (0.244±0.021M_J) exoplanet on a 18.71 day circular orbit. The low surface gravity of HD 332231 b and the relatively low stellar flux it receives make it a compelling target for transmission spectroscopy. Also, the stellar obliquity is likely measurable via the Rossiter–McLaughlin effect, an exciting prospect given the 0.14 au orbital separation of HD 332231 b. The spectroscopic observations do not provide substantial evidence for any additional planets in the HD 332231 system, but continued RV monitoring is needed to further characterize this system. We also predict that the frequency and duration of masked data in the PDC light curves for TESS Sectors 14–16 could hide transits of some exoplanets with orbital periods between 10.5 and 17.5 days
Uncovering Dwarf AGN With TESS
No full textWe present the results of a systematic search for AGN in TESS light curves of dwarf galaxies. Evidence of short-term flux changes in dwarf galaxies can reveal an AGN even when emission line ratios fail to do so. Studies of dwarf AGN are essential for a general understanding of the relationship between black hole and galaxy evolution. The timescale from the commonly-used damped random walk model has been shown to correlate with black hole mass, but further studies are required to understand the physical processes driving this empirical model’s effectiveness. Partially because of this timescale relation, TESS is a unique tool for the identification of dwarf AGN; a light curve from a single sector can reveal adequate variability. We demonstrate a successful methodology that accounts for TESS systematics and contamination by variable stars. The newly-identified AGN help populate scaling relations at the low-mass end and demonstrate the crucial role of TESS in studies of dwarf AGN and AGN in general
The near-core rotation of HD 112429: a gamma Doradus star with TESS photometry and legacy spectroscopy
No full textThe TESS space mission provides us with high-precision photometric
observations of bright stars over more than 70% of the entire sky, allowing us
to revisit and characterise well-known stars. We aim to conduct an
asteroseismic analysis of the gamma Doradus star HD112429 using both the
available ground-based spectroscopy and TESS photometry, and assess the
conditions required to measure the near-core rotation rate and buoyancy travel
time. We collect and reduce the available five sectors of short-cadence TESS
photometry of this star, as well as 672 legacy observations from six medium- to
high-resolution ground-based spectrographs. We determine the stellar pulsation
frequencies from both data sets using iterative prewhitening, do asymptotic g
mode modelling of the star and investigate the corresponding spectral line
profile variations using the pixel-by-pixel method. We validate the pulsation
frequencies from the TESS data up to , confirming recent reports
in the literature that the classical criterion does not suffice
for space-based observations. We identify the pulsations as prograde dipole g
modes and r-mode pulsations, and measure a near-core rotation rate of and a buoyancy travel time of 4190(50) s. These results are in
agreement with the observed spectral line profile variations, which were
qualitatively evaluated using a newly developed toy model. We establish a set
of conditions that have to be fulfilled for an asymptotic asteroseismic
analysis of g-mode pulsators. In the case of HD112429, two TESS sectors of
space photometry suffice. Although a detailed asteroseismic modelling analysis
is not viable for g-mode pulsators with only short or sparse light curves of
space photometry, we find that it is possible to determine global asteroseismic
quantities for a subset of these stars. (abbreviated.)Comment: 15 pages, 13 figures, 4 tables. Accepted for publication in Astronomy
and Astrophysic
POR FORA DO PRÉ-MODERNISMO
No full textResumo:Este artigo propõe uma reflexão sobre a atuação intelectual do escritor Gustavo Barroso (1888-1959) e de sua relação com o Pré-modernismo brasileiro, considerando categorias como capital cultural e pessoal, conforme Pierre Bourdieu, e que demonstram de que modo o autor se coloca à margem do período, sem ser excluído propriamente.Palavras-chave: Pré-modernismo. Gustavo Barroso. Capital pessoal.Abstract: This article is a reflection about the intellectual activity of writer Gustavo Barroso (1888-1959) and his relationship with Brazilian Pre-modernism, considering categories such as personal and cultural capital, as in Bourdieu, showing how the author was marginalized in the period without being totally excluded.Keywords: Pre-modernism. Gustavo Barroso. Personal capital
TESS Giants Transiting Giants. II. The Hottest Jupiters Orbiting Evolved Stars
No full textsponsorship: We thank Howard Isaacson and Daniel Foreman-Mackey for helpful discussions. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. S.G., N.S., and D.H. acknowledge support by the National Aeronautics and Space Administration under grant 80NSSC19K0593 issued through the TESS Guest Investigator Program. D.H. acknowledges support from the Alfred P. Sloan Foundation and the National Aeronautics and Space Administration (80NSSC21K0652), and the National Science Foundation (80NSSC21K0652). N.S., A.C., and M.R. acknowledge support from the National Science Foundation through the Graduate Research Fellowship Program under grants 1842402 and DGE-1752134. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. M.S. acknowledges funding support from NSF ACI-1663696 and AST-1716436. T.D.K. acknowledges support from the 51 Pegasi b fellowship in Planetary Astronomy sponsored by the Heising-Simons Foundation. P.D. is supported by a National Science Foundation (NSF) Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1903811. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Funding for the TESS mission is provided by NASA's Science Mission Directorate. (NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center, W. M. Keck Foundation, National Aeronautics and Space Administration|80NSSC19K0593, National Aeronautics and Space Administration|80NSSC21K0652, Alfred P. Sloan Foundation, National Science Foundation|80NSSC21K0652, National Science Foundation|1842402, National Science Foundation|DGE-1752134, NSF|ACI-1663696, NSF|AST-1716436, 51 Pegasi b fellowship in Planetary Astronomy - Heising-Simons Foundation, National Science Foundation (NSF) Astronomy and Astrophysics Postdoctoral Fellowship|AST-1903811, National Aeronautics and Space Administration)status: Publishe
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