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17,997 results on '"Frye"'

1. Intermediate Vision Following Monofocal IOL Implantation

Author

Agarwal S, Thornell E, and Frye SN

Subjects
clareon, monofocal iol, visual performance, intermediate visual acuity, spectacle independence, Ophthalmology, RE1-994
Abstract

Smita Agarwal,1,2 Erin Thornell,1 Sara Nadege Frye3 1Wollongong Eye Specialists, Wollongong, NSW, Australia; 2Graduate School of Medicine, University of Wollongong, Wollongong, NSW, Australia; 3Clinical Development & Medical Affairs, Alcon, Fort Worth, TX, USACorrespondence: Smita Agarwal, Wollongong Eye Specialists, Level 2, 2 Victoria St, Wollongong, NSW, Australia, Tel +61 2 42630500, Email smitaagarwal@hotmail.comPurpose: While providing exceptional distance visual outcomes, intermediate vision achieved with monofocal IOLs has not been thoroughly investigated.Patients and Methods: A total of 63 eyes from 52 patients (average age 73.48± 6.8 years, 56% female) were included for analysis following implantation of the Clareon and Clareon Toric monofocal intraocular IOL with AutonoMe (CNA0T0 or CNA0T2-T6) for the treatment of cataract or refractive error. Visual and refractive outcomes including uncorrected distance, intermediate and near visual acuity, distance-corrected intermediate and near visual acuity, manifest refraction and defocus were first assessed at 4– 6 weeks and then again at 12 weeks following surgery. Patient satisfaction was assessed using a modification of the IOLSAT questionnaire and subjective visual quality was assessed using a modified version of the QUVID questionnaire.Results: Average postoperative spherical equivalent (SE) was − 0.17± 0.40 D, with 82% and 96% of eyes achieving within ± 0.5 D and ± 1.0 D of the refractive SE target, respectively. Average monocular uncorrected distance visual acuity (UDVA) and uncorrected intermediate visual acuity (UIVA) were 0.03± 0.10 and 0.35± 0.13 LogMAR. Postoperative UIVA improved with more myopic SE (P < 0.0001) and spherical refractive error (P < 0.0001). Bilaterally implanted patients had higher spectacle independence for intermediate tasks compared to unilateral patients (51.1% versus 31.2% respectively).Conclusion: The Clareon monofocal IOL provided excellent distance vision with a majority of patients achieving spectacle independence for intermediate tasks. While the IOL likely contributed to these visual outcomes, surgeons can also adjust refractive targets to help achieve better intermediate vision postoperatively.Keywords: Clareon, monofocal IOL, visual performance, intermediate visual acuity, spectacle Independence

Published
2025

2. Child-directed Speech in Qaqet

Author

Frye, Henrike

Subjects
Qaqet, language, East New Britain, Papua New Guinea, child‑directed speech, Linguistics, Historical and comparative linguistics
Abstract

Qaqet is a non-Austronesian language, spoken by about 15,000 people in East New Britain, Papua New Guinea. In the remote inland, children acquire Qaqet as their first language. Much of what we know about child‑directed speech (CDS) stems from children living in middle‑class, urban, industrialised contexts. This book combines evidence from different methods, showing that the features typical for speech to children in such contexts are also found in Qaqet CDS. Preliminary insights from naturalistic audio recordings suggest that Qaqet children are infrequently addressed directly. In interviews, Qaqet caregivers express the view that children 'pick up' the language on their own. Still, they have clear ideas about how to talk to children in a way that makes it easier for them to understand what is said. In order to compare adult- and child-directed speech in Qaqet, 20 retellings of a film have been analysed, half of them told to adults and half to children. The data show that talk directed to children differs from talk directed to adults for several features, among them utterance type, mean length of utterance, amount of hesitations and intonation. Despite this clear tendency, there seems to be a cut-off point of around 40 months of age for several of those features from which the talk directed to children becomes more like the talk directed to adults.

Published
2022
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3. Explaining JWST counts with galaxy formation models

Author

Manzoni, Giorgio, Broadhurst, Tom, Lim, Jeremy, Liu, Tao, Smoot, George, Baugh, Carlton M., Tompkins, Scott, Windhorst, Rogier, Driver, Simon, Carleton, Timothy, Frye, Brenda, Fung, Leo, Zhang, Jiashuo, Cohen, Seth H., Conselice, Christopher J., Grogin, Norman A., Jansen, Rolf A., Koekemoer, Anton M., Ortiz III, Rafael, Pirzkal, Norbert, and Willmer, Christopher N. A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

A distinct power-law break is apparent m_AB approximately 21 in the deep Near-Infrared PEARLS-JWST galaxy counts. The break becomes more pronounced at longer wavelengths, with the counts slope flattening smoothly with apparent magnitude in the shortest band used at 0.9 microns, trending towards an increasingly broken slope by the longest wavelength passband of JWST NIRCam, 4.4 microns. This behaviour is remarkably well predicted by the GALFORM semi-analytical model of galaxy formation. We use the model to diagnose the origin of this behaviour. We find that the features that are responsible for the break are: 1) the inherent break in the luminosity function; 2) the change in the volume element with redshift and 3) the redshift-dependent nature of the k-correction. We study the contribution to these effects by early and late-type galaxies, using as a proxy for morphology the bulge-to-total stellar mass ratio. We find that the way in which ellipticals populate the bright end of the luminosity function while spirals dominate the faint end is preserved in the galaxy number counts, with a characteristic stellar mass at the break of approximately 10^10 M_sun. We also find that the shape of the number counts is mainly driven by galaxies with relatively low redshift (z < 2) for the PEARLS observational limit of m_AB < 28. We give a comprehensive description of why the galaxy number counts in the near-infrared PEARLS-JWST observation look the way they do and which population of galaxies is dominant at each apparent magnitude.

Published
2025

4. EPOCHS XI: The Structure and Morphology of Galaxies in the Epoch of Reionization to z ~ 12.5

Author

Westcott, Lewi, Conselice, Christopher J., Harvey, Thomas, Austin, Duncan, Adams, Nathan, Ferrari, Fabricio, Ferreira, Leonardo, Trussler, James, Li, Qiong, Rusakov, Vadim, Duan, Qiao, Harris, Honor, Goolsby, Caio, Broadhurst, Thomas J., Coe, Dan, Cohen, Seth H., Driver, Simon P., D'Silva, Jordan C. J., Frye, Brenda, Grogin, Norman A., Hathi, Nimish P., Jansen, Rolf A., Koekemoer, Anton M., Marshall, Madeline A., Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan Jr., Russell E., Summers, Jake, Willmer, Christopher N. A., Windhorst, Rogier A., and Yan, Haojing

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a structural analysis of 521 galaxy candidates at 6.5 < z < 12.5, with $SNR > 10\sigma$ in the F444W filter, taken from the EPOCHS v1 sample, consisting of uniformly reduced deep JWST NIRCam data, covering the CEERS, JADES GOOD-S, NGDEEP, SMACS0723, GLASS and PEARLS surveys. We use standard software to fit single S\'ersic models to each galaxy in the rest-frame optical and extract their parametric structural parameters (S\'ersic index, half-light radius and axis-ratio), and \texttt{Morfometryka} to measure their non-parametric concentration and asymmetry parameters. We find a wide range of sizes for these early galaxies, but with a strong galaxy-size mass correlation up to $z \sim 12$ such that galaxy sizes continue to get progressively smaller in the high-redshift regime, following $R_{e} = 2.74 \pm 0.49 \left( 1 + z \right) ^{-0.79 \pm 0.08}$ kpc. Using non-parametric methods we find that galaxy merger fractions, classified through asymmetry parameters, at these redshifts remain consistent with those in literature, maintaining a value of $f_{m} \sim 0.12 \pm 0.07$ showing little dependence with redshift when combined with literature at $z > 4$. We find that galaxies which are smaller in size also appear rounder, with an excess of high axis-ratio objects. Finally, we artificially redshift a subsample of our objects to determine how robust the observational trends we see are, determining that observed trends are due to real evolutionary effects, rather than being a consequence of redshift effects., Comment: 35 pages, 13 figures. Submitted to ApJ on 19/12/2024. Comments to corresponding author welcome at lewi.westcott@manchester.ac.uk

Published
2024

5. Cosmic Stillness: High Quiescent Galaxy Fractions Across Upper Mass Scales in the Early Universe to z = 7 with JWST

Author

Russell, Tobias A., Dobric, Neva, Adams, Nathan J., Conselice, Christopher J., Austin, Duncan, Harvey, Thomas, Trussler, James, Ferreira, Leonardo, Westcott, Lewi, Harris, Honor, Windhorst, Rogier A., Coe, Dan, Cohen, Seth H., Driver, Simon P., Frye, Brenda, Grogin, Norman A., Hathi, Nimish P., Jansen, Rolf A., Koekemoer, Anton M., Marshall, Madeline A., Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan Jr, Russell E., Summers, Jake, D'Silva, Jordan C. J., Willmer, Christopher N. A., and Yan, Haojing

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a detailed investigation into the abundance and morphology of high redshift quenched galaxies at $3 < z < 7$ using James Webb Space Telescope data in the NEP, CEERS and JADES fields. Within these fields, we identify 90 candidate passive galaxies using specific star formation rates modelled with the BAGPIPES SED fitting code, which is more effective at identifying recently quenched systems than the classical UVJ method. With this sample of galaxies, we find number densities broadly consistent with other works and a rapidly evolving passive fraction of high mass galaxies ($\log_{10}{(M_{\star}/M_{\odot})} > $ 9.5) between $3 < z < 5$. We find that the fraction of galaxies with low star formation rates and mass 9.5 $ < \log_{10}{(M_{\star}/M_{\odot})} < $ 10.5 decreases from $\sim$25% at $3 < z < 4$ to $\sim$2% at $5 < z < 7$. Our passive sample of galaxies is shown to exhibit more compact light profiles compared to star-forming counterparts and some exhibit traces of AGN activity through detections in either the X-ray or radio. At the highest redshifts ($z > 6.5$) passive selections start to include examples of 'little red dots' which complicates any conclusions until their nature is better understood., Comment: 24 pages, 5 tables, 11 figures, submitted to MNRAS

Published
2024

6. Language hooks: a modular framework for augmenting LLM reasoning that decouples tool usage from the model and its prompt

Author

de Mijolla, Damien, Yang, Wen, Duckett, Philippa, Frye, Christopher, and Worrall, Mark

Subjects
Computer Science - Computation and Language, Computer Science - Artificial Intelligence, Computer Science - Machine Learning
Abstract

Prompting and fine-tuning have emerged as two competing paradigms for augmenting language models with new capabilities, such as the use of tools. Prompting approaches are quick to set up but rely on providing explicit demonstrations of each tool's usage in the model's prompt, thus coupling tool use to the task at hand and limiting generalisation. Fine-tuning removes the need for task-specific demonstrations of tool usage at runtime; however, this ties new capabilities to a single model, thus making already-heavier setup costs a recurring expense. In this paper, we introduce language hooks, a novel framework for augmenting language models with new capabilities that is decoupled both from the model's task-specific prompt and from the model itself. The language hook algorithm interleaves text generation by the base model with the execution of modular programs that trigger conditionally based on the existing text and the available capabilities. Upon triggering, programs may call external tools, auxiliary language models (e.g. using tool specific prompts), and modify the existing context. We benchmark our method against state-of-the-art baselines, find that it outperforms task-aware approaches, and demonstrate its ability to generalise to novel tasks., Comment: This work was conducted during Summer 2023. Experimental results and references reflect the state of the field at that time and may not account for subsequent developments

Published
2024

8. Identification of more than 40 gravitationally magnified stars in a galaxy at redshift 0.725

Author

Fudamoto, Yoshinobu, Sun, Fengwu, Diego, Jose M, Dai, Liang, Oguri, Masamune, Zitrin, Adi, Zackrisson, Erik, Jauzac, Mathilde, Lagattuta, David J, Egami, Eiichi, Iani, Edoardo, Windhorst, Rogier A, Abe, Katsuya T, Bauer, Franz Erik, Bian, Fuyan, Bhatawdekar, Rachana, Broadhurst, Thomas J, Cai, Zheng, Chen, Chian-Chou, Chen, Wenlei, Cohen, Seth H, Conselice, Christopher J, Espada, Daniel, Foo, Nicholas, Frye, Brenda L, Fujimoto, Seiji, Furtak, Lukas J, Golubchik, Miriam, Hsiao, Tiger Yu-Yang, Jolly, Jean-Baptiste, Kawai, Hiroki, Kelly, Patrick L, Koekemoer, Anton M, Kohno, Kotaro, Kokorev, Vasily, Li, Mingyu, Li, Zihao, Lin, Xiaojing, Magdis, Georgios E, Meena, Ashish K, Niemiec, Anna, Nabizadeh, Armin, Richard, Johan, Steinhardt, Charles L, Wu, Yunjing, Zhu, Yongda, and Zou, Siwei

Subjects
Astronomical Sciences, Physical Sciences, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

Strong gravitational magnification enables the detection of faint background sources and allows researchers to resolve their internal structures and even identify individual stars in distant galaxies. Highly magnified individual stars are useful in various applications, including studies of stellar populations in distant galaxies and constraining dark matter structures in the lensing plane. However, these applications have been hampered by the small number of individual stars observed, as typically one or a few stars are identified from each distant galaxy. Here, we report the discovery of more than 40 microlensed stars in a single galaxy behind Abell 370 at redshift of 0.725 (dubbed ‘the Dragon arc’) when the Universe was half of its current age, using James Webb Space Telescope observations with the time-domain technique. These events were found near the expected lensing critical curves, suggesting that these are magnified stars that appear as transients from intracluster stellar microlenses. Through multi-wavelength photometry, we constrained their stellar types and found that many of them are consistent with red giants or supergiants magnified by factors of hundreds. This finding reveals a high occurrence of microlensing events in the Dragon arc and demonstrates that time-domain observations by the James Webb Space Telescope could lead to the possibility of conducting statistical studies of high-redshift stars.

Published
2025

9. Galaxy Mergers in the Epoch of Reionization II: Major Merger-Triggered Star Formation and AGN Activities at $z =$ 4.5-8.5

Author

Duan, Qiao, Li, Qiong, Conselice, Christopher J., Harvey, Thomas, Austin, Duncan, Adams, Nathan J., Ferreira, Leonardo, Duncan, Kenneth J., Trussler, James, Pascalau, Robert G., Windhorst, Rogier A., Holwerda, Benne W., Broadhurst, Thomas J., Coe, Dan, Cohen, Seth H., Du, Xiaojing, Driver, Simon P., Frye, Brenda, Grogin, Norman A., Hathi, Nimish P., Jansen, Rolf A., Koekemoer, Anton M., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan Jr, Russell E., Summers, Jake, D'Silva, Jordan C. J., Willmer, Christopher N. A., and Yan, Haojing

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Galaxy mergers are a key driver of galaxy formation and evolution, including the triggering of AGN and star formation to a still unknown degree. We thus investigate the impact of galaxy mergers on star formation and AGN activity using a sample of 3,330 galaxies at $z = [4.5, 8.5]$ from eight JWST fields (CEERS, JADES GOODS-S, NEP-TDF, NGDEEP, GLASS, El-Gordo, SMACS-0723, and MACS-0416), collectively covering an unmasked area of 189 arcmin$^2$. We focuses on star formation rate (SFR) enhancement, AGN fraction, and AGN excess in major merger ($\mu > 1/4$) close-pair samples, defined by $\Delta z < 0.3$ and projected separations $r_p < 100$ kpc, compared to non-merger samples. We find that SFR enhancement occurs only at $r_p < 20$ kpc, with values of $0.25 \pm 0.10$ dex and $0.26 \pm 0.11$ dex above the non-merger medians for $z = [4.5, 6.5]$ and $z = [6.5, 8.5]$. No other statistically significant enhancements in galaxy sSFR or stellar mass are observed at any projected separation or redshift bin. We also compare our observational results with predictions from the SC-SAM simulation and find no evidence of star formation enhancement in the simulations at any separation range. Finally, we examine the AGN fraction and AGN excess, finding that the fraction of AGNs in AGN-galaxy pairs, relative to the total AGN population, is $3.25^{+1.50}_{-1.06}$ times greater than the fraction of galaxy pairs relative to the overall galaxy population at the same redshift. We find that nearly all AGNs have a companion within 100 kpc and observe an excess AGN fraction in close-pair samples compared to non-merger samples. This excess is found to be $1.26 \pm 0.06$ and $1.34 \pm 0.06$ for AGNs identified via the inferred BPT diagram and photometric SED selection, respectively., Comment: 17 Pages, 7 Figures, Submitted to MNRAS

Published
2024

10. The Tale of Two Telescopes: How Hubble Uniquely Complements the James Webb Space Telescope: Galaxies

Author

Windhorst, Rogier A., Summers, Jake, Carleton, Timothy, Cohen, Seth H., Croker, Kevin S., Jansen, Rolf A., O'Brien, Rosalia, Smith, Brent M., Conselice, Christopher J., Diego, Jose M., Driver, Simon P., Frye, Brenda, and Yan, Haojing

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

In this paper, we present a simple but compelling argument, focusing on galaxy science, for preserving the main imagers and operational modes of the Hubble Space Telescope (HST) for as long as is technically feasible. While star-formation started at redshifts z$\gtrsim$10$-$13, when the universe was less than 300$-$500 Myr old, the CSFH did not peak until z$\simeq$1.9, and has steadily declined since that time. Hence, at least half of all stars in the universe formed in the era where HST provides its unique rest-frame UV view of unobscured young, massive stars tracing cosmic star-formation. By rendering a subset of the 556.3 hours of available HST images in 12 filters of the Hubble Ultra Deep Field (HUDF) in an appropriate mix of colors, we illustrate the unique capabilities of HST for galaxy science emphasizing that rest-frame UV$-$optical wavelength range. We then contrast this with the 52.7 publicly available hours of JWST/NIRCam images in 8 filters of the same HUDF area from the JADES project, rendering these at the redder near-IR wavelengths to illustrate the unique capabilities of JWST to detect older stellar populations at higher redshifts, as well as very dusty stellar populations and Active Galactic Nuclei (AGN). HST uniquely probes (unobscured) young, hot, massive stars in galaxies, while JWST reveals more advanced stages of older stellar populations, as well as relatively short-lived phases where galaxies produce and shed a lot of dust from intense star-formation, and the very high redshift universe (z$\gtrsim$10$-$11) not accessible by HST. We conclude that HST and JWST are highly complementary facilities that took decades to build to ensure decades of operation. To maximize return on investment on both HST and JWST, ways will need to be found to operate HST imaging instruments in all relevant modes for as long as possible into the JWST mission., Comment: White paper submitted to NASA/STScI for the HST Senior Review of 2024. The HST+JWST PDF images are too big for astro-ph. Please view their full resolution PDF files on: http://www.asu.edu/clas/hst/www/jwst2024/windhorst_HST_SeniorReview2024_v4.pdf

Published
2024

11. Personalized Speech Emotion Recognition in Human-Robot Interaction using Vision Transformers

Author

Mishra, Ruchik, Frye, Andrew, Rayguru, Madan Mohan, and Popa, Dan O.

Subjects
Electrical Engineering and Systems Science - Audio and Speech Processing, Computer Science - Human-Computer Interaction, Computer Science - Robotics, Computer Science - Sound
Abstract

Emotions are an essential element in verbal communication, so understanding individuals' affect during a human-robot interaction (HRI) becomes imperative. This paper investigates the application of vision transformer models, namely ViT (Vision Transformers) and BEiT (BERT Pre-Training of Image Transformers) pipelines, for Speech Emotion Recognition (SER) in HRI. The focus is to generalize the SER models for individual speech characteristics by fine-tuning these models on benchmark datasets and exploiting ensemble methods. For this purpose, we collected audio data from different human subjects having pseudo-naturalistic conversations with the NAO robot. We then fine-tuned our ViT and BEiT-based models and tested these models on unseen speech samples from the participants. In the results, we show that fine-tuning vision transformers on benchmark datasets and and then using either these already fine-tuned models or ensembling ViT/BEiT models gets us the highest classification accuracies per individual when it comes to identifying four primary emotions from their speech: neutral, happy, sad, and angry, as compared to fine-tuning vanilla-ViTs or BEiTs., Comment: Submitted to IEEE for possible publication

Published
2024

12. Mass & Light in Galaxy Clusters: The case of Abell 370

Author

Limousin, M., Niemiec, A., Beauchesne, B., Diego, J., Jauzac, M., Koekemoer, A., Sharon, K., Acebron, A., Lagattuta, D., Mahler, G., Williams, L., Richard, J., Jullo, E., Furtak, L., Faisst, A., Frye, B., Hibon, P., Natarajan, P., and Rich, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Parametric strong lensing studies of galaxy clusters often display "misleading features". This is the case in the galaxy cluster Abell 370. Using strong lensing techniques, it has been described parametrically by a four dark matter clumps model and galaxy scale perturbers, as well as a significant external shear component, which physical origin remains a challenge. The dark matter distribution features a mass clump with no stellar counterpart and a significant offset between one of the dark matter clumps and its associated stellar counterpart. In this paper, based on BUFFALO data, we begin by revisiting this mass model. We find a four dark matter clumps solution which does not require any external shear and provides a slightly better RMS compared to previous models. Investigating further this new solution, we present a class of models which can accurately reproduce the strong lensing data, but whose parameters for the dark matter component are poorly constrained. We then develop a model where each large scale dark matter component must be associated with a stellar counterpart. This model is unable to reproduce the observational constraints with an RMS smaller than 2.3", and the parameters describing this dark matter component remain poorly constrained. Examining the total projected mass maps, we find a good agreement between the total mass and the stellar distribution, both being bimodal. We interpret the "misleading features" of the four dark matter clumps mass model and the failure of the three dark matter clumps mass model as being symptomatic of the lack of realism of a parametric description of the dark matter distribution, and encourage caution and criticism on the outputs of parametric strong lensing modelling. We briefly discuss the implications of our results for using Abell 370 as a gravitational telescope., Comment: Abstract largely abridged - A&A accepted on 25/10/2024

Published
2024
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13. Assessment of a Single Intra-Articular Stifle Injection of Pure Platelet Rich Plasma on Symmetry Indices in Dogs with Unilateral or Bilateral Stifle Osteoarthritis from Long-Term Medically Managed Cranial Cruciate Ligament Disease

Author

Venator KP, Frye CW, Gamble LJ, and Wakshlag JJ

Subjects
platelet, stifle, canine, osteoarthritis and cruciate, Veterinary medicine, SF600-1100
Abstract

Kurt P Venator,* Christopher W Frye,* Lauri-Jo Gamble, Joseph J Wakshlag Department of Clinical Sciences, Cornell University College of Veterinary Medicine, Ithaca, NY 14853, USA*These authors contributed equally to this workCorrespondence: Joseph J WakshlagCornell University College of Veterinary Medicine, Vet. Med. Center C2-008, Ithaca, NY 14853, USATel +1 607 351 6545Email dr.joesh@gmail.comPurpose: The use of platelet-rich plasma (PRP) to treat canine osteoarthritis has gained support within the scientific community. PRP effects on pain control for degenerative joint disease induced by naturally occurring cranial cruciate ligament instability are limited, particularly in a cohort of dogs with chronic instability and osteoarthritis (> 12 months), representing a commonly encountered clinical population that often defaults to medical management. The goal of this study was to assess the effects of a single intra-articular PRP injection into an effected stifle in this cohort, to assess response to treatment, quantitative kinetic data as it relates to percent body weight for peak vertical force (PVF) and vertical impulse (VI) were collected, and symmetry indices related to PVF were determined.Methods: Twelve dogs with unilateral or bilateral osteoarthritis with ruptured, non-stabilized cranial cruciate ligaments over 12 months duration were identified. Unilateral injections of 2.5 mL of a PRP preparation into the most severely affected stifle based on kinetic analysis was performed. Repeat pressure-sensitive walkway analysis was conducted monthly for 3 months. Peak vertical force (PVF) and vertical impulse (VI) were normalized to body weight and identified in all four limbs. Previously published symmetry indices regarding PVF were calculated, comparing the treated limb with the contralateral limb, ipsilateral forelimb, and contralateral forelimb.Results: After treatment, hind limb symmetry index (SI) regarding PVF showed improved symmetry, suggesting more weight placement at all-time points after injection of the most affected limb (p < 0.01). Further, PVF asymmetry indices assessing contralateral fore (CFL) and hind limb (CHL) as well as ipsilateral forelimb (IFL) revealing a significant decrease from baseline for CHL at week 4 (p = 0.02), but not weeks 8 and 12. The CFL showed decreased differences in symmetry from baseline at each time point (p = 0.03). There were no statistically significant changes in PVF or VI over time in treated dogs.Conclusion: A single injection of PRP improved kinetics for minimally 4 weeks with some data suggesting an effect for up to 12 weeks. Therefore, PRP might be a viable therapeutic option for instability and inflammation associated with chronic osteoarthritis due to cranial cruciate ligament disease in the non-surgical patient.Keywords: platelet, stifle, canine, osteoarthritis and cruciate

Published
2020

14. Occupational Therapy Practitioners' Expectations of Entry-Level Doctorate versus Master's Graduates

Author

Monique C. Chabot, Sara Kate Frye, Nakia Lynn, Kristy Meyer, LaRonda Lockhart-Keene, Lydia Navarro-Walker, Susan M. Persia, Wendy Watcher-Schutz, Kevin Wegner, Michelle Gorenberg, and Catherine Goodman

Abstract

The dual-entry nature of occupational therapy has been a point of discussion for many years with explorations into the profession's support for the different degree programs and definitions of entry-level practice being the primary foci in the literature. There has been no comparison of the expectations of occupational therapy educators and practitioners of entry-level doctorate and master's students upon graduation despite differences in curricula and emphasis on advanced skills. This study utilized a descriptive quantitative survey to ask current educators and practitioners (n=124) to indicate their level of expectations of the two types of graduates for sixteen different clinical and professional skills and the level of expected mentorship upon graduation. Practitioners held the two groups of new graduates to the same expectations in all categories and anticipated they would need the same level of mentorship upon graduation. Despite equal expectations in all categories, there were six categories where at least 30% of participants indicated they held higher expectations of entry-level doctorate new graduates. These categories aligned with the doctoral capstone areas of foci. These results can set the foundation for further studies examining the congruence between expectations and new graduate readiness for the field and inform current curricula to prepare students to meet the professional expectations of their supervisors and colleagues.

Published
2024

15. Anatomy of a z=6 Lyman-{\alpha} emitter down to parsec scales: extreme UV slopes, metal-poor regions and possibly leaking star clusters

Author

Messa, Matteo, Vanzella, E., Loiacono, F., Bergamini, P., Castellano, M., Sun, B., Willott, C., Windhorst, R. A., Yan, H., Angora, G., Rosati, P., Adamo, A., Annibali, F., Bolamperti, A., Bradač, M., Bradley, L. D., Calura, F., Claeyssens, A., Comastri, A., Conselice, C. J., D'Silva, J. C. J., Dickinson, M., Frye, B. L., Grillo, C., Grogin, N. A., Gruppioni, C., Koekemoer, A. M., Meneghetti, M., Meštrić, U., Pascale, R., Ravindranath, S., Ricotti, M., Summers, J., and Zanella, A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a detailed JWST/NIRSpec and NIRCam analysis of a gravitationally-lensed galaxy ($\rm \mu=17-21$) at redshift 6.14 magnified by the Hubble Frontier Field galaxy cluster MACS J0416. The target galaxy is overall a typical compact and UV-faint ($\rm M_{UV}=-17.8$) Lyman-$\alpha$ emitter, yet the large magnification allows the detailed characterization of structures on sub-galactic scales (down to a few parsecs). Prominent optical $\rm H\alpha$, $\rm H\beta$ and [OIII]$\lambda\lambda4959,5007$ lines are spatially resolved with the high spectral resolution grating (G395H, R~2700), with large equivalent widths, EW($\rm H\beta$+[OIII])$\gtrsim1000$ \AA, and elevated ionising photon production efficiencies $\rm log(\xi_{ion}/erg^{-1}Hz)=25.2-25.7$. NIRCam deep imaging reveals the presence of compact rest-UV bright regions along with individual star clusters of $\rm R_{eff}=3-8~pc$ in size and $\rm M\sim2\cdot10^5-5\cdot10^{6}~M_\odot$ in mass. These clusters are characterised by steep UV slopes, $\rm\beta_{UV}\lesssim-2.5$, which in some cases are associated with a dearth of line emission, indicating possible leaking of the ionizing radiation, as also supported by a Lyman-$\rm \alpha$ emission peaking at $\rm \sim100~km~s^{-1}$ from the systemic redshift. While the entire system is characterised by low-metallicity, $\sim0.1~Z_\odot$, the NIRSpec-IFU map also reveals the presence of a low-luminosity, metal-poor region with $\rm Z\lesssim2\%~Z_\odot$, barely detected in NIRCam imaging; this region is displaced by $\rm >200~pc$ from one of the brightest structures of the system in UV, and would have been too faint to detect if not for the large magnification of the system., Comment: 18 pages (11 figures) + appendix (6 pages, 6 figures, 2 tables). Published in A&A

Published
2024
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16. Extreme Ionizing Properties of Metal-Poor, Muv ~ -12 Star Complex in the first Gyr

Author

Vanzella, E., Loiacono, F., Messa, M., Castellano, M., Bergamini, P., Zanella, A., Annibali, F., Sun, B., Dickinson, M., Adamo, A., Calura, F., Ricotti, M., Rosati, P., Meneghetti, M., Grillo, C., Bradac, M., Conselice, C. J., Yan, H., Bolamperti, A., Mestric, U., Gilli, R., Gronke, M., Willott, C., Sani, E., Acebron, A., Comastri, A., Mignoli, M., Gruppioni, C., Mercurio, A., Strait, V., Pascale, R., Annunziatella, M., Frye, B. L., Bradley, L. D., Grogin, N. A., Koekemoer, A. M., Ravindranath, S., D'Silva, J. C. J., Summers, J., Rihtar, G., and Windhorst, R.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We report the serendipitous discovery of a faint (M_UV > -12.2), low-metallicity (Z ~ 0.02 Zsun), ionizing source (dubbed T2c) with a spectroscopic redshift of z=6.146. T2c is part of a larger structure amplified by the Hubble Frontier Field galaxy cluster MACSJ0416, and was observed with JWST/NIRSpec IFU. Stacking the short-wavelength NIRCam data reveals no stellar continuum detection down to a magnitude limit of m_UV ~ 31.0 (3 sigma). However, prominent Hb, [OIII]4959,5007, and Ha emissions are detected, with equivalent widths exceeding 200A, 800A, and 1300A (3 sigma), respectively. The corresponding intrinsic (magnification-corrected x23 +/- 3) ultraviolet and optical rest-frame magnitudes exceed 34.4 and 33.9 (corresponding to M_uv and M_opt fainter than -12.2 and -12.8, at lambda_rest ~ 2000A and ~5000A, respectively), suggesting a stellar mass lower than a few 10^4 Msun under an instantaneous burst scenario. The inferred ionizing photon production efficiency (xi_ion) is high, xi_ion >~ 26.08(25.86) 3(5)sigma, assuming no dust attenuation and no Lyman continuum leakage, indicating the presence of massive stars despite the low mass of the object. The very poor sampling of the initial mass function at such low mass star-forming complex suggests that the formation of very massive stars might be favored in very low metallicity environments. T2c is surrounded by Balmer and weak oxygen emission on a spatial scale of a few hundred parsecs after correcting for lensing effects. This system resembles an HII region potentially powered by currently undetected, extremely efficient, low-metallicity star complexes or clusters. We propose that massive O-type stars populate this low-mass and metallicity high-redshift satellites, likely caught in an early and short formation phase, contributing to the ionization of the surrounding medium., Comment: 9 pages, 5 figures, 1 table. Submitted to A&A. Comments are welcome

Published
2024
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17. Spectroscopic analysis of the strongly lensed SN~Encore: Constraints on cosmic evolution of Type Ia supernovae

Author

Dhawan, S., Pierel, J. D. R., Gu, M., Newman, A. B., Larison, C., Siebert, M., Petrushevska, T., Poidevin, F., Jha, S. W., Chen, W., Ellis, Richard S., Frye, B., Hjorth, J., Koekemoer, Anton M., Pérez-Fournon, I., Rest, A., Treu, T., Windhorst, R. A., and Zenati, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Strong gravitational lensing magnifies the light from a background source, allowing us to study these sources in detail. Here, we study the spectra of a $z = 1.95$ lensed Type Ia supernova SN~Encore for its brightest Image A, taken 39 days apart. We infer the spectral age with template matching using the supernova identification (SNID) software and find the spectra to be at 29.0 $\pm 5.0$ and 37.4 $\pm 2.8$ rest-frame days post maximum respectively, consistent with separation in the observer frame after accounting for time-dilation. Since SNe~Ia measure dark energy properties by providing relative distances between low- and high-$z$ SNe, it is important to test for evolution of spectroscopic properties. Comparing the spectra to composite low-$z$ SN~Ia spectra, we find strong evidence for similarity between the local sample of SN~Encore. The line velocities of common SN~Ia spectral lines, Si II 6355 and Ca II NIR triplet are consistent with the distribution for the low-$z$ sample as well as other lensed SNe~Ia, e.g. iPTF16geu ($z = 0.409$) and SN~H0pe ($z = 1.78$). The consistency in SN~Ia spectra across cosmic time demonstrates the utility of using SNe~Ia in the very high-$z$ universe for dark energy inference. We also find that the spectra of SN~Encore match the predictions for explosion models very well. With future large samples of lensed SNe~Ia, spectra at such late phases will be important to distinguish between different explosion scenarios., Comment: 9 pages, 8 figures, submitted to MNRAS. Comments welcome

Published
2024

18. EPOCHS I. The Discovery and Star Forming Properties of Galaxies in the Epoch of Reionization at $6.5 < z < 18$ with PEARLS and Public JWST data

Author

Conselice, Christopher J., Adams, Nathan, Harvey, Thomas, Austin, Duncan, Ferreira, Leonardo, Ormerod, Katherine, Duan, Qiao, Trussler, James, Li, Qiong, Juodzbalis, Ignas, Westcott, Lewi, Harris, Honor, Seeyave, Louise T. C., Bluck, Asa F. L., Windhorst, Rogier A., Bhatawdekar, Rachana, Coe, Dan, Cohen, Seth H., Cheng, Cheng, Driver, Simon P., Frye, Brenda, Furtak, Lukas J., Grogin, Norman A., Hathi, Nimish P., Holwerda, Benne W., Jansen, Rolf A., Koekemoer, Anton M., Marshall, Madeline A., Nonino, Mario, Robotham, Aaron, Summers, Jake, Wilkins, Stephen M., Willmer, Christopher N. A., Yan, Haojing, and Zitrin, Adi

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present in this paper the discovery, properties, and a catalog of 1165 high redshift $6.5 < z < 18$ galaxies found in deep JWST NIRCam imaging from the GTO PEARLS survey combined with data from JWST public fields. We describe our bespoke homogeneous reduction process and our analysis of these areas including the NEP, CEERS, GLASS, NGDEEP, JADES, and ERO SMACS-0723 fields with over 214 arcmin$^{2}$ imaged to depths of $\sim 30$ mag. We describe our rigorous methods for identifying these galaxies, involving the use of Lyman-break strength, detection significance criteria, visual inspection, and integrated photometric redshifts probability distributions predominately at high redshift. Our sample is a robust and highly pure collection of distant galaxies from which we also remove brown dwarf stars, and calculate completeness and contamination from simulations. We include a summary of the basic properties of these $z > 6.5$ galaxies, including their redshift distributions, UV absolute magnitudes, and star formation rates. Our study of these young galaxies reveals a wide range of stellar population properties as seen in their colors and SED fits which we compare to stellar population models, indicating a range of star formation histories, dust, AGN and/or nebular emission. We find a strong trend exists between stellar mass and $(U-V)$ color, as well as the existence of the `main-sequence' of star formation for galaxies as early as $z \sim 12$. This indicates that stellar mass, or an underlying variable correlating with stellar mass, is driving galaxy formation, in agreement with simulation predictions. We also discover ultra-high redshift candidates at $z > 12$ in our sample and describe their properties. Finally, we note a significant observed excess of galaxies compared to models at $z > 12$, revealing a tension between predictions and our observations., Comment: Submitted to AAS Journals, 37 pages

Published
2024

19. Galaxy Mergers in the Epoch of Reionization I: A JWST Study of Pair Fractions, Merger Rates, and Stellar Mass Accretion Rates at $z = 4.5-11.5$

Author

Duan, Qiao, Conselice, Christopher J., Li, Qiong, Austin, Duncan, Harvey, Thomas, Adams, Nathan J., Duncan, Kenneth J., Trussler, James, Ferreira, Leonardo, Westcott, Lewi, Harris, Honor, Windhorst, Rogier A., Holwerda, Benne W., Broadhurst, Thomas J., Coe, Dan, Cohen, Seth H., Du, Xiaojing, Driver, Simon P., Frye, Brenda, Grogin, Norman A., Hathi, Nimish P., Jansen, Rolf A., Koekemoer, Anton M., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan Jr, Russell E., Summers, Jake, D'Silva, Jordan C. J., Willmer, Christopher N. A., and Yan, Haojing

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a full analysis of galaxy major merger pair fractions, merger rates, and mass accretion rates, thus uncovering the role of mergers in galaxy formation at the earliest previously unexplored epoch of $4.5

Published
2024

20. Quantum control of ion-atom collisions beyond the ultracold regime

Author

Walewski, Maks Z., Frye, Matthew D., Katz, Or, Pinkas, Meirav, Ozeri, Roee, and Tomza, Michał

Subjects
Physics - Atomic Physics, Condensed Matter - Quantum Gases, Quantum Physics
Abstract

Tunable scattering resonances are crucial for controlling atomic and molecular systems. However, their use has so far been limited to ultracold temperatures. These conditions remain hard to achieve for most hybrid trapped ion-atom systems -- a prospective platform for quantum technologies and fundamental research. Here we measure inelastic collision probabilities for ${\text{Sr}^++\text{Rb}}$ and use them to calibrate a comprehensive theoretical model of ion-atom collisions. Our theoretical results, compared with experimental observations, confirm that quantum interference effects persist to the multiple-partial-wave regime, leading to the pronounced state and mass dependence of the collision rates. Using our model, we go beyond interference and identify a rich spectrum of Feshbach resonances at moderate magnetic fields with the Rb atom in its lower ($f=1$) hyperfine state, which persist at temperatures as high as 1 mK. Future observation of these predicted resonances should allow precise control of the short-range dynamics in ${\text{Sr}^+}+{\text{Rb}}$ collisions under unprecedentedly warm conditions., Comment: 10 pages, 3 figures, and Supplementary information (including 3 supplementary figures and 1 supplementary data as an .xlsx file)

Published
2024
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21. JWST view of four infant galaxies at z=8.31-8.49 in the MACS0416 field and implications for reionization

Author

Ma, Zhiyuan, Sun, Bangzheng, Cheng, Cheng, Yan, Haojing, Sun, Fengwu, Foo, Nicholas, Egami, Eiichi, Diego, Jose M., Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Windhorst, Rogier A., D'Silva, Jordan C. J., Koekemoer, Anton M., Coe, Dan, Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Grogin, Norman A., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Adams, Nathan J., Hathi, Nimish P., Dole, Herve, Willner, S. P., Espada, Daniel, Furtak, Lukas J., Hsiao, Tiger Yu-Yang, Li, Qiong, Chen, Wenlei, Jolly, Jean-Baptiste, and Chen, Chian-Chou

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

New JWST/NIRCam wide-field slitless spectroscopy provides redshifts for four z>8 galaxies located behind the lensing cluster MACS J0416.1-2403. Two of them, "Y1" and "JD", have previously reported spectroscopic redshifts based on ALMA measurements of [OIII] 88 $\mu$m and/or [CII] 157.7 $\mu$m lines. Y1 is a merging system of three components, and the existing redshift z=8.31 is confirmed. However, JD is at z=8.34 instead of the previously claimed z=9.28. JD's close companion, "JD-N", which was a previously discovered z>8 candidate, is now identified at the same redshift as JD. JD and JD-N form an interacting pair. A new candidate at z>8, "f090d_018", is also confirmed and is at z=8.49. These four objects are likely part of an overdensity that signposts a large structure extending ~165 kpc in projected distance and ~48.7 Mpc in radial distance. They are magnified by less than one magnitude and have intrinsic $M_{UV}$ ranging from -19.57 to -20.83 mag. Their spectral energy distributions show that the galaxies are all very young with ages ~ 4-18 Myr and stellar masses about $10^{7-8}$ ${\rm M_\odot}$. These infant galaxies have very different star formation rates ranging from a few to over a hundred $\rm{M_\odot}$ yr$^{-1}$, but only two of them (JD and f090d_018) have blue rest-frame UV slopes $\beta<-2.0$ indicative of a high Lyman-continuum photon escape fraction that could contribute significantly to the cosmic hydrogen-reionizing background. Interestingly, these two galaxies are the least massive and least active ones among the four. The other two systems have much flatter UV slopes largely because of their high dust extinction ($A_{\rm V}$=0.9-1.0 mag). Their much lower indicated escape fractions show that even very young, actively star-forming galaxies can have negligible contribution to reionization when they quickly form dust throughout their bodies., Comment: 18 pages, 6 figures, after addressing the referee report

Published
2024

22. Genomics yields biological and phenotypic insights into bipolar disorder

Author

O’Connell, Kevin S., Koromina, Maria, van der Veen, Tracey, Boltz, Toni, David, Friederike S., Yang, Jessica Mei Kay, Lin, Keng-Han, Wang, Xin, Coleman, Jonathan R. I., Mitchell, Brittany L., McGrouther, Caroline C., Rangan, Aaditya V., Lind, Penelope A., Koch, Elise, Harder, Arvid, Parker, Nadine, Bendl, Jaroslav, Adorjan, Kristina, Agerbo, Esben, Albani, Diego, Alemany, Silvia, Alliey-Rodriguez, Ney, Als, Thomas D., Andlauer, Till F. M., Antoniou, Anastasia, Ask, Helga, Bass, Nicholas, Bauer, Michael, Beins, Eva C., Bigdeli, Tim B., Pedersen, Carsten Bøcker, Boks, Marco P., Børte, Sigrid, Bosch, Rosa, Brum, Murielle, Brumpton, Ben M., Brunkhorst-Kanaan, Nathalie, Budde, Monika, Bybjerg-Grauholm, Jonas, Byerley, William, Cabana-Domínguez, Judit, Cairns, Murray J., Carpiniello, Bernardo, Casas, Miquel, Cervantes, Pablo, Chatzinakos, Chris, Chen, Hsi-Chung, Clarence, Tereza, Clarke, Toni-Kim, Claus, Isabelle, Coombes, Brandon, Corfield, Elizabeth C., Cruceanu, Cristiana, Cuellar-Barboza, Alfredo, Czerski, Piotr M., Dafnas, Konstantinos, Dale, Anders M., Dalkner, Nina, Degenhardt, Franziska, DePaulo, J. Raymond, Djurovic, Srdjan, Drange, Ole Kristian, Escott-Price, Valentina, Fanous, Ayman H., Fellendorf, Frederike T., Ferrier, I. Nicol, Forty, Liz, Frank, Josef, Frei, Oleksandr, Freimer, Nelson B., Fullard, John F., Garnham, Julie, Gizer, Ian R., Gordon, Scott D., Gordon-Smith, Katherine, Greenwood, Tiffany A., Grove, Jakob, Guzman-Parra, José, Ha, Tae Hyon, Hahn, Tim, Haraldsson, Magnus, Hautzinger, Martin, Havdahl, Alexandra, Heilbronner, Urs, Hellgren, Dennis, Herms, Stefan, Hickie, Ian B., Hoffmann, Per, Holmans, Peter A., Huang, Ming-Chyi, Ikeda, Masashi, Jamain, Stéphane, Johnson, Jessica S., Jonsson, Lina, Kalman, Janos L., Kamatani, Yoichiro, Kennedy, James L., Kim, Euitae, Kim, Jaeyoung, Kittel-Schneider, Sarah, Knowles, James A., Kogevinas, Manolis, Kranz, Thorsten M., Krebs, Kristi, Kushner, Steven A., Lavebratt, Catharina, Lawrence, Jacob, Leber, Markus, Lee, Heon-Jeong, Liao, Calwing, Lucae, Susanne, Lundberg, Martin, MacIntyre, Donald J., Maier, Wolfgang, Maihofer, Adam X., Malaspina, Dolores, Manchia, Mirko, Maratou, Eirini, Martinsson, Lina, Mattheisen, Manuel, McGregor, Nathaniel W., McInnis, Melvin G., McKay, James D., Medeiros, Helena, Meyer-Lindenberg, Andreas, Millischer, Vincent, Morris, Derek W., Moutsatsou, Paraskevi, Mühleisen, Thomas W., O’Donovan, Claire, Olsen, Catherine M., Panagiotaropoulou, Georgia, Papiol, Sergi, Pardiñas, Antonio F., Park, Hye Youn, Perry, Amy, Pfennig, Andrea, Pisanu, Claudia, Potash, James B., Quested, Digby, Rapaport, Mark H., Regeer, Eline J., Rice, John P., Rivera, Margarita, Schulte, Eva C., Senner, Fanny, Shadrin, Alexey, Shilling, Paul D., Sigurdsson, Engilbert, Sindermann, Lisa, Sirignano, Lea, Siskind, Dan, Slaney, Claire, Sloofman, Laura G., Smeland, Olav B., Smith, Daniel J., Sobell, Janet L., Soler Artigas, Maria, Stein, Dan J., Stein, Frederike, Su, Mei-Hsin, Sung, Heejong, Świątkowska, Beata, Terao, Chikashi, Tesfaye, Markos, Tesli, Martin, Thorgeirsson, Thorgeir E., Thorp, Jackson G., Toma, Claudio, Tondo, Leonardo, Tooney, Paul A., Tsai, Shih-Jen, Tsermpini, Evangelia Eirini, Vawter, Marquis P., Vedder, Helmut, Vreeker, Annabel, Walters, James T. R., Winsvold, Bendik S., Witt, Stephanie H., Won, Hong-Hee, Ye, Robert, Young, Allan H., Zandi, Peter P., Zillich, Lea, Adolfsson, Rolf, Alda, Martin, Alfredsson, Lars, Backlund, Lena, Baune, Bernhard T., Bellivier, Frank, Bengesser, Susanne, Berrettini, Wade H., Biernacka, Joanna M., Boehnke, Michael, Børglum, Anders D., Breen, Gerome, Carr, Vaughan J., Catts, Stanley, Cichon, Sven, Corvin, Aiden, Craddock, Nicholas, Dannlowski, Udo, Dikeos, Dimitris, Etain, Bruno, Ferentinos, Panagiotis, Frye, Mark, Fullerton, Janice M., Gawlik, Micha, Gershon, Elliot S., Goes, Fernando S., Green, Melissa J., Grigoroiu-Serbanescu, Maria, Hauser, Joanna, Henskens, Frans A., Hjerling-Leffler, Jens, Hougaard, David M., Hveem, Kristian, Iwata, Nakao, Jones, Ian, Jones, Lisa A., Kahn, René S., Kelsoe, John R., Kircher, Tilo, Kirov, George, Kuo, Po-Hsiu, Landén, Mikael, Leboyer, Marion, Li, Qingqin S., Lissowska, Jolanta, Lochner, Christine, Loughland, Carmel, Luykx, Jurjen J., Martin, Nicholas G., Mathews, Carol A., Mayoral, Fermin, McElroy, Susan L., McIntosh, Andrew M., McMahon, Francis J., Medland, Sarah E., Melle, Ingrid, Milani, Lili, Mitchell, Philip B., Morken, Gunnar, Mors, Ole, Mortensen, Preben Bo, Müller-Myhsok, Bertram, Myers, Richard M., Myung, Woojae, Neale, Benjamin M., Nievergelt, Caroline M., Nordentoft, Merete, Nöthen, Markus M., Nurnberger, John I., O’Donovan, Michael C., Oedegaard, Ketil J., Olsson, Tomas, Owen, Michael J., Paciga, Sara A., Pantelis, Christos, Pato, Carlos N., Pato, Michele T., Patrinos, George P., Pawlak, Joanna M., Ramos-Quiroga, Josep Antoni, Reif, Andreas, Reininghaus, Eva Z., Ribasés, Marta, Rietschel, Marcella, Ripke, Stephan, Rouleau, Guy A., Roussos, Panos, Saito, Takeo, Schall, Ulrich, Schalling, Martin, Schofield, Peter R., Schulze, Thomas G., Scott, Laura J., Scott, Rodney J., Serretti, Alessandro, Smoller, Jordan W., Squassina, Alessio, Stahl, Eli A., Stefansson, Hreinn, Stefansson, Kari, Stordal, Eystein, Streit, Fabian, Sullivan, Patrick F., Turecki, Gustavo, Vaaler, Arne E., Vieta, Eduard, Vincent, John B., Waldman, Irwin D., Weickert, Cynthia S., Weickert, Thomas W., Werge, Thomas, Whiteman, David C., Zwart, John-Anker, Edenberg, Howard J., McQuillin, Andrew, Forstner, Andreas J., Mullins, Niamh, Di Florio, Arianna, Ophoff, Roel A., and Andreassen, Ole A.

Published
2025
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23. Fitting the Means to the Ends: One School’s Experience with Quantitative and Qualitative Methods in Curriculum Evaluation During Curriculum Change

Author

Frye PhD, Ann W., Solomon PhD, David J., Lieberman MD, Steven A., and Levine MD, Ruth E.

Subjects
JOURNALS: Medical Education Online: MEO Peer Reviewed, MEO Peer Reviewed
Abstract

Curriculum evaluation plays an important role in substantive curriculum change. The experience of the University of Texas Medical Branch (UTMB) with evaluation processes developed for the new Integrated Medical Curriculum (IMC) illustrates how evaluation methods may be chosen to match the goals of the curriculum evaluation process. Quantitative data such as ratings of courses or scores on external exams are useful for comparing courses or assessing whether standards have been met. Qualitative data such as students’ comments about aspects of courses are useful for eliciting explanations of observed phenomena and describing relationships between curriculum features and outcomes. The curriculum evaluation process designed for the IMC used both types of evaluation methods in a complementary fashion. Quantitative and qualitative methods have been used for formative evaluation of the new IMC courses. They are now being incorporated into processes to judge the IMC against its goals and objectives.

Published
2000

24. EPOCHS Paper X: Environmental effects on Galaxy Formation and Protocluster Galaxy candidates at $4.5<z<10$ from JWST observations

Author

Li, Qiong, Conselice, Christopher J., Sarron, Florian, Harvey, Tom, Austin, Duncan, Adams, Nathan, Trussler, James A. A., Duan, Qiao, Ferreira, Leonardo, Westcott, Lewi, Harris, Honor, Dole, Hervé, Grogin, Norman A., Frye, Brenda, Koekemoer, Anton M., Robertson, Clayton, Windhorst, Rogier A., Polletta, Maria del Carmen, and Hathi, Nimish P.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

In this paper we describe our search for galaxy protocluster candidates at $4.5< z < 10$ and explore the environmental and physical properties of their member galaxies identified through JWST wide-field surveys within the CEERS, JADES, and PEARLS NEP-TDF fields. Combining with HST data, we identify 2948 robust $z>4.5$ candidates within an area of 185.4 arcmin$^2$. We determine nearest neighbour statistics and galaxy environments. We find that high-$z$ galaxies in overdense environments exhibit higher star formation activity compared to those in underdense regions. Galaxies in dense environments have a slightly increased SFR at a given mass compared with galaxies in the lower density environments. At the high mass end we also find a gradual flattening of the $M_{\star}$-SFR slope. We find that galaxies in high-density regions often have redder UV slopes than those in low-density regions, suggesting more dust extinction, weaker Lyman-alpha emission and / or a higher damped Lyman-alpha absorption. We also find that the mass-size relation remains consistent and statistically similar across all environments. Furthermore, we quantitatively assess the probability of a galaxy belonging to a protocluster candidate. In total, we identified 26 overdensities at $z=5-7$ and estimate their dark matter halo masses. We find that all protocluster candidates could evolve into clusters with $M_{\rm halo} > 10^{14}M_{\odot}$ at $z = 0$, thereby supporting the theoretical and simulation predictions of cluster formation. Notably, this marks an early search for protocluster candidates in JWST wide field based on photometric data, providing valuable candidates to study cosmic structure formation at the early stages., Comment: 23 pages, 14 figures and 7 table, submitted to MNRAS

Published
2024

25. JWST's PEARLS: resolved study of the stellar and dust components in starburst galaxies at cosmic noon

Author

Polletta, M., Frye, B. L., Garuda, N., Willner, S. P., Berta, S., Kneissl, R., Dole, H., Jansen, R. A., Lehnert, M. D., Cohen, S. H., Summers, J., Windhorst, R. A., D'Silva, J. C. J., Koekemoer, A. M., Coe, D., Conselice, C. J., Driver, S. P., Grogin, N. A., Marshall, M. A., Nonino, M., Ortiz III, R., Pirzkal, N., Robotham, A., Ryan, Jr., R. E., Willmer, C. N. A., Yan, H., Arumugam, V., Cheng, C., Gim, H. B., Hathi, N. P., Holwerda, B., Kamieneski, P., Keel, W. C., Li, J., Pascale, M., Rottgering, H., Smith, B. M., and Yun, M. S.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Dusty star-forming galaxies (DSFGs) contribute significantly to the stellar buildup at cosmic noon. Major mergers and gas accretion are often invoked to explain DSFGs' prodigious star-formation rates (SFRs) and large stellar masses. We conducted a spatially-resolved morphological analysis of the rest-frame UV/NIR emission in three DSFGs at z~2.5. Initially discovered as CO emitters by NOEMA observations of a bright Herschel source, we observed them with the JWST/NIRCam as part of the PEARLS program. The NIRCam data reveal the galaxies' stellar populations and dust distributions on scales of 250 pc. Spatial variations in stellar mass, SFR, and dust extinction are determined in resolved maps obtained through pixel-based SED fitting. The CO emitters are massive, dusty starburst galaxies with SFRs=340-2500 Msun/yr, positioning them among the most active SFGs at 2

Published
2024
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26. DisBeaNet: A Deep Neural Network to augment Unmanned Surface Vessels for maritime situational awareness

Author

Vemula, Srikanth, Franco, Eulises, and Frye, Michael

Subjects
Computer Science - Artificial Intelligence, Computer Science - Computer Vision and Pattern Recognition
Abstract

Intelligent detection and tracking of the vessels on the sea play a significant role in conducting traffic avoidance in unmanned surface vessels(USV). Current traffic avoidance software relies mainly on Automated Identification System (AIS) and radar to track other vessels to avoid collisions and acts as a typical perception system to detect targets. However, in a contested environment, emitting radar energy also presents the vulnerability to detection by adversaries. Deactivating these Radiofrequency transmitting sources will increase the threat of detection and degrade the USV's ability to monitor shipping traffic in the vicinity. Therefore, an intelligent visual perception system based on an onboard camera with passive sensing capabilities that aims to assist USV in addressing this problem is presented in this paper. This paper will present a novel low-cost vision perception system for detecting and tracking vessels in the maritime environment. This novel low-cost vision perception system is introduced using the deep learning framework. A neural network, DisBeaNet, can detect vessels, track, and estimate the vessel's distance and bearing from the monocular camera. The outputs obtained from this neural network are used to determine the latitude and longitude of the identified vessel.

Published
2024

27. Interactions and cold collisions of AlF in the ground and excited electronic states with He

Author

Ganesan-Santhi, Sangami, Frye, Matthew D., Gronowski, Marcin, and Tomza, Michał

Subjects
Physics - Chemical Physics, Physics - Atomic Physics
Abstract

Aluminium monofluoride (AlF) is a promising candidate for laser cooling and the production of dense ultracold molecular gases, thanks to its relatively high chemical stability and diagonal Frank-Condon factors. In this study, we examine the interactions and collisions of AlF in its $X^1\Sigma^+$, $a^3\Pi$, and $A^{1}\Pi$ electronic states with ground-state He using state-of-the-art \textit{ab initio} quantum chemistry techniques. We construct accurate potential energy surfaces (PESs) employing either the explicitly correlated coupled-cluster CCSD(T)-F12 method augmented by the CCSDT correction or the multireference configuration-interaction method for higher-excited electronic states. Subsequently, we employ these PESs in coupled-channel calculations to determine the scattering cross-sections for AlF+He collisions and bound states of the complex. We estimate the uncertainty of the calculated PESs and apply it to assess the uncertainty of the scattering results. We find a relatively low sensitivity of the cross-sections to the variation of the PESs, but the positions of shape resonances remain uncertain. The present results are relevant for further improvements and optimizations of buffer-gas cooling of AlF molecules., Comment: 12 pages, 8 figures, 4 tables

Published
2024

28. EPOCHS III: Unbiased UV continuum slopes at 6.5<z<13 from combined PEARLS GTO and public JWST NIRCam imaging

Author

Austin, Duncan, Conselice, Christopher J., Adams, Nathan J., Harvey, Thomas, Duan, Qiao, Trussler, James, Li, Qiong, Juodzbalis, Ignas, Ormerod, Katherine, Ferreira, Leonardo, Westcott, Lewi, Harris, Honor, Wilkins, Stephen M., Bhatawdekar, Rachana, Caruana, Joseph, Coe, Dan, Cohen, Seth H., Driver, Simon P., D'Silva, Jordan C. J., Frye, Brenda, Furtak, Lukas J., Grogin, Norman A., Hathi, Nimish P., Holwerda, Benne W., Jansen, Rolf A., Koekemoer, Anton M., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan Jr., Russell E., Summers, Jake, Willmer, Christopher N. A., Windhorst, Rogier A., Yan, Haojing, and Zackrisson, Erik

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present an analysis of rest-frame UV continuum slopes, $\beta$, using a sample of 1011 galaxies at $6.5

Published
2024

29. PEARLS: Discovery of Point-Source Features Within Galaxies in the North Ecliptic Pole Time Domain Field

Author

Ortiz III, Rafael, Windhorst, Rogier A., Cohen, Seth H., Willner, S. P., Jansen, Rolf A., Carleton, Timothy, Kamieneski, Patrick S., Rutkowski, Michael J., Smith, Brent, Summers, Jake, McCabe, Tyler J., O'Brien, Rosalia, Diego, Jose M., Yun, Min S., D'Silva, Jordan C. J., Li, Juno, Gim, Hansung B., Hathi, Nimish P., Holwerda, Benne W., Zitrin, Adi, Cheng, Cheng, McLeod, Noah J., Conselice, Christopher J., Driver, Simon P., Yan, Haojing, Coe, Dan, Frye, Brenda, Grogin, Norman, Koekemoer, Anton, Marshall, Madeline A., Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Keel, William, Hammel, H. B., Hyun, M., Im, M., and Milam, S. N.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The first public 0.9-4.4{\mu}m NIRCam images of the North Ecliptic Pole (NEP) Time Domain Field (TDF) uncovered galaxies displaying point-source features in their cores as seen in the longer wavelength filters. We visually identified a sample of 66 galaxies (~1 galaxy per arcmin2) with point-like cores and have modeled their two-dimensional light profiles with GalFit, identifying 16 galactic nuclei with measurable point-source components. GalFit suggests the visual sample is a mix of both compact stellar bulge and point-source galaxy cores. This core classification is complemented by spectral energy distribution (SED) modeling to infer the sample's active galactic nucleus (AGN) and host-galaxy parameters. For galaxies with measurable point-source components, the median fractional AGN contribution to their 0.1-30.0{\mu}m flux is 0.44, and 14/16 are color-classified AGN. We conclude that near-infrared point-source galaxy cores are signatures of AGN. In addition, we define an automated sample-selection criterion to identify these point-source features. These criteria can be used in other extant and future NIRCam images to streamline the search for galaxies with unresolved IR-luminous AGN. The James Webb Space Telescope's superb angular resolution and sensitivity at infrared wavelengths is resurrecting the morphological identification of AGN., Comment: 17 pages, 9 figures, 2 tables

Published
2024
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30. Birds of a Feather: Resolving Stellar Mass Assembly With JWST/NIRCam in a Pair of Kindred $z \sim 2$ Dusty Star-forming Galaxies Lensed by the PLCK G165.7+67.0 Cluster

Author

Kamieneski, Patrick S., Frye, Brenda L., Windhorst, Rogier A., Harrington, Kevin C., Yun, Min S., Noble, Allison, Pascale, Massimo, Foo, Nicholas, Cohen, Seth H., Jansen, Rolf A., Carleton, Timothy, Koekemoer, Anton M., Willmer, Christopher N. A., Summers, Jake S., Garuda, Nikhil, Leimbach, Reagen, Holwerda, Benne W., Pierel, Justin D. R., Jimenez-Andrade, Eric F., Willner, S. P., Pampliega, Belen Alcalde, Vishwas, Amit, Keel, William C., Wang, Q. Daniel, Cheng, Cheng, Coe, Dan, Conselice, Christopher J., D'Silva, Jordan C. J., Driver, Simon P., Grogin, Norman A., Hinrichs, Tyler, Lowenthal, James D., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pigarelli, Alex, Pirzkal, Nor, Polletta, Maria del Carmen, Robotham, Aaron S. G., Ryan Jr., Russell E., and Yan, Haojing

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a new parametric lens model for the G165.7+67.0 galaxy cluster, which was discovered with $Planck$ through its bright submillimeter flux, originating from a pair of extraordinary dusty star-forming galaxies (DSFGs) at $z\approx 2.2$. Using JWST and interferometric mm/radio observations, we characterize the intrinsic physical properties of the DSFGs, which are separated by only $\sim 1^{\prime\prime}$ (8 kpc) and a velocity difference $\Delta V \lesssim 600~{\rm km}~{\rm s}^{-1}$ in the source plane, and thus likely undergoing a major merger. Boasting intrinsic star formation rates ${\rm SFR}_{\rm IR} = 320 \pm 70$ and $400 \pm 80~ M_\odot~{\rm yr}^{-1}$, stellar masses ${\rm log}[M_\star/M_\odot] = 10.2 \pm 0.1$ and $10.3 \pm 0.1$, and dust attenuations $A_V = 1.5 \pm 0.3$ and $1.2 \pm 0.3$, they are remarkably similar objects. We perform spatially-resolved pixel-by-pixel SED fitting using rest-frame near-UV to near-IR imaging from JWST/NIRCam for both galaxies, resolving some stellar structures down to 100 pc scales. Based on their resolved specific SFRs and $UVJ$ colors, both DSFGs are experiencing significant galaxy-scale star formation events. If they are indeed interacting gravitationally, this strong starburst could be the hallmark of gas that has been disrupted by an initial close passage. In contrast, the host galaxy of the recently discovered triply-imaged SN H0pe has a much lower SFR than the DSFGs, and we present evidence for the onset of inside-out quenching and large column densities of dust even in regions of low specific SFR. Based on the intrinsic SFRs of the DSFGs inferred from UV through FIR SED modeling, this pair of objects alone is predicted to yield an observable $1.1 \pm 0.2~{\rm CCSNe~yr}^{-1}$, making this cluster field ripe for continued monitoring., Comment: 47 pages, 21 figures, 5 tables. Submitted to ApJ, comments welcome!

Published
2024

31. Identification of $>$40 gravitationally magnified stars in a galaxy at redshift of 0.725

Author

Fudamoto, Yoshinobu, Sun, Fengwu, Diego, Jose M., Dai, Liang, Oguri, Masamune, Zitrin, Adi, Zackrisson, Erik, Jauzac, Mathilde, Lagattuta, David J., Egami, Eiichi, Iani, Edoardo, Windhorst, Rogier A., Abe, Katsuya T., Bauer, Franz Erik, Bian, Fuyan, Bhatawdekar, Rachana, Broadhurst, Thomas J., Cai, Zheng, Chen, Chian-Chou, Chen, Wenlei, Cohen, Seth H., Conselice, Christopher J., Espada, Daniel, Foo, Nicholas, Frye, Brenda L., Fujimoto, Seiji, Furtak, Lukas J., Golubchik, Miriam, Hsiao, Tiger Yu-Yang, Jolly, Jean-Baptiste, Kawai, Hiroki, Kelly, Patrick L., Koekemoer, Anton M., Kohno, Kotaro, Kokorev, Vasily, Li, Mingyu, Li, Zihao, Lin, Xiaojing, Magdis, Georgios E., Meena, Ashish K., Niemiec, Anna, Nabizadeh, Armin, Richard, Johan, Steinhardt, Charles L., Wu, Yunjing, Zhu, Yongda, and Zou, Siwei

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Strong gravitational magnifications enable to detect faint background sources, resolve their internal structures, and even identify individual stars in distant galaxies. Highly magnified individual stars allow various applications, including studies of stellar populations in distant galaxies and constraining dark matter structures in the lensing plane. However, these applications have been hampered by the small number of individual stars observed, as typically one or a few stars are identified from each distant galaxy. Here, we report the discovery of more than 40 microlensed stars in a single galaxy behind Abell 370 at redshift of 0.725 when the Universe was half of its current age (dubbed ``the Dragon arc''), using James Webb Space Telescope (JWST) observations with the time-domain technique. These events are found near the expected lensing critical curves, suggesting that these are magnified stars that appear as transients from intracluster stellar microlenses. Through multi-wavelength photometry, we constrain stellar types and find that many of them are consistent with red giants/supergiants magnified by factors of hundreds. This finding reveals an unprecedented high occurrence of microlensing events in the Dragon arc, and proves that {\it JWST}'s time-domain observations open up the possibility of conducting statistical studies of high-redshift stars., Comment: 28 pages, 5 figures, 2 tables accepted for publication in Nature Astronomy

Published
2024
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32. Collisions of Spin-polarized YO Molecules for Single Partial Waves

Author

Burau, Justin J., Mehling, Kameron, Frye, Matthew D., Chen, Mengjie, Aggarwal, Parul, Hutson, Jeremy M., and Ye, Jun

Subjects
Physics - Atomic Physics
Abstract

Efficient sub-Doppler laser cooling and optical trapping of YO molecules offer new opportunities to study collisional dynamics in the quantum regime. Confined in a crossed optical dipole trap, we achieve the highest phase-space density of $2.5 \times 10^{-5}$ for a bulk laser-cooled molecular sample. This sets the stage to study YO--YO collisions in the microkelvin temperature regime, and reveal state-dependent, single-partial-wave two-body collisional loss rates. We determine the partial-wave contributions to loss of specific rotational states (first excited $N=1$ and ground $N=0$) following two strategies. First, we measure the change of the collision rate in a spin mixture of $N=1$ by tuning the kinetic energy with respect to the p- and d-wave centrifugal barriers. Second, we compare loss rates between a spin mixture and a spin-polarized state in $N=0$. Using quantum defect theory with a partially absorbing boundary condition at short range, we show that the dependence on temperature for $N=1$ can be reproduced in the presence of a d-wave or f-wave resonance, and the dependence on a spin mixture for $N=0$ with a p-wave resonance., Comment: 5 Pages, 4 Figures. Fixed typos. Collisional loss data in $N = 1$ and $N = 0$ is now presented as density versus time instead of number versus time. This work is published in Physical Review A (Copyright 2024 by the American Physical Society). The link to the article is https://journals.aps.org/pra/abstract/10.1103/PhysRevA.110.L041306

Published
2024
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33. A complex node of the cosmic web associated with the massive galaxy cluster MACS J0600.1-2008

Author

Furtak, Lukas J., Zitrin, Adi, Richard, Johan P., Eckert, Dominique, Sayers, Jack, Ebeling, Harald, Fujimoto, Seiji, Laporte, Nicolas, Lagattuta, David, Limousin, Marceau, Mahler, Guillaume, Meena, Ashish K., Andrade-Santos, Felipe, Frye, Brenda L., Jauzac, Mathilde, Koekemoer, Anton M., Kohno, Kotaro, Espada, Daniel, Lu, Harry, Massey, Richard, and Niemiec, Anna

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

MACS J0600.1-2008 (MACS0600) is an X-ray luminous, massive galaxy cluster at $z_{\mathrm{d}}=0.43$, studied previously by the REionization LensIng Cluster Survey (RELICS) and ALMA Lensing Cluster Survey (ALCS) projects which revealed a complex, bimodal mass distribution and an intriguing high-redshift object behind it. Here, we report on the results of a combined analysis of the extended strong lensing (SL), X-ray, Sunyaev-Zeldovich (SZ), and galaxy luminosity-density properties of this system. Using new JWST and ground-based Gemini-N and Keck data, we obtain 13 new spectroscopic redshifts of multiply imaged galaxies and identify 12 new photometric multiple-image systems and candidates, including two multiply imaged $z\sim7$ objects. Taking advantage of the larger areal coverage, our analysis reveals an additional bimodal, massive SL structure which we measure spectroscopically to lie adjacent to the cluster and whose existence was implied by previous SL-modeling analyses. While based in part on photometric systems identified in ground-based imaging requiring further verification, our extended SL model suggests that the cluster may have the second-largest critical area and effective Einstein radius observed to date, $A_{\mathrm{crit}}\simeq2.16 \mathrm{arcmin}^2$ and $\theta_{\mathrm{E}}=49.7''\pm5.0''$ for a source at $z_{\mathrm{s}}=2$, enclosing a total mass of $M(<\theta_{\mathrm{E}})=(4.7\pm0.7)\times10^{14} \mathrm{M}_{\odot}$. These results are also supported by the galaxy luminosity distribution, the SZ and X-ray data. Yet another, probably related massive cluster structure, discovered in X-rays $5'$ (1.7 Mpc) further north, suggests that MACS0600 is part of an even larger filamentary structure. This discovery adds to several recent detections of massive structures around SL galaxy clusters and establishes MACS0600 as a prime target for future high-redshift surveys with JWST., Comment: Accepted for publication in MNRAS. Version updated to the accepted paper

Published
2024

34. Lensed Type Ia Supernova 'Encore' at z=2: The First Instance of Two Multiply-Imaged Supernovae in the Same Host Galaxy

Author

Pierel, J. D. R., Newman, A. B., Dhawan, S., Gu, M., Joshi, B. A., Li, T., Schuldt, S., Strolger, L. G., Suyu, S. H., Caminha, G. B., Cohen, S. H., Diego, J. M., Dsilva, J. C. J., Ertl, S., Frye, B. L., Granata, G., Grillo, C., Koekemoer, A. M., Li, J., Robotham, A., Summers, J., Treu, T., Windhorst, R. A., Zitrin, A., Agarwal, S., Agrawal, A., Arendse, N., Belli, S., Burns, C., Cañameras, R., Chakrabarti, S., Chen, W., Collett, T. E., Coulter, D. A., Ellis, R. S., Engesser, M., Foo, N., Fox, O. D., Gall, C., Garuda, N., Gezari, S., Gomez, S., Glazebrook, K., Hjorth, J., Huang, X., Jha, S. W., Kamieneski, P. S., Kelly, P., Larison, C., Moustakas, L. A., Pascale, M., Pérez-Fournon, I., Petrushevska, T., Poidevin, F., Rest, A., Shahbandeh, M., Shajib, A. J., Siebert, M., Storfer, C., Talbot, M., Wang, Q., Wevers, T., and Zenati, Y.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A bright ($m_{\rm F150W,AB}$=24 mag), $z=1.95$ supernova (SN) candidate was discovered in JWST/NIRCam imaging acquired on 2023 November 17. The SN is quintuply-imaged as a result of strong gravitational lensing by a foreground galaxy cluster, detected in three locations, and remarkably is the second lensed SN found in the same host galaxy. The previous lensed SN was called "Requiem", and therefore the new SN is named "Encore". This makes the MACS J0138.0$-$2155 cluster the first known system to produce more than one multiply-imaged SN. Moreover, both SN Requiem and SN Encore are Type Ia SNe (SNe Ia), making this the most distant case of a galaxy hosting two SNe Ia. Using parametric host fitting, we determine the probability of detecting two SNe Ia in this host galaxy over a $\sim10$ year window to be $\approx3\%$. These observations have the potential to yield a Hubble Constant ($H_0$) measurement with $\sim10\%$ precision, only the third lensed SN capable of such a result, using the three visible images of the SN. Both SN Requiem and SN Encore have a fourth image that is expected to appear within a few years of $\sim2030$, providing an unprecedented baseline for time-delay cosmography., Comment: Accepted, ApJL

Published
2024
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35. JWST Spectroscopy of SN H0pe: Classification and Time Delays of a Triply-imaged Type Ia Supernova at z = 1.78

Author

Chen, Wenlei, Kelly, Patrick L., Frye, Brenda L., Pierel, Justin, Willner, S. P., Pascale, Massimo, Cohen, Seth H., Conselice, Christopher J., Engesser, Michael, Furtak, Lukas J., Gilman, Daniel, Grogin, Norman A., Huber, Simon, Jha, Saurabh W., Johansson, Joel, Koekemoer, Anton M., Larison, Conor, Meena, Ashish K., Siebert, Matthew R., Windhorst, Rogier A., Yan, Haojing, and Zitrin, Adi

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

SN H0pe is a triply imaged supernova (SN) at redshift $z=1.78$ discovered using the James Webb Space Telescope (JWST). In order to classify the SN spectroscopically and measure the relative time delays of its three images (designated A, B, and C), we acquired NIRSpec follow-up spectroscopy spanning 0.6 to 5 microns. From the high signal-to-noise spectra of the two bright images B and C, we first classify the SN, whose spectra most closely match those of SN 1994D and SN 2013dy, as a Type Ia SN. We identify prominent blueshifted absorption features corresponding to Si II $\lambda6355$ and Ca II H $\lambda3970$ and K $\lambda3935$. We next measure the absolute phases of the three images from our spectra, which allows us to constrain their relative time delays. The absolute phases of the three images, determined by fitting the three spectra to Hsiao07 SN templates, are $6.5_{-1.8}^{+2.4}$d, $24.3_{-3.9}^{+3.9}$d, and $50.6_{-15.3}^{+16.1}$d for the brightest to faintest images. These correspond to relative time delays between Image A and Image B and between Image B and Image C of $-122.3_{-43.8}^{+43.7}$d and $49.3_{-14.7}^{+12.2}$d, respectively. The SALT3-NIR model yields phases and time delays consistent with these values. After unblinding, we additionally explored the effect of using Hsiao07 template spectra for simulations through eighty instead of sixty days past maximum, and found a small (11.5 and 1.0 days, respectively) yet statistically insignificant ($\sim$0.25$\sigma$ and $\sim$0.1$\sigma$) effect on the inferred image delays., Comment: 27 pages (including appendices), 11 figures, 13 supplemental figures

Published
2024

36. JWST Photometric Time-Delay and Magnification Measurements for the Triply-Imaged Type Ia 'Supernova H0pe' at z = 1.78

Author

Pierel, J. D. R., Frye, B. L., Pascale, M., Caminha, G. B., Chen, W., Dhawan, S., Gilman, D., Grayling, M., Huber, S., Kelly, P., Thorp, S., Arendse, N., Birrer, S., Bronikowski, M., Canameras, R., Coe, D., Cohen, S. H., Conselice, C. J., Driver, S. P., Dsilva, J. C. J., Engesser, M., Foo, N., Gall, C., Garuda, N., Grillo, C., Grogin, N. A., Henderson, J., Hjorth, J., Jansen, R. A., Johansson, J., Kamieneski, P. S., Koekemoer, A. M., Larison, C., Marshall, M. A., Moustakas, L. A., Nonino, M., Ortiz Iii, R., Petrushevska, T., Pirzkal, N., Robotham, A., Ryan, Jr., R. E., Schuldt, S., Strolger, L. G., Summers, J., Suyu, S. H., Treu, T., Willmer, C. N. A., Windhorst, R. A., Yan, H., Zitrin, A., Acebron, A., Chakrabarti, S., Coulter, D. A., Fox, O. D., Huang, X., Jha, S. W., Li, G., Mazzali, P. A., Meena, A. K., Perez-Fournon, I., Poidevin, F., Rest, A., and Riess, A. G.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Supernova (SN) H0pe is a gravitationally lensed, triply-imaged, Type Ia SN (SN Ia) discovered in James Webb Space Telescope imaging of the PLCK G165.7+67.0 cluster of galaxies. Well-observed multiply-imaged SNe provide a rare opportunity to constrain the Hubble constant ($H_0$), by measuring the relative time delay between the images and modeling the foreground mass distribution. SN H0pe is located at $z=1.783$, and is the first SN Ia with sufficient light curve sampling and long enough time delays for an $H_0$ inference. Here we present photometric time-delay measurements and SN properties of SN H0pe. Using JWST/NIRCam photometry we measure time delays of $\Delta t_{ab}=-116.6^{+10.8}_{-9.3}$ and $\Delta t_{cb}=-48.6^{+3.6}_{-4.0}$ observer-frame days relative to the last image to arrive (image 2b; all uncertainties are $1\sigma$), which corresponds to a $\sim5.6\%$ uncertainty contribution for $H_0$ assuming $70 \rm{km s^{-1} Mpc^{-1}}$. We also constrain the absolute magnification of each image to $\mu_{a}=4.3^{+1.6}_{-1.8}$, $\mu_{b}=7.6^{+3.6}_{-2.6}$, $\mu_{c}=6.4^{+1.6}_{-1.5}$ by comparing the observed peak near-IR magnitude of SN H0pe to the non-lensed population of SNe Ia., Comment: Accepted in ApJ

Published
2024
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37. SN H0pe: The First Measurement of $H_0$ from a Multiply-Imaged Type Ia Supernova, Discovered by JWST

Author

Pascale, Massimo, Frye, Brenda L., Pierel, Justin D. R., Chen, Wenlei, Kelly, Patrick L., Cohen, Seth H., Windhorst, Rogier A., Riess, Adam G., Kamieneski, Patrick S., Diego, Jose M., Meena, Ashish K., Cha, Sangjun, Oguri, Masamune, Zitrin, Adi, Jee, M. James, Foo, Nicholas, Leimbach, Reagen, Koekemoer, Anton M., Conselice, C. J., Dai, Liang, Goobar, Ariel, Siebert, Matthew R., Strolger, Lou, and Willner, S. P.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

The first James Webb Space Telescope ({\it JWST}) Near InfraRed Camera (NIRCam) imaging in the field of the galaxy cluster PLCK G165.7+67.0 ($z=0.35$) uncovered a Type Ia supernova (SN Ia) at $z=1.78$, called ``SN H0pe." Three different images of this one SN were detected as a result of strong gravitational lensing, each one traversing a different path in spacetime, thereby inducing a relative delay in the arrival of each image. Follow-up {\it JWST} observations of all three SN images enabled photometric and rare spectroscopic measurements of the two relative time delays. Following strict blinding protocols which oversaw a live unblinding and regulated post-unblinding changes, these two measured time delays were compared to the predictions of seven independently constructed cluster lens models to measure a value for the Hubble constant, $H_0=71.8^{+9.2}_{-8.1}$ km s$^{-1}$ Mpc$^{-1}$. The range of admissible $H_0$ values predicted across the lens models limits further precision, reflecting the well-known degeneracies between lens model constraints and time delays. It has long been theorized that a way forward is to leverage a standard candle, but this has not been realized until now. For the first time, the lens models are evaluated by their agreement with the SN absolute magnifications, breaking degeneracies and producing our best estimate, $H_0=75.7^{+8.1}_{-5.5}$ km s$^{-1}$ Mpc$^{-1}$. This is the first precision measurement of $H_0$ from a multiply-imaged SN Ia and only the second from any multiply-imaged SN., Comment: Accepted to ApJ. 27 pages, 7 Figures

Published
2024

38. Ground- and Space-Based Dust Observations of VV 191 Overlapping Galaxy Pair

Author

Robertson, C., Holwerda, B., Young, J., Keel, W., Berkheimer, J., Cook, K., Conselice, C., Frye, B., Grogin, N., Koekemoer, A., Nasr, C., Patel, D., Roemer, W., Smith, D., and Windhorst, R.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The Balmer decrement (H$\alpha$/H$\beta$) provides a constraint on attenuation, the cumulative effects of dust grains in the ISM. The ratio is a reliable spectroscopic tool for deriving the dust properties of galaxies that determine many different quantities such as star formation rate, metallicity, and SED models. Here we measure independently both the attenuation and H$\alpha$/H$\beta$ of an occulting galaxy pair: VV 191. Attenuation measurements in the visible spectrum (A$_{V,stars}$) from dust maps derived from the F606W filter of HST and the F090W filter of JWST are matched with spaxel-by-spaxel H$\alpha$/H$\beta$ observations from the George and Cynthia Mitchell Spectrograph (GCMS) of the McDonald Observatory. The 0.5 to 0.7 micron bandpass covers the Balmer lines for VV 191. The dust maps of JWST and HST provide the high sensitivity necessary for comparisons and tracking trends of the geometrically favorable galaxy. We present maps and plots of the Balmer lines for the VV 191 galaxy pair and for a specific region highlighting dust lanes for VV 191b in the overlap region. We compute A$_{V, HII}$ from H$\alpha$/H$\beta$ and plot both quantities against A$_{V, stars}$. Our results show that regions with higher dust content, residing closer to the spiral center, dominate ionized gas attenuation, leading to an overestimation of A$_{V, HII}$ by a factor or 2. Further out in the spiral arms, the lower dust content leads to more agreement between the attenuations, indicating lower SFR and larger contribution from older stars to the stellar continuum outside the Petrosian radius., Comment: 21 pages, 14 figures, 2 tables, accepted for publication by The Astronomical Journal

Published
2024

39. Gemini 1.5: Unlocking multimodal understanding across millions of tokens of context

Author

Gemini Team, Georgiev, Petko, Lei, Ving Ian, Burnell, Ryan, Bai, Libin, Gulati, Anmol, Tanzer, Garrett, Vincent, Damien, Pan, Zhufeng, Wang, Shibo, Mariooryad, Soroosh, Ding, Yifan, Geng, Xinyang, Alcober, Fred, Frostig, Roy, Omernick, Mark, Walker, Lexi, Paduraru, Cosmin, Sorokin, Christina, Tacchetti, Andrea, Gaffney, Colin, Daruki, Samira, Sercinoglu, Olcan, Gleicher, Zach, Love, Juliette, Voigtlaender, Paul, Jain, Rohan, Surita, Gabriela, Mohamed, Kareem, Blevins, Rory, Ahn, Junwhan, Zhu, Tao, Kawintiranon, Kornraphop, Firat, Orhan, Gu, Yiming, Zhang, Yujing, Rahtz, Matthew, Faruqui, Manaal, Clay, Natalie, Gilmer, Justin, Co-Reyes, JD, Penchev, Ivo, Zhu, Rui, Morioka, Nobuyuki, Hui, Kevin, Haridasan, Krishna, Campos, Victor, Mahdieh, Mahdis, Guo, Mandy, Hassan, Samer, Kilgour, Kevin, Vezer, Arpi, Cheng, Heng-Tze, de Liedekerke, Raoul, Goyal, Siddharth, Barham, Paul, Strouse, DJ, Noury, Seb, Adler, Jonas, Sundararajan, Mukund, Vikram, Sharad, Lepikhin, Dmitry, Paganini, Michela, Garcia, Xavier, Yang, Fan, Valter, Dasha, Trebacz, Maja, Vodrahalli, Kiran, Asawaroengchai, Chulayuth, Ring, Roman, Kalb, Norbert, Soares, Livio Baldini, Brahma, Siddhartha, Steiner, David, Yu, Tianhe, Mentzer, Fabian, He, Antoine, Gonzalez, Lucas, Xu, Bibo, Kaufman, Raphael Lopez, Shafey, Laurent El, Oh, Junhyuk, Hennigan, Tom, Driessche, George van den, Odoom, Seth, Lucic, Mario, Roelofs, Becca, Lall, Sid, Marathe, Amit, Chan, Betty, Ontanon, Santiago, He, Luheng, Teplyashin, Denis, Lai, Jonathan, Crone, Phil, Damoc, Bogdan, Ho, Lewis, Riedel, Sebastian, Lenc, Karel, Yeh, Chih-Kuan, Chowdhery, Aakanksha, Xu, Yang, Kazemi, Mehran, Amid, Ehsan, Petrushkina, Anastasia, Swersky, Kevin, Khodaei, Ali, Chen, Gowoon, Larkin, Chris, Pinto, Mario, Yan, Geng, Badia, Adria Puigdomenech, Patil, Piyush, Hansen, Steven, Orr, Dave, Arnold, Sebastien M. R., Grimstad, Jordan, Dai, Andrew, Douglas, Sholto, Sinha, Rishika, Yadav, Vikas, Chen, Xi, Gribovskaya, Elena, Austin, Jacob, Zhao, Jeffrey, Patel, Kaushal, Komarek, Paul, Austin, Sophia, Borgeaud, Sebastian, Friso, Linda, Goyal, Abhimanyu, Caine, Ben, Cao, Kris, Chung, Da-Woon, Lamm, Matthew, Barth-Maron, Gabe, Kagohara, Thais, Olszewska, Kate, Chen, Mia, Shivakumar, Kaushik, Agarwal, Rishabh, Godhia, Harshal, Rajwar, Ravi, Snaider, Javier, Dotiwalla, Xerxes, Liu, Yuan, Barua, Aditya, Ungureanu, Victor, Zhang, Yuan, Batsaikhan, Bat-Orgil, Wirth, Mateo, Qin, James, Danihelka, Ivo, Doshi, Tulsee, Chadwick, Martin, Chen, Jilin, Jain, Sanil, Le, Quoc, Kar, Arjun, Gurumurthy, Madhu, Li, Cheng, Sang, Ruoxin, Liu, Fangyu, Lamprou, Lampros, Munoz, Rich, Lintz, Nathan, Mehta, Harsh, Howard, Heidi, Reynolds, Malcolm, Aroyo, Lora, Wang, Quan, Blanco, Lorenzo, Cassirer, Albin, Griffith, Jordan, Das, Dipanjan, Lee, Stephan, Sygnowski, Jakub, Fisher, Zach, Besley, James, Powell, Richard, Ahmed, Zafarali, Paulus, Dominik, Reitter, David, Borsos, Zalan, Joshi, Rishabh, Pope, Aedan, Hand, Steven, Selo, Vittorio, Jain, Vihan, Sethi, Nikhil, Goel, Megha, Makino, Takaki, May, Rhys, Yang, Zhen, Schalkwyk, Johan, Butterfield, Christina, Hauth, Anja, Goldin, Alex, Hawkins, Will, Senter, Evan, Brin, Sergey, Woodman, Oliver, Ritter, Marvin, Noland, Eric, Giang, Minh, Bolina, Vijay, Lee, Lisa, Blyth, Tim, Mackinnon, Ian, Reid, Machel, Sarvana, Obaid, Silver, David, Chen, Alexander, Wang, Lily, Maggiore, Loren, Chang, Oscar, Attaluri, Nithya, Thornton, Gregory, Chiu, Chung-Cheng, Bunyan, Oskar, Levine, Nir, Chung, Timothy, Eltyshev, Evgenii, Si, Xiance, Lillicrap, Timothy, Brady, Demetra, Aggarwal, Vaibhav, Wu, Boxi, Xu, Yuanzhong, McIlroy, Ross, Badola, Kartikeya, Sandhu, Paramjit, Moreira, Erica, Stokowiec, Wojciech, Hemsley, Ross, Li, Dong, Tudor, Alex, Shyam, Pranav, Rahimtoroghi, Elahe, Haykal, Salem, Sprechmann, Pablo, Zhou, Xiang, Mincu, Diana, Li, Yujia, Addanki, Ravi, Krishna, Kalpesh, Wu, Xiao, Frechette, Alexandre, Eyal, Matan, Dafoe, Allan, Lacey, Dave, Whang, Jay, Avrahami, Thi, Zhang, Ye, Taropa, Emanuel, Lin, Hanzhao, Toyama, Daniel, Rutherford, Eliza, Sano, Motoki, Choe, HyunJeong, Tomala, Alex, Safranek-Shrader, Chalence, Kassner, Nora, Pajarskas, Mantas, Harvey, Matt, Sechrist, Sean, Fortunato, Meire, Lyu, Christina, Elsayed, Gamaleldin, Kuang, Chenkai, Lottes, James, Chu, Eric, Jia, Chao, Chen, Chih-Wei, Humphreys, Peter, Baumli, Kate, Tao, Connie, Samuel, Rajkumar, Santos, Cicero Nogueira dos, Andreassen, Anders, Rakićević, Nemanja, Grewe, Dominik, Kumar, Aviral, Winkler, Stephanie, Caton, Jonathan, Brock, Andrew, Dalmia, Sid, Sheahan, Hannah, Barr, Iain, Miao, Yingjie, Natsev, Paul, Devlin, Jacob, Behbahani, Feryal, Prost, Flavien, Sun, Yanhua, Myaskovsky, Artiom, Pillai, Thanumalayan Sankaranarayana, Hurt, Dan, Lazaridou, Angeliki, Xiong, Xi, Zheng, Ce, Pardo, Fabio, Li, Xiaowei, Horgan, Dan, Stanton, Joe, Ambar, Moran, Xia, Fei, Lince, Alejandro, Wang, Mingqiu, Mustafa, Basil, Webson, Albert, Lee, Hyo, Anil, Rohan, Wicke, Martin, Dozat, Timothy, Sinha, Abhishek, Piqueras, Enrique, Dabir, Elahe, Upadhyay, Shyam, Boral, Anudhyan, Hendricks, Lisa Anne, Fry, Corey, Djolonga, Josip, Su, Yi, Walker, Jake, Labanowski, Jane, Huang, Ronny, Misra, Vedant, Chen, Jeremy, Skerry-Ryan, RJ, Singh, Avi, Rijhwani, Shruti, Yu, Dian, Castro-Ros, Alex, Changpinyo, Beer, Datta, Romina, Bagri, Sumit, Hrafnkelsson, Arnar Mar, Maggioni, Marcello, Zheng, Daniel, Sulsky, Yury, Hou, Shaobo, Paine, Tom Le, Yang, Antoine, Riesa, Jason, Rogozinska, Dominika, Marcus, Dror, Badawy, Dalia El, Zhang, Qiao, Wang, Luyu, Miller, Helen, Greer, Jeremy, Sjos, Lars Lowe, Nova, Azade, Zen, Heiga, Chaabouni, Rahma, Rosca, Mihaela, Jiang, Jiepu, Chen, Charlie, Liu, Ruibo, Sainath, Tara, Krikun, Maxim, Polozov, Alex, Lespiau, Jean-Baptiste, Newlan, Josh, Cankara, Zeyncep, Kwak, Soo, Xu, Yunhan, Chen, Phil, Coenen, Andy, Meyer, Clemens, Tsihlas, Katerina, Ma, Ada, Gottweis, Juraj, Xing, Jinwei, Gu, Chenjie, Miao, Jin, Frank, Christian, Cankara, Zeynep, Ganapathy, Sanjay, Dasgupta, Ishita, Hughes-Fitt, Steph, Chen, Heng, Reid, David, Rong, Keran, Fan, Hongmin, van Amersfoort, Joost, Zhuang, Vincent, Cohen, Aaron, Gu, Shixiang Shane, Mohananey, Anhad, Ilic, Anastasija, Tobin, Taylor, Wieting, John, Bortsova, Anna, Thacker, Phoebe, Wang, Emma, Caveness, Emily, Chiu, Justin, Sezener, Eren, Kaskasoli, Alex, Baker, Steven, Millican, Katie, Elhawaty, Mohamed, Aisopos, Kostas, Lebsack, Carl, Byrd, Nathan, Dai, Hanjun, Jia, Wenhao, Wiethoff, Matthew, Davoodi, Elnaz, Weston, Albert, Yagati, Lakshman, Ahuja, Arun, Gao, Isabel, Pundak, Golan, Zhang, Susan, Azzam, Michael, Sim, Khe Chai, Caelles, Sergi, Keeling, James, Sharma, Abhanshu, Swing, Andy, Li, YaGuang, Liu, Chenxi, Bostock, Carrie Grimes, Bansal, Yamini, Nado, Zachary, Anand, Ankesh, Lipschultz, Josh, Karmarkar, Abhijit, Proleev, Lev, Ittycheriah, Abe, Yeganeh, Soheil Hassas, Polovets, George, Faust, Aleksandra, Sun, Jiao, Rrustemi, Alban, Li, Pen, Shivanna, Rakesh, Liu, Jeremiah, Welty, Chris, Lebron, Federico, Baddepudi, Anirudh, Krause, Sebastian, Parisotto, Emilio, Soricut, Radu, Xu, Zheng, Bloxwich, Dawn, Johnson, Melvin, Neyshabur, Behnam, Mao-Jones, Justin, Wang, Renshen, Ramasesh, Vinay, Abbas, Zaheer, Guez, Arthur, Segal, Constant, Nguyen, Duc Dung, Svensson, James, Hou, Le, York, Sarah, Milan, Kieran, Bridgers, Sophie, Gworek, Wiktor, Tagliasacchi, Marco, Lee-Thorp, James, Chang, Michael, Guseynov, Alexey, Hartman, Ale Jakse, Kwong, Michael, Zhao, Ruizhe, Kashem, Sheleem, Cole, Elizabeth, Miech, Antoine, Tanburn, Richard, Phuong, Mary, Pavetic, Filip, Cevey, Sebastien, Comanescu, Ramona, Ives, Richard, Yang, Sherry, Du, Cosmo, Li, Bo, Zhang, Zizhao, Iinuma, Mariko, Hu, Clara Huiyi, Roy, Aurko, Bijwadia, Shaan, Zhu, Zhenkai, Martins, Danilo, Saputro, Rachel, Gergely, Anita, Zheng, Steven, Jia, Dawei, Antonoglou, Ioannis, Sadovsky, Adam, Gu, Shane, Bi, Yingying, Andreev, Alek, Samangooei, Sina, Khan, Mina, Kocisky, Tomas, Filos, Angelos, Kumar, Chintu, Bishop, Colton, Yu, Adams, Hodkinson, Sarah, Mittal, Sid, Shah, Premal, Moufarek, Alexandre, Cheng, Yong, Bloniarz, Adam, Lee, Jaehoon, Pejman, Pedram, Michel, Paul, Spencer, Stephen, Feinberg, Vladimir, Xiong, Xuehan, Savinov, Nikolay, Smith, Charlotte, Shakeri, Siamak, Tran, Dustin, Chesus, Mary, Bohnet, Bernd, Tucker, George, von Glehn, Tamara, Muir, Carrie, Mao, Yiran, Kazawa, Hideto, Slone, Ambrose, Soparkar, Kedar, Shrivastava, Disha, Cobon-Kerr, James, Sharman, Michael, Pavagadhi, Jay, Araya, Carlos, Misiunas, Karolis, Ghelani, Nimesh, Laskin, Michael, Barker, David, Li, Qiujia, Briukhov, Anton, Houlsby, Neil, Glaese, Mia, Lakshminarayanan, Balaji, Schucher, Nathan, Tang, Yunhao, Collins, Eli, Lim, Hyeontaek, Feng, Fangxiaoyu, Recasens, Adria, Lai, Guangda, Magni, Alberto, De Cao, Nicola, Siddhant, Aditya, Ashwood, Zoe, Orbay, Jordi, Dehghani, Mostafa, Brennan, Jenny, He, Yifan, Xu, Kelvin, Gao, Yang, Saroufim, Carl, Molloy, James, Wu, Xinyi, Arnold, Seb, Chang, Solomon, Schrittwieser, Julian, Buchatskaya, Elena, Radpour, Soroush, Polacek, Martin, Giordano, Skye, Bapna, Ankur, Tokumine, Simon, Hellendoorn, Vincent, Sottiaux, Thibault, Cogan, Sarah, Severyn, Aliaksei, Saleh, Mohammad, Thakoor, Shantanu, Shefey, Laurent, Qiao, Siyuan, Gaba, Meenu, Chang, Shuo-yiin, Swanson, Craig, Zhang, Biao, Lee, Benjamin, Rubenstein, Paul Kishan, Song, Gan, Kwiatkowski, Tom, Koop, Anna, Kannan, Ajay, Kao, David, Schuh, Parker, Stjerngren, Axel, Ghiasi, Golnaz, Gibson, Gena, Vilnis, Luke, Yuan, Ye, Ferreira, Felipe Tiengo, Kamath, Aishwarya, Klimenko, Ted, Franko, Ken, Xiao, Kefan, Bhattacharya, Indro, Patel, Miteyan, Wang, Rui, Morris, Alex, Strudel, Robin, Sharma, Vivek, Choy, Peter, Hashemi, Sayed Hadi, Landon, Jessica, Finkelstein, Mara, Jhakra, Priya, Frye, Justin, Barnes, Megan, Mauger, Matthew, Daun, Dennis, Baatarsukh, Khuslen, Tung, Matthew, Farhan, Wael, Michalewski, Henryk, Viola, Fabio, Quitry, Felix de Chaumont, Lan, Charline Le, Hudson, Tom, Wang, Qingze, Fischer, Felix, Zheng, Ivy, White, Elspeth, Dragan, Anca, Alayrac, Jean-baptiste, Ni, Eric, Pritzel, Alexander, Iwanicki, Adam, Isard, Michael, Bulanova, Anna, Zilka, Lukas, Dyer, Ethan, Sachan, Devendra, Srinivasan, Srivatsan, Muckenhirn, Hannah, Cai, Honglong, Mandhane, Amol, Tariq, Mukarram, Rae, Jack W., Wang, Gary, Ayoub, Kareem, FitzGerald, Nicholas, Zhao, Yao, Han, Woohyun, Alberti, Chris, Garrette, Dan, Krishnakumar, Kashyap, Gimenez, Mai, Levskaya, Anselm, Sohn, Daniel, Matak, Josip, Iturrate, Inaki, Chang, Michael B., Xiang, Jackie, Cao, Yuan, Ranka, Nishant, Brown, Geoff, Hutter, Adrian, Mirrokni, Vahab, Chen, Nanxin, Yao, Kaisheng, Egyed, Zoltan, Galilee, Francois, Liechty, Tyler, Kallakuri, Praveen, Palmer, Evan, Ghemawat, Sanjay, Liu, Jasmine, Tao, David, Thornton, Chloe, Green, Tim, Jasarevic, Mimi, Lin, Sharon, Cotruta, Victor, Tan, Yi-Xuan, Fiedel, Noah, Yu, Hongkun, Chi, Ed, Neitz, Alexander, Heitkaemper, Jens, Sinha, Anu, Zhou, Denny, Sun, Yi, Kaed, Charbel, Hulse, Brice, Mishra, Swaroop, Georgaki, Maria, Kudugunta, Sneha, Farabet, Clement, Shafran, Izhak, Vlasic, Daniel, Tsitsulin, Anton, Ananthanarayanan, Rajagopal, Carin, Alen, Su, Guolong, Sun, Pei, V, Shashank, Carvajal, Gabriel, Broder, Josef, Comsa, Iulia, Repina, Alena, Wong, William, Chen, Warren Weilun, Hawkins, Peter, Filonov, Egor, Loher, Lucia, Hirnschall, Christoph, Wang, Weiyi, Ye, Jingchen, Burns, Andrea, Cate, Hardie, Wright, Diana Gage, Piccinini, Federico, Zhang, Lei, Lin, Chu-Cheng, Gog, Ionel, Kulizhskaya, Yana, Sreevatsa, Ashwin, Song, Shuang, Cobo, Luis C., Iyer, Anand, Tekur, Chetan, Garrido, Guillermo, Xiao, Zhuyun, Kemp, Rupert, Zheng, Huaixiu Steven, Li, Hui, Agarwal, Ananth, Ngani, Christel, Goshvadi, Kati, Santamaria-Fernandez, Rebeca, Fica, Wojciech, Chen, Xinyun, Gorgolewski, Chris, Sun, Sean, Garg, Roopal, Ye, Xinyu, Eslami, S. M. Ali, Hua, Nan, Simon, Jon, Joshi, Pratik, Kim, Yelin, Tenney, Ian, Potluri, Sahitya, Thiet, Lam Nguyen, Yuan, Quan, Luisier, Florian, Chronopoulou, Alexandra, Scellato, Salvatore, Srinivasan, Praveen, Chen, Minmin, Koverkathu, Vinod, Dalibard, Valentin, Xu, Yaming, Saeta, Brennan, Anderson, Keith, Sellam, Thibault, Fernando, Nick, Huot, Fantine, Jung, Junehyuk, Varadarajan, Mani, Quinn, Michael, Raul, Amit, Le, Maigo, Habalov, Ruslan, Clark, Jon, Jalan, Komal, Bullard, Kalesha, Singhal, Achintya, Luong, Thang, Wang, Boyu, Rajayogam, Sujeevan, Eisenschlos, Julian, Jia, Johnson, Finchelstein, Daniel, Yakubovich, Alex, Balle, Daniel, Fink, Michael, Agarwal, Sameer, Li, Jing, Dvijotham, Dj, Pal, Shalini, Kang, Kai, Konzelmann, Jaclyn, Beattie, Jennifer, Dousse, Olivier, Wu, Diane, Crocker, Remi, Elkind, Chen, Jonnalagadda, Siddhartha Reddy, Lee, Jong, Holtmann-Rice, Dan, Kallarackal, Krystal, Liu, Rosanne, Vnukov, Denis, Vats, Neera, Invernizzi, Luca, Jafari, Mohsen, Zhou, Huanjie, Taylor, Lilly, Prendki, Jennifer, Wu, Marcus, Eccles, Tom, Liu, Tianqi, Kopparapu, Kavya, Beaufays, Francoise, Angermueller, Christof, Marzoca, Andreea, Sarcar, Shourya, Dib, Hilal, Stanway, Jeff, Perbet, Frank, Trdin, Nejc, Sterneck, Rachel, Khorlin, Andrey, Li, Dinghua, Wu, Xihui, Goenka, Sonam, Madras, David, Goldshtein, Sasha, Gierke, Willi, Zhou, Tong, Liu, Yaxin, Liang, Yannie, White, Anais, Li, Yunjie, Singh, Shreya, Bahargam, Sanaz, Epstein, Mark, Basu, Sujoy, Lao, Li, Ozturel, Adnan, Crous, Carl, Zhai, Alex, Lu, Han, Tung, Zora, Gaur, Neeraj, Walton, Alanna, Dixon, Lucas, Zhang, Ming, Globerson, Amir, Uy, Grant, Bolt, Andrew, Wiles, Olivia, Nasr, Milad, Shumailov, Ilia, Selvi, Marco, Piccinno, Francesco, Aguilar, Ricardo, McCarthy, Sara, Khalman, Misha, Shukla, Mrinal, Galic, Vlado, Carpenter, John, Villela, Kevin, Zhang, Haibin, Richardson, Harry, Martens, James, Bosnjak, Matko, Belle, Shreyas Rammohan, Seibert, Jeff, Alnahlawi, Mahmoud, McWilliams, Brian, Singh, Sankalp, Louis, Annie, Ding, Wen, Popovici, Dan, Simicich, Lenin, Knight, Laura, Mehta, Pulkit, Gupta, Nishesh, Shi, Chongyang, Fatehi, Saaber, Mitrovic, Jovana, Grills, Alex, Pagadora, Joseph, Munkhdalai, Tsendsuren, Petrova, Dessie, Eisenbud, Danielle, Zhang, Zhishuai, Yates, Damion, Mittal, Bhavishya, Tripuraneni, Nilesh, Assael, Yannis, Brovelli, Thomas, Jain, Prateek, Velimirovic, Mihajlo, Akbulut, Canfer, Mu, Jiaqi, Macherey, Wolfgang, Kumar, Ravin, Xu, Jun, Qureshi, Haroon, Comanici, Gheorghe, Wiesner, Jeremy, Gong, Zhitao, Ruddock, Anton, Bauer, Matthias, Felt, Nick, GP, Anirudh, Arnab, Anurag, Zelle, Dustin, Rothfuss, Jonas, Rosgen, Bill, Shenoy, Ashish, Seybold, Bryan, Li, Xinjian, Mudigonda, Jayaram, Erdogan, Goker, Xia, Jiawei, Simsa, Jiri, Michi, Andrea, Yao, Yi, Yew, Christopher, Kan, Steven, Caswell, Isaac, Radebaugh, Carey, Elisseeff, Andre, Valenzuela, Pedro, McKinney, Kay, Paterson, Kim, Cui, Albert, Latorre-Chimoto, Eri, Kim, Solomon, Zeng, William, Durden, Ken, Ponnapalli, Priya, Sosea, Tiberiu, Choquette-Choo, Christopher A., Manyika, James, Robenek, Brona, Vashisht, Harsha, Pereira, Sebastien, Lam, Hoi, Velic, Marko, Owusu-Afriyie, Denese, Lee, Katherine, Bolukbasi, Tolga, Parrish, Alicia, Lu, Shawn, Park, Jane, Venkatraman, Balaji, Talbert, Alice, Rosique, Lambert, Cheng, Yuchung, Sozanschi, Andrei, Paszke, Adam, Kumar, Praveen, Austin, Jessica, Li, Lu, Salama, Khalid, Perz, Bartek, Kim, Wooyeol, Dukkipati, Nandita, Baryshnikov, Anthony, Kaplanis, Christos, Sheng, XiangHai, Chervonyi, Yuri, Unlu, Caglar, Casas, Diego de Las, Askham, Harry, Tunyasuvunakool, Kathryn, Gimeno, Felix, Poder, Siim, Kwak, Chester, Miecnikowski, Matt, Dimitriev, Alek, Parisi, Aaron, Liu, Dangyi, Tsai, Tomy, Shevlane, Toby, Kouridi, Christina, Garmon, Drew, Goedeckemeyer, Adrian, Brown, Adam R., Vijayakumar, Anitha, Elqursh, Ali, Jazayeri, Sadegh, Huang, Jin, Carthy, Sara Mc, Hoover, Jay, Kim, Lucy, Kumar, Sandeep, Chen, Wei, Biles, Courtney, Bingham, Garrett, Rosen, Evan, Wang, Lisa, Tan, Qijun, Engel, David, Pongetti, Francesco, de Cesare, Dario, Hwang, Dongseong, Yu, Lily, Pullman, Jennifer, Narayanan, Srini, Levin, Kyle, Gopal, Siddharth, Li, Megan, Aharoni, Asaf, Trinh, Trieu, Lo, Jessica, Casagrande, Norman, Vij, Roopali, Matthey, Loic, Ramadhana, Bramandia, Matthews, Austin, Carey, CJ, Johnson, Matthew, Goranova, Kremena, Shah, Rohin, Ashraf, Shereen, Dasgupta, Kingshuk, Larsen, Rasmus, Wang, Yicheng, Vuyyuru, Manish Reddy, Jiang, Chong, Ijazi, Joana, Osawa, Kazuki, Smith, Celine, Boppana, Ramya Sree, Bilal, Taylan, Koizumi, Yuma, Xu, Ying, Altun, Yasemin, Shabat, Nir, Bariach, Ben, Korchemniy, Alex, Choo, Kiam, Ronneberger, Olaf, Iwuanyanwu, Chimezie, Zhao, Shubin, Soergel, David, Hsieh, Cho-Jui, Cai, Irene, Iqbal, Shariq, Sundermeyer, Martin, Chen, Zhe, Bursztein, Elie, Malaviya, Chaitanya, Biadsy, Fadi, Shroff, Prakash, Dhillon, Inderjit, Latkar, Tejasi, Dyer, Chris, Forbes, Hannah, Nicosia, Massimo, Nikolaev, Vitaly, Greene, Somer, Georgiev, Marin, Wang, Pidong, Martin, Nina, Sedghi, Hanie, Zhang, John, Banzal, Praseem, Fritz, Doug, Rao, Vikram, Wang, Xuezhi, Zhang, Jiageng, Patraucean, Viorica, Du, Dayou, Mordatch, Igor, Jurin, Ivan, Liu, Lewis, Dubey, Ayush, Mohan, Abhi, Nowakowski, Janek, Ion, Vlad-Doru, Wei, Nan, Tojo, Reiko, Raad, Maria Abi, Hudson, Drew A., Keshava, Vaishakh, Agrawal, Shubham, Ramirez, Kevin, Wu, Zhichun, Nguyen, Hoang, Liu, Ji, Sewak, Madhavi, Petrini, Bryce, Choi, DongHyun, Philips, Ivan, Wang, Ziyue, Bica, Ioana, Garg, Ankush, Wilkiewicz, Jarek, Agrawal, Priyanka, Guo, Danhao, Xue, Emily, Shaik, Naseer, Leach, Andrew, Khan, Sadh MNM, Wiesinger, Julia, Jerome, Sammy, Chakladar, Abhishek, Wang, Alek Wenjiao, Ornduff, Tina, Abu, Folake, Ghaffarkhah, Alireza, Wainwright, Marcus, Cortes, Mario, Liu, Frederick, Maynez, Joshua, Terzis, Andreas, Samangouei, Pouya, Mansour, Riham, Kępa, Tomasz, Aubet, François-Xavier, Algymr, Anton, Banica, Dan, Weisz, Agoston, Orban, Andras, Senges, Alexandre, Andrejczuk, Ewa, Geller, Mark, Santo, Niccolo Dal, Anklin, Valentin, Merey, Majd Al, Baeuml, Martin, Strohman, Trevor, Bai, Junwen, Petrov, Slav, Wu, Yonghui, Hassabis, Demis, Kavukcuoglu, Koray, Dean, Jeff, and Vinyals, Oriol

Subjects
Computer Science - Computation and Language, Computer Science - Artificial Intelligence
Abstract

In this report, we introduce the Gemini 1.5 family of models, representing the next generation of highly compute-efficient multimodal models capable of recalling and reasoning over fine-grained information from millions of tokens of context, including multiple long documents and hours of video and audio. The family includes two new models: (1) an updated Gemini 1.5 Pro, which exceeds the February version on the great majority of capabilities and benchmarks; (2) Gemini 1.5 Flash, a more lightweight variant designed for efficiency with minimal regression in quality. Gemini 1.5 models achieve near-perfect recall on long-context retrieval tasks across modalities, improve the state-of-the-art in long-document QA, long-video QA and long-context ASR, and match or surpass Gemini 1.0 Ultra's state-of-the-art performance across a broad set of benchmarks. Studying the limits of Gemini 1.5's long-context ability, we find continued improvement in next-token prediction and near-perfect retrieval (>99%) up to at least 10M tokens, a generational leap over existing models such as Claude 3.0 (200k) and GPT-4 Turbo (128k). Finally, we highlight real-world use cases, such as Gemini 1.5 collaborating with professionals on completing their tasks achieving 26 to 75% time savings across 10 different job categories, as well as surprising new capabilities of large language models at the frontier; when given a grammar manual for Kalamang, a language with fewer than 200 speakers worldwide, the model learns to translate English to Kalamang at a similar level to a person who learned from the same content.

Published
2024

40. EPOCHS IV: SED Modelling Assumptions and their impact on the Stellar Mass Function at 6.5 < z < 13.5 using PEARLS and public JWST observations

Author

Harvey, Thomas, Conselice, Christopher J., Adams, Nathan J., Austin, Duncan, Juodzbalis, Ignas, Trussler, James, Li, Qiong, Ormerod, Katherine, Ferreira, Leonardo, Lovell, Christopher C., Duan, Qiao, Westcott, Lewi, Harris, Honor, Bhatawdekar, Rachana, Coe, Dan, Cohen, Seth H., Caruana, Joseph, Cheng, Cheng, Driver, Simon P., Frye, Brenda, Furtak, Lukas J., Grogin, Norman A., Hathi, Nimish P., Holwerda, Benne W., Jansen, Rolf A., Koekemoer, Anton M., Marshall, Madeline A., Nonino, Mario, Vijayan, Aswin P., Wilkins, Stephen M., Windhorst, Rogier, Willmer, Christopher N. A., Yan, Haojing, and Zitrin, Adi

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We utilize deep JWST NIRCam observations for the first direct constraints on the Galaxy Stellar Mass Function (GSMF) at $z>10$. Our EPOCHS v1 sample includes 1120 galaxy candidates at $6.5

Published
2024
Full Text
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41. Spillover of highly pathogenic avian influenza H5N1 virus to dairy cattle

Author

Caserta, Leonardo C., Frye, Elisha A., Butt, Salman L., Laverack, Melissa, Nooruzzaman, Mohammed, Covaleda, Lina M., Thompson, Alexis C., Koscielny, Melanie Prarat, Cronk, Brittany, Johnson, Ashley, Kleinhenz, Katie, Edwards, Erin E., Gomez, Gabriel, Hitchener, Gavin, Martins, Mathias, Kapczynski, Darrell R., Suarez, David L., Alexander Morris, Ellen Ruth, Hensley, Terry, Beeby, John S., Lejeune, Manigandan, Swinford, Amy K., Elvinger, François, Dimitrov, Kiril M., and Diel, Diego G.

Published
2024
Full Text
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42. Spin--spin interaction and magnetic Feshbach resonances in collisions of high-spin atoms with closed-shell atoms

Author

Frye, Matthew D., Żuchowski, Piotr S., and Tomza, Michał

Subjects
Physics - Atomic Physics
Abstract

We investigate interactions and ultracold collisions of high-spin but spherical atoms with closed-shell atoms, focussing on the example of Cr with Yb. Such a combination has only one potential energy curve but gives rise to a substantial intra-atomic spin--spin interaction, which causes Feshbach resonances due to rotationally excited states. We find such resonances are guaranteed below 250 G and can reach widths of 10s of G in favorable circumstances. We study the effect of hyperfine structure, which can create additional wide resonances at low fields. Finally, we consider isotopic substitution and show that for any realistic potential it is very likely at least one combination of commonly used isotopes will have resonances with experimentally favorable properties. Thus, this is a promising system for both molecule formation and studying quantum mixtures including dipolar species.

Published
2024
Full Text
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43. TREASUREHUNT: Transients and Variability Discovered with HST in the JWST North Ecliptic Pole Time Domain Field

Author

O'Brien, Rosalia, Jansen, Rolf A., Grogin, Norman A., Cohen, Seth H., Smith, Brent M., Silver, Ross M., Maksym III, W. P., Windhorst, Rogier A., Carleton, Timothy, Koekemoer, Anton M., Hathi, Nimish P., Willmer, Christopher N. A., Frye, Brenda L., Alpaslan, M., Ashby, M. L. N., Ashcraft, T. A., Bonoli, S., Brisken, W., Cappelluti, N., Civano, F., Conselice, C. J., Dhillon, V. S., Driver, S. P., Duncan, K. J., Dupke, R., Elvis, M., Fazio, G. G., Finkelstein, S. L., Gim, H. B., Griffiths, A., Hammel, H. B., Hyun, M., Im, M., Jones, V. R., Kim, D., Ladjelate, B., Larson, R. L., Malhotra, S., Marshall, M. A., Milam, S. N., Pierel, J. D. R., Rhoads, J. E., Rodney, S. A., Röttgering, H. J. A., Rutkowski, M. J., Ryan, Jr., R. E., Ward, M. J., White, C. W., van Weeren, R. J., Zhao, X., Summers, J., D'Silva, J. C. J., Ortiz III, R., Robotham, A. S. G., Coe, D., Nonino, M., Pirzkal, N., Yan, H., and Acharya, T.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The JWST North Ecliptic Pole (NEP) Time Domain Field (TDF) is a $>$14 arcmin diameter field optimized for multi-wavelength time-domain science with JWST. It has been observed across the electromagnetic spectrum both from the ground and from space, including with the Hubble Space Telescope (HST). As part of HST observations over 3 cycles (the "TREASUREHUNT" program), deep images were obtained with ACS/WFC in F435W and F606W that cover almost the entire JWST NEP TDF. Many of the individual pointings of these programs partially overlap, allowing an initial assessment of the potential of this field for time-domain science with HST and JWST. The cumulative area of overlapping pointings is ~88 arcmin$^2$, with time intervals between individual epochs that range between 1 day and 4$+$ years. To a depth of $m_{AB}$ $\simeq$ 29.5 mag (F606W), we present the discovery of 12 transients and 190 variable candidates. For the variable candidates, we demonstrate that Gaussian statistics are applicable, and estimate that ~80 are false positives. The majority of the transients will be supernovae, although at least two are likely quasars. Most variable candidates are AGN, where we find 0.42% of the general $z$ $<$ 6 field galaxy population to vary at the $~3\sigma$ level. Based on a 5-year timeframe, this translates into a random supernova areal density of up to ~0.07 transients per arcmin$^2$ (~245 deg$^{-2}$) per epoch, and a variable AGN areal density of ~1.25 variables per arcmin$^2$ (~4500 deg$^{-2}$) to these depths., Comment: 32 pages, 11 figures, 5 tables, 1 Appendix

Published
2024

44. Gemini: A Family of Highly Capable Multimodal Models

Author

Gemini Team, Anil, Rohan, Borgeaud, Sebastian, Alayrac, Jean-Baptiste, Yu, Jiahui, Soricut, Radu, Schalkwyk, Johan, Dai, Andrew M., Hauth, Anja, Millican, Katie, Silver, David, Johnson, Melvin, Antonoglou, Ioannis, Schrittwieser, Julian, Glaese, Amelia, Chen, Jilin, Pitler, Emily, Lillicrap, Timothy, Lazaridou, Angeliki, Firat, Orhan, Molloy, James, Isard, Michael, Barham, Paul R., Hennigan, Tom, Lee, Benjamin, Viola, Fabio, Reynolds, Malcolm, Xu, Yuanzhong, Doherty, Ryan, Collins, Eli, Meyer, Clemens, Rutherford, Eliza, Moreira, Erica, Ayoub, Kareem, Goel, Megha, Krawczyk, Jack, Du, Cosmo, Chi, Ed, Cheng, Heng-Tze, Ni, Eric, Shah, Purvi, Kane, Patrick, Chan, Betty, Faruqui, Manaal, Severyn, Aliaksei, Lin, Hanzhao, Li, YaGuang, Cheng, Yong, Ittycheriah, Abe, Mahdieh, Mahdis, Chen, Mia, Sun, Pei, Tran, Dustin, Bagri, Sumit, Lakshminarayanan, Balaji, Liu, Jeremiah, Orban, Andras, Güra, Fabian, Zhou, Hao, Song, Xinying, Boffy, Aurelien, Ganapathy, Harish, Zheng, Steven, Choe, HyunJeong, Weisz, Ágoston, Zhu, Tao, Lu, Yifeng, Gopal, Siddharth, Kahn, Jarrod, Kula, Maciej, Pitman, Jeff, Shah, Rushin, Taropa, Emanuel, Merey, Majd Al, Baeuml, Martin, Chen, Zhifeng, Shafey, Laurent El, Zhang, Yujing, Sercinoglu, Olcan, Tucker, George, Piqueras, Enrique, Krikun, Maxim, Barr, Iain, Savinov, Nikolay, Danihelka, Ivo, Roelofs, Becca, White, Anaïs, Andreassen, Anders, von Glehn, Tamara, Yagati, Lakshman, Kazemi, Mehran, Gonzalez, Lucas, Khalman, Misha, Sygnowski, Jakub, Frechette, Alexandre, Smith, Charlotte, Culp, Laura, Proleev, Lev, Luan, Yi, Chen, Xi, Lottes, James, Schucher, Nathan, Lebron, Federico, Rrustemi, Alban, Clay, Natalie, Crone, Phil, Kocisky, Tomas, Zhao, Jeffrey, Perz, Bartek, Yu, Dian, Howard, Heidi, Bloniarz, Adam, Rae, Jack W., Lu, Han, Sifre, Laurent, Maggioni, Marcello, Alcober, Fred, Garrette, Dan, Barnes, Megan, Thakoor, Shantanu, Austin, Jacob, Barth-Maron, Gabriel, Wong, William, Joshi, Rishabh, Chaabouni, Rahma, Fatiha, Deeni, Ahuja, Arun, Tomar, Gaurav Singh, Senter, Evan, Chadwick, Martin, Kornakov, Ilya, Attaluri, Nithya, Iturrate, Iñaki, Liu, Ruibo, Li, Yunxuan, Cogan, Sarah, Chen, Jeremy, Jia, Chao, Gu, Chenjie, Zhang, Qiao, Grimstad, Jordan, Hartman, Ale Jakse, Garcia, Xavier, Pillai, Thanumalayan Sankaranarayana, Devlin, Jacob, Laskin, Michael, Casas, Diego de Las, Valter, Dasha, Tao, Connie, Blanco, Lorenzo, Badia, Adrià Puigdomènech, Reitter, David, Chen, Mianna, Brennan, Jenny, Rivera, Clara, Brin, Sergey, Iqbal, Shariq, Surita, Gabriela, Labanowski, Jane, Rao, Abhi, Winkler, Stephanie, Parisotto, Emilio, Gu, Yiming, Olszewska, Kate, Addanki, Ravi, Miech, Antoine, Louis, Annie, Teplyashin, Denis, Brown, Geoff, Catt, Elliot, Balaguer, Jan, Xiang, Jackie, Wang, Pidong, Ashwood, Zoe, Briukhov, Anton, Webson, Albert, Ganapathy, Sanjay, Sanghavi, Smit, Kannan, Ajay, Chang, Ming-Wei, Stjerngren, Axel, Djolonga, Josip, Sun, Yuting, Bapna, Ankur, Aitchison, Matthew, Pejman, Pedram, Michalewski, Henryk, Yu, Tianhe, Wang, Cindy, Love, Juliette, Ahn, Junwhan, Bloxwich, Dawn, Han, Kehang, Humphreys, Peter, Sellam, Thibault, Bradbury, James, Godbole, Varun, Samangooei, Sina, Damoc, Bogdan, Kaskasoli, Alex, Arnold, Sébastien M. R., Vasudevan, Vijay, Agrawal, Shubham, Riesa, Jason, Lepikhin, Dmitry, Tanburn, Richard, Srinivasan, Srivatsan, Lim, Hyeontaek, Hodkinson, Sarah, Shyam, Pranav, Ferret, Johan, Hand, Steven, Garg, Ankush, Paine, Tom Le, Li, Jian, Li, Yujia, Giang, Minh, Neitz, Alexander, Abbas, Zaheer, York, Sarah, Reid, Machel, Cole, Elizabeth, Chowdhery, Aakanksha, Das, Dipanjan, Rogozińska, Dominika, Nikolaev, Vitaliy, Sprechmann, Pablo, Nado, Zachary, Zilka, Lukas, Prost, Flavien, He, Luheng, Monteiro, Marianne, Mishra, Gaurav, Welty, Chris, Newlan, Josh, Jia, Dawei, Allamanis, Miltiadis, Hu, Clara Huiyi, de Liedekerke, Raoul, Gilmer, Justin, Saroufim, Carl, Rijhwani, Shruti, Hou, Shaobo, Shrivastava, Disha, Baddepudi, Anirudh, Goldin, Alex, Ozturel, Adnan, Cassirer, Albin, Xu, Yunhan, Sohn, Daniel, Sachan, Devendra, Amplayo, Reinald Kim, Swanson, Craig, Petrova, Dessie, Narayan, Shashi, Guez, Arthur, Brahma, Siddhartha, Landon, Jessica, Patel, Miteyan, Zhao, Ruizhe, Villela, Kevin, Wang, Luyu, Jia, Wenhao, Rahtz, Matthew, Giménez, Mai, Yeung, Legg, Keeling, James, Georgiev, Petko, Mincu, Diana, Wu, Boxi, Haykal, Salem, Saputro, Rachel, Vodrahalli, Kiran, Qin, James, Cankara, Zeynep, Sharma, Abhanshu, Fernando, Nick, Hawkins, Will, Neyshabur, Behnam, Kim, Solomon, Hutter, Adrian, Agrawal, Priyanka, Castro-Ros, Alex, Driessche, George van den, Wang, Tao, Yang, Fan, Chang, Shuo-yiin, Komarek, Paul, McIlroy, Ross, Lučić, Mario, Zhang, Guodong, Farhan, Wael, Sharman, Michael, Natsev, Paul, Michel, Paul, Bansal, Yamini, Qiao, Siyuan, Cao, Kris, Shakeri, Siamak, Butterfield, Christina, Chung, Justin, Rubenstein, Paul Kishan, Agrawal, Shivani, Mensch, Arthur, Soparkar, Kedar, Lenc, Karel, Chung, Timothy, Pope, Aedan, Maggiore, Loren, Kay, Jackie, Jhakra, Priya, Wang, Shibo, Maynez, Joshua, Phuong, Mary, Tobin, Taylor, Tacchetti, Andrea, Trebacz, Maja, Robinson, Kevin, Katariya, Yash, Riedel, Sebastian, Bailey, Paige, Xiao, Kefan, Ghelani, Nimesh, Aroyo, Lora, Slone, Ambrose, Houlsby, Neil, Xiong, Xuehan, Yang, Zhen, Gribovskaya, Elena, Adler, Jonas, Wirth, Mateo, Lee, Lisa, Li, Music, Kagohara, Thais, Pavagadhi, Jay, Bridgers, Sophie, Bortsova, Anna, Ghemawat, Sanjay, Ahmed, Zafarali, Liu, Tianqi, Powell, Richard, Bolina, Vijay, Iinuma, Mariko, Zablotskaia, Polina, Besley, James, Chung, Da-Woon, Dozat, Timothy, Comanescu, Ramona, Si, Xiance, Greer, Jeremy, Su, Guolong, Polacek, Martin, Kaufman, Raphaël Lopez, Tokumine, Simon, Hu, Hexiang, Buchatskaya, Elena, Miao, Yingjie, Elhawaty, Mohamed, Siddhant, Aditya, Tomasev, Nenad, Xing, Jinwei, Greer, Christina, Miller, Helen, Ashraf, Shereen, Roy, Aurko, Zhang, Zizhao, Ma, Ada, Filos, Angelos, Besta, Milos, Blevins, Rory, Klimenko, Ted, Yeh, Chih-Kuan, Changpinyo, Soravit, Mu, Jiaqi, Chang, Oscar, Pajarskas, Mantas, Muir, Carrie, Cohen, Vered, Lan, Charline Le, Haridasan, Krishna, Marathe, Amit, Hansen, Steven, Douglas, Sholto, Samuel, Rajkumar, Wang, Mingqiu, Austin, Sophia, Lan, Chang, Jiang, Jiepu, Chiu, Justin, Lorenzo, Jaime Alonso, Sjösund, Lars Lowe, Cevey, Sébastien, Gleicher, Zach, Avrahami, Thi, Boral, Anudhyan, Srinivasan, Hansa, Selo, Vittorio, May, Rhys, Aisopos, Konstantinos, Hussenot, Léonard, Soares, Livio Baldini, Baumli, Kate, Chang, Michael B., Recasens, Adrià, Caine, Ben, Pritzel, Alexander, Pavetic, Filip, Pardo, Fabio, Gergely, Anita, Frye, Justin, Ramasesh, Vinay, Horgan, Dan, Badola, Kartikeya, Kassner, Nora, Roy, Subhrajit, Dyer, Ethan, Campos, Víctor Campos, Tomala, Alex, Tang, Yunhao, Badawy, Dalia El, White, Elspeth, Mustafa, Basil, Lang, Oran, Jindal, Abhishek, Vikram, Sharad, Gong, Zhitao, Caelles, Sergi, Hemsley, Ross, Thornton, Gregory, Feng, Fangxiaoyu, Stokowiec, Wojciech, Zheng, Ce, Thacker, Phoebe, Ünlü, Çağlar, Zhang, Zhishuai, Saleh, Mohammad, Svensson, James, Bileschi, Max, Patil, Piyush, Anand, Ankesh, Ring, Roman, Tsihlas, Katerina, Vezer, Arpi, Selvi, Marco, Shevlane, Toby, Rodriguez, Mikel, Kwiatkowski, Tom, Daruki, Samira, Rong, Keran, Dafoe, Allan, FitzGerald, Nicholas, Gu-Lemberg, Keren, Khan, Mina, Hendricks, Lisa Anne, Pellat, Marie, Feinberg, Vladimir, Cobon-Kerr, James, Sainath, Tara, Rauh, Maribeth, Hashemi, Sayed Hadi, Ives, Richard, Hasson, Yana, Noland, Eric, Cao, Yuan, Byrd, Nathan, Hou, Le, Wang, Qingze, Sottiaux, Thibault, Paganini, Michela, Lespiau, Jean-Baptiste, Moufarek, Alexandre, Hassan, Samer, Shivakumar, Kaushik, van Amersfoort, Joost, Mandhane, Amol, Joshi, Pratik, Goyal, Anirudh, Tung, Matthew, Brock, Andrew, Sheahan, Hannah, Misra, Vedant, Li, Cheng, Rakićević, Nemanja, Dehghani, Mostafa, Liu, Fangyu, Mittal, Sid, Oh, Junhyuk, Noury, Seb, Sezener, Eren, Huot, Fantine, Lamm, Matthew, De Cao, Nicola, Chen, Charlie, Mudgal, Sidharth, Stella, Romina, Brooks, Kevin, Vasudevan, Gautam, Liu, Chenxi, Chain, Mainak, Melinkeri, Nivedita, Cohen, Aaron, Wang, Venus, Seymore, Kristie, Zubkov, Sergey, Goel, Rahul, Yue, Summer, Krishnakumaran, Sai, Albert, Brian, Hurley, Nate, Sano, Motoki, Mohananey, Anhad, Joughin, Jonah, Filonov, Egor, Kępa, Tomasz, Eldawy, Yomna, Lim, Jiawern, Rishi, Rahul, Badiezadegan, Shirin, Bos, Taylor, Chang, Jerry, Jain, Sanil, Padmanabhan, Sri Gayatri Sundara, Puttagunta, Subha, Krishna, Kalpesh, Baker, Leslie, Kalb, Norbert, Bedapudi, Vamsi, Kurzrok, Adam, Lei, Shuntong, Yu, Anthony, Litvin, Oren, Zhou, Xiang, Wu, Zhichun, Sobell, Sam, Siciliano, Andrea, Papir, Alan, Neale, Robby, Bragagnolo, Jonas, Toor, Tej, Chen, Tina, Anklin, Valentin, Wang, Feiran, Feng, Richie, Gholami, Milad, Ling, Kevin, Liu, Lijuan, Walter, Jules, Moghaddam, Hamid, Kishore, Arun, Adamek, Jakub, Mercado, Tyler, Mallinson, Jonathan, Wandekar, Siddhinita, Cagle, Stephen, Ofek, Eran, Garrido, Guillermo, Lombriser, Clemens, Mukha, Maksim, Sun, Botu, Mohammad, Hafeezul Rahman, Matak, Josip, Qian, Yadi, Peswani, Vikas, Janus, Pawel, Yuan, Quan, Schelin, Leif, David, Oana, Garg, Ankur, He, Yifan, Duzhyi, Oleksii, Älgmyr, Anton, Lottaz, Timothée, Li, Qi, Yadav, Vikas, Xu, Luyao, Chinien, Alex, Shivanna, Rakesh, Chuklin, Aleksandr, Li, Josie, Spadine, Carrie, Wolfe, Travis, Mohamed, Kareem, Das, Subhabrata, Dai, Zihang, He, Kyle, von Dincklage, Daniel, Upadhyay, Shyam, Maurya, Akanksha, Chi, Luyan, Krause, Sebastian, Salama, Khalid, Rabinovitch, Pam G, M, Pavan Kumar Reddy, Selvan, Aarush, Dektiarev, Mikhail, Ghiasi, Golnaz, Guven, Erdem, Gupta, Himanshu, Liu, Boyi, Sharma, Deepak, Shtacher, Idan Heimlich, Paul, Shachi, Akerlund, Oscar, Aubet, François-Xavier, Huang, Terry, Zhu, Chen, Zhu, Eric, Teixeira, Elico, Fritze, Matthew, Bertolini, Francesco, Marinescu, Liana-Eleonora, Bölle, Martin, Paulus, Dominik, Gupta, Khyatti, Latkar, Tejasi, Chang, Max, Sanders, Jason, Wilson, Roopa, Wu, Xuewei, Tan, Yi-Xuan, Thiet, Lam Nguyen, Doshi, Tulsee, Lall, Sid, Mishra, Swaroop, Chen, Wanming, Luong, Thang, Benjamin, Seth, Lee, Jasmine, Andrejczuk, Ewa, Rabiej, Dominik, Ranjan, Vipul, Styrc, Krzysztof, Yin, Pengcheng, Simon, Jon, Harriott, Malcolm Rose, Bansal, Mudit, Robsky, Alexei, Bacon, Geoff, Greene, David, Mirylenka, Daniil, Zhou, Chen, Sarvana, Obaid, Goyal, Abhimanyu, Andermatt, Samuel, Siegler, Patrick, Horn, Ben, Israel, Assaf, Pongetti, Francesco, Chen, Chih-Wei "Louis", Selvatici, Marco, Silva, Pedro, Wang, Kathie, Tolins, Jackson, Guu, Kelvin, Yogev, Roey, Cai, Xiaochen, Agostini, Alessandro, Shah, Maulik, Nguyen, Hung, Donnaile, Noah Ó, Pereira, Sébastien, Friso, Linda, Stambler, Adam, Kuang, Chenkai, Romanikhin, Yan, Geller, Mark, Yan, ZJ, Jang, Kane, Lee, Cheng-Chun, Fica, Wojciech, Malmi, Eric, Tan, Qijun, Banica, Dan, Balle, Daniel, Pham, Ryan, Huang, Yanping, Avram, Diana, Shi, Hongzhi, Singh, Jasjot, Hidey, Chris, Ahuja, Niharika, Saxena, Pranab, Dooley, Dan, Potharaju, Srividya Pranavi, O'Neill, Eileen, Gokulchandran, Anand, Foley, Ryan, Zhao, Kai, Dusenberry, Mike, Liu, Yuan, Mehta, Pulkit, Kotikalapudi, Ragha, Safranek-Shrader, Chalence, Goodman, Andrew, Kessinger, Joshua, Globen, Eran, Kolhar, Prateek, Gorgolewski, Chris, Ibrahim, Ali, Song, Yang, Eichenbaum, Ali, Brovelli, Thomas, Potluri, Sahitya, Lahoti, Preethi, Baetu, Cip, Ghorbani, Ali, Chen, Charles, Crawford, Andy, Pal, Shalini, Sridhar, Mukund, Gurita, Petru, Mujika, Asier, Petrovski, Igor, Cedoz, Pierre-Louis, Li, Chenmei, Chen, Shiyuan, Santo, Niccolò Dal, Goyal, Siddharth, Punjabi, Jitesh, Kappaganthu, Karthik, Kwak, Chester, LV, Pallavi, Velury, Sarmishta, Choudhury, Himadri, Hall, Jamie, Shah, Premal, Figueira, Ricardo, Thomas, Matt, Lu, Minjie, Zhou, Ting, Kumar, Chintu, Jurdi, Thomas, Chikkerur, Sharat, Ma, Yenai, Yu, Adams, Kwak, Soo, Ähdel, Victor, Rajayogam, Sujeevan, Choma, Travis, Liu, Fei, Barua, Aditya, Ji, Colin, Park, Ji Ho, Hellendoorn, Vincent, Bailey, Alex, Bilal, Taylan, Zhou, Huanjie, Khatir, Mehrdad, Sutton, Charles, Rzadkowski, Wojciech, Macintosh, Fiona, Shagin, Konstantin, Medina, Paul, Liang, Chen, Zhou, Jinjing, Shah, Pararth, Bi, Yingying, Dankovics, Attila, Banga, Shipra, Lehmann, Sabine, Bredesen, Marissa, Lin, Zifan, Hoffmann, John Eric, Lai, Jonathan, Chung, Raynald, Yang, Kai, Balani, Nihal, Bražinskas, Arthur, Sozanschi, Andrei, Hayes, Matthew, Alcalde, Héctor Fernández, Makarov, Peter, Chen, Will, Stella, Antonio, Snijders, Liselotte, Mandl, Michael, Kärrman, Ante, Nowak, Paweł, Wu, Xinyi, Dyck, Alex, Vaidyanathan, Krishnan, R, Raghavender, Mallet, Jessica, Rudominer, Mitch, Johnston, Eric, Mittal, Sushil, Udathu, Akhil, Christensen, Janara, Verma, Vishal, Irving, Zach, Santucci, Andreas, Elsayed, Gamaleldin, Davoodi, Elnaz, Georgiev, Marin, Tenney, Ian, Hua, Nan, Cideron, Geoffrey, Leurent, Edouard, Alnahlawi, Mahmoud, Georgescu, Ionut, Wei, Nan, Zheng, Ivy, Scandinaro, Dylan, Jiang, Heinrich, Snoek, Jasper, Sundararajan, Mukund, Wang, Xuezhi, Ontiveros, Zack, Karo, Itay, Cole, Jeremy, Rajashekhar, Vinu, Tumeh, Lara, Ben-David, Eyal, Jain, Rishub, Uesato, Jonathan, Datta, Romina, Bunyan, Oskar, Wu, Shimu, Zhang, John, Stanczyk, Piotr, Zhang, Ye, Steiner, David, Naskar, Subhajit, Azzam, Michael, Johnson, Matthew, Paszke, Adam, Chiu, Chung-Cheng, Elias, Jaume Sanchez, Mohiuddin, Afroz, Muhammad, Faizan, Miao, Jin, Lee, Andrew, Vieillard, Nino, Park, Jane, Zhang, Jiageng, Stanway, Jeff, Garmon, Drew, Karmarkar, Abhijit, Dong, Zhe, Lee, Jong, Kumar, Aviral, Zhou, Luowei, Evens, Jonathan, Isaac, William, Irving, Geoffrey, Loper, Edward, Fink, Michael, Arkatkar, Isha, Chen, Nanxin, Shafran, Izhak, Petrychenko, Ivan, Chen, Zhe, Jia, Johnson, Levskaya, Anselm, Zhu, Zhenkai, Grabowski, Peter, Mao, Yu, Magni, Alberto, Yao, Kaisheng, Snaider, Javier, Casagrande, Norman, Palmer, Evan, Suganthan, Paul, Castaño, Alfonso, Giannoumis, Irene, Kim, Wooyeol, Rybiński, Mikołaj, Sreevatsa, Ashwin, Prendki, Jennifer, Soergel, David, Goedeckemeyer, Adrian, Gierke, Willi, Jafari, Mohsen, Gaba, Meenu, Wiesner, Jeremy, Wright, Diana Gage, Wei, Yawen, Vashisht, Harsha, Kulizhskaya, Yana, Hoover, Jay, Le, Maigo, Li, Lu, Iwuanyanwu, Chimezie, Liu, Lu, Ramirez, Kevin, Khorlin, Andrey, Cui, Albert, LIN, Tian, Wu, Marcus, Aguilar, Ricardo, Pallo, Keith, Chakladar, Abhishek, Perng, Ginger, Abellan, Elena Allica, Zhang, Mingyang, Dasgupta, Ishita, Kushman, Nate, Penchev, Ivo, Repina, Alena, Wu, Xihui, van der Weide, Tom, Ponnapalli, Priya, Kaplan, Caroline, Simsa, Jiri, Li, Shuangfeng, Dousse, Olivier, Piper, Jeff, Ie, Nathan, Pasumarthi, Rama, Lintz, Nathan, Vijayakumar, Anitha, Andor, Daniel, Valenzuela, Pedro, Lui, Minnie, Paduraru, Cosmin, Peng, Daiyi, Lee, Katherine, Zhang, Shuyuan, Greene, Somer, Nguyen, Duc Dung, Kurylowicz, Paula, Hardin, Cassidy, Dixon, Lucas, Janzer, Lili, Choo, Kiam, Feng, Ziqiang, Zhang, Biao, Singhal, Achintya, Du, Dayou, McKinnon, Dan, Antropova, Natasha, Bolukbasi, Tolga, Keller, Orgad, Reid, David, Finchelstein, Daniel, Raad, Maria Abi, Crocker, Remi, Hawkins, Peter, Dadashi, Robert, Gaffney, Colin, Franko, Ken, Bulanova, Anna, Leblond, Rémi, Chung, Shirley, Askham, Harry, Cobo, Luis C., Xu, Kelvin, Fischer, Felix, Xu, Jun, Sorokin, Christina, Alberti, Chris, Lin, Chu-Cheng, Evans, Colin, Dimitriev, Alek, Forbes, Hannah, Banarse, Dylan, Tung, Zora, Omernick, Mark, Bishop, Colton, Sterneck, Rachel, Jain, Rohan, Xia, Jiawei, Amid, Ehsan, Piccinno, Francesco, Wang, Xingyu, Banzal, Praseem, Mankowitz, Daniel J., Polozov, Alex, Krakovna, Victoria, Brown, Sasha, Bateni, MohammadHossein, Duan, Dennis, Firoiu, Vlad, Thotakuri, Meghana, Natan, Tom, Geist, Matthieu, Girgin, Ser tan, Li, Hui, Ye, Jiayu, Roval, Ofir, Tojo, Reiko, Kwong, Michael, Lee-Thorp, James, Yew, Christopher, Sinopalnikov, Danila, Ramos, Sabela, Mellor, John, Sharma, Abhishek, Wu, Kathy, Miller, David, Sonnerat, Nicolas, Vnukov, Denis, Greig, Rory, Beattie, Jennifer, Caveness, Emily, Bai, Libin, Eisenschlos, Julian, Korchemniy, Alex, Tsai, Tomy, Jasarevic, Mimi, Kong, Weize, Dao, Phuong, Zheng, Zeyu, Liu, Frederick, Zhu, Rui, Teh, Tian Huey, Sanmiya, Jason, Gladchenko, Evgeny, Trdin, Nejc, Toyama, Daniel, Rosen, Evan, Tavakkol, Sasan, Xue, Linting, Elkind, Chen, Woodman, Oliver, Carpenter, John, Papamakarios, George, Kemp, Rupert, Kafle, Sushant, Grunina, Tanya, Sinha, Rishika, Talbert, Alice, Wu, Diane, Owusu-Afriyie, Denese, Thornton, Chloe, Pont-Tuset, Jordi, Narayana, Pradyumna, Li, Jing, Fatehi, Saaber, Wieting, John, Ajmeri, Omar, Uria, Benigno, Ko, Yeongil, Knight, Laura, Héliou, Amélie, Niu, Ning, Gu, Shane, Pang, Chenxi, Li, Yeqing, Levine, Nir, Stolovich, Ariel, Santamaria-Fernandez, Rebeca, Goenka, Sonam, Yustalim, Wenny, Strudel, Robin, Elqursh, Ali, Deck, Charlie, Lee, Hyo, Li, Zonglin, Levin, Kyle, Hoffmann, Raphael, Holtmann-Rice, Dan, Bachem, Olivier, Arora, Sho, Koh, Christy, Yeganeh, Soheil Hassas, Põder, Siim, Tariq, Mukarram, Sun, Yanhua, Ionita, Lucian, Seyedhosseini, Mojtaba, Tafti, Pouya, Liu, Zhiyu, Gulati, Anmol, Liu, Jasmine, Ye, Xinyu, Chrzaszcz, Bart, Wang, Lily, Sethi, Nikhil, Li, Tianrun, Brown, Ben, Singh, Shreya, Fan, Wei, Parisi, Aaron, Stanton, Joe, Koverkathu, Vinod, Choquette-Choo, Christopher A., Li, Yunjie, Lu, TJ, Shroff, Prakash, Varadarajan, Mani, Bahargam, Sanaz, Willoughby, Rob, Gaddy, David, Desjardins, Guillaume, Cornero, Marco, Robenek, Brona, Mittal, Bhavishya, Albrecht, Ben, Shenoy, Ashish, Moiseev, Fedor, Jacobsson, Henrik, Ghaffarkhah, Alireza, Rivière, Morgane, Walton, Alanna, Crepy, Clément, Parrish, Alicia, Zhou, Zongwei, Farabet, Clement, Radebaugh, Carey, Srinivasan, Praveen, van der Salm, Claudia, Fidjeland, Andreas, Scellato, Salvatore, Latorre-Chimoto, Eri, Klimczak-Plucińska, Hanna, Bridson, David, de Cesare, Dario, Hudson, Tom, Mendolicchio, Piermaria, Walker, Lexi, Morris, Alex, Mauger, Matthew, Guseynov, Alexey, Reid, Alison, Odoom, Seth, Loher, Lucia, Cotruta, Victor, Yenugula, Madhavi, Grewe, Dominik, Petrushkina, Anastasia, Duerig, Tom, Sanchez, Antonio, Yadlowsky, Steve, Shen, Amy, Globerson, Amir, Webb, Lynette, Dua, Sahil, Li, Dong, Bhupatiraju, Surya, Hurt, Dan, Qureshi, Haroon, Agarwal, Ananth, Shani, Tomer, Eyal, Matan, Khare, Anuj, Belle, Shreyas Rammohan, Wang, Lei, Tekur, Chetan, Kale, Mihir Sanjay, Wei, Jinliang, Sang, Ruoxin, Saeta, Brennan, Liechty, Tyler, Sun, Yi, Zhao, Yao, Lee, Stephan, Nayak, Pandu, Fritz, Doug, Vuyyuru, Manish Reddy, Aslanides, John, Vyas, Nidhi, Wicke, Martin, Ma, Xiao, Eltyshev, Evgenii, Martin, Nina, Cate, Hardie, Manyika, James, Amiri, Keyvan, Kim, Yelin, Xiong, Xi, Kang, Kai, Luisier, Florian, Tripuraneni, Nilesh, Madras, David, Guo, Mandy, Waters, Austin, Wang, Oliver, Ainslie, Joshua, Baldridge, Jason, Zhang, Han, Pruthi, Garima, Bauer, Jakob, Yang, Feng, Mansour, Riham, Gelman, Jason, Xu, Yang, Polovets, George, Liu, Ji, Cai, Honglong, Chen, Warren, Sheng, XiangHai, Xue, Emily, Ozair, Sherjil, Angermueller, Christof, Li, Xiaowei, Sinha, Anoop, Wang, Weiren, Wiesinger, Julia, Koukoumidis, Emmanouil, Tian, Yuan, Iyer, Anand, Gurumurthy, Madhu, Goldenson, Mark, Shah, Parashar, Blake, MK, Yu, Hongkun, Urbanowicz, Anthony, Palomaki, Jennimaria, Fernando, Chrisantha, Durden, Ken, Mehta, Harsh, Momchev, Nikola, Rahimtoroghi, Elahe, Georgaki, Maria, Raul, Amit, Ruder, Sebastian, Redshaw, Morgan, Lee, Jinhyuk, Zhou, Denny, Jalan, Komal, Li, Dinghua, Hechtman, Blake, Schuh, Parker, Nasr, Milad, Milan, Kieran, Mikulik, Vladimir, Franco, Juliana, Green, Tim, Nguyen, Nam, Kelley, Joe, Mahendru, Aroma, Hu, Andrea, Howland, Joshua, Vargas, Ben, Hui, Jeffrey, Bansal, Kshitij, Rao, Vikram, Ghiya, Rakesh, Wang, Emma, Ye, Ke, Sarr, Jean Michel, Preston, Melanie Moranski, Elish, Madeleine, Li, Steve, Kaku, Aakash, Gupta, Jigar, Pasupat, Ice, Juan, Da-Cheng, Someswar, Milan, M., Tejvi, Chen, Xinyun, Amini, Aida, Fabrikant, Alex, Chu, Eric, Dong, Xuanyi, Muthal, Amruta, Buthpitiya, Senaka, Jauhari, Sarthak, Khandelwal, Urvashi, Hitron, Ayal, Ren, Jie, Rinaldi, Larissa, Drath, Shahar, Dabush, Avigail, Jiang, Nan-Jiang, Godhia, Harshal, Sachs, Uli, Chen, Anthony, Fan, Yicheng, Taitelbaum, Hagai, Noga, Hila, Dai, Zhuyun, Wang, James, Hamer, Jenny, Ferng, Chun-Sung, Elkind, Chenel, Atias, Aviel, Lee, Paulina, Listík, Vít, Carlen, Mathias, van de Kerkhof, Jan, Pikus, Marcin, Zaher, Krunoslav, Müller, Paul, Zykova, Sasha, Stefanec, Richard, Gatsko, Vitaly, Hirnschall, Christoph, Sethi, Ashwin, Xu, Xingyu Federico, Ahuja, Chetan, Tsai, Beth, Stefanoiu, Anca, Feng, Bo, Dhandhania, Keshav, Katyal, Manish, Gupta, Akshay, Parulekar, Atharva, Pitta, Divya, Zhao, Jing, Bhatia, Vivaan, Bhavnani, Yashodha, Alhadlaq, Omar, Li, Xiaolin, Danenberg, Peter, Tu, Dennis, Pine, Alex, Filippova, Vera, Ghosh, Abhipso, Limonchik, Ben, Urala, Bhargava, Lanka, Chaitanya Krishna, Clive, Derik, Li, Edward, Wu, Hao, Hongtongsak, Kevin, Li, Ianna, Thakkar, Kalind, Omarov, Kuanysh, Majmundar, Kushal, Alverson, Michael, Kucharski, Michael, Patel, Mohak, Jain, Mudit, Zabelin, Maksim, Pelagatti, Paolo, Kohli, Rohan, Kumar, Saurabh, Kim, Joseph, Sankar, Swetha, Shah, Vineet, Ramachandruni, Lakshmi, Zeng, Xiangkai, Bariach, Ben, Weidinger, Laura, Vu, Tu, Andreev, Alek, He, Antoine, Hui, Kevin, Kashem, Sheleem, Subramanya, Amar, Hsiao, Sissie, Hassabis, Demis, Kavukcuoglu, Koray, Sadovsky, Adam, Le, Quoc, Strohman, Trevor, Wu, Yonghui, Petrov, Slav, Dean, Jeffrey, and Vinyals, Oriol

Subjects
Computer Science - Computation and Language, Computer Science - Artificial Intelligence, Computer Science - Computer Vision and Pattern Recognition
Abstract

This report introduces a new family of multimodal models, Gemini, that exhibit remarkable capabilities across image, audio, video, and text understanding. The Gemini family consists of Ultra, Pro, and Nano sizes, suitable for applications ranging from complex reasoning tasks to on-device memory-constrained use-cases. Evaluation on a broad range of benchmarks shows that our most-capable Gemini Ultra model advances the state of the art in 30 of 32 of these benchmarks - notably being the first model to achieve human-expert performance on the well-studied exam benchmark MMLU, and improving the state of the art in every one of the 20 multimodal benchmarks we examined. We believe that the new capabilities of the Gemini family in cross-modal reasoning and language understanding will enable a wide variety of use cases. We discuss our approach toward post-training and deploying Gemini models responsibly to users through services including Gemini, Gemini Advanced, Google AI Studio, and Cloud Vertex AI.

Published
2023

45. JWST's PEARLS: 119 multiply imaged galaxies behind MACS0416, lensing properties of caustic crossing galaxies, and the relation between halo mass and number of globular clusters at $z=0.4$

Author

Diego, Jose M., Adams, Nathan J., Willner, Steven, Harvey, Tom, Broadhurst, Tom, Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Windhorst, Rogier A., D'Silva, Jordan C. J., Koekemoer, Anton M., Coe, Dan, Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Grogin, Norman A., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Yan, Haojing, Sun, Fengwu, Hainline, Kevin, Berkheimer, Jessica, Polletta, Maria del Carmen, and Zitrin, Adi

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present a new lens model for the $z=0.396$ galaxy cluster MACS J0416.1$-$2403 based on a previously known set of 77 spectroscopically confirmed, multiply imaged galaxies plus an additional set of 42 candidate multiply imaged galaxies from past HST and new JWST data. The new galaxies lack spectroscopic redshifts but have geometric and/or photometric redshift estimates that are presented here. The new model predicts magnifications and time delays for all multiple images. The full set of constraints totals 343, constituting the largest sample of multiple images lensed by a single cluster to date. Caustic-crossing galaxies lensed by this cluster are especially interesting. Some of these galaxies show transient events, most of which are interpreted as micro-lensing of stars at cosmological distances. These caustic-crossing arcs are expected to show similar events in future, deeper JWST observations. We provide time delay and magnification models for all these arcs. The time delays and the magnifications for different arcs are generally anti-correlated, as expected from $N$-body simulations. In the major sub-halos of the cluster, the dark-matter mass from our lens model correlates well with the observed number of globular clusters. This confirms earlier results, derived at lower redshifts, which suggest that globular clusters can be used as powerful mass proxies for the halo masses when lensing constraints are scarce or not available., Comment: 21 pages and 11 figures. Accepted for publication in A&A

Published
2023
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46. X-ray detection of the most extreme star-forming galaxies at the cosmic noon via strong lensing

Author

Wang, Q. Daniel, Diaz, Carlos Garcia, Kamieneski, Patrick S., Harrington, Kevin C., Yun, Min S., Foo, Nicholas, Frye, Brenda L., Jimenez-Andrade, Eric F., Liu, Daizhong, Lowenthal, James D., Pampliega, Belen Alcalde, Pascale, Massimo, Vishwas, Amit, and Gurwell, Mark A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Hyper-luminous infrared galaxies (HyLIRGs) are the most extreme star-forming systems observed in the early Universe, and their properties still elude comprehensive understanding. We have undertaken a large XMM-Newton observing program to probe the total accreting black hole population in three HyLIRGs at z = 2.12, 3.25, and 3.55, gravitationally lensed by foreground galaxies. Selected from the Planck All-Sky Survey to Analyze Gravitationally-lensed Extreme Starbursts (PASSAGES), these HyLIRGs have apparent infrared luminosities > E14 Lsun. Our observations revealed X-ray emission in each of them. PJ1336+49 appears to be dominated by high-mass X-ray binaries (HMXBs). Remarkably, the luminosity of this non-AGN X-ray emission exceeds by a factor of about three the value obtained by calibration with local galaxies with much lower star formation rates. This enhanced X-ray emission most likely highlights the efficacy of dynamical HMXB production within compact clusters, which is an important mode of star formation in HyLIRGs. The remaining two (PJ0116-24 and PJ1053+60) morphologically and spectrally exhibit a compact X-ray component in addition to the extended non-AGN X-ray emission, indicating the presence of Active Galactic Nuclei (AGNs). The AGN appears to be centrally located in the reconstructed source plane images of PJ0116-24, which manifests its star-forming activity predominantly within an extended galactic disk. In contrast, the AGN in the field of PJ1053+60 is projected 60 kpc away from the extreme star-forming galaxy and could be ejected from it. These results underline the synergistic potential of deep X-ray observations with strong lensing for the study of high-energy astrophysical phenomena in HyLIRGs., Comment: Just accepted for publication in MNRAS; comments are welcome

Published
2023

47. Minimal gains for minimal pairs: Difficulty in learning similar-sounding words continues into preschool

Author

Creel, Sarah C and Frye, Conor I

Subjects
Cognitive and Computational Psychology, Psychology, Pediatric, Minority Health, Infant, Young Adult, Child, Humans, Child, Preschool, Phonetics, Learning, Language, Language Development, Verbal Learning, Speech Perception, Phonological acquisition, Minimal pairs, Eye tracking, Word learning, Cognitive Sciences, Experimental Psychology, Applied and developmental psychology, Biological psychology, Social and personality psychology
Abstract

A critical indicator of spoken language knowledge is the ability to discern the finest possible distinctions that exist between words in a language-minimal pairs, for example, the distinction between the novel words beesh and peesh. Infants differentiate similar-sounding novel labels like "bih" and "dih" by 17 months of age or earlier in the context of word learning. Adult word learners readily distinguish similar-sounding words. What is unclear is the shape of learning between infancy and adulthood: Is there a nonlinear increase early in development, or is there protracted improvement as experience with spoken language amasses? Three experiments tested monolingual English-speaking children aged 3 to 6 years and young adults. Children underperformed when learning minimal-pair words compared with adults (Experiment 1), compared with learning dissimilar words even when speech materials were optimized for young children (Experiment 2), and when the number of word instances during learning was quadrupled (Experiment 3). Nonetheless, the youngest group readily recognized familiar minimal pairs (Experiment 3). Results are consistent with a lengthy trajectory for detailed sound pattern learning in one's native language(s), although other interpretations are possible. Suggestions for research on developmental trajectories across various age ranges are made.

Published
2024

48. Association between a large change between the minimum and maximum monthly values of solar insolation and a history of suicide attempts in bipolar I disorder

Author

Ritter, Philipp, Glenn, Tasha, Achtyes, Eric D., Alda, Martin, Agaoglu, Esen, Altınbaş, Kürsat, Andreassen, Ole A., Angelopoulos, Elias, Ardau, Raffaella, Aydin, Memduha, Ayhan, Yavuz, Baethge, Christopher, Bauer, Rita, Baune, Bernhard T., Balaban, Ceylan, Becerra-Palars, Claudia, Behere, Aniruddh P., Behere, Prakash B., Belete, Habte, Belete, Tilahun, Belizario, Gabriel Okawa, Bellivier, Frank, Belmaker, Robert H., Benedetti, Francesco, Berk, Michael, Bersudsky, Yuly, Bicakci, Şule, Birabwa-Oketcho, Harriet, Bjella, Thomas D., Brady, Conan, Cabrera, Jorge, Cappucciati, Marco, Castro, Angela Marianne Paredes, Chen, Wei-Ling, Cheung, Eric Y. W., Chiesa, Silvia, Chanopoulou, Margarita, Crowe, Marie, Cuomo, Alessandro, Dallaspezia, Sara, Desai, Pratikkumar, Dodd, Seetal, Etain, Bruno, Fagiolini, Andrea, Fellendorf, Frederike T., Ferensztajn-Rochowiak, Ewa, Fiedorowicz, Jess G., Fountoulakis, Kostas N., Frye, Mark A., Geoffroy, Pierre A., Gitlin, Michael J., Gonzalez-Pinto, Ana, Gottlieb, John F., Grof, Paul, Haarman, Bartholomeus C. M., Harima, Hirohiko, Hasse-Sousa, Mathias, Henry, Chantal, Hoffding, Lone, Houenou, Josselin, Imbesi, Massimiliano, Isometsä, Erkki T., Ivkovic, Maja, Janno, Sven, Johnsen, Simon, Kapczinski, Flávio, Karakatsoulis, Grigorios N., Kardell, Mathias, Kessing, Lars Vedel, Kim, Seong Jae, König, Barbara, Kot, Timur L., Koval, Michael, Kunz, Mauricio, Lafer, Beny, Landén, Mikael, Larsen, Erik R., Licht, Rasmus W., Ludwig, Vera M., Lopez-Jaramillo, Carlos, MacKenzie, Alan, Madsen, Helle Østergaard, Madsen, Simone Alberte Kongstad A., Mahadevan, Jayant, Mahardika, Agustine, Manchia, Mirko, Marsh, Wendy, Martinez-Cengotitabengoa, Monica, Martini, Julia, Martiny, Klaus, Mashima, Yuki, McLoughlin, Declan M., Meesters, Alie N. R., Meesters, Ybe, Melle, Ingrid, Meza-Urzúa, Fátima, Michaelis, Elisabeth, Mikolas, Pavol, Mok, Yee Ming, Monteith, Scott, Moorthy, Muthukumaran, Morken, Gunnar, Mosca, Enrica, Mozzhegorov, Anton A., Munoz, Rodrigo, Mythri, Starlin V., Nacef, Fethi, Nadella, Ravi K., Nakanotani, Takako, Nielsen, René Ernst, O’Donovan, Claire, Omrani, Adel, Osher, Yamima, Ouali, Uta, Pantovic-Stefanovic, Maja, Pariwatcharakul, Pornjira, Petite, Joanne, Petzold, Johannes, Pfennig, Andrea, Pilhatsch, Maximilian, Ruiz, Yolanda Pica, Pinna, Marco, Pompili, Maurizio, Porter, Richard, Quiroz, Danilo, Rabelo-da-Ponte, Francisco Diego, Ramesar, Raj, Rasgon, Natalie, Ratta-apha, Woraphat, Redahan, Maria, Reddy, M. S., Reif, Andreas, Reininghaus, Eva Z., Richards, Jenny Gringer, Rybakowski, Janusz K., Sathyaputri, Leela, Scippa, Angela M., Simhandl, Christian, Smith, Daniel, Smith, José, Stackhouse, Jr., Paul W., Stein, Dan J., Stilwell, Kellen, Strejilevich, Sergio, Su, Kuan-Pin, Subramaniam, Mythily, Sulaiman, Ahmad Hatim, Suominen, Kirsi, Tanra, Andi J., Tatebayashi, Yoshitaka, Teh, Wen Lin, Tondo, Leonardo, Torrent, Carla, Tuinstra, Daniel, Uchida, Takahito, Vaaler, Arne E., Vieta, Eduard, Viswanath, Biju, Volf, Carlo, Yang, Kai-Jie, Yoldi-Negrete, Maria, Yalcinkaya, Oguz Kaan, Young, Allan H., Zgueb, Yosra, Whybrow, Peter C., and Bauer, Michael

Published
2024
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