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1. Ousiometrics and Telegnomics: The essence of meaning conforms to a two-dimensional powerful-weak and dangerous-safe framework with diverse corpora presenting a safety bias

Author: Dodds, P. S., Alshaabi, T., Fudolig, M. I., Zimmerman, J. W., Lovato, J., Beaulieu, S., Minot, J. R., Arnold, M. V., Reagan, A. J., Danforth, C. M., Dodds, P. S., Alshaabi, T., Fudolig, M. I., Zimmerman, J. W., Lovato, J., Beaulieu, S., Minot, J. R., Arnold, M. V., Reagan, A. J., and Danforth, C. M.
Abstract: We define `ousiometrics' to be the study of essential meaning in whatever context that meaningful signals are communicated, and `telegnomics' as the study of remotely sensed knowledge. From work emerging through the middle of the 20th century, the essence of meaning has become generally accepted as being well captured by the three orthogonal dimensions of evaluation, potency, and activation (EPA). By re-examining first types and then tokens for the English language, and through the use of automatically annotated histograms -- `ousiograms' -- we find here that: 1. The essence of meaning conveyed by words is instead best described by a compass-like power-danger (PD) framework, and 2. Analysis of a disparate collection of large-scale English language corpora -- literature, news, Wikipedia, talk radio, and social media -- shows that natural language exhibits a systematic bias toward safe, low danger words -- a reinterpretation of the Pollyanna principle's positivity bias for written expression. To help justify our choice of dimension names and to help address the problems with representing observed ousiometric dimensions by bipolar adjective pairs, we introduce and explore `synousionyms' and `antousionyms' -- ousiometric counterparts of synonyms and antonyms. We further show that the PD framework revises the circumplex model of affect as a more general model of state of mind. Finally, we use our findings to construct and test a prototype `ousiometer', a telegnomic instrument that measures ousiometric time series for temporal corpora. We contend that our power-danger ousiometric framework provides a complement for entropy-based measurements, and may be of value for the study of a wide variety of communication across biological and artificial life., Comment: 40 pages (34 page main manuscript, 6 page appendix), 15 figures (9 main, 6 appendix), 4 tables
Published: 2021

2. Computational Paremiology: Charting the temporal, ecological dynamics of proverb use in books, news articles, and tweets

Author: Davis, E., Danforth, C. M., Mieder, W., Dodds, P. S., Davis, E., Danforth, C. M., Mieder, W., and Dodds, P. S.
Abstract: Proverbs are an essential component of language and culture, and though much attention has been paid to their history and currency, there has been comparatively little quantitative work on changes in the frequency with which they are used over time. With wider availability of large corpora reflecting many diverse genres of documents, it is now possible to take a broad and dynamic view of the importance of the proverb. Here, we measure temporal changes in the relevance of proverbs within three corpora, differing in kind, scale, and time frame: Millions of books over centuries; hundreds of millions of news articles over twenty years; and billions of tweets over a decade. We find that proverbs present heavy-tailed frequency-of-usage rank distributions in each venue; exhibit trends reflecting the cultural dynamics of the eras covered; and have evolved into contemporary forms on social media., Comment: Main paper: 16 pages, 9 figures, 1 table; Supplementary: 5 pages, 4 tables, 4 figures
Published: 2021

3. Gauging the happiness benefit of US urban parks through Twitter

Author: Schwartz, A. J., Dodds, P. S., O'Neil-Dunne, J. P. M., Ricketts, T. H., Danforth, C. M., Schwartz, A. J., Dodds, P. S., O'Neil-Dunne, J. P. M., Ricketts, T. H., and Danforth, C. M.
Abstract: The relationship between nature contact and mental well-being has received increasing attention in recent years. While a body of evidence has accumulated demonstrating a positive relationship between time in nature and mental well-being, there have been few studies comparing this relationship in different locations over long periods of time. In this study, we estimate a happiness benefit, the difference in expressed happiness between in- and out-of-park tweets, for the 25 largest cities in the US by population. People write happier words during park visits when compared with non-park user tweets collected around the same time. While the words people write are happier in parks on average and in most cities, we find considerable variation across cities. Tweets are happier in parks at all times of the day, week, and year, not just during the weekend or summer vacation. Across all cities, we find that the happiness benefit is highest in parks larger than 100 acres. Overall, our study suggests the happiness benefit associated with park visitation is on par with US holidays such as Thanksgiving and New Year's Day., Comment: 13 pages including appendix, 9 figures, 2 tables
Published: 2020

4. How the world's collective attention is being paid to a pandemic: COVID-19 related n-gram time series for 24 languages on Twitter

Author: Alshaabi, T., Minot, J. R., Arnold, M. V., Adams, J. L., Dewhurst, D. R., Reagan, A. J., Muhamad, R., Danforth, C. M., Dodds, P. S., Alshaabi, T., Minot, J. R., Arnold, M. V., Adams, J. L., Dewhurst, D. R., Reagan, A. J., Muhamad, R., Danforth, C. M., and Dodds, P. S.
Abstract: In confronting the global spread of the coronavirus disease COVID-19 pandemic we must have coordinated medical, operational, and political responses. In all efforts, data is crucial. Fundamentally, and in the possible absence of a vaccine for 12 to 18 months, we need universal, well-documented testing for both the presence of the disease as well as confirmed recovery through serological tests for antibodies, and we need to track major socioeconomic indices. But we also need auxiliary data of all kinds, including data related to how populations are talking about the unfolding pandemic through news and stories. To in part help on the social media side, we curate a set of 2000 day-scale time series of 1- and 2-grams across 24 languages on Twitter that are most 'important' for April 2020 with respect to April 2019. We determine importance through our allotaxonometric instrument, rank-turbulence divergence. We make some basic observations about some of the time series, including a comparison to numbers of confirmed deaths due to COVID-19 over time. We broadly observe across all languages a peak for the language-specific word for 'virus' in January 2020 followed by a decline through February and then a surge through March and April. The world's collective attention dropped away while the virus spread out from China. We host the time series on Gitlab, updating them on a daily basis while relevant. Our main intent is for other researchers to use these time series to enhance whatever analyses that may be of use during the pandemic as well as for retrospective investigations., Comment: 13 pages, 6 figures, 3 tables, website: http://compstorylab.org/covid19ngrams
Published: 2020
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5. Probability-turbulence divergence: A tunable allotaxonometric instrument for comparing heavy-tailed categorical distributions

Author: Dodds, P. S., Minot, J. R., Arnold, M. V., Alshaabi, T., Adams, J. L., Dewhurst, D. R., Reagan, A. J., Danforth, C. M., Dodds, P. S., Minot, J. R., Arnold, M. V., Alshaabi, T., Adams, J. L., Dewhurst, D. R., Reagan, A. J., and Danforth, C. M.
Abstract: Real-world complex systems often comprise many distinct types of elements as well as many more types of networked interactions between elements. When the relative abundances of types can be measured well, we further observe heavy-tailed categorical distributions for type frequencies. For the comparison of type frequency distributions of two systems or a system with itself at different time points in time -- a facet of allotaxonometry -- a great range of probability divergences are available. Here, we introduce and explore `probability-turbulence divergence', a tunable, straightforward, and interpretable instrument for comparing normalizable categorical frequency distributions. We model probability-turbulence divergence (PTD) after rank-turbulence divergence (RTD). While probability-turbulence divergence is more limited in application than rank-turbulence divergence, it is more sensitive to changes in type frequency. We build allotaxonographs to display probability turbulence, incorporating a way to visually accommodate zero probabilities for `exclusive types' which are types that appear in only one system. We explore comparisons of example distributions taken from literature, social media, and ecology. We show how probability-turbulence divergence either explicitly or functionally generalizes many existing kinds of distances and measures, including, as special cases, $L^{(p)}$ norms, the S{\o}rensen-Dice coefficient (the $F_1$ statistic), and the Hellinger distance. We discuss similarities with the generalized entropies of R{\'e}nyi and Tsallis, and the diversity indices (or Hill numbers) from ecology. We close with thoughts on open problems concerning the optimization of the tuning of rank- and probability-turbulence divergence., Comment: 14 pages, 7 figures
Published: 2020

6. Long-term word frequency dynamics derived from Twitter are corrupted: A bespoke approach to detecting and removing pathologies in ensembles of time series

Author: Dodds, P. S., Minot, J. R., Arnold, M. V., Alshaabi, T., Adams, J. L., Dewhurst, D. R., Reagan, A. J., Danforth, C. M., Dodds, P. S., Minot, J. R., Arnold, M. V., Alshaabi, T., Adams, J. L., Dewhurst, D. R., Reagan, A. J., and Danforth, C. M.
Abstract: Maintaining the integrity of long-term data collection is an essential scientific practice. As a field evolves, so too will that field's measurement instruments and data storage systems, as they are invented, improved upon, and made obsolete. For data streams generated by opaque sociotechnical systems which may have episodic and unknown internal rule changes, detecting and accounting for shifts in historical datasets requires vigilance and creative analysis. Here, we show that around 10\% of day-scale word usage frequency time series for Twitter collected in real time for a set of roughly 10,000 frequently used words for over 10 years come from tweets with, in effect, corrupted language labels. We describe how we uncovered problematic signals while comparing word usage over varying time frames. We locate time points where Twitter switched on or off different kinds of language identification algorithms, and where data formats may have changed. We then show how we create a statistic for identifying and removing words with pathological time series. While our resulting process for removing `bad' time series from ensembles of time series is particular, the approach leading to its construction may be generalizeable., Comment: 8 pages, 5 figures
Published: 2020

7. Computational timeline reconstruction of the stories surrounding Trump: Story turbulence, narrative control, and collective chronopathy

Author: Dodds, P. S., Minot, J. R., Arnold, M. V., Alshaabi, T., Adams, J. L., Reagan, A. J., Danforth, C. M., Dodds, P. S., Minot, J. R., Arnold, M. V., Alshaabi, T., Adams, J. L., Reagan, A. J., and Danforth, C. M.
Abstract: Measuring the specific kind, temporal ordering, diversity, and turnover rate of stories surrounding any given subject is essential to developing a complete reckoning of that subject's historical impact. Here, we use Twitter as a distributed news and opinion aggregation source to identify and track the dynamics of the dominant day-scale stories around Donald Trump, the 45th President of the United States. Working with a data set comprising around 20 billion 1-grams, we first compare each day's 1-gram and 2-gram usage frequencies to those of a year before, to create day- and week-scale timelines for Trump stories for 2016 through 2020. We measure Trump's narrative control, the extent to which stories have been about Trump or put forward by Trump. We then quantify story turbulence and collective chronopathy -- the rate at which a population's stories for a subject seem to change over time. We show that 2017 was the most turbulent overall year for Trump. In 2020, story generation slowed dramatically during the first two major waves of the COVID-19 pandemic, with rapid turnover returning first with the Black Lives Matter protests following George Floyd's murder and then later by events leading up to and following the 2020 US presidential election, including the storming of the US Capitol six days into 2021. Trump story turnover for 2 months during the COVID-19 pandemic was on par with that of 3 days in September 2017. Our methods may be applied to any well-discussed phenomenon, and have potential to enable the computational aspects of journalism, history, and biography., Comment: 13 pages, 5 figures (4 main, 1 appendix), 1 table. Analysis complete for 6 calendar years, from 2015/01/01 through to 2021/12/31
Published: 2020
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8. Joint Representation of a Riesz Space and Its Conjugate Space

Author: Buskes, G., Jeu, M. de, Dodds, P., Schep, A., Sukochev, F., Neerven, J. van, Wickstead, A., Rooij, A.C.M. van, Buskes, G., Jeu, M. de, Dodds, P., Schep, A., Sukochev, F., Neerven, J. van, Wickstead, A., and Rooij, A.C.M. van
Abstract: Item does not contain fulltext
Published: 2019

9. Joint Representation of a Riesz Space and Its Conjugate Space

Author: Buskes, G., Jeu, M. de, Dodds, P., Schep, A., Sukochev, F., Neerven, J. van, Wickstead, A., Rooij, A.C.M. van, Buskes, G., Jeu, M. de, Dodds, P., Schep, A., Sukochev, F., Neerven, J. van, Wickstead, A., and Rooij, A.C.M. van
Abstract: Item does not contain fulltext
Published: 2019

10. Improved prediction of fungal effector proteins from secretomes with EffectorP 2.0

Author: Sperschneider, J., Dodds, P., Gardiner, D., Singh, Karam, Taylor, J., Sperschneider, J., Dodds, P., Gardiner, D., Singh, Karam, and Taylor, J.
Abstract: © 2018 BSPP and John Wiley & Sons Ltd Plant-pathogenic fungi secrete effector proteins to facilitate infection. We describe extensive improvements to EffectorP, the first machine learning classifier for fungal effector prediction. EffectorP 2.0 is now trained on a larger set of effectors and utilizes a different approach based on an ensemble of classifiers trained on different subsets of negative data, offering different views on classification. EffectorP 2.0 achieves an accuracy of 89%, compared with 82% for EffectorP 1.0 and 59.8% for a small size classifier. Important features for effector prediction appear to be protein size, protein net charge as well as the amino acids serine and cysteine. EffectorP 2.0 decreases the number of predicted effectors in secretomes of fungal plant symbionts and saprophytes by 40% when compared with EffectorP 1.0. However, EffectorP 1.0 retains value, and combining EffectorP 1.0 and 2.0 results in a stringent classifier with a low false positive rate of 9%. EffectorP 2.0 predicts significant enrichments of effectors in 12 of 13 sets of infection-induced proteins from diverse fungal pathogens, whereas a small cysteine-rich classifier detects enrichment in only seven of 13. EffectorP 2.0 will fast track the prioritization of high-confidence effector candidates for functional validation and aid in improving our understanding of effector biology. EffectorP 2.0 is available at http://effectorp.csiro.au.
Published: 2018

11. Multiple functional self-association interfaces in plant TIR domains

Author: Zhang, X., Bernoux, M., Bentham, A., Newman, Toby, Ve, T., Casey, L., Raaymakers, T., Hu, J., Croll, T., Schreiber, K., Staskawicz, B., Anderson, P., Sohn, K., Williams, S., Dodds, P., Kobe, B., Zhang, X., Bernoux, M., Bentham, A., Newman, Toby, Ve, T., Casey, L., Raaymakers, T., Hu, J., Croll, T., Schreiber, K., Staskawicz, B., Anderson, P., Sohn, K., Williams, S., Dodds, P., and Kobe, B.
Published: 2017

12. ApoplastP: Prediction of effectors and plant proteins in the apoplast using machine learning

Author: Sperschneider, J., Dodds, P., Singh, Karam, Taylor, J., Sperschneider, J., Dodds, P., Singh, Karam, and Taylor, J.
Abstract: © 2017 New Phytologist Trust. The plant apoplast is integral to intercellular signalling, transport and plant-pathogen interactions. Plant pathogens deliver effectors both into the apoplast and inside host cells, but no computational method currently exists to discriminate between these localizations. We present ApoplastP, the first method for predicting whether an effector or plant protein localizes to the apoplast. ApoplastP uncovers features of apoplastic localization common to both effectors and plant proteins, namely depletion in glutamic acid, acidic amino acids and charged amino acids and enrichment in small amino acids. ApoplastP predicts apoplastic localization in effectors with a sensitivity of 75% and a false positive rate of 5%, improving the accuracy of cysteine-rich classifiers by > 13%. ApoplastP does not depend on the presence of a signal peptide and correctly predicts the localization of unconventionally secreted proteins. The secretomes of fungal saprophytes as well as necrotrophic, hemibiotrophic and extracellular fungal pathogens are enriched for predicted apoplastic proteins. Rust pathogens have low proportions of predicted apoplastic proteins, but these are highly enriched for predicted effectors. ApoplastP pioneers apoplastic localization prediction using machine learning. It will facilitate functional studies and will be valuable for predicting if an effector localizes to the apoplast or if it enters plant cells.
Published: 2017

13. LOCALIZER: Subcellular localization prediction of both plant and effector proteins in the plant cell

Author: Sperschneider, J., Catanzariti, A., Deboer, K., Petre, B., Gardiner, D., Singh, Karam, Dodds, P., Taylor, J., Sperschneider, J., Catanzariti, A., Deboer, K., Petre, B., Gardiner, D., Singh, Karam, Dodds, P., and Taylor, J.
Abstract: Pathogens secrete effector proteins and many operate inside plant cells to enable infection. Some effectors have been found to enter subcellular compartments by mimicking host targeting sequences. Although many computational methods exist to predict plant protein subcellular localization, they perform poorly for effectors. We introduce LOCALIZER for predicting plant and effector protein localization to chloroplasts, mitochondria, and nuclei. LOCALIZER shows greater prediction accuracy for chloroplast and mitochondrial targeting compared to other methods for 652 plant proteins. For 107 eukaryotic effectors, LOCALIZER outperforms other methods and predicts a previously unrecognized chloroplast transit peptide for the ToxA effector, which we show translocates into tobacco chloroplasts. Secretome-wide predictions and confocal microscopy reveal that rust fungi might have evolved multiple effectors that target chloroplasts or nuclei. LOCALIZER is the first method for predicting effector localisation in plants and is a valuable tool for prioritizing effector candidates for functional investigations. © The Author(s) 2017.
Published: 2017

14. MiNDSTEp differential photometry of the gravitationally lensed quasars WFI2033-4723 and HE0047-1756: Microlensing and a new time delay

Author: Giannini, E., Schmidt, R. W., Wambsganß, J., Alsubai, K., Andersen, J. M., Anguita, T., Bozza, V., Bramich, D. M., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Jaimes, R. Figuera, Finet, F., Gerner, T., Gu, S., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M. S., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Zimmer, F., Giannini, E., Schmidt, R. W., Wambsganß, J., Alsubai, K., Andersen, J. M., Anguita, T., Bozza, V., Bramich, D. M., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Jaimes, R. Figuera, Finet, F., Gerner, T., Gu, S., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M. S., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Zimmer, F.
Abstract: We present V and R photometry of the gravitationally lensed quasars WFI2033-4723 and HE0047-1756. The data were taken by the MiNDSTEp collaboration with the 1.54 m Danish telescope at the ESO La Silla observatory from 2008 to 2012. Differential photometry has been carried out using the image subtraction method as implemented in the HOTPAnTS package, additionally using GALFIT for quasar photometry. The quasar WFI2033-4723 showed brightness variations of order 0.5 mag in V and R during the campaign. The two lensed components of quasar HE0047-1756 varied by 0.2-0.3 mag within five years. We provide, for the first time, an estimate of the time delay of component B with respect to A of $\Delta t= 7.6\pm1.8$ days for this object. We also find evidence for a secular evolution of the magnitude difference between components A and B in both filters, which we explain as due to a long-duration microlensing event. Finally we find that both quasars WFI2033-4723 and HE0047-1756 become bluer when brighter, which is consistent with previous studies., Comment: 16 pages, 15 figures, 10 tables. Accepted for publication in A&A
Published: 2016
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15. MiNDSTEp differential photometry of the gravitationally lensed quasars WFI2033-4723 and HE0047-1756: Microlensing and a new time delay

Author: Giannini, E., Schmidt, R. W., Wambsganß, J., Alsubai, K., Andersen, J. M., Anguita, T., Bozza, V., Bramich, D. M., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Jaimes, R. Figuera, Finet, F., Gerner, T., Gu, S., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M. S., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Zimmer, F., Giannini, E., Schmidt, R. W., Wambsganß, J., Alsubai, K., Andersen, J. M., Anguita, T., Bozza, V., Bramich, D. M., Browne, P., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Jaimes, R. Figuera, Finet, F., Gerner, T., Gu, S., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Juncher, D., Kains, N., Kerins, E., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M. S., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rabus, M., Rahvar, S., Ricci, D., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Zimmer, F.
Abstract: We present V and R photometry of the gravitationally lensed quasars WFI2033-4723 and HE0047-1756. The data were taken by the MiNDSTEp collaboration with the 1.54 m Danish telescope at the ESO La Silla observatory from 2008 to 2012. Differential photometry has been carried out using the image subtraction method as implemented in the HOTPAnTS package, additionally using GALFIT for quasar photometry. The quasar WFI2033-4723 showed brightness variations of order 0.5 mag in V and R during the campaign. The two lensed components of quasar HE0047-1756 varied by 0.2-0.3 mag within five years. We provide, for the first time, an estimate of the time delay of component B with respect to A of $\Delta t= 7.6\pm1.8$ days for this object. We also find evidence for a secular evolution of the magnitude difference between components A and B in both filters, which we explain as due to a long-duration microlensing event. Finally we find that both quasars WFI2033-4723 and HE0047-1756 become bluer when brighter, which is consistent with previous studies., Comment: 16 pages, 15 figures, 10 tables. Accepted for publication in A&A
Published: 2016
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16. Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry (Corrigendum)

Author: Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jorgensen, U. G., Giridhar, S., Penny, M. T., Alsubai, Khalid A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X.-S, Giannini, Edward H, Hardis, S., Harpsoe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, Jens, Juncher, D., Kerins, E., Kjeldsen, H, Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Williams, A., Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jorgensen, U. G., Giridhar, S., Penny, M. T., Alsubai, Khalid A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X.-S, Giannini, Edward H, Hardis, S., Harpsoe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, Jens, Juncher, D., Kerins, E., Kjeldsen, H, Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Williams, A.
Published: 2016

17. Erratum: Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry (Astronomy and Astrophysics (2013) 555 (A36))

Author: Kains, N., Bramich, D., Arellano Ferro, A., Figuera Jaimes, R., Jørgensen, U., Giridhar, S., Penny, M., Alsubai, K., Andersen, J., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Giannini, E., Gu, S., Hardis, S., Harpsøe, K., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Williams, Andrew, Kains, N., Bramich, D., Arellano Ferro, A., Figuera Jaimes, R., Jørgensen, U., Giridhar, S., Penny, M., Alsubai, K., Andersen, J., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X., Giannini, E., Gu, S., Hardis, S., Harpsøe, K., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Williams, Andrew
Published: 2016

18. EffectorP: Predicting fungal effector proteins from secretomes using machine learning

Author: Sperschneider, J., Gardiner, D., Dodds, P., Tini, F., Covarelli, L., Singh, Karambir, Manners, J., Taylor, J., Sperschneider, J., Gardiner, D., Dodds, P., Tini, F., Covarelli, L., Singh, Karambir, Manners, J., and Taylor, J.
Abstract: Eukaryotic filamentous plant pathogens secrete effector proteins that modulate the host cell to facilitate infection. Computational effector candidate identification and subsequent functional characterization delivers valuable insights into plant-pathogen interactions. However, effector prediction in fungi has been challenging due to a lack of unifying sequence features such as conserved N-terminal sequence motifs. Fungal effectors are commonly predicted from secretomes based on criteria such as small size and cysteine-rich, which suffers from poor accuracy. We present EffectorP which pioneers the application of machine learning to fungal effector prediction. EffectorP improves fungal effector prediction from secretomes based on a robust signal of sequence-derived properties, achieving sensitivity and specificity of over 80%. Features that discriminate fungal effectors from secreted noneffectors are predominantly sequence length, molecular weight and protein net charge, as well as cysteine, serine and tryptophan content. We demonstrate that EffectorP is powerful when combined with in planta expression data for predicting high-priority effector candidates. EffectorP is the first prediction program for fungal effectors based on machine learning. Our findings will facilitate functional fungal effector studies and improve our understanding of effectors in plant-pathogen interactions. EffectorP is available at http://effectorp.csiro.au.
Published: 2016

19. Transits and starspots in the WASP-6 planetary system

Author: Tregloan-Reed, Jeremy, Southworth, John, Burgdorf, M., Novati, S. Calchi, Dominik, M., Finet, F., Jørgensen, U. G., Maier, G., Mancini, L., Proft, S., Ricci, D., Snodgrass, C., Bozza, V., Browne, P., Dodds, P., Gerner, T., Harpsøe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Penny, M. T., Rahvar, S., Sahu, K., Scarpetta, G., Schäfer, S., Schönebeck, F., Skottfelt, J., Surdej, J., Tregloan-Reed, Jeremy, Southworth, John, Burgdorf, M., Novati, S. Calchi, Dominik, M., Finet, F., Jørgensen, U. G., Maier, G., Mancini, L., Proft, S., Ricci, D., Snodgrass, C., Bozza, V., Browne, P., Dodds, P., Gerner, T., Harpsøe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Penny, M. T., Rahvar, S., Sahu, K., Scarpetta, G., Schäfer, S., Schönebeck, F., Skottfelt, J., and Surdej, J.
Abstract: We present updates to \textsc{prism}, a photometric transit-starspot model, and \textsc{gemc}, a hybrid optimisation code combining MCMC and a genetic algorithm. We then present high-precision photometry of four transits in the WASP-6 planetary system, two of which contain a starspot anomaly. All four transits were modelled using \textsc{prism} and \textsc{gemc}, and the physical properties of the system calculated. We find the mass and radius of the host star to be $0.836\pm 0.063\,{\rm M}_\odot$ and $0.864\pm0.024\,{\rm R}_\odot$, respectively. For the planet we find a mass of $0.485\pm 0.027\,{\rm M}_{\rm Jup}$, a radius of $1.230\pm0.035\,{\rm R}_{\rm Jup}$ and a density of $0.244\pm0.014\,\rho_{\rm Jup}$. These values are consistent with those found in the literature. In the likely hypothesis that the two spot anomalies are caused by the same starspot or starspot complex, we measure the stars rotation period and velocity to be $23.80 \pm 0.15$\,d and $1.78 \pm 0.20$\,km\,s$^{-1}$, respectively, at a co-latitude of 75.8$^\circ$. We find that the sky-projected angle between the stellar spin axis and the planetary orbital axis is $\lambda = 7.2^{\circ} \pm 3.7^{\circ}$, indicating axial alignment. Our results are consistent with and more precise than published spectroscopic measurements of the Rossiter-McLaughlin effect. These results suggest that WASP-6\,b formed at a much greater distance from its host star and suffered orbital decay through tidal interactions with the protoplanetary disc., Comment: 11 Pages, 6 Figures, MNRAS accepted
Published: 2015
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20. Transits and starspots in the WASP-6 planetary system

Author: Tregloan-Reed, Jeremy, Southworth, John, Burgdorf, M., Novati, S. Calchi, Dominik, M., Finet, F., Jørgensen, U. G., Maier, G., Mancini, L., Proft, S., Ricci, D., Snodgrass, C., Bozza, V., Browne, P., Dodds, P., Gerner, T., Harpsøe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Penny, M. T., Rahvar, S., Sahu, K., Scarpetta, G., Schäfer, S., Schönebeck, F., Skottfelt, J., Surdej, J., Tregloan-Reed, Jeremy, Southworth, John, Burgdorf, M., Novati, S. Calchi, Dominik, M., Finet, F., Jørgensen, U. G., Maier, G., Mancini, L., Proft, S., Ricci, D., Snodgrass, C., Bozza, V., Browne, P., Dodds, P., Gerner, T., Harpsøe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Penny, M. T., Rahvar, S., Sahu, K., Scarpetta, G., Schäfer, S., Schönebeck, F., Skottfelt, J., and Surdej, J.
Abstract: We present updates to \textsc{prism}, a photometric transit-starspot model, and \textsc{gemc}, a hybrid optimisation code combining MCMC and a genetic algorithm. We then present high-precision photometry of four transits in the WASP-6 planetary system, two of which contain a starspot anomaly. All four transits were modelled using \textsc{prism} and \textsc{gemc}, and the physical properties of the system calculated. We find the mass and radius of the host star to be $0.836\pm 0.063\,{\rm M}_\odot$ and $0.864\pm0.024\,{\rm R}_\odot$, respectively. For the planet we find a mass of $0.485\pm 0.027\,{\rm M}_{\rm Jup}$, a radius of $1.230\pm0.035\,{\rm R}_{\rm Jup}$ and a density of $0.244\pm0.014\,\rho_{\rm Jup}$. These values are consistent with those found in the literature. In the likely hypothesis that the two spot anomalies are caused by the same starspot or starspot complex, we measure the stars rotation period and velocity to be $23.80 \pm 0.15$\,d and $1.78 \pm 0.20$\,km\,s$^{-1}$, respectively, at a co-latitude of 75.8$^\circ$. We find that the sky-projected angle between the stellar spin axis and the planetary orbital axis is $\lambda = 7.2^{\circ} \pm 3.7^{\circ}$, indicating axial alignment. Our results are consistent with and more precise than published spectroscopic measurements of the Rossiter-McLaughlin effect. These results suggest that WASP-6\,b formed at a much greater distance from its host star and suffered orbital decay through tidal interactions with the protoplanetary disc., Comment: 11 Pages, 6 Figures, MNRAS accepted
Published: 2015
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21. OGLE-2011-BLG-0265Lb: A JOVIAN MICROLENSING PLANET ORBITING AN M DWARF

Author: Skowron, J., Shin, I. -G., Udalski, A., Han, C., Sumi, T., Shvartzvald, Y., Gould, A., Prester, D. Dominis, Street, R. A., Jorgensen, U. G., Bennett, D. P., Bozza, V., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Abe, F., Bhattacharya, A., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Ling, C. H., Koshimoto, N., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Philpott, L. C., Rattenbury, N., Saito, T., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yock, P. C. M., Maoz, D., Kaspi, S., Friedmann, M., Almeida, L. A., Batista, V., Christie, G., Choi, J. -Y., Depoy, D. L., Gaudi, B. S., Henderson, C., Hwang, K. -H., Jablonski, F., Jung, Y. K., Lee, C. -U., McCormick, J., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Yee, J. C., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, C. H., Dieters, S., Donatowicz, J., Fouque, P., Greenhill, J., Kains, N., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J., Pollard, K. R., Ranc, C., Sahu, K. C., Wambsganss, J., Williams, A., Wouters, D., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Gu, C. -H., Hardis, Harpsøe, Kennet Bomann West, Hessman, F. V., Hinse, T. C., Hornstrup, A., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Skowron, J., Shin, I. -G., Udalski, A., Han, C., Sumi, T., Shvartzvald, Y., Gould, A., Prester, D. Dominis, Street, R. A., Jorgensen, U. G., Bennett, D. P., Bozza, V., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Abe, F., Bhattacharya, A., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Ling, C. H., Koshimoto, N., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Philpott, L. C., Rattenbury, N., Saito, T., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yock, P. C. M., Maoz, D., Kaspi, S., Friedmann, M., Almeida, L. A., Batista, V., Christie, G., Choi, J. -Y., Depoy, D. L., Gaudi, B. S., Henderson, C., Hwang, K. -H., Jablonski, F., Jung, Y. K., Lee, C. -U., McCormick, J., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Yee, J. C., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, C. H., Dieters, S., Donatowicz, J., Fouque, P., Greenhill, J., Kains, N., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J., Pollard, K. R., Ranc, C., Sahu, K. C., Wambsganss, J., Williams, A., Wouters, D., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Gu, C. -H., Hardis, Harpsøe, Kennet Bomann West, Hessman, F. V., Hinse, T. C., Hornstrup, A., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., and Wertz, O.
Published: 2015

22. Transits and starspots in the WASP-6 planetary system

Author: Tregloan-Reed, Jeremy, Southworth, John, Burgdorf, M., Novati, S. Calchi, Dominik, M., Finet, F., Jorgensen, U. G., Maier, G., Mancini, L., Prof, S., Ricci, D., Snodgrass, C., Bozza, V., Browne, P., Dodds, P., Gerner, T., Harpsoe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Penny, M. T., Rahvar, S., Sahu, K., Scarpetta, G., Schaefer, S., Schoenebeck, F., Skottfelt, J., Surdej, J., Tregloan-Reed, Jeremy, Southworth, John, Burgdorf, M., Novati, S. Calchi, Dominik, M., Finet, F., Jorgensen, U. G., Maier, G., Mancini, L., Prof, S., Ricci, D., Snodgrass, C., Bozza, V., Browne, P., Dodds, P., Gerner, T., Harpsoe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Penny, M. T., Rahvar, S., Sahu, K., Scarpetta, G., Schaefer, S., Schoenebeck, F., Skottfelt, J., and Surdej, J.
Published: 2015

23. The Lexicocalorimeter: Gauging public health through caloric input and output on social media

Author: Alajajian, S. E., Williams, J. R., Reagan, A. J., Alajajian, S. C., Frank, M. R., Mitchell, L., Lahne, J., Danforth, C. M., Dodds, P. S., Alajajian, S. E., Williams, J. R., Reagan, A. J., Alajajian, S. C., Frank, M. R., Mitchell, L., Lahne, J., Danforth, C. M., and Dodds, P. S.
Abstract: We propose and develop a Lexicocalorimeter: an online, interactive instrument for measuring the "caloric content" of social media and other large-scale texts. We do so by constructing extensive yet improvable tables of food and activity related phrases, and respectively assigning them with sourced estimates of caloric intake and expenditure. We show that for Twitter, our naive measures of "caloric input", "caloric output", and the ratio of these measures are all strong correlates with health and well-being measures for the contiguous United States. Our caloric balance measure in many cases outperforms both its constituent quantities, is tunable to specific health and well-being measures such as diabetes rates, has the capability of providing a real-time signal reflecting a population's health, and has the potential to be used alongside traditional survey data in the development of public policy and collective self-awareness. Because our Lexicocalorimeter is a linear superposition of principled phrase scores, we also show we can move beyond correlations to explore what people talk about in collective detail, and assist in the understanding and explanation of how population-scale conditions vary, a capacity unavailable to black-box type methods., Comment: Manuscript: 17 pages, 8 figures, 1 table, Supplementary Information: 10 pages, 7 figures, 3 tables
Published: 2015

24. Social media affects the timing, location, and severity of school shootings

Author: Garcia-Bernardo, J., Qi, H., Shultz, J. M., Cohen, A. M., Johnson, N. F., Dodds, P. S., Garcia-Bernardo, J., Qi, H., Shultz, J. M., Cohen, A. M., Johnson, N. F., and Dodds, P. S.
Abstract: Over the past two decades, school shootings within the United States have repeatedly devastated communities and shaken public opinion. Many of these attacks appear to be `lone wolf' ones driven by specific individual motivations, and the identification of precursor signals and hence actionable policy measures would thus seem highly unlikely. Here, we take a system-wide view and investigate the timing of school attacks and the dynamical feedback with social media. We identify a trend divergence in which college attacks have continued to accelerate over the last 25 years while those carried out on K-12 schools have slowed down. We establish the copycat effect in school shootings and uncover a statistical association between social media chatter and the probability of an attack in the following days. While hinting at causality, this relationship may also help mitigate the frequency and intensity of future attacks., Comment: Main text: 7 pages, 4 figures; Supplementary: 6 pages, 7 figures
Published: 2015

25. Reply to Garcia et al.: Common mistakes in measuring frequency dependent word characteristics

Author: Dodds, P. S., Clark, E. M., Desu, S., Frank, M. R., Reagan, A. J., Williams, J. R., Mitchell, L., Harris, K. D., Kloumann, I. M., Bagrow, J. P., Megerdoomian, K., McMahon, M. T., Tivnan, B. F., Danforth, C. M., Dodds, P. S., Clark, E. M., Desu, S., Frank, M. R., Reagan, A. J., Williams, J. R., Mitchell, L., Harris, K. D., Kloumann, I. M., Bagrow, J. P., Megerdoomian, K., McMahon, M. T., Tivnan, B. F., and Danforth, C. M.
Abstract: We demonstrate that the concerns expressed by Garcia et al. are misplaced, due to (1) a misreading of our findings in [1]; (2) a widespread failure to examine and present words in support of asserted summary quantities based on word usage frequencies; and (3) a range of misconceptions about word usage frequency, word rank, and expert-constructed word lists. In particular, we show that the English component of our study compares well statistically with two related surveys, that no survey design influence is apparent, and that estimates of measurement error do not explain the positivity biases reported in our work and that of others. We further demonstrate that for the frequency dependence of positivity---of which we explored the nuances in great detail in [1]---Garcia et al. did not perform a reanalysis of our data---they instead carried out an analysis of a different, statistically improper data set and introduced a nonlinearity before performing linear regression., Comment: 5 pages, 2 figures, 1 table. Expanded version of reply appearing in PNAS 2015
Published: 2015
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26. Advances and Challenges in Computational Prediction of Effectors from Plant Pathogenic Fungi

Author: Sperschneider, J., Dodds, P., Gardiner, D., Manners, J., Singh, Karambir, Taylor, J., Sperschneider, J., Dodds, P., Gardiner, D., Manners, J., Singh, Karambir, and Taylor, J.
Published: 2015

27. OGLE-2011-BLG-0265Lb: a Jovian Microlensing Planet Orbiting an M Dwarf

Author: Skowron, J., Shin, I. -G., Udalski, A., Han, C., Sumi, T., Shvartzvald, Y., Gould, A., Dominis-Prester, D., Street, R. A., Jørgensen, U. G., Bennett, D. P., Bozza, V., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Poleski, R., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, Ł., Abe, F., Bhattacharya, A., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Ling, C. H., Koshimoto, N., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Philpott, L. C., Rattenbury, N., Saito, T., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yock, P. C. M., Maoz, D., Kaspi, S., Friedman, M., Almeida, L. A., Batista, V., Christie, G., Choi, J. -Y., DePoy, D. L., Gaudi, B. S., Henderson, C., Hwang, K. -H., Jablonski, F., Jung, Y. K., Lee, C. -U., McCormick, J., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Yee, J., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Donatowicz, J., Fouqué, P., Greenhill, J., Kains, N., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J., Pollard, K. R., Ranc, C., Sahu, K. C., Wambsganss, J., Williams, A., Wouters, D., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Gu, C. -H., Hardis, Harpsøe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Skowron, J., Shin, I. -G., Udalski, A., Han, C., Sumi, T., Shvartzvald, Y., Gould, A., Dominis-Prester, D., Street, R. A., Jørgensen, U. G., Bennett, D. P., Bozza, V., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Poleski, R., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, Ł., Abe, F., Bhattacharya, A., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Ling, C. H., Koshimoto, N., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Philpott, L. C., Rattenbury, N., Saito, T., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yock, P. C. M., Maoz, D., Kaspi, S., Friedman, M., Almeida, L. A., Batista, V., Christie, G., Choi, J. -Y., DePoy, D. L., Gaudi, B. S., Henderson, C., Hwang, K. -H., Jablonski, F., Jung, Y. K., Lee, C. -U., McCormick, J., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Yee, J., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Donatowicz, J., Fouqué, P., Greenhill, J., Kains, N., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J., Pollard, K. R., Ranc, C., Sahu, K. C., Wambsganss, J., Williams, A., Wouters, D., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Gu, C. -H., Hardis, Harpsøe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., and Wertz, O.
Abstract: We report the discovery of a Jupiter-mass planet orbiting an M-dwarf star that gave rise to the microlensing event OGLE-2011-BLG-0265. Such a system is very rare among known planetary systems and thus the discovery is important for theoretical studies of planetary formation and evolution. High-cadence temporal coverage of the planetary signal combined with extended observations throughout the event allows us to accurately model the observed light curve. The final microlensing solution remains, however, degenerate yielding two possible configurations of the planet and the host star. In the case of the preferred solution, the mass of the planet is $M_{\rm p} = 0.9\pm 0.3\ M_{\rm J}$, and the planet is orbiting a star with a mass $M = 0.22\pm 0.06\ M_\odot$. The second possible configuration (2$\sigma$ away) consists of a planet with $M_{\rm p}=0.6\pm 0.3\ M_{\rm J}$ and host star with $M=0.14\pm 0.06\ M_\odot$. The system is located in the Galactic disk 3 -- 4 kpc towards the Galactic bulge. In both cases, with an orbit size of 1.5 -- 2.0 AU, the planet is a "cold Jupiter" -- located well beyond the "snow line" of the host star. Currently available data make the secure selection of the correct solution difficult, but there are prospects for lifting the degeneracy with additional follow-up observations in the future, when the lens and source star separate., Comment: 10 pages, 2 tables, 5 figures. Accepted in ApJ
Published: 2014
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28. The JCMT Gould Belt Survey: low-mass proto-planetary discs from a SCUBA-2 census of NGC1333

Author: Dodds, P., Greaves, J., Scholz, A., Hatchell, J., Holland, W. S., Team, JCMT Gould Belt Survey, Dodds, P., Greaves, J., Scholz, A., Hatchell, J., Holland, W. S., and Team, JCMT Gould Belt Survey
Abstract: NGC1333 is a 1-2 Myr old cluster of stars in the Perseus molecular cloud. We used 850mu data from the Gould Belt Survey with SCUBA-2 on the JCMT to measure or place limits on disc masses for 82 Class II sources in this cluster. Eight disc-candidates were detected; one is estimated to have mass of about 9 Jupiter masses in dust plus gas, while the others host only 2-4 Jupiter masses of circumstellar material. None of these discs exceeds the threshold for the 'Minimum Mass Solar Nebula' (MMSN). This reinforces previous claims that only a small fraction of Class II sources at an age of 1-2 Myr has discs exceeding the MMSN threshold and thus can form a planetary system like our own. However, other regions with similarly low fractions of MMSN discs (IC348, UpSco, SigmaOri) are thought to be older than NGC1333. Compared with coeval regions, the exceptionally low fraction of massive discs in NGC1333 cannot easily be explained by the effects of UV radiation or stellar encounters. Our results indicate that additional environmental factors significantly affect disc evolution and the outcome of planet formation by core accretion., Comment: 7 pages, 3 figures, MNRAS in press
Published: 2014
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29. High-precision photometry by telescope defocussing. VI. WASP-24, WASP-25 and WASP-26

Author: Southworth, John, Hinse, T. C., Burgdorf, M., Novati, S. Calchi, Dominik, M., Galianni, P., Gerner, T., Giannini, E., Gu, S. -H., Hundertmark, M., Jorgensen, U. G., Juncher, D., Kerins, E., Mancini, L., Rabus, M., Ricci, D., Schaefer, S., Skottfelt, J., Tregloan-Reed, J., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Browne, P., Ciceri, S., D'Ago, G., Damerdji, Y., Diehl, C., Dodds, P., Elyiv, A., Fang, X. -S., Finet, F., Jaimes, R. Figuera, Hardis, S., Harpsoe, K., Jessen-Hansen, J., Kains, N., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Penny, M. T., Popovas, A., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Schmidt, R. W., Schoenebeck, F., Snodgrass, C., Street, R. A., Surdej, J., Tsapras, Y., Vilela, C., Southworth, John, Hinse, T. C., Burgdorf, M., Novati, S. Calchi, Dominik, M., Galianni, P., Gerner, T., Giannini, E., Gu, S. -H., Hundertmark, M., Jorgensen, U. G., Juncher, D., Kerins, E., Mancini, L., Rabus, M., Ricci, D., Schaefer, S., Skottfelt, J., Tregloan-Reed, J., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Browne, P., Ciceri, S., D'Ago, G., Damerdji, Y., Diehl, C., Dodds, P., Elyiv, A., Fang, X. -S., Finet, F., Jaimes, R. Figuera, Hardis, S., Harpsoe, K., Jessen-Hansen, J., Kains, N., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Penny, M. T., Popovas, A., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Schmidt, R. W., Schoenebeck, F., Snodgrass, C., Street, R. A., Surdej, J., Tsapras, Y., and Vilela, C.
Abstract: We present time-series photometric observations of thirteen transits in the planetary systems WASP-24, WASP-25 and WASP-26. All three systems have orbital obliquity measurements, WASP-24 and WASP-26 have been observed with Spitzer, and WASP-25 was previously comparatively neglected. Our light curves were obtained using the telescope-defocussing method and have scatters of 0.5 to 1.2 mmag relative to their best-fitting geometric models. We used these data to measure the physical properties and orbital ephemerides of the systems to high precision, finding that our improved measurements are in good agreement with previous studies. High-resolution Lucky Imaging observations of all three targets show no evidence for faint stars close enough to contaminate our photometry. We confirm the eclipsing nature of the star closest to WASP-24 and present the detection of a detached eclipsing binary within 4.25 arcmin of WASP-26., Comment: Accepted for publication in MNRAS. 14 pages, 10 figures, 8 tables. Data and supplementary information are available on request
Published: 2014
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30. The JCMT Gould Belt Survey: low-mass proto-planetary discs from a SCUBA-2 census of NGC1333

Author: Dodds, P., Greaves, J., Scholz, A., Hatchell, J., Holland, W. S., Team, JCMT Gould Belt Survey, Dodds, P., Greaves, J., Scholz, A., Hatchell, J., Holland, W. S., and Team, JCMT Gould Belt Survey
Abstract: NGC1333 is a 1-2 Myr old cluster of stars in the Perseus molecular cloud. We used 850mu data from the Gould Belt Survey with SCUBA-2 on the JCMT to measure or place limits on disc masses for 82 Class II sources in this cluster. Eight disc-candidates were detected; one is estimated to have mass of about 9 Jupiter masses in dust plus gas, while the others host only 2-4 Jupiter masses of circumstellar material. None of these discs exceeds the threshold for the 'Minimum Mass Solar Nebula' (MMSN). This reinforces previous claims that only a small fraction of Class II sources at an age of 1-2 Myr has discs exceeding the MMSN threshold and thus can form a planetary system like our own. However, other regions with similarly low fractions of MMSN discs (IC348, UpSco, SigmaOri) are thought to be older than NGC1333. Compared with coeval regions, the exceptionally low fraction of massive discs in NGC1333 cannot easily be explained by the effects of UV radiation or stellar encounters. Our results indicate that additional environmental factors significantly affect disc evolution and the outcome of planet formation by core accretion., Comment: 7 pages, 3 figures, MNRAS in press
Published: 2014
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31. OGLE-2011-BLG-0265Lb: a Jovian Microlensing Planet Orbiting an M Dwarf

Author: Skowron, J., Shin, I. -G., Udalski, A., Han, C., Sumi, T., Shvartzvald, Y., Gould, A., Dominis-Prester, D., Street, R. A., Jørgensen, U. G., Bennett, D. P., Bozza, V., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Poleski, R., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, Ł., Abe, F., Bhattacharya, A., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Ling, C. H., Koshimoto, N., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Philpott, L. C., Rattenbury, N., Saito, T., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yock, P. C. M., Maoz, D., Kaspi, S., Friedman, M., Almeida, L. A., Batista, V., Christie, G., Choi, J. -Y., DePoy, D. L., Gaudi, B. S., Henderson, C., Hwang, K. -H., Jablonski, F., Jung, Y. K., Lee, C. -U., McCormick, J., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Yee, J., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Donatowicz, J., Fouqué, P., Greenhill, J., Kains, N., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J., Pollard, K. R., Ranc, C., Sahu, K. C., Wambsganss, J., Williams, A., Wouters, D., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Gu, C. -H., Hardis, Harpsøe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wertz, O., Skowron, J., Shin, I. -G., Udalski, A., Han, C., Sumi, T., Shvartzvald, Y., Gould, A., Dominis-Prester, D., Street, R. A., Jørgensen, U. G., Bennett, D. P., Bozza, V., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Poleski, R., Kozłowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, Ł., Abe, F., Bhattacharya, A., Bond, I. A., Botzler, C. S., Freeman, M., Fukui, A., Fukunaga, D., Itow, Y., Ling, C. H., Koshimoto, N., Masuda, K., Matsubara, Y., Muraki, Y., Namba, S., Ohnishi, K., Philpott, L. C., Rattenbury, N., Saito, T., Sullivan, D. J., Suzuki, D., Tristram, P. J., Yock, P. C. M., Maoz, D., Kaspi, S., Friedman, M., Almeida, L. A., Batista, V., Christie, G., Choi, J. -Y., DePoy, D. L., Gaudi, B. S., Henderson, C., Hwang, K. -H., Jablonski, F., Jung, Y. K., Lee, C. -U., McCormick, J., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Yee, J., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Donatowicz, J., Fouqué, P., Greenhill, J., Kains, N., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J., Pollard, K. R., Ranc, C., Sahu, K. C., Wambsganss, J., Williams, A., Wouters, D., Tsapras, Y., Bramich, D. M., Horne, K., Hundertmark, M., Snodgrass, C., Steele, I. A., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Gu, C. -H., Hardis, Harpsøe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., and Wertz, O.
Abstract: We report the discovery of a Jupiter-mass planet orbiting an M-dwarf star that gave rise to the microlensing event OGLE-2011-BLG-0265. Such a system is very rare among known planetary systems and thus the discovery is important for theoretical studies of planetary formation and evolution. High-cadence temporal coverage of the planetary signal combined with extended observations throughout the event allows us to accurately model the observed light curve. The final microlensing solution remains, however, degenerate yielding two possible configurations of the planet and the host star. In the case of the preferred solution, the mass of the planet is $M_{\rm p} = 0.9\pm 0.3\ M_{\rm J}$, and the planet is orbiting a star with a mass $M = 0.22\pm 0.06\ M_\odot$. The second possible configuration (2$\sigma$ away) consists of a planet with $M_{\rm p}=0.6\pm 0.3\ M_{\rm J}$ and host star with $M=0.14\pm 0.06\ M_\odot$. The system is located in the Galactic disk 3 -- 4 kpc towards the Galactic bulge. In both cases, with an orbit size of 1.5 -- 2.0 AU, the planet is a "cold Jupiter" -- located well beyond the "snow line" of the host star. Currently available data make the secure selection of the correct solution difficult, but there are prospects for lifting the degeneracy with additional follow-up observations in the future, when the lens and source star separate., Comment: 10 pages, 2 tables, 5 figures. Accepted in ApJ
Published: 2014
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32. High-precision photometry by telescope defocussing. VI. WASP-24, WASP-25 and WASP-26

Author: Southworth, John, Hinse, T. C., Burgdorf, M., Novati, S. Calchi, Dominik, M., Galianni, P., Gerner, T., Giannini, E., Gu, S. -H., Hundertmark, M., Jorgensen, U. G., Juncher, D., Kerins, E., Mancini, L., Rabus, M., Ricci, D., Schaefer, S., Skottfelt, J., Tregloan-Reed, J., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Browne, P., Ciceri, S., D'Ago, G., Damerdji, Y., Diehl, C., Dodds, P., Elyiv, A., Fang, X. -S., Finet, F., Jaimes, R. Figuera, Hardis, S., Harpsoe, K., Jessen-Hansen, J., Kains, N., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Penny, M. T., Popovas, A., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Schmidt, R. W., Schoenebeck, F., Snodgrass, C., Street, R. A., Surdej, J., Tsapras, Y., Vilela, C., Southworth, John, Hinse, T. C., Burgdorf, M., Novati, S. Calchi, Dominik, M., Galianni, P., Gerner, T., Giannini, E., Gu, S. -H., Hundertmark, M., Jorgensen, U. G., Juncher, D., Kerins, E., Mancini, L., Rabus, M., Ricci, D., Schaefer, S., Skottfelt, J., Tregloan-Reed, J., Wang, X. -B., Wertz, O., Alsubai, K. A., Andersen, J. M., Bozza, V., Bramich, D. M., Browne, P., Ciceri, S., D'Ago, G., Damerdji, Y., Diehl, C., Dodds, P., Elyiv, A., Fang, X. -S., Finet, F., Jaimes, R. Figuera, Hardis, S., Harpsoe, K., Jessen-Hansen, J., Kains, N., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Penny, M. T., Popovas, A., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Schmidt, R. W., Schoenebeck, F., Snodgrass, C., Street, R. A., Surdej, J., Tsapras, Y., and Vilela, C.
Abstract: We present time-series photometric observations of thirteen transits in the planetary systems WASP-24, WASP-25 and WASP-26. All three systems have orbital obliquity measurements, WASP-24 and WASP-26 have been observed with Spitzer, and WASP-25 was previously comparatively neglected. Our light curves were obtained using the telescope-defocussing method and have scatters of 0.5 to 1.2 mmag relative to their best-fitting geometric models. We used these data to measure the physical properties and orbital ephemerides of the systems to high precision, finding that our improved measurements are in good agreement with previous studies. High-resolution Lucky Imaging observations of all three targets show no evidence for faint stars close enough to contaminate our photometry. We confirm the eclipsing nature of the star closest to WASP-24 and present the detection of a detached eclipsing binary within 4.25 arcmin of WASP-26., Comment: Accepted for publication in MNRAS. 14 pages, 10 figures, 8 tables. Data and supplementary information are available on request
Published: 2014
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33. Diversifying selection in the wheat stem rust fungus acts predominantly on pathogen-associated gene families and reveals candidate effectors

Author: Sperschneider, J., Ying, H., Dodds, P., Gardiner, D., Upadhyaya, N., Singh, Karam, Manners, J., Taylor, J., Sperschneider, J., Ying, H., Dodds, P., Gardiner, D., Upadhyaya, N., Singh, Karam, Manners, J., and Taylor, J.
Abstract: Plant pathogens cause severe losses to crop plants and threaten global food production. One striking example is the wheat stem rust fungus, Puccinia graminis f. sp. tritici, which can rapidly evolve new virulent pathotypes in response to resistant host lines. Like several other filamentous fungal and oomycete plant pathogens, its genome features expanded gene families that have been implicated in host-pathogen interactions, possibly encoding effector proteins that interact directly with target host defense proteins. Previous efforts to understand virulence largely relied on the prediction of secreted, small and cysteine-rich proteins as candidate effectors and thus delivered an overwhelming number of candidates. Here, we implement an alternative analysis strategy that uses the signal of adaptive evolution as a line of evidence for effector function, combined with comparative information and expression data. We demonstrate that in planta up-regulated genes that are rapidly evolving are found almost exclusively in pathogen-associated gene families, affirming the impact of host-pathogen co-evolution on genome structure and the adaptive diversification of specialized gene families. In particular, we predict 42 effector candidates that are conserved only across pathogens, induced during infection and rapidly evolving. One of our top candidates has recently been shown to induce genotype-specific hypersensitive cell death in wheat. This shows that comparative genomics incorporating the evolutionary signal of adaptation is powerful for predicting effector candidates for laboratory verification. Our system can be applied to a wide range of pathogens and will give insight into host-pathogen dynamics, ultimately leading to progress in strategies for disease control.
Published: 2014

34. REDUCING ALCOHOL-RELATED HARM IN SPORT: A CLUSTER RANDOMISED TRIAL WITH FOOTBALL CLUBS

Author: Kingsland, M, Wolfenden, L, Tindall, J, Rowland, Bosco, Gillham, K, Dodds, P, Lecathelinais, C, McElduff, P, Sidey, M, Crundall, I, Rogerson, J, Wiggers, J, Kingsland, M, Wolfenden, L, Tindall, J, Rowland, Bosco, Gillham, K, Dodds, P, Lecathelinais, C, McElduff, P, Sidey, M, Crundall, I, Rogerson, J, and Wiggers, J
Published: 2013

35. MOA-2010-BLG-328Lb: a sub-Neptune orbiting very late M dwarf ?

Author: Furusawa, K., Udalski, A., Sumi, T., Bennett, D. P., Bond, I. A., Gould, A., Jorgensen, U. G., Snodgrass, C., Prester, D. Dominis, Albrow, M. D., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymanski, M. K., Soszynski, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzynski, G., Wyrzykowski, L., Choi, J. Y., Christie, G. W., DePoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Han, C., Hung, L. -W., Jung, Y. -K., Lee, C. -U., McCormick, J., Moorhouse, D., Natusch, T., Nola, M., Ofek, E., Park, B. G., Park, H., Pogge, R. W., Shin, I. -G., Skowron, J., Thornley, G., Yee, J. C., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., Surdej, J., Wambsganss, J., Street, R. A., Bramich, D. M., Steele, I. A., Tsapras, Y., Horne, K., Donatowicz, J., Sahu, K. C., Bachelet, E., Batista, V., Beatty, T. G., Beaulieu, J. -P., Bennett, C. S., Black, C., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Fouque, P., Greenhill, J., Henderson, C. B., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J. W., Shappee, B., Williams, A., Wouters, D., van Saders, J., Zellem, R., Zub, M., Furusawa, K., Udalski, A., Sumi, T., Bennett, D. P., Bond, I. A., Gould, A., Jorgensen, U. G., Snodgrass, C., Prester, D. Dominis, Albrow, M. D., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymanski, M. K., Soszynski, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzynski, G., Wyrzykowski, L., Choi, J. Y., Christie, G. W., DePoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Han, C., Hung, L. -W., Jung, Y. -K., Lee, C. -U., McCormick, J., Moorhouse, D., Natusch, T., Nola, M., Ofek, E., Park, B. G., Park, H., Pogge, R. W., Shin, I. -G., Skowron, J., Thornley, G., Yee, J. C., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., Surdej, J., Wambsganss, J., Street, R. A., Bramich, D. M., Steele, I. A., Tsapras, Y., Horne, K., Donatowicz, J., Sahu, K. C., Bachelet, E., Batista, V., Beatty, T. G., Beaulieu, J. -P., Bennett, C. S., Black, C., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Fouque, P., Greenhill, J., Henderson, C. B., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J. W., Shappee, B., Williams, A., Wouters, D., van Saders, J., Zellem, R., and Zub, M.
Abstract: We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of Mh = 0.11+/-0.01 M_{sun} and Mp = 9.2+/-2.2M_Earth, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at DL = 0.81 +/- 0.10 kpc with projected separation r = 0.92 +/- 0.16 AU. Because of the host's a-priori-unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions., Comment: 30 pages, 6 figures. accepted for publication in ApJ. Figure 1 and 2 are updated
Published: 2013
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36. Physical properties, transmission and emission spectra of the WASP-19 planetary system from multi-colour photometry

Author: Mancini, L., Ciceri, S., Chen, G., Tregloan-Reed, J., Fortney, J. J., Southworth, J., Tan, T. G., Burgdorf, M., Novati, S. Calchi, Dominik, M., Fang, X. -S., Finet, F., Gerner, T., Hardis, S., Hinse, T. C., Jorgensen, U. G., Liebig, C., Nikolov, N., Ricci, D., Schaefer, S., Schoenebeck, F., Skottfelt, J., Wertz, O., Alsubai, K. A., Bozza, V., Browne, P., Dodds, P., Gu, S. -H., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kains, N., Kerins, E., Kjeldsen, H., Lund, M. N., Lundkvist, M., Madhusudhan, N., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Snodgrass, C., Surdej, J., Mancini, L., Ciceri, S., Chen, G., Tregloan-Reed, J., Fortney, J. J., Southworth, J., Tan, T. G., Burgdorf, M., Novati, S. Calchi, Dominik, M., Fang, X. -S., Finet, F., Gerner, T., Hardis, S., Hinse, T. C., Jorgensen, U. G., Liebig, C., Nikolov, N., Ricci, D., Schaefer, S., Schoenebeck, F., Skottfelt, J., Wertz, O., Alsubai, K. A., Bozza, V., Browne, P., Dodds, P., Gu, S. -H., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kains, N., Kerins, E., Kjeldsen, H., Lund, M. N., Lundkvist, M., Madhusudhan, N., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Snodgrass, C., and Surdej, J.
Abstract: We present new ground-based, multi-colour, broad-band photometric measurements of the physical parameters, transmission and emission spectra of the transiting extrasolar planet WASP-19b. The measurements are based on observations of 8 transits and four occultations using the 1.5m Danish Telescope, 14 transits at the PEST observatory, and 1 transit observed simultaneously through four optical and three near-infrared filters, using the GROND instrument on the ESO 2.2m telescope. We use these new data to measure refined physical parameters for the system. We find the planet to be more bloated and the system to be twice as old as initially thought. We also used published and archived datasets to study the transit timings, which do not depart from a linear ephemeris. We detected an anomaly in the GROND transit light curve which is compatible with a spot on the photosphere of the parent star. The starspot position, size, spot contrast and temperature were established. Using our new and published measurements, we assembled the planet's transmission spectrum over the 370-2350 nm wavelength range and its emission spectrum over the 750-8000 nm range. By comparing these data to theoretical models we investigated the theoretically-predicted variation of the apparent radius of WASP-19b as a function of wavelength and studied the composition and thermal structure of its atmosphere. We conclude that: there is no evidence for strong optical absorbers at low pressure, supporting the common idea that the planet's atmosphere lacks a dayside inversion; the temperature of the planet is not homogenized, because the high warming of its dayside causes the planet to be more efficient in re-radiating than redistributing energy to the night side; the planet seems to be outside of any current classification scheme., Comment: 18 pages, 12 figures, 11 tables
Published: 2013
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37. High-precision photometry by telescope defocussing. V. WASP-15 and WASP-16

Author: Southworth, J., Mancini, L., Browne, P., Burgdorf, M., Novati, S. Calchi, Dominik, M., Gerner, T., Hinse, T. C., Jorgensen, U. G., Kains, N., Ricci, D., Schafer, S., Schonebeck, F., Tregloan-Reed, J., Alsubai, K. A., Bozza, V., Chen, G., Dodds, P., Dreizler, S., Fang, X. -S., Finet, F., Gu, S. -H., Hardis, S., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Kjeldsen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., Wertz, O., Southworth, J., Mancini, L., Browne, P., Burgdorf, M., Novati, S. Calchi, Dominik, M., Gerner, T., Hinse, T. C., Jorgensen, U. G., Kains, N., Ricci, D., Schafer, S., Schonebeck, F., Tregloan-Reed, J., Alsubai, K. A., Bozza, V., Chen, G., Dodds, P., Dreizler, S., Fang, X. -S., Finet, F., Gu, S. -H., Hardis, S., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Kjeldsen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., and Wertz, O.
Abstract: We present new photometric observations of WASP-15 and WASP-16, two transiting extrasolar planetary systems with measured orbital obliquities but without photometric follow-up since their discovery papers. Our new data for WASP-15 comprise observations of one transit simultaneously in four optical passbands using GROND on the MPG/ESO 2.2m telescope, plus coverage of half a transit from DFOSC on the Danish 1.54m telescope, both at ESO La Silla. For WASP-16 we present observations of four complete transits, all from the Danish telescope. We use these new data to refine the measured physical properties and orbital ephemerides of the two systems. Whilst our results are close to the originally-determined values for WASP-15, we find that the star and planet in the WASP-16 system are both larger and less massive than previously thought., Comment: Accepted for publication in MNRAS; 9 pages, 7 tables, 6 figures. The light curves are available from http://www.astro.keele.ac.uk/jkt/data-teps.html and the results are included in TEPCat at http://www.astro.keele.ac.uk/jkt/tepcat
Published: 2013
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38. Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry

Author: Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jørgensen, U. G., Giridhar, S., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X. -S., Giannini, E., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Williams, A., Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jørgensen, U. G., Giridhar, S., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X. -S., Giannini, E., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Williams, A.
Abstract: We present the analysis of 26 nights of V and I time-series observations from 2011 and 2012 of the globular cluster M 30 (NGC 7099). We used our data to search for variable stars in this cluster and refine the periods of known variables; we then used our variable star light curves to derive values for the cluster's parameters. We used difference image analysis to reduce our data to obtain high-precision light curves of variable stars. We then estimated the cluster parameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible. We also derive an estimate for the age of the cluster by fitting theoretical isochrones to our colour-magnitude diagram (CMD). Out of 13 stars previously catalogued as variables, we find that only 4 are bona fide variables. We detect two new RR Lyrae variables, and confirm two additional RR Lyrae candidates from the literature. We also detect four other new variables, including an eclipsing blue straggler system, and an SX Phoenicis star. This amounts to a total number of confirmed variable stars in M 30 of 12. We perform Fourier decomposition of the light curves of the RR Lyrae stars to derive cluster parameters using empirical relations. We find a cluster metallicity [Fe/H]_ZW=-2.01 +- 0.04, or [Fe/H]_UVES=-2.11 +- 0.06, and a distance of 8.32 +- 0.20 kpc (using RR0 variables), 8.10 kpc (using one RR1 variable), and 8.35 +- 0.42 kpc (using our SX Phoenicis star detection in M 30). Fitting isochrones to the CMD, we estimate an age of 13.0 +- 1.0 Gyr for M 30., Comment: 16 pages, 10 figures, 10 tables, A&A in press
Published: 2013
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39. A Giant Planet beyond the Snow Line in Microlensing Event OGLE-2011-BLG-0251

Author: Kains, N., Street, R., Choi, J. -Y., Han, C., Udalski, A., Almeida, L. A., Jablonski, F., Tristram, P., Jorgensen, U. G., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsoe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Sahu, K. C., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D. M., Horne, K., Ipatov, S., Steele, I. A., Tsapras, Y., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D. J., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Wada, K., Yock, P. C. M., Allen, W., Batista, V., Chung, S. -J., Christie, G., DePoy, D. L., Drummond, J., Gaudi, B. S., Gould, A., Henderson, C., Jung, Y. -K., Koo, J. -R., Lee, C. -U., McCormick, J., McGregor, D., Munoz, J. A., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Shin, I. -G., Yee, J., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Williams, A., Wouters, D., Zub, M., Kains, N., Street, R., Choi, J. -Y., Han, C., Udalski, A., Almeida, L. A., Jablonski, F., Tristram, P., Jorgensen, U. G., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsoe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Sahu, K. C., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D. M., Horne, K., Ipatov, S., Steele, I. A., Tsapras, Y., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D. J., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Wada, K., Yock, P. C. M., Allen, W., Batista, V., Chung, S. -J., Christie, G., DePoy, D. L., Drummond, J., Gaudi, B. S., Gould, A., Henderson, C., Jung, Y. -K., Koo, J. -R., Lee, C. -U., McCormick, J., McGregor, D., Munoz, J. A., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Shin, I. -G., Yee, J., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Williams, A., Wouters, D., and Zub, M.
Abstract: We present the analysis of the gravitational microlensing event OGLE-2011-BLG-0251. This anomalous event was observed by several survey and follow-up collaborations conducting microlensing observations towards the Galactic Bulge. Based on detailed modelling of the observed light curve, we find that the lens is composed of two masses with a mass ratio q=1.9 x 10^-3. Thanks to our detection of higher-order effects on the light curve due to the Earth's orbital motion and the finite size of source, we are able to measure the mass and distance to the lens unambiguously. We find that the lens is made up of a planet of mass 0.53 +- 0.21,M_Jup orbiting an M dwarf host star with a mass of 0.26 +- 0.11 M_Sun. The planetary system is located at a distance of 2.57 +- 0.61 kpc towards the Galactic Centre. The projected separation of the planet from its host star is d=1.408 +- 0.019, in units of the Einstein radius, which corresponds to 2.72 +- 0.75 AU in physical units. We also identified a competitive model with similar planet and host star masses, but with a smaller orbital radius of 1.50 +- 0.50 AU. The planet is therefore located beyond the snow line of its host star, which we estimate to be around 1-1.5 AU., Comment: 12 pages, 7 figures, 3 tables; A&A in press
Published: 2013
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40. Microlensing Discovery of a Population of Very Tight, Very Low-mass Binary Brown Dwarfs

Author: Choi, J. -Y., Han, C., Udalski, A., Sumi, T., Gaudi, B. S., Gould, A., Bennett, D. P., Dominik, M., Beaulieu, J. -P., Tsapras, Y., Bozza, V., Abe, F., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, K., Sweatman, W. L., Suzuki, D., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Skowron, J., Kozłowski, S., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Pietrukowicz, P., Almeida, L. A., DePoy, D. L., Dong, Subo, Gorbikov, E., Jablonski, F., Henderson, C. B., Hwang, K. -H., Janczak, J., Jung, Y. -K., Kaspi, S., Lee, C. -U., Malamud, U., Maoz, D., McGregor, D., Munoz, J. A., Park, B. -G., Park, H., Pogge, R. W., Shvartzvald, Y., Shin, I. -G., Yee, J. C., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Fang, X. -S., Finet, F., Glitrup, M., Grundahl, F., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M. N., Lundkvist, M., Maier, G., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Zimmer, F., Albrow, M. D., Bachelet, E., Batista, V., Brillant, S., Cassan, A., Cole, A. A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Kubas, D., Marquette, J. -B., Menzies, J. W., Sahu, K. C., Zub, M., Bramich, D. M., Horne, K., Steele, I. A., Street, R. A., Choi, J. -Y., Han, C., Udalski, A., Sumi, T., Gaudi, B. S., Gould, A., Bennett, D. P., Dominik, M., Beaulieu, J. -P., Tsapras, Y., Bozza, V., Abe, F., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, K., Sweatman, W. L., Suzuki, D., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Skowron, J., Kozłowski, S., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Pietrukowicz, P., Almeida, L. A., DePoy, D. L., Dong, Subo, Gorbikov, E., Jablonski, F., Henderson, C. B., Hwang, K. -H., Janczak, J., Jung, Y. -K., Kaspi, S., Lee, C. -U., Malamud, U., Maoz, D., McGregor, D., Munoz, J. A., Park, B. -G., Park, H., Pogge, R. W., Shvartzvald, Y., Shin, I. -G., Yee, J. C., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Fang, X. -S., Finet, F., Glitrup, M., Grundahl, F., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M. N., Lundkvist, M., Maier, G., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Zimmer, F., Albrow, M. D., Bachelet, E., Batista, V., Brillant, S., Cassan, A., Cole, A. A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Kubas, D., Marquette, J. -B., Menzies, J. W., Sahu, K. C., Zub, M., Bramich, D. M., Horne, K., Steele, I. A., and Street, R. A.
Abstract: Although many models have been proposed, the physical mechanisms responsible for the formation of low-mass brown dwarfs are poorly understood. The multiplicity properties and minimum mass of the brown-dwarf mass function provide critical empirical diagnostics of these mechanisms. We present the discovery via gravitational microlensing of two very low-mass, very tight binary systems. These binaries have directly and precisely measured total system masses of 0.025 Msun and 0.034 Msun, and projected separations of 0.31 AU and 0.19 AU, making them the lowest-mass and tightest field brown-dwarf binaries known. The discovery of a population of such binaries indicates that brown dwarf binaries can robustly form at least down to masses of ~0.02 Msun. Future microlensing surveys will measure a mass-selected sample of brown-dwarf binary systems, which can then be directly compared to similar samples of stellar binaries., Comment: 7 pages, 5 figures, 3 tables, ApJ submitted
Published: 2013
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41. Flux and color variations of the doubly imaged quasar UM673

Author: Ricci, D., Elyiv, A., Finet, F., Wertz, O., Alsubai, K., Anguita, T., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Schmidt, R., Skottfelt, J., Snodgrass, C., Southworth, J., Thöne, C. C., Wambsganss, J., Zimmer, F., Zub, M., Surdej, J., Ricci, D., Elyiv, A., Finet, F., Wertz, O., Alsubai, K., Anguita, T., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Schmidt, R., Skottfelt, J., Snodgrass, C., Southworth, J., Thöne, C. C., Wambsganss, J., Zimmer, F., Zub, M., and Surdej, J.
Abstract: With the aim of characterizing the flux and color variations of the multiple components of the gravitationally lensed quasar UM673 as a function of time, we have performed multi-epoch and multi-band photometric observations with the Danish 1.54m telescope at the La Silla Observatory. The observations were carried out in the VRi spectral bands during four seasons (2008--2011). We reduced the data using the PSF (Point Spread Function) photometric technique as well as aperture photometry. Our results show for the brightest lensed component some significant decrease in flux between the first two seasons (+0.09/+0.11/+0.05 mag) and a subsequent increase during the following ones (-0.11/-0.11/-0.10 mag) in the V/R/i spectral bands, respectively. Comparing our results with previous studies, we find smaller color variations between these seasons as compared with previous ones. We also separate the contribution of the lensing galaxy from that of the fainter and close lensed component., Comment: 7 pages, 8 figures, 4 tables
Published: 2013
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42. A giant planet beyond the snow line in microlensing event OGLE-2011-BLG-0251

Author: Kains, N., Street, R., Choi, J., Han, C., Udalski, A., Almeida, L., Jablonski, F., Tristram, P., Jorgensen, U., Szymanski, M., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Fang, X., Grundahl, F., Gu, C., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D., Horne, K., Ipatov, S., Steele, I., Tsapras, Y., Abe, F., Bennett, D., Bond, I., Botzler, C., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W., Takino, S., Wada, K., Yock, P., Allen, W., Batista, V., Chung, S., Christie, G., DePoy, D., Drummond, J., Gaudi, B., Gould, A., Henderson, C., Jung, Y., Koo, J., Lee, C., McCormick, J., McGregor, D., Munoz, J., Natusch, T., Ngan, H., Park, H., Pogge, R., Shin, I., Yee, J., Albrow, M., Bachelet, E., Beaulieu, J., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque, P., Greenhill, J., Kane, S., Kubas, D., Marquette, J., Martin, R., Meintjes, P., Menzies, J., Pollard, K., Williams, Andrew, Wouters, D., Zub, M., Kains, N., Street, R., Choi, J., Han, C., Udalski, A., Almeida, L., Jablonski, F., Tristram, P., Jorgensen, U., Szymanski, M., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Fang, X., Grundahl, F., Gu, C., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D., Horne, K., Ipatov, S., Steele, I., Tsapras, Y., Abe, F., Bennett, D., Bond, I., Botzler, C., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W., Takino, S., Wada, K., Yock, P., Allen, W., Batista, V., Chung, S., Christie, G., DePoy, D., Drummond, J., Gaudi, B., Gould, A., Henderson, C., Jung, Y., Koo, J., Lee, C., McCormick, J., McGregor, D., Munoz, J., Natusch, T., Ngan, H., Park, H., Pogge, R., Shin, I., Yee, J., Albrow, M., Bachelet, E., Beaulieu, J., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque, P., Greenhill, J., Kane, S., Kubas, D., Marquette, J., Martin, R., Meintjes, P., Menzies, J., Pollard, K., Williams, Andrew, Wouters, D., and Zub, M.
Abstract: Aims. We present the analysis of the gravitational microlensing event OGLE-2011-BLG-0251. This anomalous event was observed by several survey and follow-up collaborations conducting microlensing observations towards the Galactic bulge.Methods. Based on detailed modelling of the observed light curve, we find that the lens is composed of twomasses with a mass ratio q = 1.9 × 10-3. Thanks to our detection of higher-order effects on the light curve due to the Earth’s orbital motion and the finite size of source, we are able to measure the mass and distance to the lens unambiguously.Results. We find that the lens is made up of a planet of mass 0.53 ± 0.21 MJ orbiting an M dwarf host star with a mass of 0.26 ± 0.11 M. The planetary system is located at a distance of 2.57 ± 0.61 kpc towards the Galactic centre. The projected separation of the planet from its host star is d = 1.408 ± 0.019, in units of the Einstein radius, which corresponds to 2.72 ± 0.75 AU in physical units. We also identified a competitive model with similar planet and host star masses, but with a smaller orbital radius of 1.50 ± 0.50 AU. The planet is therefore located beyond the snow line of its host star, which we estimate to be around ~1-1.5 AU.
Published: 2013

43. A Giant Planet beyond the Snow Line in Microlensing Event OGLE-2011-BLG-0251

Author: Kains, N., Street, R., Choi, J. -Y., Han, C., Udalski, A., Almeida, L. A., Jablonski, F., Tristram, P., Jorgensen, U. G., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsoe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Sahu, K. C., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D. M., Horne, K., Ipatov, S., Steele, I. A., Tsapras, Y., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D. J., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Wada, K., Yock, P. C. M., Allen, W., Batista, V., Chung, S. -J., Christie, G., DePoy, D. L., Drummond, J., Gaudi, B. S., Gould, A., Henderson, C., Jung, Y. -K., Koo, J. -R., Lee, C. -U., McCormick, J., McGregor, D., Munoz, J. A., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Shin, I. -G., Yee, J., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Williams, A., Wouters, D., Zub, M., Kains, N., Street, R., Choi, J. -Y., Han, C., Udalski, A., Almeida, L. A., Jablonski, F., Tristram, P., Jorgensen, U. G., Szymanski, M. K., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsoe, K., Hessman, F. V., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Sahu, K. C., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D. M., Horne, K., Ipatov, S., Steele, I. A., Tsapras, Y., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D. J., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Wada, K., Yock, P. C. M., Allen, W., Batista, V., Chung, S. -J., Christie, G., DePoy, D. L., Drummond, J., Gaudi, B. S., Gould, A., Henderson, C., Jung, Y. -K., Koo, J. -R., Lee, C. -U., McCormick, J., McGregor, D., Munoz, J. A., Natusch, T., Ngan, H., Park, H., Pogge, R. W., Shin, I. -G., Yee, J., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A., Corrales, E., Coutures, Ch., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouque, P., Greenhill, J., Kane, S. R., Kubas, D., Marquette, J. -B., Martin, R., Meintjes, P., Menzies, J., Pollard, K. R., Williams, A., Wouters, D., and Zub, M.
Abstract: We present the analysis of the gravitational microlensing event OGLE-2011-BLG-0251. This anomalous event was observed by several survey and follow-up collaborations conducting microlensing observations towards the Galactic Bulge. Based on detailed modelling of the observed light curve, we find that the lens is composed of two masses with a mass ratio q=1.9 x 10^-3. Thanks to our detection of higher-order effects on the light curve due to the Earth's orbital motion and the finite size of source, we are able to measure the mass and distance to the lens unambiguously. We find that the lens is made up of a planet of mass 0.53 +- 0.21,M_Jup orbiting an M dwarf host star with a mass of 0.26 +- 0.11 M_Sun. The planetary system is located at a distance of 2.57 +- 0.61 kpc towards the Galactic Centre. The projected separation of the planet from its host star is d=1.408 +- 0.019, in units of the Einstein radius, which corresponds to 2.72 +- 0.75 AU in physical units. We also identified a competitive model with similar planet and host star masses, but with a smaller orbital radius of 1.50 +- 0.50 AU. The planet is therefore located beyond the snow line of its host star, which we estimate to be around 1-1.5 AU., Comment: 12 pages, 7 figures, 3 tables; A&A in press
Published: 2013
Full Text: View/download PDF

44. A giant planet beyond the snow line in microlensing event OGLE-2011-BLG-0251

Author: Kains, N., Street, R., Choi, J., Han, C., Udalski, A., Almeida, L., Jablonski, F., Tristram, P., Jorgensen, U., Szymanski, M., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Fang, X., Grundahl, F., Gu, C., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D., Horne, K., Ipatov, S., Steele, I., Tsapras, Y., Abe, F., Bennett, D., Bond, I., Botzler, C., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W., Takino, S., Wada, K., Yock, P., Allen, W., Batista, V., Chung, S., Christie, G., DePoy, D., Drummond, J., Gaudi, B., Gould, A., Henderson, C., Jung, Y., Koo, J., Lee, C., McCormick, J., McGregor, D., Munoz, J., Natusch, T., Ngan, H., Park, H., Pogge, R., Shin, I., Yee, J., Albrow, M., Bachelet, E., Beaulieu, J., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque, P., Greenhill, J., Kane, S., Kubas, D., Marquette, J., Martin, R., Meintjes, P., Menzies, J., Pollard, K., Williams, Andrew, Wouters, D., Zub, M., Kains, N., Street, R., Choi, J., Han, C., Udalski, A., Almeida, L., Jablonski, F., Tristram, P., Jorgensen, U., Szymanski, M., Kubiak, M., Pietrzynski, G., Soszynski, I., Poleski, R., Kozlowski, S., Pietrukowicz, P., Ulaczyk, K., Wyrzykowski, L., Skowron, J., Alsubai, K., Bozza, V., Browne, P., Burgdorf, M., Calchi Novati, S., Dodds, P., Dominik, M., Dreizler, S., Fang, X., Grundahl, F., Gu, C., Hardis, S., Harpsoe, K., Hessman, F., Hinse, T., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Liebig, C., Lund, M., Lundkvist, M., Mancini, L., Mathiasen, M., Penny, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Bajek, D., Bramich, D., Horne, K., Ipatov, S., Steele, I., Tsapras, Y., Abe, F., Bennett, D., Bond, I., Botzler, C., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N., Saito, T., Sullivan, D., Sumi, T., Suzuki, D., Suzuki, K., Sweatman, W., Takino, S., Wada, K., Yock, P., Allen, W., Batista, V., Chung, S., Christie, G., DePoy, D., Drummond, J., Gaudi, B., Gould, A., Henderson, C., Jung, Y., Koo, J., Lee, C., McCormick, J., McGregor, D., Munoz, J., Natusch, T., Ngan, H., Park, H., Pogge, R., Shin, I., Yee, J., Albrow, M., Bachelet, E., Beaulieu, J., Brillant, S., Caldwell, J., Cassan, A., Cole, A., Corrales, E., Coutures, C., Dieters, S., Dominis Prester, D., Donatowicz, J., Fouque, P., Greenhill, J., Kane, S., Kubas, D., Marquette, J., Martin, R., Meintjes, P., Menzies, J., Pollard, K., Williams, Andrew, Wouters, D., and Zub, M.
Abstract: Aims. We present the analysis of the gravitational microlensing event OGLE-2011-BLG-0251. This anomalous event was observed by several survey and follow-up collaborations conducting microlensing observations towards the Galactic bulge.Methods. Based on detailed modelling of the observed light curve, we find that the lens is composed of twomasses with a mass ratio q = 1.9 × 10-3. Thanks to our detection of higher-order effects on the light curve due to the Earth’s orbital motion and the finite size of source, we are able to measure the mass and distance to the lens unambiguously.Results. We find that the lens is made up of a planet of mass 0.53 ± 0.21 MJ orbiting an M dwarf host star with a mass of 0.26 ± 0.11 M. The planetary system is located at a distance of 2.57 ± 0.61 kpc towards the Galactic centre. The projected separation of the planet from its host star is d = 1.408 ± 0.019, in units of the Einstein radius, which corresponds to 2.72 ± 0.75 AU in physical units. We also identified a competitive model with similar planet and host star masses, but with a smaller orbital radius of 1.50 ± 0.50 AU. The planet is therefore located beyond the snow line of its host star, which we estimate to be around ~1-1.5 AU.
Published: 2013

45. MOA-2010-BLG-328Lb: a sub-Neptune orbiting very late M dwarf ?

Author: Furusawa, K., Udalski, A., Sumi, T., Bennett, D. P., Bond, I. A., Gould, A., Jorgensen, U. G., Snodgrass, C., Prester, D. Dominis, Albrow, M. D., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymanski, M. K., Soszynski, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzynski, G., Wyrzykowski, L., Choi, J. Y., Christie, G. W., DePoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Han, C., Hung, L. -W., Jung, Y. -K., Lee, C. -U., McCormick, J., Moorhouse, D., Natusch, T., Nola, M., Ofek, E., Park, B. G., Park, H., Pogge, R. W., Shin, I. -G., Skowron, J., Thornley, G., Yee, J. C., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., Surdej, J., Wambsganss, J., Street, R. A., Bramich, D. M., Steele, I. A., Tsapras, Y., Horne, K., Donatowicz, J., Sahu, K. C., Bachelet, E., Batista, V., Beatty, T. G., Beaulieu, J. -P., Bennett, C. S., Black, C., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Fouque, P., Greenhill, J., Henderson, C. B., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J. W., Shappee, B., Williams, A., Wouters, D., van Saders, J., Zellem, R., Zub, M., Furusawa, K., Udalski, A., Sumi, T., Bennett, D. P., Bond, I. A., Gould, A., Jorgensen, U. G., Snodgrass, C., Prester, D. Dominis, Albrow, M. D., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Harris, P., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymanski, M. K., Soszynski, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzynski, G., Wyrzykowski, L., Choi, J. Y., Christie, G. W., DePoy, D. L., Dong, S., Drummond, J., Gaudi, B. S., Han, C., Hung, L. -W., Jung, Y. -K., Lee, C. -U., McCormick, J., Moorhouse, D., Natusch, T., Nola, M., Ofek, E., Park, B. G., Park, H., Pogge, R. W., Shin, I. -G., Skowron, J., Thornley, G., Yee, J. C., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dominik, M., Finet, F., Gerner, T., Hardis, S., Harpsoe, K., Hinse, T. C., Hundertmark, M., Kains, N., Kerins, E., Liebig, C., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schafer, S., Schonebeck, F., Southworth, J., Surdej, J., Wambsganss, J., Street, R. A., Bramich, D. M., Steele, I. A., Tsapras, Y., Horne, K., Donatowicz, J., Sahu, K. C., Bachelet, E., Batista, V., Beatty, T. G., Beaulieu, J. -P., Bennett, C. S., Black, C., Bowens-Rubin, R., Brillant, S., Caldwell, J. A. R., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Fouque, P., Greenhill, J., Henderson, C. B., Kubas, D., Marquette, J. -B., Martin, R., Menzies, J. W., Shappee, B., Williams, A., Wouters, D., van Saders, J., Zellem, R., and Zub, M.
Abstract: We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of Mh = 0.11+/-0.01 M_{sun} and Mp = 9.2+/-2.2M_Earth, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at DL = 0.81 +/- 0.10 kpc with projected separation r = 0.92 +/- 0.16 AU. Because of the host's a-priori-unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions., Comment: 30 pages, 6 figures. accepted for publication in ApJ. Figure 1 and 2 are updated
Published: 2013
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46. Physical properties, transmission and emission spectra of the WASP-19 planetary system from multi-colour photometry

Author: Mancini, L., Ciceri, S., Chen, G., Tregloan-Reed, J., Fortney, J. J., Southworth, J., Tan, T. G., Burgdorf, M., Novati, S. Calchi, Dominik, M., Fang, X. -S., Finet, F., Gerner, T., Hardis, S., Hinse, T. C., Jorgensen, U. G., Liebig, C., Nikolov, N., Ricci, D., Schaefer, S., Schoenebeck, F., Skottfelt, J., Wertz, O., Alsubai, K. A., Bozza, V., Browne, P., Dodds, P., Gu, S. -H., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kains, N., Kerins, E., Kjeldsen, H., Lund, M. N., Lundkvist, M., Madhusudhan, N., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Snodgrass, C., Surdej, J., Mancini, L., Ciceri, S., Chen, G., Tregloan-Reed, J., Fortney, J. J., Southworth, J., Tan, T. G., Burgdorf, M., Novati, S. Calchi, Dominik, M., Fang, X. -S., Finet, F., Gerner, T., Hardis, S., Hinse, T. C., Jorgensen, U. G., Liebig, C., Nikolov, N., Ricci, D., Schaefer, S., Schoenebeck, F., Skottfelt, J., Wertz, O., Alsubai, K. A., Bozza, V., Browne, P., Dodds, P., Gu, S. -H., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kains, N., Kerins, E., Kjeldsen, H., Lund, M. N., Lundkvist, M., Madhusudhan, N., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Snodgrass, C., and Surdej, J.
Abstract: We present new ground-based, multi-colour, broad-band photometric measurements of the physical parameters, transmission and emission spectra of the transiting extrasolar planet WASP-19b. The measurements are based on observations of 8 transits and four occultations using the 1.5m Danish Telescope, 14 transits at the PEST observatory, and 1 transit observed simultaneously through four optical and three near-infrared filters, using the GROND instrument on the ESO 2.2m telescope. We use these new data to measure refined physical parameters for the system. We find the planet to be more bloated and the system to be twice as old as initially thought. We also used published and archived datasets to study the transit timings, which do not depart from a linear ephemeris. We detected an anomaly in the GROND transit light curve which is compatible with a spot on the photosphere of the parent star. The starspot position, size, spot contrast and temperature were established. Using our new and published measurements, we assembled the planet's transmission spectrum over the 370-2350 nm wavelength range and its emission spectrum over the 750-8000 nm range. By comparing these data to theoretical models we investigated the theoretically-predicted variation of the apparent radius of WASP-19b as a function of wavelength and studied the composition and thermal structure of its atmosphere. We conclude that: there is no evidence for strong optical absorbers at low pressure, supporting the common idea that the planet's atmosphere lacks a dayside inversion; the temperature of the planet is not homogenized, because the high warming of its dayside causes the planet to be more efficient in re-radiating than redistributing energy to the night side; the planet seems to be outside of any current classification scheme., Comment: 18 pages, 12 figures, 11 tables
Published: 2013
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47. High-precision photometry by telescope defocussing. V. WASP-15 and WASP-16

Author: Southworth, J., Mancini, L., Browne, P., Burgdorf, M., Novati, S. Calchi, Dominik, M., Gerner, T., Hinse, T. C., Jorgensen, U. G., Kains, N., Ricci, D., Schafer, S., Schonebeck, F., Tregloan-Reed, J., Alsubai, K. A., Bozza, V., Chen, G., Dodds, P., Dreizler, S., Fang, X. -S., Finet, F., Gu, S. -H., Hardis, S., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Kjeldsen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., Wertz, O., Southworth, J., Mancini, L., Browne, P., Burgdorf, M., Novati, S. Calchi, Dominik, M., Gerner, T., Hinse, T. C., Jorgensen, U. G., Kains, N., Ricci, D., Schafer, S., Schonebeck, F., Tregloan-Reed, J., Alsubai, K. A., Bozza, V., Chen, G., Dodds, P., Dreizler, S., Fang, X. -S., Finet, F., Gu, S. -H., Hardis, S., Harpsoe, K., Henning, Th., Hundertmark, M., Jessen-Hansen, J., Kerins, E., Kjeldsen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mathiasen, M., Nikolov, N., Penny, M. T., Proft, S., Rahvar, S., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Surdej, J., and Wertz, O.
Abstract: We present new photometric observations of WASP-15 and WASP-16, two transiting extrasolar planetary systems with measured orbital obliquities but without photometric follow-up since their discovery papers. Our new data for WASP-15 comprise observations of one transit simultaneously in four optical passbands using GROND on the MPG/ESO 2.2m telescope, plus coverage of half a transit from DFOSC on the Danish 1.54m telescope, both at ESO La Silla. For WASP-16 we present observations of four complete transits, all from the Danish telescope. We use these new data to refine the measured physical properties and orbital ephemerides of the two systems. Whilst our results are close to the originally-determined values for WASP-15, we find that the star and planet in the WASP-16 system are both larger and less massive than previously thought., Comment: Accepted for publication in MNRAS; 9 pages, 7 tables, 6 figures. The light curves are available from http://www.astro.keele.ac.uk/jkt/data-teps.html and the results are included in TEPCat at http://www.astro.keele.ac.uk/jkt/tepcat
Published: 2013
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48. Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry

Author: Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jørgensen, U. G., Giridhar, S., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X. -S., Giannini, E., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., Williams, A., Kains, N., Bramich, D. M., Ferro, A. Arellano, Jaimes, R. Figuera, Jørgensen, U. G., Giridhar, S., Alsubai, K. A., Andersen, J. M., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Damerdji, Y., Diehl, C., Dodds, P., Dominik, M., Elyiv, A., Fang, X. -S., Giannini, E., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Juncher, D., Kerins, E., Kjeldsen, H., Korhonen, H., Liebig, C., Lund, M. N., Lundkvist, M., Mancini, L., Martin, R., Mathiasen, M., Penny, M. T., Rabus, M., Rahvar, S., Ricci, D., Sahu, K., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Vilela, C., Wertz, O., and Williams, A.
Abstract: We present the analysis of 26 nights of V and I time-series observations from 2011 and 2012 of the globular cluster M 30 (NGC 7099). We used our data to search for variable stars in this cluster and refine the periods of known variables; we then used our variable star light curves to derive values for the cluster's parameters. We used difference image analysis to reduce our data to obtain high-precision light curves of variable stars. We then estimated the cluster parameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible. We also derive an estimate for the age of the cluster by fitting theoretical isochrones to our colour-magnitude diagram (CMD). Out of 13 stars previously catalogued as variables, we find that only 4 are bona fide variables. We detect two new RR Lyrae variables, and confirm two additional RR Lyrae candidates from the literature. We also detect four other new variables, including an eclipsing blue straggler system, and an SX Phoenicis star. This amounts to a total number of confirmed variable stars in M 30 of 12. We perform Fourier decomposition of the light curves of the RR Lyrae stars to derive cluster parameters using empirical relations. We find a cluster metallicity [Fe/H]_ZW=-2.01 +- 0.04, or [Fe/H]_UVES=-2.11 +- 0.06, and a distance of 8.32 +- 0.20 kpc (using RR0 variables), 8.10 kpc (using one RR1 variable), and 8.35 +- 0.42 kpc (using our SX Phoenicis star detection in M 30). Fitting isochrones to the CMD, we estimate an age of 13.0 +- 1.0 Gyr for M 30., Comment: 16 pages, 10 figures, 10 tables, A&A in press
Published: 2013
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49. Microlensing Discovery of a Population of Very Tight, Very Low-mass Binary Brown Dwarfs

Author: Choi, J. -Y., Han, C., Udalski, A., Sumi, T., Gaudi, B. S., Gould, A., Bennett, D. P., Dominik, M., Beaulieu, J. -P., Tsapras, Y., Bozza, V., Abe, F., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, K., Sweatman, W. L., Suzuki, D., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Skowron, J., Kozłowski, S., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Pietrukowicz, P., Almeida, L. A., DePoy, D. L., Dong, Subo, Gorbikov, E., Jablonski, F., Henderson, C. B., Hwang, K. -H., Janczak, J., Jung, Y. -K., Kaspi, S., Lee, C. -U., Malamud, U., Maoz, D., McGregor, D., Munoz, J. A., Park, B. -G., Park, H., Pogge, R. W., Shvartzvald, Y., Shin, I. -G., Yee, J. C., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Fang, X. -S., Finet, F., Glitrup, M., Grundahl, F., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M. N., Lundkvist, M., Maier, G., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Zimmer, F., Albrow, M. D., Bachelet, E., Batista, V., Brillant, S., Cassan, A., Cole, A. A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Kubas, D., Marquette, J. -B., Menzies, J. W., Sahu, K. C., Zub, M., Bramich, D. M., Horne, K., Steele, I. A., Street, R. A., Choi, J. -Y., Han, C., Udalski, A., Sumi, T., Gaudi, B. S., Gould, A., Bennett, D. P., Dominik, M., Beaulieu, J. -P., Tsapras, Y., Bozza, V., Abe, F., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, K., Sweatman, W. L., Suzuki, D., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., Szymański, M. K., Kubiak, M., Pietrzyński, G., Soszyński, I., Skowron, J., Kozłowski, S., Poleski, R., Ulaczyk, K., Wyrzykowski, Ł., Pietrukowicz, P., Almeida, L. A., DePoy, D. L., Dong, Subo, Gorbikov, E., Jablonski, F., Henderson, C. B., Hwang, K. -H., Janczak, J., Jung, Y. -K., Kaspi, S., Lee, C. -U., Malamud, U., Maoz, D., McGregor, D., Munoz, J. A., Park, B. -G., Park, H., Pogge, R. W., Shvartzvald, Y., Shin, I. -G., Yee, J. C., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Fang, X. -S., Finet, F., Glitrup, M., Grundahl, F., Gu, S. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M. N., Lundkvist, M., Maier, G., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Snodgrass, C., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Zimmer, F., Albrow, M. D., Bachelet, E., Batista, V., Brillant, S., Cassan, A., Cole, A. A., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Fouqué, P., Greenhill, J., Kubas, D., Marquette, J. -B., Menzies, J. W., Sahu, K. C., Zub, M., Bramich, D. M., Horne, K., Steele, I. A., and Street, R. A.
Abstract: Although many models have been proposed, the physical mechanisms responsible for the formation of low-mass brown dwarfs are poorly understood. The multiplicity properties and minimum mass of the brown-dwarf mass function provide critical empirical diagnostics of these mechanisms. We present the discovery via gravitational microlensing of two very low-mass, very tight binary systems. These binaries have directly and precisely measured total system masses of 0.025 Msun and 0.034 Msun, and projected separations of 0.31 AU and 0.19 AU, making them the lowest-mass and tightest field brown-dwarf binaries known. The discovery of a population of such binaries indicates that brown dwarf binaries can robustly form at least down to masses of ~0.02 Msun. Future microlensing surveys will measure a mass-selected sample of brown-dwarf binary systems, which can then be directly compared to similar samples of stellar binaries., Comment: 7 pages, 5 figures, 3 tables, ApJ submitted
Published: 2013
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50. Flux and color variations of the doubly imaged quasar UM673

Author: Ricci, D., Elyiv, A., Finet, F., Wertz, O., Alsubai, K., Anguita, T., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Schmidt, R., Skottfelt, J., Snodgrass, C., Southworth, J., Thöne, C. C., Wambsganss, J., Zimmer, F., Zub, M., Surdej, J., Ricci, D., Elyiv, A., Finet, F., Wertz, O., Alsubai, K., Anguita, T., Bozza, V., Browne, P., Burgdorf, M., Novati, S. Calchi, Dodds, P., Dominik, M., Dreizler, S., Gerner, T., Glitrup, M., Grundahl, F., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Maier, G., Mancini, L., Masi, G., Mathiasen, M., Penny, M., Proft, S., Rahvar, S., Scarpetta, G., Sahu, K., Schäfer, S., Schönebeck, F., Schmidt, R., Skottfelt, J., Snodgrass, C., Southworth, J., Thöne, C. C., Wambsganss, J., Zimmer, F., Zub, M., and Surdej, J.
Abstract: With the aim of characterizing the flux and color variations of the multiple components of the gravitationally lensed quasar UM673 as a function of time, we have performed multi-epoch and multi-band photometric observations with the Danish 1.54m telescope at the La Silla Observatory. The observations were carried out in the VRi spectral bands during four seasons (2008--2011). We reduced the data using the PSF (Point Spread Function) photometric technique as well as aperture photometry. Our results show for the brightest lensed component some significant decrease in flux between the first two seasons (+0.09/+0.11/+0.05 mag) and a subsequent increase during the following ones (-0.11/-0.11/-0.10 mag) in the V/R/i spectral bands, respectively. Comparing our results with previous studies, we find smaller color variations between these seasons as compared with previous ones. We also separate the contribution of the lensing galaxy from that of the fainter and close lensed component., Comment: 7 pages, 8 figures, 4 tables
Published: 2013
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