bluuebunny/crossref_metadata_2025 huggingface dataset:
Fibroblast cell line establishment, cryopreservation and interspecies embryos reconstruction in red panda (Ailurus fulgens)
Authors: Tao Yong , Liu Jianming , Zhang Yunhai , Zhang Meiling , Fang Junshun , Han Wei , Zhang Zhizhong , Liu Ya , Ding Jianping , Zhang Xiaorong
Published: February 2009

In evolution, the red panda (Ailurus fulgens) plays a pivotal role in the higher level phylogeny of arctoides carnivore mammals. The red panda inhabits certain Asian countries only and its numbers are decreasing. Therefore, the development of feasible ways to preserve this species is necessary. Genetic resource cryopreservation and somatic cell nuclear transfer (SCNT) have been used extensively to rescue this endangered species. The present study describes the establishment, for the first time, of a red panda ear fibroblast cell line, which was then cryopreserved, thawed and cultured. Through micromanipulation, interspecies embryos were reconstructed using the cryopreserved–thawed fibroblasts of the red panda as the donor and rabbit oocytes as recipients. A total of 194 enucleated rabbit oocytes were reconstructed with red panda ear fibroblasts; enucleated oocytes were activated without fusion as the control. The results show that the fibroblast cell line was established successfully by tissue culture and then cryopreserved in liquid nitrogen. Supplementation with 20% fetal bovine serum and 8% dimethyl sulphoxide in basic medium facilitated the cryopreservation. The interspecies embryos were successfully reconstructed. The cleavage, morulae and blastocyst rates after in vitro culture were 71, 47 and 23% (31/194), respectively. This study indicated that a somatic cell line could be established and cryopreserved from red panda and that rabbit cytoplast supports mitotic cleavage of the red panda karyoplasts and is capable of reprogramming the nucleus to achieve blastocysts.
Social, economic, health and environmental determinants of child nutritional status in three Central Asian Republics
Authors: Bomela Nolunkcwe J
Published: February 2009

Objective

To investigate the comparative effect of social, economic, health and environmental characteristics on the nutritional status of children aged <3 years in Central Asia.

Design

Cross-sectional analysis using data from Demographic and Health Surveys.

Setting

Uzbekistan, Kyrgyzstan and Kazakhstan.

Subjects

Information on demographic health was gathered by Macro International Inc., Uzbekistan, Kyrgyzstan and Kazakhstan governments from a random sample of 14 067 households in the three countries. Anthropometric measurements were performed using standardized procedures on all children <3 years of age (n 2358). Only children with plausible Z-scores (n 1989) were selected for subsequent analyses.

Results

The main results indicated that country of residence, number of people in household, household wealth, birth weight, age of child, knowledge of oral rehydration therapy, maternal education, number of children <5 years of age and source of drinking water were strong predictors of child nutritional status in these countries. Furthermore, chronic malnutrition was most prevalent in all three countries but at varied levels. An unexpected finding was that fully vaccinated children were more likely to be malnourished than children who were partially vaccinated. A further unexpected finding was that breast-feeding especially in children >6 months old had a strong negative association with stunting and underweight.

Conclusions

In summary, the results from both the descriptive and binary logistic regression analysis are similar in terms of the explanatory variables and the statistical significance in the models.
Perceived health and medicinal properties of six species of wild edible plants in north-east Lebanon
Authors: Jeambey Zeinab , Johns Timothy , Talhouk Salma , Batal Malek
Published: February 2009

Objectives

Wild edible plants (WEP) play the dual role of securing food diversity and promoting health in traditional societies. Current simplified dietary habits contribute to increasing population health risks. Since WEP are integral to the diet of traditional communities, identifying their significance as foods to people provides further evidence to conserve them and promote their consumption. Six species of WEP were identified as integral to the diet of rural Lebanese communities. We investigated their patterns of consumption and knowledge regarding their health and medicinal properties.

Design

An ethnobotanical survey, employing a qualitative questionnaire, was conducted among thirty informants. The identified species were Cichorium intybus, Eryngium creticum, Foeniculum vulgare, Malva sylvestris, Thymus syriacus and Gundelia tournifortii.

Results

Most informants consumed the six plants as a regular part of their diet. Seasonal variability in consumption was evident. C. intybus was renowned for its digestive and blood strengthening properties. F. vulgare was used as a digestive stimulant. M. sylvestris was distinguished for its anti-inflammatory qualities. T. syriacus was popular for its digestive and anti-poisonous properties. E. creticum was attributed less pronounced health benefits. G. tournifortii was considered a nutritious food.

Conclusions

All six species were popular for their edible uses as well as their health and/or medicinal benefits. These properties are supported by scientific evidence. Our results highlight the importance of these plants for local people and support efforts for their conservation. However, we noticed a decline in indigenous knowledge. We encourage efforts to record it for other plants and in other communities.
Changes in food and nutrient intake of 6- to 17-year-old Germans between the 1980s and 2006
Authors: Stahl Anna , Vohmann Claudia , Richter Almut , Heseker Helmut , Mensink Gert BM
Published: February 2009

Objective

To compare the food consumption and nutrient intakes of German children and adolescents in the 1980s with present dietary habits.

Design

Two cross-sectional representative surveys, the German National Food Consumption Study (Nationale Verzehrsstudie, NVS) from 1985–8 and the nutrition module ‘EsKiMo’ of the German Health Interview and Examination Survey for Children and Adolescents (KiGGS) from 2006, were analysed for differences in food and nutrient intakes stratified by age and sex groups.

Setting

Secondary analyses of data from representative observational studies.

Subjects

Children and adolescents aged 6–17 years living in Germany in the 1980s (n 2265) and in 2006 (n 2506).

Results

Food consumption was characterised by higher amounts of vegetables/pulses, fruits/nuts and beverages and less meat products/sausages, butter, fats/oils, potatoes/potato products and bread/pastries in 2006 than in 1985–8. The overall changes in food intake were reflected in improvements of macronutrient composition, increased water intake and lower energy density of the diet. Intake of most vitamins and minerals increased in relation to energy intake, but the nutrient density of the diet for vitamins B12 and D decreased. The most critical nutrients observed in NVS and EsKiMo were folate, vitamin D, vitamin A, vitamin E, Ca and Fe. In addition, dietary fibre intake was relatively low and fatty acid and carbohydrate compositions were not favourable.

Conclusions

Further efforts will be necessary to improve dietary habits among children and adolescents.
Do lifestyle interventions affect dietary diversity score in the general population?
Authors: Sarrafzadegan Nizal , Azadbakht Leila , Mohammadifard Noushin , Esmaillzadeh Ahmad , Safavi Morteza , Sajadi Firoozeh , Alikhasi Hasan , Maghroun Maryam , Kelishadi Roya
Published: February 2009

Objective

The dietary diversity score (DDS) is a good indicator of diet quality as well as of diet–disease relationships; therefore, the present study was undertaken to reveal the effect of a lifestyle intervention on this index.

Design

A baseline and three evaluation studies were conducted in two intervention districts (Isfahan and Najaf-Abad) and a reference area (Arak), all located in central Iran. The Isfahan Healthy Hearth Programme (IHHP) targeted the entire population of nearly 2 million in urban and rural areas of the intervention communities. One of the main strategies of the lifestyle intervention phase in the IHHP was healthy nutrition. Usual dietary intake was assessed using a forty-nine-item FFQ. A diversity score for each food group was calculated and the DDS was considered the sum of the diversity scores of the food groups.

Results

There were significant increases in DDS in both intervention areas (P = 0·0001) after controlling for confounding factors. There was a significant interaction between area and evaluation stage with regard to DDS (P = 0·0001). The effect of the intervention on the diversity scores of all food groups was also significant (P = 0·0001 for all) after adjusting for socio-economic status.

Conclusion

The community-based lifestyle intervention in the IHHP was successful in improving DDS which might be related to an increase of diet quality of the population that in turn might decrease the risks of chronic diseases.
The Rise of the Vulcans
Authors: Charbonneau David
Published: February 2009

In this introductory review, I summarize the path from the initial 1995 radial-velocity discovery of hot Jupiters to the current rich panoply of investigations that are afforded when such objects are observed to transit their parent stars. Forty transiting exoplanets are now known, and the time for that population to double has dropped below one year. Only for these objects do we have direct estimates of their masses and radii, and can we (at the current time) undertake direct studies of the chemistries and dynamics of their atmospheres. Informed by the successes of hot Jupiter studies, I outline a path for the spectroscopic study of certain habitable exoplanets that obviates the need for direct imaging.
Ground-Based Photometric Searches for Transiting Planets
Authors: Mazeh Tsevi
Published: February 2009

This paper reviews the basic technical characteristics of the ground-based photometric searches for transiting planets, and discusses a possible observational selection effect. I suggest that additional photometric observations of the already observed fields might discover new transiting planets with periods around 4–6 days. The set of known transiting planets supports the intriguing correlation between the planetary mass and the orbital period suggested already in 2005.
The WASP transit surveys
Authors: Cameron Andrew Collier , Pollacco Don , Hellier Coel , West Richard ,   the WASP Consortium and the SOPHIE & CORALIE Planet-Search Teams
Published: February 2009

The WASP consortium operates two wide-field camera arrays in the northern (La Palma) and southern (Sutherland) hemispheres. Each installation comprises a robotic mount bearing 8 cameras, forming a mosaic with a field of view of 30 degrees in declination by 1 hour in right ascension. Here we describe the system performance, observing strategy, candidate selection procedures and follow-up campaigns, and the yield and physical characteristics of the 16 planets discovered in the course of the survey to date.
The MEarth project: searching for transiting habitable super-Earths around nearby M dwarfs
Authors: Irwin Jonathan , Charbonneau David , Nutzman Philip , Falco Emilio
Published: February 2009

Due to their small radii, M dwarfs are very promising targets to search for transiting super-Earths, with a planet of 2 Earth radii orbiting an M5 dwarf in the habitable zone giving rise to a 0.5% photometric signal, with a period of two weeks. This can be detected from the ground using modest-aperture telescopes by targeting samples of nearby M dwarfs. Such planets would be very amenable to follow-up studies due to the brightness of the parent stars, and the favourable planet-star flux ratio. MEarth is such a transit survey of ~2000 nearby M dwarfs. Since the targets are distributed over the entire (Northern) sky, it is necessary to observe them individually, which will be done by using 8 independent 0.4m robotic telescopes, two of which have been in operation since December 2007 at the Fred Lawrence Whipple Observatory (FLWO) located on Mount Hopkins, Arizona. We discuss the survey design and hardware, and report on the current status of the survey, and preliminary results obtained from the commissioning data.
Transiting Planets in the Galactic Bulge from SWEEPS Survey and Implications
Authors: Sahu Kailash C. , Casertano Stefano , Valenti Jeff , Bond Howard E. , Brown Thomas M. , Smith T. Ed , Clarkson Will , Minniti Dante , Zoccali Manuela , Livio Mario , Renzini Alvio , Rich R. M. , Panagia Nino , Lubow Stephen , Brown Timothy , Piskunov Nikolai
Published: February 2009

The SWEEPS (Sagittarius Window Eclipsing Extrasolar Planet Search) program was aimed at detecting planets around stars in the Galactic bulge, not only to determine their physical properties, but also to determine whether the properties of planets found in the solar neighborhood, such as their frequency and the metallicity dependence, also hold for the planets in the Galactic bulge. We used the Hubble Space Telescope to monitor 180,000 F, G, K, and M dwarfs in the Galactic bulge continuously for 7 days in order to look for transiting planets. We discovered 16 candidate transiting extrasolar planets with periods of 0.6 to 4.2 days, including a possible new class of ultra-short period planets (USPPs) with P < 1 day. The facts that (i) the coverage in the monitoring program is continuous, (ii) most of the stars are at a known distance (in the Galctic bulge), (iii) monitoring was carried out in 2 passbands, and (iv) the images have high spatial resolution, were crucial in minimizing and estimating the false positive rates. We estimate that at least 45% of the candidates are genuine planets. Radial velocity observations of the two brightest host stars further support the planetary nature of the transiting companions. These results suggest that the planet frequency in the Galactic bulge is similar to that in the solar neighborhood. They also suggest that higher metallicity favors planet formation even in the Galactic bulge. The USPPs occur only around low-mass stars which may suggest that close-in planets around higher-mass stars are irradiately evaporated, or that planets are able to migrate to and survive in close-in orbits only around such old and low-mass stars.
CoRoT: Description of the Mission and Early Results
Authors: Baglin Annie , Auvergne Michel , Barge Pierre , Deleuil Magali , Michel Eric ,   The CoRoT Exoplanet Science Team
Published: February 2009

The CoRoT Mission and its performances in flight are summarised. After more than 500 days in orbit, the early results in the exoplanet finding programme are highlighted. The first 5 planets discovered are compared to the previous population of exoplanets.
The first planets discovered from space with the CoRoT mission
Authors: Barge Pierre ,   the CoRoT Exoplanet Science Team
Published: February 2009

The pioneer space mission for photometric planet searches CoRoT continuously monitors about 12,000 stars in each of its fields of view. Thanks to the so-called “alarm mode”, transit candidates can be detected early in the processing of the data and before the end of a run of observation. This specificity offers the possibility of rapidly triggering follow-up operations for the confirmation and characterization of the best transit candidates. We present the first objects discovered in this way: four planets and a transition object between brown dwarf and planet. We describe the organization of the CoRoT Exoplanet Science Team and briefly comment on the set of periodic signals identified by the various detection groups in the first three runs of observation.
Measuring accurate transit parameters
Authors: Winn Joshua N.
Published: February 2009

By observing the transits of exoplanets, one may determine many fundamental system parameters. I review current techniques and results for the parameters that can be measured with the greatest precision, specifically, the transit times, the planetary mass and radius, and the projected spin-orbit angle.
Characterizing the Eccentricities of Transiting Extrasolar Planets with Kepler and CoRoT
Authors: Ford Eric B. , Colón Knicole D.
Published: February 2009

Radial velocity planet searches have revealed that many giant planets have large eccentricities, in striking contrast with the giant planets in the solar system and prior theories of planet formation. The realization that many giant planets have large eccentricities raises a fundamental question: Do terrestrial-size planets of other stars typically have significantly eccentric orbits or nearly circular orbits like the Earth? While space-based missions such as CoRoT and Kepler will be capable of detecting nearly Earth-sized planets, it will be extremely challenging to measure their eccentricities using radial velocity observations. We review several ways that photometric measurements of transit light curves can constrain the eccentricity of transiting planets. In particular, photometric observations of transit durations can be used to characterize the distribution of orbital eccentricities for various populations of transiting planets (e.g., nearly Earth-sized planets in the habitable zone) without relying on radial velocity measurements. Applying this technique to rocky planets to be found by CoRoT and Kepler will enable constraints on theories for the excitation of eccentricities and tidal dissipation. We also remind observers that several short-period transiting planets are known to have significant eccentricities and caution that assuming they are on a circular orbit can reduce the probability of detecting transits, impact planning for follow-up observations, and adversely affect measurements of the physical parameters of the star and planet.
Radial velocity follow-up for confirmation and characterization of transiting exoplanets
Authors: Bouchy François , Moutou Claire , Queloz Didier ,   the CoRoT Exoplanet Science Team
Published: February 2009

Radial Velocity follow-up is essential to establish or exclude the planetary nature of a transiting companion as well as to accurately determine its mass. Here we present some elements of an efficient Doppler follow-up strategy, based on high-resolution spectroscopy, devoted to the characterization of transiting candidates. Some aspects and results of the radial velocity follow-up of the CoRoT space mission are presented in order to illustrate the strategy used to deal with the zoo of transiting candidates.
Precision radial velocities of double-lined binary stars and the spectroscopic follow-up of circumbinary transiting planet candidates
Authors: Konacki Maciej
Published: February 2009

We present a new iodine cell based approach that allows one to obtain radial velocities of the components of double-lined spectroscopic binary stars (SB2s) with a precision reaching 5 m/s. Such an RV precision is up to 100 times better than what is currently available in the literature for the SB2s. We discuss the applications of our method to the radial velocity searches for circumbinary planets and spectroscopic follow-up of transiting planet candidates around eclipsing binary stars.
The case for a close-in perturber to GJ 436 b
Authors: Ribas Ignasi , Font-Ribera Andreu , Beaulieu Jean-Philippe , Morales Juan Carlos , García-Melendo Enrique
Published: February 2009

The increasing number of transiting planets raises the possibility of finding changes in their transit time, duration and depth that could be indicative of further planets in the system. Experience from eclipsing binaries indeed shows that such changes may be expected. A first obvious candidate to look for a perturbing planet is GJ 436, which hosts a hot transiting Neptune-mass planet in an eccentric orbit. Ribas et al. (2008) suggested that such eccentricity and a possible change in the orbital inclination might be due to a perturbing small planet in a close-in orbit. A radial velocity signal of a 5 M⊕ planet close to the 2:1 mean-motion resonance seemed to provide the perfect candidate. Recent new radial velocities have deemed such signal spurious. Here we put all the available information in context and we evaluate the possibility of a small perturber to GJ 436 b to explain its eccentricity and possible inclination change. In particular, we discuss the constraints provided by the transit time variation data. We conclude that, given the current data, the close-in perturber scenario still offers a plausible explanation to the observed orbital and physical properties of GJ 436 b.
Precision Radial Velocities in the Near Infrared with TEDI
Authors: Lloyd James P. , Czeszumska Agnieszka , Edelstein Jerry , Erskine David , Feuerstein Michael , Halverson Sam , Marckwordt Mario , Mercer Tony , Muirhead Philip , Schwehr Jackie , Muterspaugh Matthew , Wishnow Ed , Wright Jason
Published: February 2009

The TEDI (TripleSpec - Exoplanet Discovery Instrument) is a dedicated instrument for the near-infrared radial velocity search for planetary companions to low-mass stars with the goal of achieving meters-per-second radial velocity precision. Heretofore, such planet searches have been limited almost entirely to the optical band and to stars that are bright in this band. Consequently, knowledge about planetary companions to the populous but visibly faint low-mass stars is limited. In addition to the opportunity afforded by precision radial velocity searches directly for planets around low mass stars, transits around the smallest M dwarfs offer a chance to detect the smallest possible planets in the habitable zones of the parent stars. As has been the the case with followup of planet candidates detected by the transit method requiring radial velocity confirmation, the capability to undertake efficient precision radial velocity measurements of mid-late M dwarfs will be required. TEDI has been commissioned on the Palomar 200” telescope in December 2007, and is currently in a science verification phase.
Probing the Interiors of Very Hot Jupiters Using Transit Light Curves
Authors: Wolf Aaron S. , Ragozzine Darin
Published: February 2009

Accurately understanding the interior structure of extra-solar planets is critical for inferring their formation and evolution and resolving the origin of anomalous planetary radii. The internal density distribution of the planet has a direct effect on the star-planet orbit through the gravitational quadrupole of rotational and tidal bulges, measured by the planetary Love number (k2p, twice the apsidal motion constant). We find that the quadrupole of the planetary tidal bulges dominates the rate of apsidal precession of single very hot Jupiters by more than an order of magnitude over general relativity and the stellar quadrupole. For the shortest-period planets, the planetary interior induces precession of a few degrees per year. By investigating the full photometric signal of apsidal precession, we find that transit timing induces a relatively small signal compared to the changes in transit shapes. With its long baseline of ultra-precise photometry, the future space-basedKeplermission should be able to realistically detect the presence or absence of a core in very hot Jupiters with orbital eccentricities as low ase~ 0.001. We show that the signal due tok2pis not degenerate with other parameters and has a unique signature on the transit light curve. This technique, outlined in more detail in Ragozzine & Wolf 2008 provides the first readily employed method for directly probing the interiors of extra-solar planets.
Induced Kozai Migration and Formation of Close-in Planets in Binaries
Authors: Takeda Genya , Kita Ryosuke , Rasio Frederic A.
Published: February 2009

Many recent observational studies have concluded that planetary systems commonly exist in multiple-star systems. At least ~20%, and presumably a larger fraction, of the known extrasolar planetary systems are associated with one or more stellar companions. These stellar companions normally exist at large distances from the planetary systems (typical projected binary separations are 102–104AU) and are often faint (ranging from F to T spectral types). Yet, secular cyclic angular momentum exchange with these distant stellar companions can significantly alter the orbital configuration of the planets around the primaries. One of the most interesting and fairly common outcomes seen in numerical simulations is the opening of a large mutual inclination angle between the planetary orbits, forced by differential nodal precessions caused by the binary companion. The growth of the mutual inclination angle between planetary orbits induces additional large-amplitude eccentricity oscillations of the inner planet due to the quadrupole gravitational perturbation by the outer planet. This eccentricity oscillation may eventually result in the orbital decay of the inner planet through tidal friction, as previously proposed as Kozai migration or Kozai cycles with tidal friction (KCTF). This orbital decay mechanism induced by the binary perturbation and subsequent tidal dissipation may stand as an alternative formation channel for close-in extrasolar planets.
On the Origins of Eccentric Close-in Planets
Authors: Matsumura Soko , Takeda Genya , Rasio Fred A.
Published: February 2009

Strong tidal interaction with the central star can circularize the orbits of close-in planets. With the standard tidal quality factorQof our solar system, estimated circularization timescales for close-in extrasolar planets are typically shorter than the age of the host stars. While most extrasolar planets with orbital radiia≲ 0.1 AU indeed have circular orbits, some close-in planets with substantial orbital eccentricities have recently been discovered. This new class of eccentric close-in planets implies that either their tidalQfactor is considerably higher, or circularization is prevented by an external perturbation. Here we constrain the tidalQfactor for transiting extrasolar planets by comparing their circularization times with accurately determined stellar ages. Using estimated secular perturbation timescales, we also provide constraints on the properties of hypothetical second planets exterior to the known eccentric close-in planets.
Emergent Exoplanet Flux: Review of the Spitzer Results
Authors: Deming Drake
Published: February 2009

Observations using theSpitzer Space Telescopeprovided the first detections of photons from extrasolar planets.Spitzerobservations are allowing us to infer the temperature structure, composition, and dynamics of exoplanet atmospheres. The Spitzer studies extend from many hot Jupiters to the hot Neptune orbiting GJ436. Here I review the current status ofSpitzersecondary eclipse observations, and summarize the results from the viewpoint of what is robust, what needs more work, and what the observations are telling us about the physical nature of exoplanet atmospheres.
Two Classes of Hot Jupiter Atmospheres
Authors: Fortney Jonathan J.
Published: February 2009

We highlight the potential importance of gaseous TiO and VO opacity on the highly irradiated close-in giant planets. The day-side atmospheres of these planets may naturally fall into two classes that are somewhat analogous to the M- and L-type dwarfs. Those that are warm enough to have appreciable opacity due to TiO and VO gases we term the “pM Class” planets, and those that are cooler, such that Ti and V are predominantly in solid condensates, we term “pL Class” planets. The optical spectra of pL Class planets are dominated by neutral atomic Na and K absorption. We discuss a connection between temperature inversions and large day/night temperature contrasts for the pM Class planets. Around a Sun-like primary, for solar composition, this boundary likely occurs at ~0.04-0.05 AU, but we discuss important uncertainties. The difference in the observed day/night contrast between υ And b (pM Class) and HD 189733b (pL Class) is naturally explained in this scenario.
Characterizing the Atmospheres of Hot Jupiters: From Spectra to Multi-Color Maps
Authors: Knutson Heather A.
Published: February 2009

We present new observations of the emission spectrum of the hot Jupiter TrES-4 designed to test the theory that the presence of temperature inversions in the atmospheres of these planets are correlated with the amount of radiation received by the planet. Our observations reveal that TrES-4 has an emission spectrum similar to that of HD 209458b, which requires the presence of an inversion layer high in the atmosphere and water emission bands in order to explain the observed features, providing additional support for that theory. We also present new observations of the thermal phase curve of HD 189733b at 24 μm, which we combine with our previous observations at 8 μm to examine how circulation in this planet's atmosphere varies as a function of depth. We discuss the relationship between the strength of the day-night circulation on both planets and their other observable properties, in particular their emission spectra.
Thermosphere and exosphere of hot Jupiters
Authors: des Etangs Alain Lecavelier
Published: February 2009

Here we describe the observations and the resulting constraints on the upper atmosphere (thermosphere and exosphere) of hot Jupiters. In particular, observations and theoretical modeling of hot-Jupiter evaporation are described. The observations allowed the discovery that the planet orbiting HD209458 has an extended atmosphere of escaping hydrogen and showed the presence of oxygen and carbon at very high altitude. These observations give unique constraints on the escape rate and mechanism in the atmosphere of these planets. The most recent Lyman-alpha HST observations of HD189733b allow for the first time to compare the evaporation from two different planets in different environments. We present models to quantify the escape rate from the measured occultation depths, and an energy diagram to describe the evaporation state of hot Jupiters. Using this diagram, it is shown that few already known planets could be remnants of former giant planets.
Future Observations of Transits and Light Curves from Space
Authors: Beichman Charles A. , Greene Tom , Krist John
Published: February 2009

A variety of new observational opportunities have made transit and more generally light curve analysis central to the study of exoplanets. Talks at this IAU 253 Symposium have dramatically highlighted the measurement of the radius, density, atmospheric composition and atmospheric thermal structure, presently for relatively large, hot planets, but soon for smaller planets orbiting further from their host stars. On-going and future space observations will play a key role in the detection and characterization of these planetary systems. After a brief review, I focus on two topics: the need for a sensitive all-sky survey for planets transiting the brightest, closest stars and the follow-up opportunities afforded by the James Webb Space Telescope (JWST).
SuperLupus: A Deep, Long Duration Transit Survey
Authors: Bayliss Daniel D. R. , Sackett Penny D. , Weldrake David T. F.
Published: February 2009

SuperLupus is a deep transit survey monitoring a Galactic Plane field in the Southern hemisphere. The project is building on the successful Lupus Survey, and will double the number of images of the field from 1700 to 3400, making it one of the longest duration deep transit surveys. The immediate motivation for this expansion is to search for longer period transiting planets (5-8 days) and smaller radii planets. It will also provide near complete recovery for the shorter period planets (1-3 days). In March, April, and May 2008 we obtained the new images and work is currently in progress reducing these new data.
ASTEP South: An Antarctic Search for Transiting Planets around the celestial South pole
Authors: Crouzet N. , Agabi K. , Blazit A. , Bonhomme S. , Fanteï-Caujolle Y. , Fressin F. , Guillot T. , Schmider F.-X. , Valbousquet F. , Bondoux E. , Challita Z. , Abe L. , Daban J.-B. , Gouvret C. ,   the ASTEP team
Published: February 2009

ASTEP South is the first phase of the ASTEP project that aims to determine the quality of Dome C as a site for future photometric searches for transiting exoplanets and discover extrasolar planets from the Concordia base in Antarctica. ASTEP South consists of a front-illuminated 4k × 4k CCD camera, a 10 cm refractor, and a simple mount in a thermalized enclosure. A double-glass window is used to reduce temperature variations and the associated turbulence on the optical path. The telescope is fixed and observes a 4° × 4° field of view centered on the celestial South pole. With this design, A STEP South is very stable and observes with low and constant airmass, both being important issues for photometric precision. We present the project, we show that enough stars are present in our field of view to allow the detection of one to a few transiting giant planets, and that the photometric precision of the instrument should be a few mmag for stars brighter than magnitude 12 and better than 10 mmag for stars of magnitude 14 or less.
A search for transiting planets in the Galactic Plane
Authors: Miller Veronica R. , Albrow Michael D.
Published: February 2009

We are carrying out a deep survey for transiting extrasolar planets in a 1 square degree field in the Galactic Plane. The images to date were taken using the Wide Field Imager on the ESO 2.2m telescope at La Silla. We present details of the analysis and initial results from the survey.
Searching for Planetary Companions to Ultracool Dwarfs: Planet Hunting in the Near Infrared
Authors: Blake Cullen H. , Charbonneau David , Latham David W.
Published: February 2009

Owing to their small masses and radii, Ultracool Dwarfs (UCDs; late-M, L, and T dwarfs) may be excellent targets for planet searches and may afford astronomers the opportunity to detect terrestrial planets in the habitable zone. The precise measurements necessary to detect extrasolar planets orbiting UCDs represent a major challenge. We describe two efforts to obtain precise measurements of UCDs in the Near Infrared (NIR). The first involves the robotic NIR observatory PAIRITEL and efforts to obtain photometric precision sufficient for the detection of terrestrial planets transiting UCDs. The second effort involves precise radial velocity measurements of UCDs in the NIR and a survey undertaken with the NIRSPEC spectrograph on Keck.
KELT: A Wide-Field Survey of Bright Stars for Transiting Planets
Authors: Siverd Robert J. , Pepper Joshua , Stanek Kris , Pogge Richard W. , Gaudi B. Scott , DePoy Darren L.
Published: February 2009

The Kilodegree Extremely Little Telescope (KELT) is a wide-field (26° × 26°) robotic survey telescope currently operating in Sonoita, Arizona. Assembled from commercial and off-the-shelf devices, KELT currently surveys ~40% of the Northern sky with sufficient precision to detect transiting planets around bright (8 < V < 12) stars. In the past several years of operation, over 30,000 science images have been acquired. Planet candidate selection and follow-up are currently underway. A brief overview of past and present survey operations, the data reduction pipeline, and initial results follows below.
Comparing the performance of stellar variability filters for the detection of planetary transits
Authors: Bonomo A. S. , Lanza A. F.
Published: February 2009

We have developed a new method to improve the transit detection of Earth-sized planets in front of solar-like stars by fitting stellar microvariability by means of a spot model. A large Monte Carlo numerical experiment has been designed to test the performance of our approach in comparison with other variability filters and fitting techniques for stars of different magnitudes and planets of different radius and orbital period, as observed by the space missions CoRoT and Kepler. Here we report on the results of this experiment.
Transits in Poorly Sampled Data – Gaia and Beyond
Authors: Tingley Brandon
Published: February 2009

Gaia, an ESA cornerstone mission, will obtain of the order of 100 high-precision photometric observations over five years for tens of millions of stars with V < 17. The vast number of red dwarfs in this data set, with their correspondingly deep (high S/N) transits, makes it worthwhile to explore the possibility of detecting transits in such data. Searching for transits under these circumstances requires a very different approach from that used for a normal, highly-sampled transit survey if the search is to be performed in a reasonable amount of time. It should be possible to identify a portion of the transiting Hot Jupiter/M dwarf systems in the data set, if the photometry is as stable and precise as specified by design. This same approach could be applied to ground-based transit searches – a transit survey targeted at red dwarfs with Jupiter-sized companions.
How to use the Phoebe code to solve transiting exoplanet light curve
Authors: Poddaný Stanislav
Published: February 2009

A brief demonstration of photometric light curves solutions for eight transiting exoplanets using the Phoebe 0.29c code is presented. We determined radii and inclinations for TrES-1b, TrES-2b, Wasp-1b, XO-1b, XO-2b, OGLE-TR-10b, OGLE-TR-111b and HD 189733b. All our results are in good agreement with the last results published.
Towards a fully automated eclipsing binary solver for Gaia
Authors: Tingley Brandon , Sadowski Gilles , Siopis Christos
Published: February 2009

Gaia, an ESA cornerstone mission, will obtain of the order of 100 high-precision photometric observations and lower precision radial velocity measurements over five years for around a billion stars – several hundred thousand of which will be eclipsing binaries. In order to extract the characteristics of these systems, a fully automated code must be available. During the process of this development, two tools that may be of use to the transit community have emerged: a very fast, simple, detached eclipsing binary simulator/solver based on a new approach and an interacting eclipsing binary simulator with most of the features of the Wilson-Devinney and Nightfall codes, but fully documented and written in easy-to-follow and highly portable Java. Currently undergoing development and testing, this code includes an intuitive graphical interface and an optimizer for the estimation of the physical parameters of the system.
From stars to planets
Authors: Gazzano Jean-Christophe , Deleuil Magali , De Laverny Patrick , Blanco Alejandra Recio , Bouchy François , Gandolfi Davide , Loeillet Benoît
Published: February 2009

A large program of multi-fibre (FLAMES) spectroscopic observations of the stellar population in two CoRoT/Exoplanet field with the GIRAFFE/VLT, took place in spring 2008. It aims at characterizing the brightest dwarf population and providing the ground for statistical analysis of the planetary population found by CoRoT.

To perform such an ambitious analysis, we use an automated software based on the MATISSE algorithm, originally designed for the GAIA/RVS spectral analysis. This software derives the atmospheric stellar parameters: effective temperature, surface gravity and the overall metallicity.

Further improvements are foreseen in order to measure also individual abundances. By comparing the main physical and chemical properties of the host stars to those of the stellar population they belong to, this will bring new insights into the formation and evolution of exoplanetary systems and the star-planet connection.
Photometric Follow-up of the CoRoT Mission
Authors:   The CoRoT Photometric Follow-Up Team
Published: February 2009

A short overview of the motivation and techniques of the ground-based photometric follow-up program of the CoRoT mission is given.
DEMONEX: The DEdicated MONitor of EXotransits
Authors: Eastman J. D. , Gaudi B. S. , DePoy D. L.
Published: February 2009

DEMONEX is a low-cost, 0.5 meter, robotic telescope assembled mostly from commercially available parts dedicated to obtaining precise photometry of bright stars with transiting planets. This photometry will provide a homogeneous data set for all transits visible from its location at Winer Observatory in Sonoita, Arizona. We will also search for additional planets via transit timing variations, measure or place limits on the albedos from secondary eclipses, systematically search known radial velocity planets for those that transit, and follow up promising KELT candidates. Despite its modest size, the signal-to-noise ratio per transit is comparable to that obtained with larger, 1m-class telescopes because of its short readout time and high z-band quantum efficiency. However, its main strength is that it will be used every night for transit follow-up and gather an unprecedented data set on transiting planets. With the 24 known transiting planets and 112 radial velocity planets visible from Winer Observatory, over 90% of all nights have at least one full event to observe.
GJ 436c? The contribution of transit timings
Authors: Demory B.-O. , Gillon M. , Waelkens C. , Queloz D. , Udry S.
Published: February 2009

From recent high-accuracy transit timings measurements, we discard the 5 M⊕ planet recently proposed by Ribas et al. (2008). Thanks to a combined radial-velocity and transit timings overview we also define a mass/period domain in which a secondary planet may be found in the system. We also show that timings obtained until now, although not sufficient to remove degeneracies on mass and period, can still restrict the parameter space of the potential secondary planet.
Transit timing variability in TrES-1
Authors: Rabus M. , Alonso R. , Deeg H. J. , Belmonte J. A. , Almenara J. M. , Gilliland R. L. , Brown T. M.
Published: February 2009

We observed several transits of the exoplanet TrES-1 distributed over four years from 2004 to 2007. On the basis of these observations and additional published data, we present a mid-transit time analysis. The aim is to find indications of the presence of a third body by analysing the difference between the calculated and observed transit times.
Searching for transit timing variations in transiting exoplanet systems
Authors: Hrudková Marie , Skillen Ian , Benn Chris , Pollacco Don , Gibson Neale , Joshi Yogesh , Harmanec Petr , Tulloch Simon
Published: February 2009

Searching for transit timing variations in the known transiting exoplanet systems can reveal the presence of other bodies in the system. Here we report such searches for two transiting exoplanet systems, TrES-1 and WASP-2. Their new transits were observed with the 4.2m William Herschel Telescope located on La Palma, Spain. In a continuing programme, three consecutive transits were observed for TrES-1, and one for WASP-2 during September 2007. We used the Markov Chain Monte Carlo simulations to derive transit times and their uncertainties. The resulting transit times are consistent with the most recent ephemerides and no conclusive proof of additional bodies in either system was found.
Period variations in extrasolar transiting planet OGLE-TR-111b
Authors: Díaz Rodrigo F. , Rojo Patricio , Melita Mario , Hoyer Sergio , Minniti Dante , Mauas Pablo J. D. , Ruíz María Teresa
Published: February 2009

Two consecutive transits of planetary companion OGLE-TR-111b were observed in the I band. Combining these observations with data from the literature, we find that the timing of the transits cannot be explained by a constant period, and that the observed variations cannot be originated by the presence of a satellite. However, a perturbing planet with the mass of the Earth in an exterior orbit could explain the observations if the orbit of OGLE-TR-111b is eccentric. We also show that the eccentricity needed to explain the observations is not ruled out by the radial velocity data found in the literature.
Stellar activity of planetary host star HD 189733
Authors: Boisse I. , Moutou C. , Vidal-Madjar A. , Bouchy F. , Pont F. , Hébrard G. , Bonfils X. , Delfosse X. , Desort M. , Forveille T. , Lagrange A.-M. , Loeillet B. , Lovis C. , Mayor M. , Pepe F. , Perrier C. , Queloz D. , Santos N. , Ségransan D. , Udry S.
Published: February 2009

Exoplanet search programs need to study how to disentangle radial-velocity (RV) variations due to Doppler motion and the noise induced by stellar activity. We monitored the active K2V HD 189733 with the high-resolution SOPHIE spectrograph (OHP, France). We refined the orbital parameters of HD 189733b and put limitations on the eccentricity and on a long-term velocity gradient. We subtracted the orbital motion of the planet and compared the variability of activity spectroscopic indices (HeI, Hα, Ca II H&K lines) to the evolution of the RV residuals and the shape of spectral lines. All are in agreement with an active stellar surface in rotation. We used such correlations to correct for the RV jitter due to stellar activity. This results in achieving a high precision on the orbital parameters, with a semi-amplitude: K=200.56±0.88m⋅s−1 and a derived planet mass of MP=1.13±0.03 MJup.
A Precise Estimate of the Radius of HD 149026b
Authors: Nutzman Philip , Charbonneau David , Winn Joshua N. , Knutson Heather A. , Fortney Jonathan J. , Holman Matthew J. , Agol Eric
Published: February 2009

We present Spitzer 8 μm transit observations of the extrasolar planet system HD 149026b. At this wavelength, transit light curves are weakly affected by stellar limb-darkening, allowing for a simpler and more accurate determination of planetary parameters. We measure a planet-star radius ratio of Rp/R∗=0.05158±0.00077, and in combination with ground-based data and independent constraints on the stellar mass and radius, we derive an orbital inclination of i = 85°.4+0°.9−0°.8 and a planet radius of 0.755 ± 0.040 RJ. These measurements further support models in which the planet is greatly enriched in heavy elements.
The NStED Stellar and Exoplanet Hosting Star Service
Authors: Ramirez S. , Ali B. , Baker R. , Berriman G. B. , von Braun K. , Chiu N-M. , Ciardi D. R. , Good J. , Kane S. R. , Laity A. C. , McElroy D. L. , Monkewitz S. , Payne A. N. , Schmitz M. , Stauffer J. R. , Wyatt P. L. , Zhang A.
Published: February 2009

The NASA Star and Exoplanet Database (NStED) is a general purpose stellar archive with the aim of providing support for NASA's planet finding and characterization goals, stellar astrophysics, and the planning of NASA and other space missions. There are two principal components of NStED: a database of (currently) 140,000 nearby stars and exoplanet-hosting stars, and an archive dedicated to high precision photometric surveys for transiting exoplanets. We present a summary of the NStED stellar database, functionality, tools, and user interface. NStED currently serves the following kinds of data for 140,000 stars (where available): coordinates, multiplicity, proper motion, parallax, spectral type, multiband photometry, radial velocity, metallicity, chromospheric and coronal activity index, and rotation velocity/period. Furthermore, the following derived quantities are given wherever possible: distance, effective temperature, mass, radius, luminosity, space motions, and physical/angular dimensions of habitable zone. Queries to NStED can be made using constraints on any combination of the above parameters. In addition, NStED provides tools to derive specific inferred quantities for the stars in the database, cross-referenced with available extra-solar planetary data for those host stars. NStED can be accessed at http://nsted.ipac.caltech.edu.