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The detection of exoplanets using any method is prone to confusion due to the intrinsic variability of the host star. We investigate the effect of cool starspots on the detectability of the exoplanets around solar-like stars using the radial velocity method. For investigating this activity-caused "jitter" we calculate synthetic spectra using radiative transfer, known stellar atomic and molecular lines, different surface spot configurations, and an added planetary signal. Here, the methods are described in detail, tested and compared to previously published studies. The methods are also applied to investigate the activity jitter in old and young solar-like stars, and over a solar-like activity cycles. We find that the mean full jitter amplitude obtained from the spot surfaces mimicking the solar activity varies during the cycle approximately between 1 m/s and 9 m/s. With a realistic observing frequency a Neptune mass planet on a one year orbit can be reliably recovered. On the other hand, the recovery of an Earth mass planet on a similar orbit is not feasible with high significance. The methods developed in this study have a great potential for doing statistical studies of planet detectability, and also for investigating the effect of stellar activity on recovered planetary parameters., Comment: Accepted to MNRAS

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

Accurate measurements of the physical characteristics of a large number of exoplanets are useful to strongly constrain theoretical models of planet formation and evolution, which lead to the large variety of exoplanets and planetary-system configurations that have been observed. We present a study of the planetary systems WASP-45 and WASP-46, both composed of a main-sequence star and a close-in hot Jupiter, based on 29 new high-quality light curves of transits events. In particular, one transit of WASP-45 b and four of WASP-46 b were simultaneously observed in four optical filters, while one transit of WASP-46 b was observed with the NTT obtaining precision of 0.30 mmag with a cadence of roughly three minutes. We also obtained five new spectra of WASP-45 with the FEROS spectrograph. We improved by a factor of four the measurement of the radius of the planet WASP-45 b, and found that WASP-46 b is slightly less massive and smaller than previously reported. Both planets now have a more accurate measurement of the density (0.959 +\- 0.077 \rho Jup instead of 0.64 +\- 0.30 \rho Jup for WASP-45 b, and 1.103 +\- 0.052 \rho Jup instead of 0.94 +\- 0.11 \rho Jup for WASP-46 b). We tentatively detected radius variations with wavelength for both planets, in particular in the case of WASP-45 b we found a slightly larger absorption in the redder bands than in the bluer ones. No hints for the presence of an additional planetary companion in the two systems were found either from the photometric or radial velocity measurements., Comment: 14 pages, 10 figures. Accepted for publication in MNRAS

We report the discovery of a planet --- OGLE-2014-BLG-0676Lb --- via gravitational microlensing. Observations for the lensing event were made by the MOA, OGLE, Wise, RoboNET/LCOGT, MiNDSTEp and $\mu$FUN groups. All analyses of the light curve data favour a lens system comprising a planetary mass orbiting a host star. The most favoured binary lens model has a mass ratio between the two lens masses of $(4.78 \pm 0.13)\times 10^{-3}$. Subject to some important assumptions, a Bayesian probability density analysis suggests the lens system comprises a $3.09_{-1.12}^{+1.02}$ M_jup planet orbiting a $0.62_{-0.22}^{+0.20}$ M_sun host star at a deprojected orbital separation of $4.40_{-1.46}^{+2.16}$ AU. The distance to the lens system is $2.22_{-0.83}^{+0.96}$ kpc. Planet OGLE-2014-BLG-0676Lb provides additional data to the growing number of cool planets discovered using gravitational microlensing against which planetary formation theories may be tested. Most of the light in the baseline of this event is expected to come from the lens and thus high-resolution imaging observations could confirm our planetary model interpretation., Comment: 10 pages, 5 figures, MNRAS accepted

Stellar magnetic activity manifests itself in a variety of ways including starspots–cool, dark regions on the stellar surface. Starspots can cause variations (‘jitter’) in spectral line-profiles which can mimic the radial velocity (RV) variations caused by an orbiting planet, or create RV noise that can drown out a planetary signature. Cool, low-mass M dwarf stars can be highly active, which can make detection of potentially habitable planets around these stars difficult. We investigate radial velocity variations caused by different activity (spot) patterns on M dwarf stars in order to determine the limits of detectability for small planets orbiting active M dwarfs. We report on our progress toward the aim of answering the following questions: What types of spot patterns are realistic for M dwarf stars? What effect will spots have on M dwarf RV measurements? Can jitter from M dwarf spots mimic planetary signals? What is the ideal observing wavelength to reduce M dwarf jitter?

The ubiquity of M dwarf stars combined with their low masses and luminosities make them prime targets in the search for nearby, habitable exoplanets. We investigate the effects of starspot-induced radial velocity (RV) jitter on detection and characterization of planets orbiting M dwarfs. We create surface spot configurations with both random spot coverage and active regions. Synthetic stellar spectra are calculated from a given spot map, and RV measurements are obtained using cross-correlation technique. We add the RV signal of an orbiting planet to these jitter measurements, and reduce the data to "measure" the planetary parameters. We investigate the detectability of planets around M dwarfs of different activity levels, and the recovery of input planetary parameters. When studying the recovery of the planetary period we note that while our original orbital radius places the planet inside the HZ of its star, even at a filling factor of 2% a few of our measurements fall outside the "conservative Habitable Zone". Higher spot filling factors result in more and higher deviations. Our investigations suggest that caution should be used when characterizing planets discovered with the RV method around stars that are (or are potentially) active., Comment: 20 pages (2 columns), 19 figures, accepted for publication in MNRAS

We present 13 high-precision and four additional light curves of four bright southern-hemisphere transiting planetary systems: WASP-22, WASP-41, WASP-42 and WASP-55. In the cases of WASP-42 and WASP-55, these are the first follow-up observations since their discovery papers. We present refined measurements of the physical properties and orbital ephemerides of all four systems. No indications of transit timing variations were seen. All four planets have radii inflated above those expected from theoretical models of gas-giant planets; WASP-55b is the most discrepant with a mass of 0.63 Mjup and a radius of 1.34 Rjup. WASP-41 shows brightness anomalies during transit due to the planet occulting spots on the stellar surface. Two anomalies observed 3.1 d apart are very likely due to the same spot. We measure its change in position and determine a rotation period for the host star of 18.6 +/- 1.5 d, in good agreement with a published measurement from spot-induced brightness modulation, and a sky-projected orbital obliquity of lambda = 6 +/- 11 degrees. We conclude with a compilation of obliquity measurements from spot-tracking analyses and a discussion of this technique in the study of the orbital configurations of hot Jupiters., Comment: 13 pages, 8 tables, 11 figures. Version 2 is the final accepted version of the paper

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

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We report CCD $V$ and $I$ time-series photometry of the globular cluster NGC 6333 (M9). The technique of difference image analysis has been used, which enables photometric precision better than 0.05 mag for stars brighter than $V \sim 19.0$ mag, even in the crowded central regions of the cluster. The high photometric precision has resulted in the discovery of two new RRc stars, three eclipsing binaries, seven long-term variables and one field RRab star behind the cluster. A detailed identification chart and equatorial coordinates are given for all the variable stars in the field of our images of the cluster. Our data together with literature $V$-data obtained in 1994 and 1995 allowed us to refine considerably the periods for all RR Lyrae stars. The nature of the new variables is discussed. We argue that variable V12 is a cluster member and an Anomalous Cepheid. Secular period variations, double mode pulsations and/or the Blazhko-like modulations in some RRc variables are addressed. Through the light curve Fourier decomposition of 12 RR Lyrae stars we have calculated a mean metallicity of [Fe/H]$_{\rm ZW}$=$-1.70 \pm 0.01{\rm(statistical)} \pm 0.14{\rm(systematic)}$ or [Fe/H]$_{UVES}=-1.67 \pm 0.01{\rm(statistical)} \pm 0.19{\rm(systematic)}$.Absolute magnitudes, radii and masses are also estimated for the RR Lyrae stars. A detailed search for SX Phe stars in the Blue Straggler region was conducted but none were discovered. If SX Phe exist in the cluster then their amplitudes must be smaller than the detection limit of our photometry. The CMD has been corrected for heavy differential reddening using the detailed extinction map of the cluster of Alonso-Garc\'ia et al. (2012). This has allowed us to set the mean cluster distance from two independent estimates; from the RRab and RRc absolute magnitudes, we find $8.04\pm 0.19$ kpc and $7.88\pm0.30$ kpc respectively., Comment: 20 pages, 17 figures, 5 tables, 1 electronic table

Two previously unknown variable stars in the crowded central region of the globular cluster NGC 6981 are presented. The observations were made using the Electron Multiplying CCD (EMCCD) camera at the Danish 1.54m Telescope at La Silla, Chile.The two variables were not previously detected by conventional CCD imaging because of their proximity to a bright star. This discovery demonstrates that EMCCDs are a powerful tool for performing high-precision time-series photometry in crowded fields and near bright stars, especially when combined with difference image analysis (DIA)., Comment: 4 pages, 3 figures, Submitted to A&A, Version 3 contains the correct celestial coordinates in Table 1

The syntheses and catalytic behaviour of rhodium catalysts encapsulated in zeolites are reported. Several parameters are investigated in this catalyst system, including the auxiliary ligands and the zeolite supports used. It is demonstrated that the zeolite support can be crucial in determining the types of products formed from catalytic hydroform-ylation reactions. The results are rationulised in terms of fundamental principles of organometallic chemistry. This enhances the understanding of these catalyst systems at a molecular level and demonstrates that a synergy exists between the development of new, efficient catalyst systems and understanding chemistry at a fundamental level. Many organometallic complexes are used successfully in homogeneous catalysis, and as catalysts they are highly selective and operate under relatively mild reaction conditions. However, the benefits of homogeneous catalysts can be compromised by a diacult separation of catalyst from reaction products, or deactivation due to irreversible structural changes. In an attempt

We determine absolute dimensions and abundances for the three F-type main-sequence detached eclipsing binaries AD Boo, VZ Hya, and WZ Oph and perform a detailed comparison with results from recent stellar evolutionary models. uvby light curves and standard photometry were obtained at ESO,radial velocity observations at CfA facilities, and high-resolution spectra with ESO's FEROS spectrograph. State-of-the-art methods were applied for the analyses. Masses and radii that are precise to 0.5-0.7% and 0.4-0.9%, respectively, have been established for the components, which span the ranges of 1.1 to 1.4 M_sun and 1.1 to 1.6 R_sun. The [Fe/H] abundances are from -0.27 to +0.10, with uncertainties between 0.07 and 0.15 dex. We find indications of a slight alpha-element overabundance of [alpha/Fe] ~ +0.1$ for WZ Oph. The secondary component of AD Boo and both components of WZ Oph appear to be slightly active. Yale-Yonsai and Victoria-Regina evolutionary models fit the components of AD Boo and VZ Hya almost equally well, assuming coeval formation, at ages of about 1.75/1.50 Gyr (AD Boo) and 1.25/1.00 Gyr (VZ Hya). BaSTI models, however, predict somewhat different ages for the primary and secondary components. For WZ Oph, the models from all three grids are significantly hotter than observed. A low He content, decreased envelope convection coupled with surface activity, and/or higher interstellar absorption would remove the discrepancy, but its cause has not been definitively identified. We have demonstrated the power of testing and comparing recent stellar evolutionary models using eclipsing binaries, provided their abundances are known. The strongest limitations and challenges are set by T_eff and interstellar absorption determinations, and by their effects on and correlation with abundance results., Only revision is: Bottom lines (hopefully) not truncated anymore. Accepted for publication in Astronomy and Astrophysics

A 43-year-old man with a 19-year history of Crohn's disease experienced serum sickness with acute lobular panniculitis and vasculitis within 2 weeks of initiating 6-mercaptopurine therapy. He had no history of extraintestinal manifestations of Crohn's disease or drug allergy. Symptoms included disabling joint pain, proteinuria, fever, rash, and malaise. To our knowledge, this adverse drug reaction has not been described in association with 6-mercaptopurine.

Changes in alpha-2 adrenoreceptor density and affinity during antidepressant treatment were studied using 3H-yohimbine binding to human platelet membranes. Baseline measurements were conducted in 21 patients diagnosed as having major depressive disorder with melancholia, and an equal number of age and sex matched normal controls. No differences were observed in receptor density or binding between pre-treatment subject groups and normal matched controls. Subjects participated for 6 weeks in a trial of placebo, adinazolam, or amitriptyline. Alpha-2 adrenoreceptor binding was not significantly changed from baseline following antidepressant treatment.

Tracheal cilia of cows exposed, in vitro, for 20 hours to different acidities and alkalinities of sulfuric acid and sodium hydroxide, respectively, showed ciliomotility at pH values as low as 4.9, while the epithelial cells began to be expelled from the mucosa at pH 6.7, initiating a reduction of ciliary function around this pH value. In alkaline reactions, ciliostasis occurred at pH 9.76. Destroyed cilia were found above pH 10.15, while they were morphologically unchanged at pH values as low as 4.0, the lowest value examined. The first symptoms, however, of adverse effects were intracellular edema and the simultaneous occurrence of cellular polyps in both acid and alkaline reactions at pH 6.7 and 9.5, respectively. The results indicate that the early effects of air pollutants are better demonstrated by transmission electron microscopy studies than by, e.g., studies of ciliomotility.

The utility of a 30-drug, limited formulary in an adult internal medicine, ambulatory-care clinic was investigated. The formulary was developed using a mail survey of a random sample of members of the ASHP Ambulatory Care Pharmacy Practice Special Interest Group. The consensus formulary comprised the 30 most frequently recommended drugs; the utility of the formulary was then tested by chart review in a primary-care internal medicine clinic. Over a two-month period, the charts of alternating patients were reviewed daily; patient data collected included demographic information and prescribed drug therapy. A panel of two physicians and one pharmacist reviewed each patient's data and determined the appropriateness of drug treatment. If an agent was prescribed that was not on the consensus formulary, the panel determined whether an appropriate formulary agent could have been prescribed. Of the prescribed drug orders, 57.8% were for agents in the consensus formulary; by including patients who could have received formulary drugs appropriately, 73.7% of all prescription orders were or could have been for formulary drugs. Age, race, and sex of patients had no significant effect on utility of formulary agents. Had the 30 drugs most commonly prescribed in this clinic been in the formulary, 82.6% of all prescription orders would have been covered. This approach to establishing a new formulary and selecting drugs for inclusion is potentially useful.

Obstructive asphyxia, also known as cafe coronary, has been linked to both medicated and nonmedicated psychiatric patients. An 18-month prospective audit of choking patients was conducted in a psychiatric hospital. Based upon all medications received in the 5 days preceding the event, mean daily chlorpromazine and atropine equivalent dosages were also calculated for age, sex, and diagnosis matched controls based upon all medications received during their entire hospital stay. Paired t-tests showed no significant differences between choking patients and their matched controls except that greater mean daily chlorpromazine equivalents were present in the severe choking subgroup. Computation of log odds of choking risk increases with interaction of increased mean doses of each drug type and age, and also with interaction of increased chlorpromazine equivalents and increased atropine equivalents. Patients receiving high dosages of drug(s) with antidopaminergic or anticholinergic activity are at greater risk of choking and should be monitored closely.

These studies were done to characterize the rate of uptake of high (HDL) and low (LDL) density lipoprotein cholesterol by the adrenal gland of the rat under in vivo conditions. Animals were pretreated for 4 days with 4-aminopyrazolo[3,4-d]pyrimidine to essentially eliminate endogenous plasma lipoproteins and with aminoglutethimide for 1 h to block conversion of cholesterol to adrenal hormones. Such animals were then infused with varying amounts of HDL and LDL from both human and rat plasma, and this led to rapid accumulation of cholesterol, both free and esterified, in the adrenal glands over the subsequent 4-h period of observation. This uptake process was linear with respect to time and manifested saturation kinetics with respect to the steady state level of plasma lipoprotein cholesterol. When human lipoproteins were infused, the maximal rate of cholesterol uptake was approximately 0.45 mg/pair of adrenal glands/h for both HDL and LDL; however, the half-maximal rate of uptake (Km) was achieved at a plasma HDL cholesterol concentration of only 12 mg/dl while a concentration of 61 mg/dl was required to achieve the same velocity with LDL. When similar experiments were carried out with rat HDL, the Km equaled 7.2 mg/dl and a maximal rate of uptake of 0.32 mg/pair of adrenal glands/h was achieved. It was not possible to obtain complete kinetic curves using rat LDL, but at physiological plasma concentrations, there was no difference in the rate of cholesterol uptake from LDL of rat or human origin. When large amounts of both HDL (5.8 times Km) and LDL (3.1 times Km) were infused into the same animals, the rate of cholesterol uptake essentially equaled the sum of the maximal transport rates for the two lipoproteins. These data provide additional support for the concept that the adrenal gland (and ovary) of the rat can take up HDL and LDL cholesterol by separate mechanisms. However, from the quantitative data on the kinetics of these uptake processes, it is apparent that in this species HDL cholesterol must be the major substrate for the synthesis of adrenal hormones.

A case of protamine-associated hypertension in a 76-year-old Caucasian woman with chronic renal failure (CRF) undergoing hemodialysis is reported. Four dialysis runs during March 1977 are described in this report; all involved the i.v. administration of heparin sodium (2500-5000 units) during the five-hour procedures. Protamine sulfate (25-50 mg) was given i.v. at the end of each procedure to neutralize excess heparin. In three of the four dialyses, the patient became short of breath, hypertensive, and tachycardic, usually for less than 10 minutes. In the last of these runs, the patient first became hypotensive and then hypertensive, and was incontinent of urine and feces. Treatment in each case consisted of elevation of the head of the bed and oxygen administration. During the forth dialysis, no adverse reaction occurred. Possible explanations of this phenomenon are discussed, including hypersensitivity to protamine sulfate products and the action of protamine on platelets resulting in serotonin or histamine release. In dialyses where the patient became hypertensive, more protamine on platelets resulting in serotonin or histamine release. In dialyses where the patient became hypertensive, more protamine sulfate was given than was needed to neutralize the heparin. In the run where symptoms were most severe, the patient received only 2500 units of heparin but was given 50 mg protamine sulfate. It is concluded that this reaction occurred as a result of administering excess protamine sulfate, which then acted on platelets. The platelets released either histamine or serotonin, which mediated rapid changes in blood pressure, heart rate, and breathing pattern.

The relative rates of sterol synthesis in the liver and ten extrahepatic tissues of normal and cholesterol-fed rabbits were determined by measuring the rates of incorporation of [1-14C]octanoate into digitonin-precipitable sterols by tissue slices. In normal rabbits the rate of sterol synthesis in the liver was very low compared to that in several extrahepatic tissues, particularly the small intestine. The rate of synthesis in the small intestine showed marked regional variation, with the highest rate occurring in the section proximal to the entry of the common bile duct and the lowest rate in the mid-sections of the intestine. The regional differences in intestinal sterol synthesis correlated inversely with the cholesteryl ester content of the tissue. Rabbits fed the cholesterol diet developed marked hypercholesterolemia, with much of the additional cholesterol appearing in the VLDL and LDL fractions. The cholesteryl ester content of the liver, small intestine and various other extrahepatic tissues increased significantly. Coincident with these changes was a marked suppression of sterol synthesis, not only in the liver, but also in the small intestine, adrenal gland, kidney, lung, spleen and ovary. Thus, the rabbit, like the guinea pig, normally exhibits a very low rate of hepatic sterol synthesis compared to that found in other species such as the rat, squirrel monkey and baboon and, furthermore, manifests feedback inhibition of both hepatic and extrahepatic sterol synthesis when dietary cholesterol intake is increased. This general suppression of synthesis correlates with an accumulation of cholesteryl ester in the tissues which, in turn, presumably is related to the uptake of lipoprotein cholesterol from the hypercholesterolemic plasma that develops under such dietary conditions.

We present a spectroscopic catalog of 70,841 visually inspected M dwarfs from the seventh data release of the Sloan Digital Sky Survey (SDSS). For each spectrum, we provide measurements of the spectral type, a number of molecular bandheads, and the H-alpha, H-beta, H-gamma, H-delta and Ca II K emission lines. In addition, we calculate the metallicity-sensitive parameter zeta and identify a relationship between zeta and the g-r and r-z colors of M dwarfs. We assess the precision of our spectral types (which were assigned by individual examination), review the bulk attributes of the sample, and examine the magnetic activity properties of M dwarfs, in particular those traced by the higher order Balmer transitions. Our catalog is cross-matched to Two Micron All Sky Survey (2MASS) infrared data, and contains photometric distances for each star. Lastly, we identify eight new late-type M dwarfs that are possibly within 25 pc of the Sun. Future studies will use these data to thoroughly examine magnetic activity and kinematics in late-type M dwarfs and examine the chemical and dynamical history of the local Milky Way., Comment: 14 pages, 10 figures, 5 tables (in emulateapj format), accepted for publication in the Astronomical Journal

Primary production of phytoplankton in a eutrophic lake and of laboratory cultures of Selenastrum capricornutum was investigated using the 02 and `4C light and dark bottle techniques. The quotient Q (gross oxygen production divided by carbon fixation) ranged between 1.14 and 1.35 at light saturation, but at low light intensities it increased to values ranging from 2 to 8. This pattern is ascribed to underestimation of gross photosynthesis by `4C fixation rates due to reassimilation of respired C02, which is most important at low light levels. It is proposed to estimate gross photosynthesis from '4C fixation rates by adding the same value (e.g. 60% of dark respiration or 6% of maximal photosynthesis) at each light intensity down to the compensation point instead of using a constant multiplication factor.