Search

We report on the discovery of HAT-P-10b, the lowest mass (0.46 +/- 0.03 MJ) transiting extrasolar planet (TEP) discovered to date by transit searches. HAT-P-10b orbits the moderately bright V=11.89 K dwarf GSC 02340-01714, with a period P = 3.7224690 +/- 0.0000067 d, transit epoch Tc = 2454729.90631 +/- 0.00030 (BJD) and duration 0.1100 +/- 0.0015 d. HAT-P-10b has a radius of 1.05 +(0.05)-(0.03) RJ yielding a mean density of 0.498+/-0.064 g cm^-3 . Comparing these observations with recent theoretical models we find that HAT-P-10 is consistent with a ~4.5 Gyr, coreless, pure hydrogen and helium gas giant planet. With an equilibrium temperature of Teq = 1030 +(26)-(19)K, HAT-P-10b is one of the coldest TEPs. Curiously, its Safronov number Theta = 0.047 +/- 0.003 falls close to the dividing line between the two suggested TEP populations., 6 pages, 5 figures, submitted to ApJ. V2: added cross-reference to WASP-11b

We describe two cases of pregnancy in women with congenital heart disease, single ventricle. The first one underwent Fontan surgery at the age of 5 years due to a single ventricle of the left ventricular morphology. The second one, had uncorrected single ventricle. There were no maternal complications. Both deliveries were by cesarean section. Infants were premature, being delivered at 33 and 27 weeks, and weighing 1,250 and 625 g, respectively.

We report a case of a pregnant patient with a twin of 29 gestational weeks, and partial hydatidiform mole with coexistent living fetus. She was admitted at gyneco-obstetric urgencies due to a mild preeclampsia that evolves to severe. She has a complicated vaginal delivery with obstetric bleeding and there was practiced a total abdominal hysterectomy. Newborn dies 30 days later due to secondary complications (extreme prematurity). Patient evolution was satisfactory and she is currently under follow-up therapy to gestational trophoblastic disease without clinical or biochemical evidence of persistence or recurrence.

Abdominal advanced pregnancy is an obstetric complication that put at risk maternal and fetal life. We report a case of advanced abdominal pregnancy with intact ovaries and fallopian tubes, without ureteroperitoneal fistulae and, late prenatal diagnosis, in a multiparous patient without risk factors, with alive newborn, and whose pregnancy was attended at Unidad Medica de Alta Especialidad, Hospital de Gineco-Obstetricia, Centro Medico Nacional de Occidente del IMSS, Guadalajara, Jalisco, México.

Hypertension is associated with increased maternal and fetal mortality and morbidity. While there is consensus that severe hypertension should be treated, antihypertensive treatment for mild chronic hypertension during pregnancy remains controversial.To evaluate clinical course, and maternal and perinatal outcomes of pregnant women with mild chronic hypertension without other disease, under strict control of maternal hypertension (target dBP of 85-89 mmHg).We conducted a prospective cohort study of 110 pregnant women with mild chronic hypertension without other disease; clinical course was classified in three groups: stable condition, exacerbation of hypertension and superimposed preeclampsia. We compare maternal and perinatal outcomes; statistical comparisons were performed by ANOVA test. Relative risk (RR) was calculated for adverse perinatal outcomes.Atotal of 110 women were included, mean maternal age was 33 +/- 5.8 years. There were 78 (71%) women with stable condition, 26 (24%) with exacerbation of hypertension and 6 (5%) with superimposed preeclampsia (PE). Women with superimposed PE and exacerbation of hypertension delivered earlier and had more small for gestational age (SGA) babies than women with stable condition and exacerbation. Delivery route was vaginal in 45 patients (40%) while 65 patients (60%) underwent cesarean section in order to avoid fetal distress.Results demonstrated that fetuses in the stable condition group (strict control) did not have worst outcomes than those in the other groups. This cohort study shows efficacy and safety of treating mild chronic hypertension during pregnancy.

The Ebstein's anomaly is a congenital malformation of the tricuspid valve and of the right ventricle that usually is associated with interauricular communication, foramen oval, and arrhythmias of Wolff-Parkinson-White syndrome type.To analyze the association between Ebstein's anomaly and pregnancy.A prospective study was made in five pregnant women's with Ebstein's anomaly without surgery. We analyzed the clinical history, physical examination, electrocardiogram, x-ray of thorax, Doppler color heart ultrasound, and fetal valoration by means of pelvic ecosonogram and cardiotocographic registry, and routinely prenatal paraclinic tests.We observed severe expansion of the ventricle and 3rd degree index of atrialization in two patients. In two pregnancies there were interatrial communication (patients with cyanosis) and in three was detected severe tricuspid insufficiency. The average of gestacional age was of 36.4 +/- 1.8 weeks. Two of the five pregnancies has preterm birth. Only one childbirth was short weight to gestational age. The rest stayed within percentile 10. There were no obits or neonatal deaths, either congenital abnormality by Doppler heart ultrasound.The pregnancy is well tolerated in patients with Ebstein's anomaly; nevertheless, participation of multidisciplinary team is recommended to establish the treatment.

We present new V-band differential brightness measurements as well as new radial-velocity measurements of the detached, circular, 0.84-day period, double-lined eclipsing binary system CV Boo. These data along with other observations from the literature are combined to derive improved absolute dimensions of the stars for the purpose of testing various aspects of theoretical modeling. Despite complications from intrinsic variability we detect in the system, and despite the rapid rotation of the components, we are able to determine the absolute masses and radii to better than 1.3% and 2%, respectively. We obtain M(A) = 1.032 +/- 0.013 M(Sun) and R(B) = 1.262 +/- 0.023 R(Sun) for the hotter, larger, and more massive primary (star A), and M(B) = 0.968 +/- 0.012 M(Sun) and R(B) = 1.173 +/- 0.023 R(Sun) for the secondary. The estimated effective temperatures are 5760 +/- 150 K and 5670 +/- 150 K. The intrinsic variability with a period about 1% shorter than the orbital period is interpreted as being due to modulation by spots on one or both components. This implies that the spotted star(s) must be rotating faster than the synchronous rate, which disagrees with predictions from current tidal evolution models according to which both stars should be synchronized. We also find that the radius of the secondary is larger than expected from stellar evolution calculations by about 10%, a discrepancy also seen in other (mostly lower-mass and active) eclipsing binaries. We estimate the age of the system to be approximately 9 Gyr. Both components are near the end of their main-sequence phase, and the primary may have started the shell hydrogen-burning stage., 17 pages in emulateapj format, including figures and tables. To appear in The Astronomical Journal

We describe the discovery of a 0.68+0.52 solar mass eclipsing binary (EB) with an 8.4-day orbital period, found through a systematic search of ten fields of the Trans-atlantic Exoplanet Survey (TrES). Such long-period low-mass EBs constitute critical test cases for resolving the long standing discrepancy between the theoretical and observational mass-radius relations at the bottom of the main sequence. It has been suggested that this discrepancy may be related to strong stellar magnetic fields, which are not properly accounted for in current theoretical models. All previously well-characterized low-mass main sequence EBs have periods of a few days or less, and their components are therefore expected to be rotating rapidly as a result of tidal synchronization, thus generating strong magnetic fields. In contrast, the binary system described here has a period that is over three times longer than previously characterized low-mass main sequence EBs, and its components rotate relatively slowly. It is therefore expected to have a weaker magnetic field and to better match the assumptions of theoretical stellar models. Our follow-up observations of this EB yield preliminary stellar properties that suggest it is indeed consistent with current models. If further observations confirm a low level of activity in this system, these determinations would provide support for the hypothesis that the mass-radius discrepancy is at least partly due to magnetic activity., 29 pages, 9 figures, accepted for publication in ApJ

With 40 or more transiting exoplanets now known, the time is ripe to seek patterns and correlations among their observed properties, which may give important insights into planet formation, structure, and evolution. This task is made difficult by the widely different methodologies that have been applied to measure their properties in individual cases. Furthermore, in many systems our knowledge of the planet properties is limited by the knowledge of the properties of the parent stars. To address these difficulties we have undertaken the first comprehensive analysis of the data for 23 transiting planets using a uniform methodology. We revisit several of the recently proposed correlations, and find new ones involving the metallicity of the parent stars., 4 pages including figures. To appear in Proceedings of IAU Symposium 253, "Transiting Planets", May 2008, Cambridge, MA

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

We report the discovery of a single-lined spectroscopic binary with an Ultra Cool Dwarf (UCD) primary with a spectral type between M8 and L0.5. This system was discovered during the course of an ongoing survey to monitor L dwarfs for radial velocity variations and is the first known small separation (a, 11 pages, 2 figures. Accepted for publication in ApJ Letters

The periodic velocity variation with amplitude 0.57 krn s "1 for the solar-type dwarf star HI) 114762 is almost certainly due to the presence of an unseen low-mass companion. The sharp peak in the power spectrum, shown in Fig. 1, suggests that the period has been strictly constant over the 56 cycles observed. No photometric variations have been observed for this star, supporting strongly the argument against pulsation or rotation with surface features as the source of the velocity variations. The period of 84 days implies a mass of 12 Jupiters if the orbit is viewed edge-on. The orbital solution based on 401 CfA velocities, shown in Fig. 2, has an eccentricity of 0.26, about five times the estimated error. We find no evidence for a second periodicity in these data.

Context {The young binary system V773 Tau A exhibits a persistent radio flaring activity that gradually increases from a level of a few mJy at apoastron to more than 100 mJy at periastron. Interbinary collisions between very large (> 15 R) magnetic structures anchored on the two rotating stars of the system have been proposed to be the origin of these periodic radio flares. Magnetic structures extended over tens of stellar radii, that can also account for the observed fast decay of the radio flares, seem to correspond to the typical solar semi-open quite extended magnetic configurations called helmet streamers.} Aims {We aim to find direct observational evidence for the postulated, solar-like, coronal topologies.} Methods {We performed seven-consecutive-day VLBI observations at 8.4 GHz using an array consisting of the VLBA and the 100-m Effelsberg telescope.} Results {Two distintive structures appear in the radio images here presented. They happen to be associated with the primary and secondary stars of the V773 Tau A system. In one image (Fig.2-B) the two features are extended up to 18 R each and are nearly parallel revealing the presence of two interacting helmet streamers. One image (Fig.2-E) taken a few hours after a flare monitored by the 100-m Effelsberg telescope shows one elongated fading structure substantially rotated with respect to those seen in the B run. The same decay scenario is seen in Fig.2-G for the helmet streamer associated with the other star.} Conclusions {This is the very first direct evidence revealing that even if the flare origin is magnetic reconnection due to interbinary collision, both stars independently emit in the radio range with structures of their own. These structures are helmet streamers, observed for the first time in stars other than the Sun.}, 7 pages, 3 figures, A&A in press

Most of deceases due to pregnancy, delivery, puerperium and them attention are avoidable with current medicine resources.To analyze some basic elements of epidemiologic behavior of a hospital environment maternal mortality in a third level hospital during a period of 21 years.Analytical cross-sectional study, 222 maternal deaths registered at Hospital de Ginecologia y Obstetricia, Centro Medico Nacional de Occidente del Instituto Mexicano del Seguro Social, were included, during the period 1985-2005. Deaths were analyzed in three periods of 7 years each one. The analysis of results was made based on descriptive statistic. chi2 was used for comparison between periods.Maternal death ratio was 73 per 100,000 live births during the 21 years. Maternal mortality was lower in the group of women under 20 years and increase agreed maternal age. Frequency of direct obstetric deaths decreased when comparing the 3 periods. The main causes of maternal death were preeclampsia/eclampsia and obstetric hemorrhage, which were responsible for almost 50% of maternal deaths. There was no significant difference to anticipation by comparing periods, between 28 and 37% of deaths were foreseen. 98% of deaths occurred at Intensive Care Units.Direct and indirect maternal deaths show very similar values in the third period, which translates in an improvement in anticipation. It must be reinforce the simple and opportune information to the patient with regard to warning signs and the permanent medical training must be a priority at the 3 medical levels.

We report a case of a 30-year-old woman, who had two previous caesarean sections, attended for the first time at 18 weeks of gestation. Pelvic ultrasonography and color Doppler imaging showed a placenta percreta invading the urinary bladder. A caesarean section was carried out at 27th week of gestation for preterm premature rupture of membranes. Placental tissue was firmly attached to the anterior surface of the bladder. A cesarean hysterectomy was performed with bilateral anterior internal iliac artery ligation before hysterectomy was finished. The bladder was repaired, leaving a suprapubic catheter.

We present refined values for the physical parameters of transiting exoplanets, based on a self-consistent and uniform analysis of transit light curves and the observable properties of the host stars. Previously it has been difficult to interpret the ensemble properties of transiting exoplanets, because of the widely different methodologies that have been applied in individual cases. Furthermore, previous studies often ignored an important constraint on the mean stellar density that can be derived directly from the light curve. The main contributions of this work are 1) a critical compilation and error assessment of all reported values for the effective temperature and metallicity of the host stars; 2) the application of a consistent methodology and treatment of errors in modeling the transit light curves; and 3) more accurate estimates of the stellar mass and radius based on stellar evolution models, incorporating the photometric constraint on the stellar density. We use our results to revisit some previously proposed patterns and correlations within the ensemble. We confirm the mass-period correlation, and we find evidence for a new pattern within the scatter about this correlation: planets around metal-poor stars are more massive than those around metal-rich stars at a given orbital period. Likewise, we confirm the proposed dichotomy of planets according to their Safronov number, and we find evidence that the systems with small Safronov numbers are more metal-rich on average. Finally, we confirm the trend that led to the suggestion that higher-metallicity stars harbor planets with a greater heavy-element content., To appear in The Astrophysical Journal. 23 pages in emulateapj format, including figures and tables. Figures 7, 8, and 9 are low resolution; higher resolution versions will be available from the journal when published. Acknowledgement added, and minor changes made to TrES-3 and TrES-4 in the Appendix

We present photometry of 13 transits of XO-3b, a massive transiting planet on an eccentric orbit. Previous data led to two inconsistent estimates of the planetary radius. Our data strongly favor the smaller radius, with increased precision: R_p = 1.217 +/- 0.073 R_Jup. A conflict remains between the mean stellar density determined from the light curve, and the stellar surface gravity determined from the shapes of spectral lines. We argue the light curve should take precedence, and revise the system parameters accordingly. The planetary radius is about 1 sigma larger than the theoretical radius for a hydrogen-helium planet of the given mass and insolation. To help in planning future observations, we provide refined transit and occultation ephemerides., Comment: To appear in ApJ [22 pages]

En este artículo se abordan el contexto, las características y el impacto de la Ley de Desarrollo Rural Sustentable (LDRS), que norma las actividades agropecuarias y rurales con un enfoque de integralidad, apoyos multianuales focalizados y de acuerdo con una tipología de productores. Se discute la relación entre los problemas productivos y los apoyos otorgados, las contradicciones internas de la Ley, cuáles han sido sus consecuencias en el campo mexicano y si es pertinente o no frente a la degradación socioambiental, todo ello considerando el pluralismo económico y jurídico. La LDRS constituye un documento desordenado, ambiguo y repetitivo y su principal dificultad es que carece de un concepto operativo del desarrollo rural sustentable. Así, no hay claridad en la conexión de las esferas ecológica, económica y soial. Sin embargo, pese a esas limitaciones constituye un instrumento -aunque no idóneo- para reordenar el campo mexicano. Además, es la típica ley que no se cumple en la práctica. Como resultado, no se encuentran avances concretos, menos en cuanto a la soberanía alimentaria y el pago justo de los servicios ambientales. El principal motivo es la carencia de una Ley General de Desarrollo Sustentable que norme la transición energético-ambiental.

Photometry is presented of the Dec. 25, 2007 transit of HD 17156b, which has the longest orbital period and highest orbital eccentricity of all the known transiting exoplanets. New measurements of the stellar radial velocity are also presented. All the data are combined and integrated with stellar-evolutionary modeling to derive refined system parameters. The planet's mass and radius are found to be 3.212_{-0.082}^{+0.069} Jupiter masses and 1.023_{-0.055}^{+0.070} Jupiter radii. The corresponding stellar properties are 1.263_{-0.047}^{+0.035} solar masses and 1.446_{-0.067}^{+0.099} solar radii. The planet is smaller by 1 sigma than a theoretical solar-composition gas giant with the same mass and equilibrium temperature, a possible indication of heavy-element enrichment. The midtransit time is measured to within 1 min, and shows no deviation from a linear ephemeris (and therefore no evidence for orbital perturbations from other planets). We provide ephemerides for future transits and superior conjunctions. There is an 18% chance that the orbital plane is oriented close enough to edge-on for secondary eclipses to occur at superior conjunction. Observations of secondary eclipses would reveal the thermal emission spectrum of a planet that experiences unusually large tidal heating and insolation variations., Comment: To appear in ApJ [26 pages]

12 pages, 7 figures.-- ArXiv pre-print available at: http://arxiv.org/abs/0810.1541, Spectroscopic and eclipsing binary systems offer the best means for determining accurate physical properties of stars, including their masses and radii. The data available for low-mass stars have yielded firm evidence that stellar structure models predict smaller radii and higher effective temperatures than observed, but the number of systems with detailed analyses is still small. In this paper, we present a complete reanalysis of one of such eclipsing systems, CM Dra, composed of two dM4.5 stars. New and existing light curves as well as a radial velocity curve are modeled to measure the physical properties of both components. The masses and radii determined for the components of CM Dra are M1 = 0.2310 ± 0.0009 Msun, M2 = 0.2141 ± 0.0010 Msun, R1 = 0.2534 ± 0.0019 Rsun, and R2 = 0.2396 ± 0.0015 Rsun. With relative uncertainties well below the 1% level, these values constitute the most accurate properties to date for fully convective stars. This makes CM Dra a valuable benchmark for testing theoretical models. In comparing our measurements with theory, we confirm the discrepancies previously reported for other low-mass eclipsing binaries. These discrepancies seem likely to be due to the effects of magnetic activity. We find that the orbit of this system is slightly eccentric, and we have made use of eclipse timings spanning three decades to infer the apsidal motion and other related properties., JCM, IR and CJ acknowledge support from the Spanish Ministerio de Educación y Ciencia via grants AYA2006-15623-C02-01 and AYA2006-15623-C02-02. GT acknowledges partial support for this work from NSF grant AST-0708229 and NASA’s MASSIF SIM Key Project (BLF57-04). EFG acknowledges support for the FCAPT research under NSF/RUI grant AST05-07536. DC and FTOD acknowledge support for the Sleuth Observatory work by the National Aeronautics and Space Administration under grant NNG05GJ29G issued through the Origins of Solar Systems Program. FTOD also acknowledges partial support for this work provided through the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. The investigation of MW was supported by the Grant Agency of the Czech Republic under grant No. 205/06/0217.

We present HATNet observations of XO-5b, confirming its planetary nature based on evidence beyond that described in the announcement of Burke et al. (2008), namely, the lack of significant correlation between spectral bisector variations and orbital phase. In addition, using extensive spectroscopic measurements spanning multiple seasons, we investigate the relatively large scatter in the spectral line bisectors. We also examine possible blended stellar configurations (hierarchical triples, chance alignments) that can mimic the planet signals, and we are able to show that none are consistent with the sum of all the data. The analysis of the S activity index shows no significant stellar activity. Our results for the planet parameters are consistent with values in Burke et al. (2008), and we refine both the stellar and planetary parameters using our data. XO-5b orbits a slightly evolved, late G type star with mass M_s = 0.88 +/- 0.03, radius R_s = 1.08 +/- 0.04, and metallicity close to solar. The planetary mass and radius are M_p = 1.059 +/- 0.028 M_Jup and R_p = 1.109 +/- 0.050 R_Jup, respectively, corresponding to a mean density of 0.96 -0.11 +0.14 g/cm^3. The ephemeris for the orbit is P = 4.187757 +/- 0.000011, E= 2454552.67168 +/- 0.00029 (BJD) with transit duration of 0.1307 +/- 0.0013 d. By measuring four individual transit centers, we found no signs for transit timing variations. The planet XO-5b is notable for its anomalously high Safronov number, and has a high surface gravity when compared to other transiting exoplanets with similar period., Comment: Accepted for publication in ApJ, 8 pages in emulateapj style

Knowledge of the stellar parameters for the parent stars of transiting exoplanets is pre-requisite for establishing the planet properties themselves, and often relies on stellar evolution models. GJ 436, which is orbited by a transiting Neptune-mass object, presents a difficult case because it is an M dwarf. Stellar models in this mass regime are not as reliable as for higher mass stars, and tend to underestimate the radius. Here we use constraints from published transit light curve solutions for GJ 436 along with other spectroscopic quantities to show how the models can still be used to infer the mass and radius accurately, and at the same time allow the radius discrepancy to be estimated. Similar systems should be found during the upcoming Kepler mission, and could provide in this way valuable constraints to stellar evolution models in the lower main sequence. The stellar mass and radius of GJ 436 are M = 0.452 [-0.012,+0.014] M(Sun) and R = 0.464 [-0.011,+0.009] R(Sun), and the radius is 10% larger than predicted by the standard models, in agreement with previous results from well studied double-lined eclipsing binaries. We obtain an improved planet mass and radius of M = 23.17 +/- 0.79 M(Earth) and R = 4.22 [-0.10,+0.09] R(Earth), a density of rho = 1.69 [-0.12,+0.14] g/cm3, and an orbital semimajor axis of a = 0.02872 +/- 0.00027 AU., Accepted for publication in The Astrophysical Journal Letters, 5 pages including figures and tables, in emulateapj format

In the ongoing HATNet survey we have detected a giant planet, with radius 1.33 +/- 0.06 RJup and mass 1.06 +/- 0.12 MJup, transiting the bright (V = 10.5) star GSC 03239-00992. The planet is in a circular orbit with period 3.852985 +/- 0.000005 days and mid-transit epoch 2,454,035.67575 +/- 0.00028 (HJD). The parent star is a late F star with mass 1.29 +/- 0.06 Msun, radius 1.46 +/- 0.06 Rsun, Teff ~ 6570 +/- 80 K, [Fe=H] = -0.13 +/- 0.08 and age ~ 2.3+/-^{0.5}_{0.7}Gy. With this radius and mass, HAT-P-6b has somewhat larger radius than theoretically expected. We describe the observations and their analysis to determine physical properties of the HAT-P-6 system, and briefly discuss some implications of this finding., Accepted for publication in ApJL, 5 pages, minor changes compared to V1

We describe the discovery of HAT-P-4b, a low-density extrasolar planet transiting BD+36 2593, a V = 11.2 mag slightly evolved metal-rich late F star. The planet's orbital period is 3.056536+/-0.000057 d with a mid-transit epoch of 2,454,245.8154 +/- 0.0003 (HJD). Based on high-precision photometric and spectroscopic data, and by using transit light curve modeling, spectrum analysis and evolutionary models, we derive the following planet parameters: Mp= 0.68 +/- 0.04 MJ, Rp= 1.27 +/- 0.05 RJ, rho = 0.41 +/- 0.06 g cm-3 and a = 0.0446 +/- 0.0012 AU. Because of its relatively large radius, together with its assumed high metallicity of that of its parent star, this planet adds to the theoretical challenges to explain inflated extrasolar planets., 5 pages, accepted for publication in ApJL

We report the discovery of a Jupiter-size planet transiting a relatively bright (V = 11.56) and metal-rich early K dwarf star with a period of about 2.9 days. On the basis of follow-up photometry and spectroscopy we determine the mass and radius of the planet, HAT-P-3b, to be M_p = 0.599 +/- 0.026 M_Jup and R_p = 0.890 +/- 0.046 R_Jup. The relatively small size of the object for its mass implies the presence of about 75 Earth masses worth of heavy elements (1/3 of the total mass) based on current theories of irradiated extrasolar giant planets, similar to the mass of the core inferred for the transiting planet HD 149026b. The bulk density of HAT-P-3b is found to be rho_p = 1.06 +/- 0.17 g/cm^3, and the planet orbits the star at a distance of 0.03894 AU. Ephemerides for the transit centers are T_c = 2,454,218.7594 +/- 0.0029 + N (2.899703 +/- 0.000054) (HJD)., To appear in ApJL

Driven by the incomplete understanding of the formation of gas giant extrasolar planets and of their mass-radius relationship, several ground-based, wide-field photometric campaigns are searching the skies for new transiting extrasolar gas giants. As part of the Trans-atlantic Exoplanet Survey (TrES), in 2003/4 we monitored approximately 30,000 stars (9 .5 < V < 15.5) in a 5.7 degree x 5.7 degree field in Andromeda with three telescopes over five months. We identified six candidate transiting planets from the stellar light curves. From subsequent follow-up observations, we rejected each of these as an astrophysical false positive, i.e. a stellar system containing an eclipsing binary, whose light curve mimics that of a Jupiter-sized planet transiting a sun-like star. We discuss here the procedures followed by the TrES team to reject false positives from our list of candidate transiting hot Jupiters. We present these candidates as early examples of the various types of astrophysical false postives found in the TrES campaign, and discuss what we learned from the analysis., v1. Submitted to ApJ, 22 July 2006. 14 pages, 8 figures, 4 tables. Updated references, author order and author affiliations. v.2 Substantial changes made to text. Accepted for publication in ApJ. v3. Corrections made to source that do not impact text

Of the nearby transiting exoplanets that are amenable to detailed study, TrES-2 is both the most massive and has the largest impact parameter. We present z-band photometry of three transits of TrES-2. We improve upon the estimates of the planetary, stellar, and orbital parameters, in conjunction with the spectroscopic analysis of the host star by Sozzetti and co-workers. We find the planetary radius to be 1.222 +/- 0.038 R_Jup and the stellar radius to be 1.003 +/- 0.027 R_Sun. The quoted uncertainties include the systematic error due to the uncertainty in the stellar mass (0.980 +/- 0.062 M_Sun). The timings of the transits have an accuracy of 25s and are consistent with a uniform period, thus providing a baseline for future observations with the NASA Kepler satellite, whose field of view will include TrES-2., 15 pages, including 2 figures, accepted ApJ

We develop a technique to measure radial velocities of stars from spectra that present four sets of lines. The algorithm is an extension of the two-dimensional cross-correlation method TODCOR to four dimensions. It computes the correlation of the observed spectrum against a combination of four templates with all possible shifts, and allows also for the derivation of the light ratios of the components. After testing the algorithm and demonstrating its ability to measure Doppler shifts accurately even under conditions of heavy line blending, we apply it to the case of the quadruple-lined system HD 110555. The primary and secondary components of this previously known visual binary (separation about 0.4 arcsec) are each shown to be double-lined spectroscopic binaries with periods of 57 days and 76 days, respectively, making the system a hierarchical quadruple. The secondary in the 76-day subsystem contributes only 2.5% to the total light, illustrating the ability of the method to measure velocities of very faint components., Total of 15 pages including figures and tables, in emulateapj format. To appear in The Astrophysical Journal, June 2007 issue

We report on interferometric and radial-velocity observations of the double-lined 51-d period binary (A) component of the quadruple pre-main sequence (PMS) system V773 Tau. With these observations we have estimated preliminary visual and physical orbits of the V773 Tau A subsystem. Among other parameters, our orbit model includes an inclination of 66.0 $\pm$ 2.4 deg, and allows us to infer the component dynamical masses and system distance. In particular we find component masses of 1.54 $\pm$ 0.14 and 1.332 $\pm$ 0.097 M$_{\sun}$ for the Aa (primary) and Ab (secondary) components respectively. Our modeling of the subsystem component spectral energy distributions finds temperatures and luminosities consistent with previous studies, and coupled with the component mass estimates allows for comparison with PMS stellar models in the intermediate-mass range. We compare V773 Tau A component properties with several popular solar-composition models for intermediate-mass PMS stars. All models predict masses consistent to within 2-sigma of the dynamically determined values, though some models predict values that are more consistent than others., Comment: ApJ in press; 25 pages, 6 figures; data tables available in journal version

We report the discovery of TrES-4, a hot Jupiter that transits the star GSC 02620-00648 every 3.55 days. From high-resolution spectroscopy of the star, we estimate a stellar effective temperature of T_(eff) = 6100 ± 150 K, and from high-precision z and B photometry of the transit we constrain the ratio of the semimajor axis a and the stellar radius R_* to be a/R_* = 6.03 ± 0.13. We compare these values to model stellar isochrones to constrain the stellar mass to be M_* = 1.22 ± 0.17 M_⊙. Based on this estimate and the photometric time series, we constrain the stellar radius to be R_* = 1.738 ± 0.092 R_⊙ and the planet radius to be R_p = 1.674 ± 0.094 R_(Jup). We model our radial velocity data assuming a circular orbit and find a planetary mass of 0.84 ± 0.10 M_(Jup). Our radial velocity observations rule out line-bisector variations that would indicate a specious detection resulting from a blend of an eclipsing binary system. TrES-4 has the largest radius and lowest density of any of the known transiting planets. It presents a challenge to current models of the physical structure of hot Jupiters and indicates that the diversity of physical properties among the members of this class of exoplanets has yet to be fully explored.

The previously known, 6-yr spectroscopic binary HR 6046 has been speculated in the past to contain a compact object as the secondary. A recent study has re-determined the orbit with great accuracy, and shown that the companion is an evolved but otherwise normal star of nearly identical mass as the primary, which is also a giant. The binary motion was detected by the Hipparcos mission but was not properly accounted for in the published astrometric solution. Here we use the Hipparcos intermediate data in combination with the spectroscopic results to revise that solution and establish the orbital inclination angle for the first time, and with it the absolute masses M(A) = 1.38 [-0.03,+0.09] M(Sun) and M(B) = 1.36 [-0.02,+0.07] M(Sun). Aided by other constraints, we investigate the evolutionary status and confirm that the primary star is approaching the tip of the red-giant branch, while the secondary is beginning its first ascent., Comment: To appear in The Astronomical Journal. 8 pages including tables and figures, in emulateapj format

We present new photometry of HD 149026 spanning five transits of its "super-Neptune" planet. In combination with previous data, we improve upon the determination of the planet-to-star radius ratio: R_p/R_star = 0.0491^{+0.0018}_{-0.0005}. We find the planetary radius to be 0.71 +/- 0.05 R_Jup, in accordance with previous theoretical models invoking a high metal abundance for the planet. The limiting error is the uncertainty in the stellar radius. Although we find agreement among four different ways of estimating the stellar radius, the uncertainty remains at 7%. We also present a refined transit ephemeris and a constraint on the orbital eccentricity and argument of pericenter, e cos(omega) = -0.0014 +/- 0.0012, based on the measured interval between primary and secondary transits., Comment: To appear in ApJ [19 pages]

We present a survey of 41 Kepler Objects of Interest (KOIs) for exomoons using Bayesian photodynamics, more than tripling the number of KOIs surveyed with this technique. We find no compelling evidence for exomoons although thirteen KOIs yield spurious detections driven by instrumental artifacts, stellar activity and/or perturbations from unseen bodies. Regarding the latter, we find seven KOIs exhibiting >5 sigma evidence of transit timing variations, including the 'mega-Earth' Kepler-10c, likely indicating an additional planet in that system. We exploit the moderately large sample of 57 unique KOIs surveyed to date to infer several useful statistics. For example, although there is a diverse range in sensitivities, we find that we are sensitive to Pluto-Charon mass-ratio systems for ~40% of KOIs studied and Earth-Moon mass-ratios for 1 in 8 cases. In terms of absolute mass, our limits probe down to 1.7 Ganymede masses, with a sensitivity to Earth-mass moons for 1 in 3 cases studied and to the smallest moons capable of sustaining an Earth-like atmosphere (0.3 Earth masses) for 1 in 4. Despite the lack of positive detections to date, we caution against drawing conclusions yet, since our most interesting objects remain under analysis. Finally, we point out that had we searched for the photometric transit signals of exomoons alone, rather than using photodynamics, we estimate that 1 in 4 KOIs would have erroneously been concluded to harbor exomoons due to residual time correlated noise in the Kepler data, posing a serious problem for alternative methods., 18 pages, 9 figures, 4 tables. Accepted in ApJ

To measure the properties of both components of the RS CVn binary sigma Geminorum (sigma Gem), we directly detect the faint companion, measure the orbit, obtain model-independent masses and evolutionary histories, detect ellipsoidal variations of the primary caused by the gravity of the companion, and measure gravity darkening. We detect the companion with interferometric observations obtained with the Michigan InfraRed Combiner (MIRC) at Georgia State University's Center for High Angular Resolution Astronomy (CHARA) Array with a primary-to-secondary H-band flux ratio of 270+/-70. A radial velocity curve of the companion was obtained with spectra from the Tillinghast Reflector Echelle Spectrograph (TRES) on the 1.5-m Tillinghast Reflector at Fred Lawrence Whipple Observatory (FLWO). We additionally use new observations from the Tennessee State University Automated Spectroscopic and Photometric Telescopes (AST and APT, respectively). From our orbit, we determine model-independent masses of the components (M_1 = 1.28 +/- 0.07 M_Sun, M_2 = 0.73 +/- 0.03 M_Sun), and estimate a system age of 5 -/+ 1 Gyr. An average of the 27-year APT light curve of sigma Gem folded over the orbital period (P = 19.6027 +/- 0.0005 days) reveals a quasi-sinusoidal signature, which has previously been attributed to active longitudes 180 deg apart on the surface of sigma Gem. With the component masses, diameters, and orbit, we find that the predicted light curve for ellipsoidal variations due to the primary star partially filling its Roche lobe potential matches well with the observed average light curve, offering a compelling alternative explanation to the active longitudes hypothesis. Measuring gravity darkening from the light curve gives beta < 0.1, a value slightly lower than that expected from recent theory., Accepted to ApJ, 11 pages, 6 figures, 8 tables

We present spatially and spectrally resolved Atacama Large Millimeter/submillimeter Array (ALMA) observations of gas and dust in the disk orbiting the pre-main sequence (pre-MS) binary AK Sco. By forward-modeling the disk velocity field traced by CO J = 2?1 line emission, we infer the mass of the central binary, , a new dynamical measurement that is independent of stellar evolutionary models. Assuming the disk and binary are co-planar within ?2?, this disk-based binary mass measurement is in excellent agreement with constraints from radial velocity monitoring of the combined stellar spectra. These ALMA results are also compared with the standard approach of estimating masses from the location of the binary in the Hertzsprung?Russell diagram, using several common pre-MS model grids. These models predict stellar masses that are marginally consistent with our dynamical measurement (at ?2?), but are systematically high (by ?10%). These same models consistently predict an age of 18 ? 1 Myr for AK Sco, in line with its membership in the Upper Centaurus?Lupus association but surprisingly old for it to still host a gas-rich disk. As ALMA accumulates comparable data for large samples of pre-MS stars, the methodology employed here to extract a dynamical mass from the disk rotation curve should prove extraordinarily useful for efforts to characterize the fundamental parameters of early stellar evolution.

We present an investigation of twelve candidate transiting planets from Kepler with orbital periods ranging from 34 to 207 days, selected from initial indications that they are small and potentially in the habitable zone (HZ) of their parent stars. Few of these objects are known. The expected Doppler signals are too small to confirm them by demonstrating that their masses are in the planetary regime. Here we verify their planetary nature by validating them statistically using the BLENDER technique, which simulates large numbers of false positives and compares the resulting light curves with the Kepler photometry. This analysis was supplemented with new follow-up observations (high-resolution optical and near-infrared spectroscopy, adaptive optics imaging, and speckle interferometry), as well as an analysis of the flux centroids. For eleven of them (KOI-0571.05, 1422.04, 1422.05, 2529.02, 3255.01, 3284.01, 4005.01, 4087.01, 4622.01, 4742.01, and 4745.01) we show that the likelihood they are true planets is far greater than that of a false positive, to a confidence level of 99.73% (3 sigma) or higher. For KOI-4427.01 the confidence level is about 99.2% (2.6 sigma). With our accurate characterization of the GKM host stars, the derived planetary radii range from 1.1 to 2.7 R_Earth. All twelve objects are confirmed to be in the HZ, and nine are small enough to be rocky. Excluding three of them that have been previously validated by others, our study doubles the number of known rocky planets in the HZ. KOI-3284.01 (Kepler-438b) and KOI-4742.01 (Kepler-442b) are the planets most similar to the Earth discovered to date when considering their size and incident flux jointly.

The discovery of an exomoon would provide deep insights into planet formation and the habitability of planetary systems, with transiting examples being particularly sought after. Of the hundreds of Kepler planets now discovered, the seven-planet system Kepler-90 is unusual for exhibiting an unidentified transit-like signal in close proximity to one of the transits of the long-period gas-giant Kepler-90g, as noted by Cabrera et. al. (2014). As part of the 'Hunt for Exomoons with Kepler' (HEK) project, we investigate this possible exomoon signal and find it passes all conventional photometric, dynamical and centroid diagnostic tests. However, pixel-level light curves indicate that the moon-like signal occurs on nearly all of the target's pixels, which we confirm using a novel way of examining pixel-level data which we dub the 'transit centroid'. This test reveals that the possible exomoon to Kepler-90g is likely a false positive, perhaps due to a cosmic ray induced Sudden Pixel Sensitivity Dropout (SPSD). This work highlights the extreme care required for seeking non-periodic low-amplitude transit signals, such as exomoons., Comment: 5 pages, 4 figures. Accepted for publication in The Astrophysical Journal Letters

IM Per is a detached A7 eccentric eclipsing binary star. We have obtained extensive measurements of the light curve (28,225 differential magnitude observations) and radial velocity curve (81 spectroscopic observations) which allow us to fit orbits and determine the absolute properties of the components very accurately: masses of 1.7831 ± 0.0094 and 1.7741 ± 0.0097 solar masses, and radii of 2.409 ± 0.018 and 2.366 ± 0.017 solar radii. The orbital period is 2.25422694(15) days and the eccentricity is 0.0473(26). A faint third component was detected in the analysis of the light curves, and also directly observed in the spectra. The observed rate of apsidal motion is consistent with theory (U = 151.4 ± 8.4 year). We determine a distance to the system of 566 ± 46 pc.

Drug prescription is the most frequent medical intervention in Gynecology and Obstetrics; however, studies of prescription profile are limited. In this study, we analyzed differences of expense by drug prescription for gynecologic and obstetrics health problems.It was performed a cross sectional study for one year analysis in each medical area that shape IMSS western district. We calculated spending and consumption coefficients for each drug and therapeutic groups. User coefficients were ordered to compare consumption differences. Besides the statistical ratio of consumption between drugs groups, we described the differences found and analyzed the prescription profile among medical regions.Data related to the expenses in each one of the regions show important differences in each one of the drugs and therapeutic groups. The most common expense for drugs is related to the treatment of osteoporosis, menopause and fertility problems. We also found differences in prescription drug preferences in each therapeutic subgroup.Drug prescription studies are useful as a basis for further specific studies in each pharmacologic subgroup. There are few studies that analyze the drug prescription profile on Gynecology and Obstetrics. In this study it is possible to suppose that medical prescription was not based on known medical evidences; therefore, we must reconsider the need of a permanent actualization and systematic medical evaluation.

Using small automated telescopes in Arizona and Hawaii, the HATNet project has detected an object transiting one member of the double star system ADS 16402 AB. This system is a pair of G0 main-sequence stars with age about 3 Gyr at a distance of ~139 pc and projected separation of ~1550 AU. The transit signal has a period of 4.46529 days and depth of 0.015 mag. From follow-up photometry and spectroscopy, we find that the object is a "hot Jupiter" planet with mass about 0.53 M_jup and radius ~1.36 R_jup traveling in an orbit with semimajor axis 0.055 AU and inclination about 85.9 deg, thus transiting the star at impact parameter 0.74 of the stellar radius. Based on a data set spanning three years, ephemerides for the transit center are: T_C = 2453984.397 + N_tr * 4.46529. The planet, designated HAT-P-1b, appears to be at least as large in radius, and smaller in mean density, than any previously-known planet., 8 pages, accepted for publication in ApJ, see also http://www.hatnet.hu (www.hatnet.hu)

We announce the discovery of the second transiting hot Jupiter discovered by the Trans-atlantic Exoplanet Survey. The planet, which we dub TrES-2, orbits the nearby star GSC 03549-02811 every 2.47063 days. From high-resolution spectra, we determine that the star has T_eff = 5960 +/- 100 K and log(g) = 4.4 +/- 0.2, implying a spectral type of G0V and a mass of 1.08 +0.11/-0.05 M_sun. High-precision radial-velocity measurements confirm a sinusoidal variation with the period and phase predicted by the photometry, and rule out the presence of line-bisector variations that would indicate that the spectroscopic orbit is spurious. We estimate a planetary mass of 1.28 +0.09/-0.04 M_Jup. We model B, r, R, and I photometric timeseries of the 1.4%-deep transits and find a planetary radius of 1.24 +0.09/-0.06 R_Jup. This planet lies within the field of view of the NASA Kepler mission, ensuring that hundreds of upcoming transits will be monitored with exquisite precision and permitting a host of unprecedented investigations., Accepted for publication in ApJL. 15 pages, 2 figures

Determinations of stellar mass and radius with realistic uncertainties at the level of 1% provide important constraints on models of stellar structure and evolution. We present a high-precision light curve of the A0IV star Psi Centauri, from the star tracker on board the WIRE satellite and the Solar Mass Ejection Imager camera on the Coriolis spacecraft. The data show that Psi Cen is an eccentric eclipsing binary system with a relatively long orbital period. The WIRE light curve extends over 28.7 nights and contains 41334 observations with 2 mmag point-to-point scatter. The eclipse depths are 0.28 and 0.16 mag, and show that the two eclipsing components of Psi Cen have very different radii. As a consequence, the secondary eclipse is total. We find the eccentricity to be e=0.55 with an orbital period of 38.8 days from combining the WIRE light curve with data taken over two years from the Solar Mass Ejection Imager camera. We have fitted the light curve with EBOP and have assessed the uncertainties of the resulting parameters using Monte Carlo simulations. The fractional radii of the stars and the inclination of the orbit have random errors of only 0.1% and 0.01 degrees, respectively, but the systematic uncertainty in these quantities may be somewhat larger. We have used photometric calibrations to estimate the effective temperatures of the components of Psi Cen to be 10450+-300 and 8800+-300 K, indicating masses of about 3.1 and 2.0 Msun. There is evidence in the WIRE light curve for g-mode pulsations in the primary star., 9 pages, 4 figures, accepted for publication in A&A. Photometric data will be made available at the CDS once the final version appears. The resolution in Fig. 1 has been reduced

The most fundamental parameter of a star is its mass. For low mass pre-main sequence (pms) stars this parameter is practically always derived by comparing the location of the star in the Hertzsprung-Russell diagram with theoretically calculated evolutionary tracks. In order to really test the tracks, determination of the masses of a number of pms-stars are necessary. Up to now, masses could only be derived for a few individual cases. In the near future the VLTI will allow us to determine the masses of many pms-stars with high accuracy. In order to prepare for the VLTI-observation, we have begun a survey for long period pms-spectroscopic binaries that should be resolvable with the VLTI. We find that 8% of the stars surveyed show significant radial-velocity variations, and are thus most likely spectroscopic binaries. In addition to these, 6% of the targets are double-lined spectroscopic binaries. The second aim of the survey is to find also all eclipsing binaries amongst these stars, and we have in fact found a highly promising candidate. An eclipsing binary announced previously by other authors turned out to be a spotted star.

Sin resumen.

The bright K1 III-IV star gamma Cep has been reported previously to have a companion in a 2.5-yr orbit that is possibly substellar, and also has a stellar companion at a larger separation that has never been seen. Here we determine for the first time the three-dimensional orbit of the stellar companion accounting also for the perturbation from the closer object. We combine new and existing radial velocity measurements (of both classical precision and high precision) with intermediate astrometric data from the Hipparcos mission (abscissa residuals) as well as ground-based positional observations going back more than a century. The orbit of the secondary star is eccentric and has a period of 66.8 yr. We establish the primary star to be on the first ascent of the giant branch, and to have a mass of 1.18 M_Sun, an effective temperature of 4800 K, and an age around 6.6 Gyr (for an assumed metallicity [Fe/H] = +0.01). The unseen secondary star is found to be an M4 dwarf with a mass of 0.362 M_Sun, and is expected to be about 6.4 mag fainter than the primary in K. The minimum mass of the putative planetary companion is M_p sin i = 1.43 M_Jup. Taking advantage again of the high-precision Hipparcos observations we are able to place a dynamical upper limit on this mass of 13.3 M_Jup (95% confidence level) and 16.9 M_Jup (99.73%, or 3 sigma) thus confirming that it is indeed substellar in nature. (Abridged), Comment: 28 pages in emulateapj style, including tables and figures. Accepted for publication in ApJ

The star gamma Cep is known as a single-lined spectroscopic triple system at a distance of 13.8 pc, composed of a K1 III-IV primary star with V = 3.2 mag, a stellar-mass companion in a 66--67 year orbit (Torres 2006), and a substellar companion with M_p sin i = 1.7 M_Jup that is most likely a planet (Hatzes et al. 2003). We aim to obtain a first direct detection of the stellar companion, to determine its current orbital position (for comparison with the spectroscopic and astrometric data), its infrared magnitude and, hence, mass. We use the Adaptive Optics camera CIAO at the Japanese 8m telescope Subaru on Mauna Kea, Hawaii, with the semi-transparent coronograph to block most of the light from the bright primary gamma Cep A, and to detect at the same time the faint companion B. In addition, we also used the IR camera Omega-Cass at the Calar Alto 3.5m telescope, Spain, to image gamma Cep A and B by adding up many very short integrations (without AO). gamma Cep B is clearly detected on our CIAO and Omega-Cass images. We use a photometric standard star to determine the magnitude of B after PSF subtraction in the Subaru image, and the magnitude difference between A and B in the Calar Alto images, and find an average value of K = 7.3 \pm 0.2 mag. The separations and position angles between A and B are measured on 15 July 2006 and 11 and 12 Sept 2006, B is slightly south of west of A. By combining the radial velocity, astrometric, and imaging data, we have refined the binary orbit and determined the dynamical masses of the two stars in the gamma Cep system, namely 1.40 \pm 0.12 M_sun for the primary and 0.409 \pm 0.018 M_sun for the secondary (consistent with being a M4 dwarf). We also determine the minimum mass of the sub-stellar companion to be M_p sin i = 1.60 \pm 0.13 M_Jup., Comment: A&A in press, 5 pages with 4 figures

We present the first direct distance determination to a detached eclipsing binary in M33, which was found by the DIRECT Project. Located in the OB 66 association at coordinates (alpha, delta)=(01:33:46.17,+30:44:39.9) for J2000.0, it was one of the most suitable detached eclipsing binaries found by DIRECT for distance determination, given its apparent magnitude and orbital period. We obtained follow-up BV time series photometry, JHKs photometry and optical spectroscopy from which we determined the parameters of the system. It contains two O7 main sequence stars with masses of 33.4+/-3.5 Mo and 30.0+/-3.3 Mo and radii of 12.3+/-0.4 Ro and 8.8+/-0.3 Ro, respectively. We derive temperatures of 37000+/-1500 K and 35600+/-1500 K. Using BVRJHKs photometry for the flux calibration, we obtain a distance modulus of 24.92+/-0.12 mag (964+/-54 kpc), which is ~0.3 mag longer than the Key Project distance to M33. We discuss the implications of our result and the importance of establishing M33 as an independent rung on the cosmological distance ladder., Comment: 36 pages, 12 figures, accepted for publication in ApJ

We report spectroscopic and interferometric observations of the high-proper motion double-lined binary system HD 9939, with an orbital period of approximately 25 days. By combining our radial-velocity and visibility measurements we estimate the system physical orbit and derive dynamical masses for the components of $M_A = 1.072 \pm 0.014$ M$_{\sun}$ and $M_B = 0.8383 \pm 0.0081$ M$_{\sun}$; fractional errors of 1.3% and 1.0%, respectively. We also determine a system distance of $42.23 \pm 0.21$ pc, corresponding to an orbital parallax of $\pi_{\rm orb} = 23.68 \pm 0.12$ mas. The system distance and the estimated brightness difference between the stars in $V$, $H$, and $K$ yield component absolute magnitudes in these bands. By spectroscopic analysis and spectral energy distribution modeling we also estimate the component effective temperatures and luminosities as $T_{\rm eff}^A = 5050 \pm 100$ K and $T_{\rm eff}^B = 4950 \pm 200$ K and $L_A$ = 2.451 $\pm$ 0.041 $L_{\sun}$ and $L_B$ = 0.424 $\pm$ 0.023 $L_{\sun}$. Both our spectral analysis and comparison with stellar models suggest that HD 9939 has elemental abundances near solar values. Further, comparison with stellar models suggests the HD 9939 primary has evolved off the main sequence and appears to be traversing the Hertzsprung gap as it approaches the red giant phase of its evolution. Our measurements of the primary properties provide new empirical constraints on stellar models during this particularly dynamic evolutionary phase. That HD 9939 is currently in a relatively short-lived evolutionary state allows us to estimate the system age as 9.12 $\pm$ 0.25 Gyr. In turn the age and abundance of the system place a potentially interesting, if anecdotal, constraint on star formation in the galactic disk., Comment: 19 pages, 6 figures, ApJ in press; tables 1 and 3 to appear in ApJ on-line version