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Objective: To determine if dopamine (D3) receptor genotypes are associated with anovulation and response to ovulation induction with clomiphene citrate., Design: Clinical and laboratory characteristics of anovulatory patients and ovulatory controls were compared with findings at the DNA level., Setting: An outpatient clinic at an university medical center., Patients: One hundred eighty human Hispanic female volunteers (130 of these with documented ovulatory status) were studied., Interventions: Genomic DNAs were extracted from each patient. Polymerase chain reaction with subsequent restriction digest was performed to analyze the D3 receptor allele status (two possible alleles)., Main Outcome Measures: Menstrual history, serum T, and midluteal serum Ps from spontaneous and clomiphene cycles were correlated with D3 receptor genotype., Results: Hispanic females with the 22 genotype compared with the other genotypes (11 and 12) were more likely to have irregular menses, an elevated serum T (> or = 70 ng/dL [conversion factor to SI unit, 3.467]), and hyperandrogenic chronic anovulation. These patients tended to be resistant to ovulation induction requiring a significantly higher dose of clomiphene to achieve an ovulatory response (22 genotype [mean +/- SEM] [140.0 +/- 19.0 mg] versus 11 [77.1 +/- 17.5 mg] or 12 [69.2 +/- 13.1 mg]). This effect was independent of patient age, weight, or serum T level., Conclusions: Hyperandrogenic chronic anovulation may have a genetic component. Genetic analysis may be useful in predicting resistance to ovulation induction with clomiphene.

Indolamine 2,3-dioxygenase and tryptophan 2,3-dioxygenase are two enzymes that degrade tryptophan to N-formylkynurenine. The gene (TDO2) for tryptophane 2,3-dioxygenase has been localized to 4q31-->32. We now report localization of INDO (the gene encoding indolamine 2,3-dioxygenase) by fluorescent in situ hybridization to 8p12-->p11.

The first unambiguous full-disk radar mapping of Mercury at 3.5-centimeter wavelength, with the Goldstone 70-meter antenna transmitting and 26 antennas of the Very Large Array receiving, has provided evidence for the presence of polar ice. The radar experiments, conducted on 8 and 23 August 1991, were designed to image the half of Mercury not photographed by Mariner 10. The orbital geometry allowed viewing beyond the north pole of Mercury; a highly reflective region was clearly visible on the north pole during both experiments. This polar region has areas in which the circular polarization ratio (pt) was 1.0 to 1.4; values < approximately 0.1 are typical for terrestrial planets. Such high values of have hitherto been observed in radar observations only from icy regions of Mars and icy outer planet satellites.

Full disk images of Mars have been obtained with the use of the Very Large Array (VLA) to map the radar reflected flux density. The transmitter system was the 70-m antenna of the Deep Space Network at Goldstone, California. The surface of Mars was illuminated with continuous wave radiation at a wavelength of 3,5 cm. The reflected energy was mapped in individual 12-minute snapshots with the VLA in its largest configuration; fringe spacings as small as 67 km were obtained. The images reveal near-surface features including a region in the Tharsis volcano area, over 2000 km in east-west extent, that displayed no echo to the very low level of the radar system noise. The feature, called Stealth, is interpreted as a deposit of dust or ash with a density less than about 0.5 gram per cubic centimeter and free of rocks larger than 1 cm across. The deposit must be several meters thick and may be much deeper. The strongest reflecting geological feature was the south polar ice cap, which was reduced in size to the residual south polar ice cap at the season of observation. The cap image is interpreted as arising from nearly pure CO(2) or H(2)O ice with a small amount of martian dust (less than 2 percent by volume) and a depth greater than 2 to 5 m. Only one anomalous reflecting feature was identified outside of the Tharsis region, although the Elysium region was poorly sampled in this experiment and the north pole was not visible from Earth.

A human tryptophan oxygenase clone was isolated by screening a liver cDNA library with a rat tryptophan oxygenase cDNA clone. Analysis showed extensive homology between the rat and the human DNA and protein sequences. The combined use of cell hybrids and in situ hydridization indicated that human tryptophan oxygenase was localized to chromosome band 4q31. The tryptophan oxygenase gene may be important in some human behavior disorders, especially those associated with abnormalities of serotonin metabolism.

The present understanding of the atmosphere and surface conditions on Saturn's largest moon, Titan, including the stability of methane, and an application of thermodynamics leads to a strong prediction of liquid hydrocarbons in an ethane-methane mixture on the surface. Such a surface would have nearly unique microwave reflection properties due to the low dielectric constant. Attempts were made to obtain reflections at a wavelength of 3.5 centimeters by means of a 70-meter antenna in California as the transmitter and the Very Large Array in New Mexico as the receiving instrument. Statistically significant echoes were obtained that show Titan is not covered with a deep, global ocean of ethane, as previously thought. The experiment yielded radar cross sections normalized by the Titan disk of 0.38 +/- 0.15, 0.78 +/- 0.15, and 0.25 +/- 0.15 on three consecutive nights during which the sub-Earth longitude on Titan moved 50 degrees. The result for the combined data for the entire experiment is 0.35 +/- 0.08. The cross sections are very high, most consistent with those of the Galilean satellites; no evidence of the putative liquid ethane was seen in the reflection data. A global ocean as shallow as about 200 meters would have exhibited reflectivities smaller by an order of magnitude, and below the detection limit of the experiment. The measured emissivity at similar wavelengths of about 0.9 is somewhat inconsistent with the high reflectivity.

We observed the radio emission of Callisto with a three-element interferometer at the time of the 1973 opposition of Jupiter. Special care was taken to remove the residual, unresolved contribution from Jupiter itself in the antenna side lobes. The resulting disk temperature at a wavelength of 3.71 centimeters, assuming a radius of 2500+/-75 kilometers for Callisto, was 101 degrees +/-25 degrees K. This temperature is much more consistent with emission from a simple dielectric sphere than the considerably higher temnperatures that have been reported for wavelengths of 3.5 and 8.2 millimeters.

An analysis of high-resolution microwave images of Saturn and Saturn's individual rings is presented. Radio interferometric observations of Saturn taken at the Very Large Array in New Mexico at wavelengths of 2 and 6 centimeters reveal interesting new features in both the atmosphere and rings. The resulting maps show an increase in brightness temperature of about 3 K from equator to pole at both wavelengths, while the 6-centimeter map shows a bright band at northern mid-latitudes. The data are consistent with a radiative transfer model of the atmosphere that constrains the well-mixed, fully saturated, NH(3) mixing ratio to be 1.2 x 10(-4) in a region just below the NH(3) clouds, while the observed bright band indicates a 25 percent relative decrease of NH(3) in northern mid-latitudes. Brightness temperatures for the classical rings are presented. Ring brightness shows a variation with azimuth and is linearly polarized at an average value of about 5 percent. The variations in ring polarization suggest that at least 20 percent of the ring brightness is the result of a single scattering process.

The ratio of the flux density of Titan was measured in two 200-megahertz bands, one centered on the (1-0) rotation line of carbon monoxide at 115.3 gigahertz and the other 2600 megahertz lower. The measurements were made with a complex-correlation technique on the new millimeter-wavelength interferometer at the Owens Valley Radio Observatory, Big Pine, California. The excess flux in the carbon monoxide band is interpreted as a strong detection of carbon monoxide and a mixing ratio, assumed constant, of 6 x 10(-5). The brightness temperature of Titan at 112.6 gigahertz is 69 +/- 10 kelvins, consistent with atmospheric emission from just below the tropopause.

The radius of Venus has been determined from radar-range data taken at the Jet Propulsion Laboratory's Goldstone facility. A simultaneous intergration of the equations of motion of the solar-system fit to this time-delay data gave a value of 6053.7 +/- 2.2 kilometers. A discussion of other Venusian radius determinations is made.

During the period 13 August to 22 August, day-to-day determinaitions of the average orbital elements of the 100-foot Echo I balloon, based on observations taken at the Jet Propulsion Laboratory's Goldstone tracking station, indicated a decrease in perigee height of 3.0 km/day and an increase in the eccentricity of 0.00038 per day.