We have observed the center of the Local Group dwarf irregular galaxy IC 1613 with WFPC2 aboard the Hubble Space Telescope in the F439W, F555W, and F814W filters. We find a dominant old stellar population (aged ~7 Gyr), identifiable by the strong red giant branch (RGB) and red clump populations. From the (V-I) color of the RGB, we estimate a mean metallicity of the intermediate-age stellar population [Fe/H] = -1.38 +/- 0.31. We confirm a distance of 715 +/- 40 kpc using the I-magnitude of the RGB tip. The main-sequence luminosity function down to I ~25 provides evidence for a roughly constant SFR of approximately 0.00035 solar masses per year across the WFPC2 field of view (0.22 square kpc) during the past 250-350 Myr. Structure in the blue loop luminosity function implies that the SFR was ~50% higher 400-900 Myr ago than today. The mean heavy element abundance of these young stars is 1/10th solar. The best explanation for a red spur on the main-sequence at I = 24.7 is the blue horizontal branch component of a very old stellar population at the center of IC 1613. We have also imaged a broader area of IC 1613 using the 3.5-meter WIYN telescope under excellent seeing conditions. The AGB-star luminosity function is consistent with a period of continuous star formation over at least the age range 2-10 Gyr. We present an approximate age-metallicity relation for IC 1613, which appears similar to that of the Small Magellanic Cloud. We compare the Hess diagram of IC 1613 to similar data for three other Local Group dwarf galaxies, and find that it most closely resembles the nearby, transition-type dwarf galaxy Pegasus (DDO 216).Comment: To appear in the September 1999 Astronomical Journal. LaTeX, uses AASTeX v4.0, emulateapj style file, 19 pages, 12 postscript figures, 2 tables. 5 of the figures available separately via the WW

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A significant minority of Louisiana students in grades 6 through 12-15.9 percent--acknowledged gambling-related symptoms and life problems. The association of problem and pathological gambling with use of alcohol, tobacco, and marijuana provides preliminary support for the inclusion of gambling among other adolescent risk behaviors.

A substantial portion of gamblers in treatment may have co-occurring mental health disorders including substance use disorders, especially alcohol dependency, personality disorders, affective disorders, anxiety disorders and impulse control disorders. Co-occurring mental health disorders affect treatment seeking, the treatment process and its outcome, quality of life and functioning in many mental health disorders. Participants in this study were 78 adults enrolled in state-supported out-patient services for pathological gambling and current Gamblers Anonymous attendees. The majority of participants (76.6%) had co-occurring behaviours; 55.8% had multiple co-occurring behaviours. Participants with multiple co-occurring behaviours were more likely to report that a co-occurring behaviour increased the severity of their gambling symptoms. A dose/response relationship between number of co-occurring behaviours and severity of gambling problems was found. Co-occurring behaviours can interact with gambling behaviour. Brief, validated screening instruments are available for screening and diagnosing co-occurring behaviours among gamblers presenting for treatment.

Broad-band photoelectric measurements on nine nights between 1969 February and 1970 February show constant intensity and colors for the pulsar of V = 16.5, B-V = +o.5, U-B =-0.45, and V-R =-0.75, with an accuracy of 10-15 percent in each passband. The ratio of the intensity in the main pulse to that in the subpulse is about 1.8 in each color, with the same accuracy. In the passband >.>.3800-6000, the pulsar intensity repeated within 3 percent on nights 2 months apart. Measurements of linear polarization on four nights in 1969 February, August, and October show repeatable behavior, with the amount of polarization changing smoothly through the pulse from at least 25 percent to near zero and the plane of polarization sweeping through 150° during 60° of the pulsar's rotation. The time behavior was similar in the main pulse and the subpulse. The discontinuous change of the pulsar's period in 1969 September had no discernible effect upcm the intensity, colors, or polarization of the pulses. It is argued that the observed pulses are due to a :fix¢d, polarized emission pattern which is azimuthally scanned as the object rotates, and the sweep of the plane of polarization is interpreted in terms of a very general geometrical model. If the model is valid, then the projection of the rotation axis of the pulsar on the plane of the sky is found directly from the data, with an ambiguity of 90°, and is either parallel or orthogonal to the integrated magnetic field of the nebula within 20" of the pulsar. This agreement between the angles of the rotation axis and the magnetic field of the nebula seems too close to be accidental, and implies that the external field, at least in the vicinity of the pulsar, was produced by the pulsar at some stage in its history.

The optical flux of Seo X-1 was continuously monitored on five separate nights between April and June 1967. Pulse counting was used with sampling intervals of 5 sec on the 100-and 200-inch telescopes and 15 sec on the 60-inch reflector. The error due to photon statistics per sample interval was smaller than 0.007 mag in all cases. The data were processed entirely by computer, using a variety of special digital techniques.Rapid optical flickering with amplitudes of "'0.02 mag on a time scale of minutes was found on all five nights. These high-frequency fluctuations are superposed on slower continuous variations with amplitudes "-'0.15 mag, and on occasional bursts of 0.2 mag which last about 10 min with very short rise and decay times.Radial velocities have been measured by a digital method of cross-correlation of microphotometer records of the original photographic plates (Westphal 1966). Velocity changes of about 100 km sec-1 were found on two different singly trailed plates, each of 3 hours' duration. The hydrogen lines and He II (A4686) change in opposite directions, similar to the extar Cyg X-2, suggesting, but not proving, binary motion. Systematic changes of velocity from night to night are set out in Table 2.The distance to Seo X-1 is estimated to be D c..' 500 pc by three methods, based on the strength of interstellar Ca II K, and on the old nova hypothesis. A firm lower limit of D 2 300 pc seems well established. The total X-ray power is c..'2 X 1(}'!7 h 2 ergs sec 1 , where his the distance in units of 500 pc. If the Xray energy is due to bremsstrahlung, this level requires Seo X-1 to continuously pump energy into the hot plasma, replenishing the entire energy store of gas in the cooling time of tc = 3 X 10-10 h-1 R 312 sec where R is the radius (in centimeters) of the plasma system. Reasonable values of 10 11 cm < R < 10 12 cm give 100 h-1 < t. < 3000 h-1 sec, which, remarkably, is the characteristic time of the light flicker.Mechanical energy due to some type of low-Q oscillation of the system, similar in many respects to that observed in the Sun, seems capable of providing 10 37 ergs sec 1 to the plasma gas. The crucial experiment remains to simultaneously monitor the optical and the X-ray flux over periods of several hours. Detailed correlation of fluctuations is not expected, but the mean X-ray flux might plausibly be expected to vary in periods of fractions of an hour as the mean amplitude of the optical fluctuations changes.

Either supportive counseling (SC) or cognitive training (CT) was used in an attempt to enhance the efficiency of a standard pharmacologic treatment for dementia, viz, dihydroergotoxine mesylate (DEM, Hydergine). DEM was administered orally to 21 moderately demented subjects, in a dosage of 1 mg three times daily; and SC or CT was conducted for one hour every two weeks for a total of 12 weeks. The CT was designed to enhance memory and other intellectual functions by the teaching of organizational schemes and mnemonic devices. Outcome measurements included the Sandoz Clinical Assessment-Geriatric (SCAG), a behavioral rating scale measuring selected symptoms and signs of dementia; the Hamilton Rating Scale for Depression (HRSD); and the Buschke Selective Reminding Scale (BSRT), a psychometric test of memory and learning. The DEM + CT group of patients improved more than did the DEM + SC group for the measures of memory and learning (BSRT). However, no differences between groups were noted for the HRSD or SCAG behavioral measures.

Background Studies of clinical trials across the field of healthcare found use of designs that overestimate treatment effects. Objective review clinical trial designs used to develop gambling treatment evidence base for suitability to assess cause and effect and to accurately assess treatment effects. Methods literature review, grading of evidence, proportions and confidence limits Results The majority of published studies on gambling treatment are methodologically unsuited to determine treatment effects. Suitable (randomized and controlled) trails often use designs that can overestimate treatment effects. Attrition in published studies of gambling treatment is substantial, ranging from 11 to 83%. If attrition is not included in the analysis, overestimation of treatment effects may be similar in magnitude. Conclusions The current evidence may overestimate gambling treatment effects. The inclusion of intention to treat analysis, careful blinding, more equivalent control groups and measures of adherence to treatment would improve problem gambling treatment clinical trial design.