Search

Data are presented on single particle distributions from the inclusive reactions π+p⇒π+… and π+p⇒p+… carried out at 10.0 and 15.5 GeV/c. All four pion charge combinations were studied at both energies. Data are available for x≥0 and for transverse momenta up to 0.9 GeV/c. Positive identification of final state particles was accomplished with a Cerenkov counter and time of flight system. Production angles and momentum were measured with spark chambers, proportional chamber and a large aperture magnet.

The NA34 (HELIOS) calorimeter has measured e/{pi} {congruent} 1.1 in a uranium/liquid argon calorimeter with a shaping time of 135 nsec. Lead may be a viable alternative, but e/{pi} must first be measured at fast shaping times in lead. We re preparing to measure e/{pi} at momenta ranging from 0.5 to 20 GeV/c and with shaping times of 50, 100 and 150 nsec.

A search has been made for the 1(10)-- 1(11) transition of thioformaldehyde in interstellar clouds where formaldehyde is known to exist. Failure to detect this transition indicates that the ratio of thioformaldehyde abundance to that of formaldehyde is probably less than the abundance ratio of sulfur to oxygen.

THE existence of a large number of discrete sources of extraterrestrial radio radiation (radio stars) has now been established. For the majority of the sources there is no information about their distance; only a few have been identified with celestial objects observed photographically. Attempts to measure the radio parallax of the sources have been made by Ryle1, Mills and Thomas2 and Smith3. These experiments failed to measure any parallax and could only establish that the radio stars were at a distance greater than ½ parsec. The present communication describes a new method for the measurement of the distance of radio stars in the Galaxy, and gives preliminary results for the two intense sources in Cygnus and Cassiopeia.

High-resolution ground-based measurements have been made of the J = 0 → 1 and the J = 1 → 2 rotational transitions of carbon monoxide in the earth’s atmosphere. These transitions, which occur at frequencies near 115 and 230 GHz, were observed in absorption against the solar continuum. The two absorption profiles have been used to derive the CO mixing ratio as a function of altitude between 50 and 80 km in the atmosphere.

We report observations of the J=2..-->..1 and J=1..-->..0 rotational transitions of carbon monoxide in eight molecular clouds, including several dark clouds. For each of these eight sources, the 2..-->..1 and 1..-->..0 line profiles and intensities are strikingly similar. This similarity is predicted by cloud models in which the CO line widths are produced primarily by radial collapse or other large-scale motions within the clouds, but is not easily explained by models in which the line widths result from turbulence on a scale small compared with the photon mean free paths.

Observations of the J=2-1 and J=1-0 rotational transitions of /sup 12/CO, /sup 13/CO, and C/sup 18/O are reported for 10 molecular clouds. An analysis of the data based on a large-velocity-gradient cloud model suggests that in most of these sources the average molecular hydrogen densities lie between 2000 and 8000 cm/sup -3/, while /sup 13/CO fractional abundances are approximately 3 x 10/sup -6/. These hydrogen densities are typically a factor of 10 lower than those inferred from observations of other molecules such as HCN, CS, or H/sub 2/CO; possible explanations for this discrepancy are discussed.

ALTHOUGH aneurysm of the splenic artery has been known for some 100 to 110 years, its occurrence is so uncommon that no one surgeon's experience with the lesion can be wide. The autopsy incidence has been reported between 0.02% (4 in 19,300 autopsies — Schroetter) and 0.2% (7 in 3,108 autopsies — Bosdorf). 1 Yet the lesion is of great significance, as evidenced by the fact that until 1942, of 124 reported cases, there had been but 20 survivals. 8 It is also estimated that about onethird of all splenic aneurysms will rupture in time if left untreated. 1 On this account, it would seem wise that cases be reported so that everyone may be as familiar as possible with the condition and the problems of its surgical therapy. In addition to presenting one case of large aneurysm of the splenic artery, we feel that the principle of dissecting in

There have been numerous case reports and discussions of jejunogastric intussusception following gastroenterostomy since the first mention by Bozzi 11 in 1914. However, it is not so well known that jejunogastric intussusception may occur after subtotal gastrectomy. Lundberg 32 was apparently the first to report such a case in 1922. A review of essential features of 28 cases reported by 25 authors through 1958 strongly suggests that unfamiliarity with this rare complication of gastrectomy was the cause of delay in instituting proper therapy in many instances. Several references to retrograde jejunogastric intussusception after gastrectomy were not available to us but are appended for the sake of completeness.* The term retrograde intussusception was introduced by John Hunter 27 in 1789, and may be defined as an intussusception in which the intussusceptum invaginates in a cephalad direction rather than in the caudad direction which is commoner. It is interesting that in the

WE would like to confirm Weinreb, Barrett, Meeks and Henry's1 discovery of the hydroxyl (OH) radical in the interstellar medium at frequency 1667.36 Mc/s. Fig. 1. shows observations of the Sagittarius A source in the frequency range 1,667.672–1,667.210 Mc/s. These observations were made between December 2 and December 9, 1963, with the 33-ft. antenna at the Hat Creek Radio Astronomy Observatory of the University of California, Berkeley. We used a switched-frequency receiver in which the comparison channel was fixed at 1,669 Mc/s and the signal channel, of bandwidth 50 kc/s, was scanned over the spectrum at the rate of 0.93 Mc/s per hour. The output of the receiver was digitized. ‘Print-out’ occurred every 23.3 kc/s during the scan; this corresponds to an integration time of 90 sec per point. For the receiver used we found an excess system noise of 750° K. We may thus expect (and we find) a root mean square uncertainty of 0.7° K for a single readout. The mean error of a plotted point on the OH curve in Fig. 1 is ± 0.13° K. The plotted frequency profile represents the mean of 29 scans.