Concerns regarding global warming have increased the pressure on automobile manufacturers to decrease emissions of CO2 from vehicles. Diesel vehicles have higher fuel economy and lower CO2 emissions than their gasoline counterparts. Increased penetration of diesel powered vehicles into the market is a possible transition strategy toward a more sustainable transportation system. To facilitate discussions regarding the relative merits of diesel vehicles it is important to have a clear understanding of their CO2 emission benefits. Based on European diesel and gasoline certification data, this report quantifies such CO2 reduction opportunities for cars and light duty trucks in today's vehicles and those in the year 2015. Overall, on a well-to-wheels per vehicle per mile basis, the CO2 reduction opportunity for today's vehicles is approximately 24-33%. We anticipate that the gap between diesel and gasoline well-to-wheel vehicle CO2 emissions will decrease to approximately 14-27% by the year 2015.

The black hole candidate Cygnus X-1 was observed in the hard X ray - soft γ ray energy range by the MISO telescope on two different occasions: in September 1979 and May 1980. We have measured two hard X-ray states of the source: in 1979 the observed spectrum confirms the superlow state measured in the same period by the HEAO-3 satellite, while in 1980 the MISO X-ray data are consistent with the so called low state of Cygnus X-1. In both occasions, no γ -ray excess has been observed above 200 KeV.

view Abstract Citations (14) References (36) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS A Broad-Band Contemporaneous Study of the Seyfert Galaxy NGC 4151 Bassani, L. ; Butler, R. C. ; Di Cocco, G. ; Della Ventura, A. ; Perotti, F. ; Villa, G. ; Baker, R. E. ; Dean, A. J. ; Lee, T. J. Abstract The authors observed the Seyfert galaxy NGC 4151 on 1980 May 18 at hard X-ray/low gamma-ray energies using the MISO telescope. No gamma-ray signal was found between 100 keV and 16 MeV and only a 3.5 σ signal was detected in the hard X-ray detector in the energy range 35 - 105 keV. Concurrently with this measurement, a program of ultraviolet and infrared observations was organized. Contemporaneous observations are also available in the optical and soft X-ray (2 - 10 keV) spectral regions. These observations are used to discuss the spectrum and the variability of NGC 4151 over a wide range of frequencies. Publication: The Astrophysical Journal Pub Date: December 1986 DOI: 10.1086/164802 Bibcode: 1986ApJ...311..623B Keywords: Astronomical Spectroscopy; Gamma Ray Spectra; Infrared Spectra; Seyfert Galaxies; Ultraviolet Spectra; X Ray Spectra; Luminosity; Radiant Flux Density; Visible Spectrum; Astrophysics; GALAXIES: INDIVIDUAL NGC NUMBER: NGC 4151; GALAXIES: SEYFERT; GAMMA RAYS: GENERAL; INFRARED: SOURCES; ULTRAVIOLET: SPECTRA; X-RAYS: SOURCES full text sources ADS | data products SIMBAD (1) NED (1) MAST (1) INES (1)

There is a clinical impression among physicians that puberty may prompt growth of hemangiomas. We observed significant growth of a large cavernous hemangioma in a patient at the onset of puberty despite absent estrogen and progesterone receptors in the hemangioma tissue.

A balloon-borne hard X-ray telescope is described that has been designed to make highly sensitive observations of cosmic sources in the energy range 15 to 300 keV. The payload is characterized by a combination of NaI(Tl) based detector of a novel design and spectroscopic proportional counters, providing a total sensitive area of 5000 cm2 and a 1 standard deviation sensitivity at the level of about 4 × 10−6 photons cm−2 s−1 keV−1. All of the telescope sub-systems are described including the micro-processor based orientation platform that provides a pointing stability of better than 10 arc min. The physical characteristics of the detectors are included along with a summary of the telescope performance during a balloon flight in 1982.

The MISO telescope is a gamma-ray detector operating in the (0.1÷20) MeV energy range. This instrument was flown success-fully from Palestine, Texas (U.S.A.) in May 1977, October 1978, September 1979 and May 1980. During the four flights, the telescope observed a number of galactic and extragalactic sources. The Crab Nebula was detected in 1980 and its spectrum was measured up to 2 MeV. Cygnus X-1 was observed in 1979 and 1980 and was found to be in different hard X-ray states on each occasion: in a superlow state in 1979 and in a low state in 1980. The COS-B high-energy (E>50 MeV) gamma-ray sources CG 135+1 (1978) and CG 195+4 (1978) were also observed by the same instrument. From the region containing CG 135+1 a 5σ excess was measured in the counting rate of the telescope above 120 keV. No statistically significant low-energy gamma-ray flux was detected from CG 195+4. The Seyfert galaxies NCG 4151 (1977, 1979, 1980), and MCG 8-11-11 (1979), the BL LAC object MK 501 (1979) and the «peculiar» galaxy NGC 1275 (1979) were also searched for gamma-ray emission. The data on NGC 4151 and MCG 8-11-11 are consistent with power law spectra having photon indices α∼1 in the (0.1÷3) MeV energy range. Above this energy, the MISO and SAS-2/COS-B measurements require spectral breaks to α≥3. Upper limits were obtained on the emission from both MK 501 and NGC 1275.

A large area (6000 cm2) actively shielded low energy gamma-ray telescope is going to be built by an Anglo-Italian collaboration. The telescope, named ZEBRA, will be capable of producing images of the X and gamma ray sky in the energy range 0.015–20 MeV with an intrinsic angular resolution of a few tenths of a degree. A prototype detector has been built in order to experimentally study the main characteristics of the detection plane. The preliminary results obtained during a balloon flight from Trapani, Sicily in July 1981 are presented.

During a balloon flight of the MISO telescope on 1980 May 17, the Crab Nebula and the Seyfert galaxy NGC 4151 were studied over the photon energy range 0.03 –16 MeV. The photon spectrum of the Crab Nebula was measured up to ∼ 2 MeV. No gamma-ray emission from NGC 4151 was detected on this occasion.

Rhodamine-conjugated antibodies specific for phenylalanine hydroxylase and serum albumin were employed as cytochemical probes to identify these two proteins in H4 hepatoma cells and in isolated rat hepatocytes. Each fluorescent antibody stained the cells specifically and in a distinctive manner. In both cell types, albumin staining was discretely localized in cytoplasmic and in H4 cultures varied somewhat from cell to cell. Evidence from cultures of REB15 cells, a strain derived by cloning H4 cells in tyrosine-free medium, suggested that the staining variability of H4 cells could reflect a variability in phenylalanine hydroxylase content. Hydrocortisone-treated H4 cells and REB15 cultures contain increased amounts of phenylalanine hydroxylase; and all cells in the culture appear to be induced by the hormone. Evidence was presented to show that the albumin visualized within the isolated hepatocytes had been synthesized by these cells, and, furthermore, that quantitatively nearly all intracellular albumin in the isolated rat hepatocytes appeared to be entrained in the secretion pathway (analogous data already exist for H4 cells [Baker, R.E., and R. Shiman. 1979. J. Biol. Chem. 254:9633-9639]). By scoring specific fluorescence, 86 and 98% of the H4 cells and 89 and 98% of the isolated hepatocytes were found to contain phenylalanine hydroxylase and albumin, respectively. Therefore, almost all cells in each population appeared to synthesize both proteins. An implication of these findings is that in rat virtually all liver parenchymal cells must synthesize both phenylalanine hydroxylase and albumin.

A substantially new method has been developed to measure protein turnover. Its basis is the notion that in labeling experiments a secreted protein can be used to determine the specific radioactivity of the intracellular amino acid precursor pool. To measure protein turnover in the Reuber hepatoma H4 cell line, cultures were labeled with [3H]leucine for specified periods after which phenylalanine hydroxylase was isolated and its leucine specific radioactivity determined. Serum albumin secreted by the cultures was also isolated and used to estimate the leucine precursor pool specific radioactivity. The protein half-life of phenylalanine hydroxylase could them be calculated. Experiments performed at long and short labeling times and with high and low concentrations of leucine in the medium yielded equivalent results. Phenylalanine hydroxylase half-life in the H4 cells was investigated under both normal and hydrocortisone-induced growth conditions. Average half-lives of 7.4 and 8.2 h were found for induced and uninduced cultures, respectively. Although these measured enzyme half-lives were not essentially different, the steady state level of phenylalanine hydroxylase was increased 6.2-fold upon hydrocortisone induction, from 0.076 to 0.47 microgram/10(6) cells. The results demonstrated that hydrocortisone induces phenylalanine hydroxylase in the H4 cells by causing an increase in the rate of enzyme synthesis.

Following the first detection of X-ray emission from the Seyfert galaxy NGC41511, later observations2–4 have demonstrated that the X-ray spectrum up to 100 keV may be described by a power law having a differential spectral index 1<α<1.6 with a turnover at low energies caused by photoelectric absorption. Recently the results of an observation of this galaxy in the energy range 25–190 keV (ref. 5) have shown it to have a very hard spectrum with α≅0.9. Here more detailed results of the original observation of NGC4151 (ref. 6) using the MISO telescope are presented.

OBSERVATIONS of the Seyfert galaxy NGC4151 by Ariel V, OSOI VII and UCSD (refs 1–3 respectively) have demonstrated that it has a relatively flat X-ray spectrum up to photon energies greater than 100 keV. The X-ray luminosity of this object is of the order of 4 × 1043 erg s−1 if a distance of 20 Mpc is assumed, and exceeds the integrated luminosity at all the other observed greater wavelengths. Long-term observations4 by Ariel V indicate that the X-ray emission may originate from a compact object with dimensions less than 8 × 1015 cm, presumably the nucleus of the Galaxy. Here we present the preliminary results of a positive measurement in the low energy γ-ray region of the spectrum, which are in good agreement with the X-ray data and confirm the intense high energy luminosity of the object.

As part of a study of techniques for γ-ray astronomy in the MeV energy range, several balloon payloads have been launched by the Southampton University group from Palestine, Texas. The following results are from a payload launched on September 23, 1972, which floated at a depth of 8 g cm−2 for 7 h from 0600 GMT. The payload consisted of an anticollimation telescope using two 12 cm by 5 cm NaI(Tl) crystals side by side, each viewed by a single 12 cm phot omul tiplier and protected from charged particles by a plastic scintillator box. These detectors were made directional for low energy γ rays by a lead occulting disk, 18 cm in diameter and 10 cm thick, placed 50 cm above the crystals, the axis of the whole assembly being pointed so as to track a celestial source continuously. The occulting disk alternated between positions over each detector at intervals of 5 min. In-flight energy calibration was carried out using a 223Th γ-ray source. In addition to the γ-ray detectors, the payload contained a thin NaI(Tl) detector sensitive to 100 keV X rays. The null results obtained on some celestial sources indicating that the movement of the lead disk did not, by itself, affect the counting rate of a detector.

ABSTRACT A simple and quantitative procedure for the extraction and measurement of total urinary radioactive steroid metabolites is described. The urinary excretion of topically applied 14C oestrone + 3H 17β-oestradiol and of 14C cortisol (11β, 17, 21-trihydroxy-pregn-4-ene-3, 20-dione) alone was studied with and without the addition of carrier oestrone, in both premenopausal and postmenopausal women. Over 80 percent of the cortisol, 7.5 to 41 percent of the oestrone, and 3.4 to 20 percent of the 17β-oestradiol metabolites appeared in the urine within 72 hours. Neither the ovarian status of the subjects nor the presence of carrier oestrone appeared to influence these results.

The in vitro distribution of C-14 and H-3 labelled estrone, estradiol-17β and estriol between the erythrocytes and serum of horse blood has been studied over concentrations ranging from 0.0001 to 1,000 µg./ml. 30.2 ± 1.1% of estrone radioactivity, 20.7 ± 2.7 of estradiol-17β radioactivity and 37.3 ± 3.0% of estriol radioactivity was associated with the erythrocytes at a 50% hematocrit. The distributions were independent of concentration and equilibrium was achieved in less than one hour.