Utilization of Biogas for Farm Production Energy

Williams, David W.; McCarty, Thomas R.; Morris, G. R.; Gunkel, W. W.; Price, D.

doi:10.13031/2013.36170

Cited by 69 publications

(85 citation statements)

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“…The GASS brightness temperature scale may also be compared with calibrations at IAU standard position S8 (Williams 1973) as determined by Kalberla et al (1982) for the Effelsberg telescope. For the S8 line integral within the velocity range −5.1 < v lsr < 22.3 km s −1 , we obtain W GASS III /W Eff = 1.033 ± 0.005.…”

Section: Comparison With Other Telescopesmentioning

confidence: 99%

GASS: The Parkes Galactic All-Sky Survey

Kalberla

Haud

2015

A&A

139

148

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Context. The Galactic All-Sky Survey (GASS) is a survey of Galactic atomic hydrogen (H i) emission in the southern sky observed with the Parkes 64-m Radio Telescope. The first data release (GASS I) concerned survey goals and observing techniques, the second release (GASS II) focused on stray radiation and instrumental corrections. Aims. We seek to remove the remaining instrumental effects and present a third data release. Methods. We use the HEALPix tessellation concept to grid the data on the sphere. Individual telescope records are compared with averages on the nearest grid position for significant deviations. All averages are also decomposed into Gaussian components with the aim of segregating unacceptable solutions. Improved priors are used for an iterative baseline fitting and cleaning. In the last step we generate 3D FITS data cubes and examine them for remaining problems. Results. We have removed weak, but systematic baseline offsets with an improved baseline fitting algorithm. We have unraveled correlator failures that cause time dependent oscillations; errors cause stripes in the scanning direction. The remaining problems from radio frequency interference (RFI) are spotted. Classifying the severeness of instrumental errors for each individual telescope record (dump) allows us to exclude bad data from averages. We derive parameters that allow us to discard dumps without compromising the noise of the resulting data products too much. All steps are reiterated several times: in each case, we check the Gaussian parameters for remaining problems and inspect 3D FITS data cubes visually. We find that in total ∼1.5% of the telescope dumps need to be discarded in addition to ∼0.5% of the spectral channels that were excluded in GASS II. Conclusions. The new data release (GASS III) facilitates data products with improved quality. A new web interface, compatible with the previous version, is available for download of GASS III FITS cubes and spectra.

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Section: Comparison With Other Telescopesmentioning

confidence: 99%

GASS: The Parkes Galactic All-Sky Survey

Kalberla

Haud

2015

A&A

139

148

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“…Information on large structures, corresponding to baselines shorter than about 100j, was provided from a fully sampled observation of an area of 4¡ ] 4¡ surrounding DA 530 made with the DRAO 26 m Telescope and using velocity coverage and spectrometer resolution identical to those used on the Synthesis Telescope. The single-antenna data were calibrated against the standard region S7 (Williams 1973). The two data sets were combined after appropriate spatial Ðltering, with overlap from 33j to 71j and equal weight at 52j.…”

Section: Radio Observationsmentioning

confidence: 99%

DA 530: A Supernova Remnant in a Stellar Wind Bubble

Landecker

Routledge

Reynolds

et al. 1999

ApJ

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The high-latitude supernova remnant (SNR) DA 530 (G93.3]6.9), apparently a typical shell remnant, has highly polarized radio continuum emission and a very uniform circumferential magnetic Ðeld. We present new radio continuum (408 and 1420 MHz) and H I line observations, made with the Dominion Radio Astrophysical Observatory Synthesis Telescope, and we have made the Ðrst detection of X-ray emission from the SNR, using the ROSAT Position-Sensitive Proportional Counter. The SNR lies within a shell of H I, possibly created by an earlier stellar wind, whose kinematic distance is nominally 2.5 kpc but whose actual distance may be larger. The X-ray emission is extremely faint. A Raymond-Smith ionization-equilibrium model Ðts the data and suggests a very low density, D0.05 cm~3, consistent with the occurrence of the supernova in a stellar wind cavity, but this model yields an explosion energy 100 times lower than the accepted value. A nonequilibrium shock model, incorporating a range of ionization timescales, is able to give more realistic physical parameters for the supernova remnant. On the balance of the evidence, we place DA 530 at a distance of 3.5 kpc, the largest distance permitted by the H I observations, where it lies 420 pc above the Galactic plane. The explosion, probably a Type Ia supernova, in a low-density cavity has resulted in weak X-ray emission and slow evolution. The explosion energy was 3.9 ] 1050 ergs and the age is D5000 years. The remnant, having swept up 3.9in an M _ ambient density of D0.01 cm~3, is only now in the adiabatic phase, and this explains the absence of detected optical emission. Despite the low ambient density the efficiency of generation of synchrotron radio emission is D0.4%, higher than in some historical SNRs. The ratio of radio to X-ray Ñux is about 100 times that for the remnant of SN 1006, which has comparable radio continuum properties. The very uniform magnetic Ðeld is not explained. DA 530 joins a small group of remnants at high Galactic latitude with unusual features, perhaps resulting from low ambient densities. Inhomogeneous nonequilibrium ionization models may be required for the interpretation of the X-ray emission from many other older SNRs.

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“…1) Williams, Mullikin & Lefkowitz, 1976;Davis, Strittmatter, Hoyler & Lefkowitz, 1977;) and a two-site model of the a-receptor has been proposed (Peroutka, Greenberg, U'Prichard & Snyder, 1978). There is also evidence that [aH]dihydroergokryptine labels dopamine receptors (Tittler, Weinreich & Seeman, 1977).…”

Section: Introductionmentioning

confidence: 99%