Determination of the Orientation of the Electric Axis for the East—West Array of the DKR-1000 Cruciform Radio Telescope by Statistical Reduction of Observations of Many Discrete Sources

1971 ◽  
pp. 139-141
Author(s):  
V. V. Vitkevich ◽  
V. N. Kozhukhov
Keyword(s):  
2002 ◽  
Vol 199 ◽  
pp. 25-31
Author(s):  
N. Udaya Shankar

The Mauritius Radio Telescope (MRT) is a Fourier synthesis instrument which has been built to fill the gap in the availability of deep sky surveys at low radio frequencies in the southern hemisphere. It is situated in the north-east of Mauritius at a southern latitude of 20°.14 and an eastern longitude of 57°.73. The aim of the survey with the MRT is to contribute to the database of southern sky sources in the declination range −70° ≤ δ ≤ −10°, covering the entire 24 hours of right ascension, with a resolution of 4' × 4'.6sec(δ + 20.14°) and a point source sensitivity of 200 mJy (3σ level) at 151.5 MHz.MRT is a T-shaped non-coplanar array consisting of a 2048 m long East-West arm and a 880 m long South arm. In the East-West arm 1024 fixed helices are arranged in 32 groups and in the South arm 16 trolleys, with four helices on each, which move on a rail are used. A 512 channel, 2-bit 3-level complex correlation receiver is used to measure the visibility function. At least 60 days of observing are required for obtaining the visibilities up to the 880 m spacing. The calibrated visibilities are transformed taking care of the non-coplanarity of the array to produce an image of the area of the sky under observation.This paper will describe the telescope, the observations carried out so far, a few interesting aspects of imaging with this non-coplanar array and present results of a low resolution survey (13' × 18') covering roughly 12 hours of right ascension, and also present an image with a resolution of 4' × 4'.6sec(δ + 20.14°) made using the telescope.


2020 ◽  
Vol 15 (4) ◽  
pp. 613-619
Author(s):  
Li Kong ◽  
Yunpeng Zhang ◽  
Zhijian Lin ◽  
Zhongzhu Qiu ◽  
Chunying Li ◽  
...  

Abstract The present work aimed to select the optimum solar tracking mode for parabolic trough concentrating collectors using numerical simulation. The current work involved: (1) the calculation of daily solar radiation on the Earth’s surface, (2) the comparison of annual direct solar radiation received under different tracking modes and (3) the determination of optimum tilt angle for the north-south tilt tracking mode. It was found that the order of solar radiation received in Shanghai under the available tracking modes was: dual-axis tracking > north-south Earth’s axis tracking > north-south tilt tracking (β = 15°) > north-south tilt tracking (β = 45) > north-south horizontal tracking > east-west horizontal tracking. Single-axis solar tracking modes feature simple structures and low cost. This study also found that the solar radiation received under the north-south tilt tracking mode was higher than that of the north-south Earth’s axis tracking mode in 7 out of 12 months. Therefore, the north-south tilt tracking mode was studied separately to determine the corresponding optimum tilt angles in Haikou, Lhasa, Shanghai, Beijing and Hohhot, respectively, which were shown as follows: 18.81°, 27.29°, 28.67°, 36.21° and 37.97°.


1967 ◽  
Vol 1 (2) ◽  
pp. 45-46
Author(s):  
D. G. Cole ◽  
R. F. Mullaly ◽  
A. Watkinson

During the period 1966 July 12 to August 5 observations were made of the Sun at three radio observatories. The instruments used were the east-west arm of the Mills cross at Molonglo (408 MHz) and the Christiansen cross at Fleurs (696 MHz and 1424 MHz). The aim of these observations was to study the discrete sources of the slowly varying component of solar radio emission, while activity was comparatively quiet. The three frequencies enabled the variation of source structure with height of solar atmosphere to be studied. It has been pointed out by Swarup et al., and Christiansen et al. that the determination of the frequency dependence of these discrete sources is important for defining the physical mechanisms causing the radio emission.


Author(s):  
Ruth María Grajeda-Rosado ◽  
Elia Mercedes Alonso-Guzman ◽  
Carlos Escobar-Del Pozo ◽  
Carlos Javier Esparza-Lopez

The complexity of the urban environment and its undeniable connection with the energy balance equation opens the doors for researchers to understand phenomena such as the Urban Heat Island (UHI). The least studied factor of the UHI is vehicular anthropogenic heat. Using Computational Fluid Dynamics (CFD) software, the aim is to understand the thermal environment within an urban canyon, based on two variables, the heat produced by the vehicle combustion engine and the orientation of the street (North - South and East -West). The analysis of the correlation of these variables is based on the information obtained from the simulation in different height strata, considering constant values such as direct radiation, diffuse radiation, emissivity and absorptivity of materials and a fixed temperature for the bonnet or hood of the car, altering the number of automotive vehicles and the orientation to examine the different patterns of the thermal profiles. The research opens the way to understand this phenomenon and be considered in simulations for the energy efficiency of buildings, since it directly impacts the facades of buildings and the determination of passive and active cooling techniques.


1967 ◽  
Vol 20 (6) ◽  
pp. 715 ◽  
Author(s):  
HM Tovmassian ◽  
IG Moiseev

From Abell's (1958) list of clusters of galaxies, 137 clusters of distance group 5 were observed at 1410 MHz with the 210 ft radio telescope of the Australian National Radio Astronomy Observatory at Parkes. The detected radio sources were further confirmed hy observations at 2650 MHz with the same telescope and at 408 MHz with the east-west arm of the Mills Cross at the Molonglo Radio Astronomical Observatory. A total of 25 radio sources was detected within 5' arc of the centres of corresponding clusters of galaxies, while the mathematical expectation of the number of random coincidences with clusters is about two or three


2018 ◽  
Vol 619 ◽  
pp. A127 ◽  
Author(s):  
N. Biver ◽  
D. Bockelée-Morvan ◽  
G. Paubert ◽  
R. Moreno ◽  
J. Crovisier ◽  
...  

We present a multi-wavelength study of comet C/2016 R2 (PanSTARRS). This comet was observed on 23 and 24 January 2018 with the IRAM 30 m telescope, and in January to March 2018 with the Nançay radio telescope. Visible spectroscopy was performed in December 2017 and February 2018 with small amateur telescopes. We report on measurements of CO, CH3OH, H2CO and HCN production rates, and on the determination of the N2/CO abundance ratio. Several other species, especially OH, were searched for but not detected. The inferred relative abundances, including upper limits for sulfur species, are compared to those measured in other comets at about the same heliocentric distance of ~2.8 AU. The coma composition of comet C/2016 R2 is very different from all other comets observed so far, being rich in N2 and CO and dust poor. This suggests that this comet might belong to a very rare group of comets formed beyond the N2 ice line. Alternatively, comet C/2016 R2 (PanSTARRS) could be the fragment of a large and differentiated transneptunian object, with properties characteristic of volatile-enriched layers.


2012 ◽  
Vol 29 (3) ◽  
pp. 262-268 ◽  
Author(s):  
A. J. Walsh ◽  
C. Purcell ◽  
S. Longmore ◽  
C. H. Jordan ◽  
V. Lowe

AbstractThe H2O Southern Galactic Plane Survey (HOPS) has observed 100 deg2 of the Galactic plane, using the Mopra radio telescope to search for emission from multiple spectral lines in the 12-mm band (19.5–27.5 GHz). Perhaps the most important of these spectral lines is the 22.2-GHz water-maser transition. We describe the methods used to identify water-maser candidates and subsequent confirmation of the sources. Our methods involve a simple determination of likely candidates by searching peak emission maps, utilising the intrinsic nature of water-maser emission, spatially unresolved and spectrally narrow-lined. We estimate completeness limits and compare our method with results from the duchamp source finder. We find that the two methods perform similarly. We conclude that the similarity in performance is due to the intrinsic limitation of the noise characteristics of the data. The advantages of our method are that it is slightly more efficient in eliminating spurious detections and is simple to implement. The disadvantage is that it is a manual method of finding sources and so is not practical on datasets much larger than HOPS, or for datasets with extended emission that needs to be characterised. We outline a two-stage method for the most efficient means of finding masers, using duchamp.


1973 ◽  
Vol 10 (7) ◽  
pp. 1023-1058 ◽  
Author(s):  
D. F. Coates ◽  
H. U. Bielenstein ◽  
D. G. F. Hedley

The Elliot Lake area is characterized by Proterozoic sediments containing uranium-bearing conglomerates separated by quartzite beds 10 to 100 ft (3.0 to 30.5 m) thick. The geological structure consists of a broad syncline with an east–west axis plunging about 5 °W, cut by northwest trending faults, and with steeply dipping east–west extension joints. All the mines use a stope-and-pillar method of extraction with narrow rib pillars about 250 ft (76 m) long on dip and sill pillars on strike.After the Elliot Lake Laboratory was established, detailed studies were undertaken to evaluate the methods that were available for the determination of the mechanical properties of the rock mass and its state of stress before mining. Practical studies were then made on the pillars, roofs, and abutments.Testing techniques were improved for the rock substance and the rock mass; however, much remains to be done to be able to characterize adequately the mechanical properties of the rock mass. A novel random sampling approach produced a suite of specimens many of which included fractures, with a mean uniaxial strength that was surprisingly little lower than the mean of only the solid specimens. The dispersion of values in such a suite was, of course, quite large. Of the other tests used, Brazilian tests were found to be useful for quality control of stress determinations using a strain recovery technique.The use of borehole pressure cells, seismic velocity, and borehole penetrometers as techniques for the determination of the mechanical properties of the rock mass remains questionable.The tectonic history of the region was resolved; it provides an explanation for the existence of horizontal stresses greater than vertical stresses and for the major principal stress to be oriented parallel to the axis of the syncline. It was also shown that the major principal stress axis is essentially parallel to the strike of extension joint surfaces, even when the strike deviates from the predominant 090° azimuth direction.After considerable experience with mining in these geologic conditions, which probably are more uniform than in most metal mines, the determination of stable spans of stopes and breadths of pillars can be done very well by judgment. However, for examining new layouts relatively simple theoretical analyses, particularly for the determination of stable pillar sizes, were found to provide a rational and useful basis for extrapolation.The stresses determined in pillars and abutment zones and the deformations of the roofs corresponded fairly well to values predicted by analytical and model techniques. The increased stress in the abutment zones extended into the solid for a relatively limited distance, which, in this relatively hard rock, seems to be related substantially to the span of the adjacent stope. All field measurements were subject to dispersion. The electrolytic analogue, which takes into account the three-dimensional aspects of the geometry of the tabular orebodies, showed that irregular mining boundaries have a distinct contribution to the variance of the pillar stresses. The finite element method was found to be flexible and useful in studying specific questions, particularly related to novel mining plans.


1974 ◽  
Vol 64 (1) ◽  
pp. 115-129
Author(s):  
J. C. Savage ◽  
W. T. Kinoshita ◽  
W. H. Prescott

abstract Repeated surveys of a trilateration network (aperture greater than 20 km) centered on ground zero for the HANDLEY event, a nuclear explosion at the Nevada Test Site with yield in excess of 1 megaton, suggest that the explosion induced an east-west extension of the network by more than 50 mm. In the year following the detonation, this deformation reversed such that the final configuration represented a small east-west contraction from the pre-HANDLEY state. In the subsequent 2-year period, only minor deformation was detected. Thus, the overall response of Pahute Mesa may be described as stable. The explosion-induced deformation is thought to be partly due to slip on faults driven by the large-amplitude seismic waves from the explosion. The mechanism of the postshot relaxation is not understood.


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