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|A study of CO and FIR dust emission of lynds 694/695 dark clouds|
We present the results of the high resolution observations in thetransition of J = 1 0 of 12CO and 13CO towardsLynds 694 and 695 dark cloud region, using the fifteen beam arrayreceiver at Five College Radio Astronomy Observatory (FCRAO) and the 3mm SIS receiver on the 14-m telescope at Taeduk Radio AstronomyObservatory (TRAO). This region is prominently opaque on the POSSplates, and shows a remarkable morphology of an alphabet C. Weinvestigate the gas and dust properties in Lynds 694/695 dark clouds,and find that there are a few sign of dense core formation, but it hasno evidence for any star forming activities. We estimate severalphysical parameters, and describe the dynamics of the gas component.Lynds 694/695 cloud is found to be rotating along the Right Ascensionaxis at α(1950) = 10h50m. Mass estimateusing the conversion factor (MCO) is found to be 170Mȯ, and dust mass is 1.34 Mȯ. Theaverage temperature of the dust based on the extended emission at 60 and100 μm is 26 K. The low dust temperature and low ratio offar-infrared emission to hydrogen column density are probably due tolack of the internal heating source. The weaker ISRF can explain theexceptionally low dust temperatures found in this region. Overall, thegas and dust properties of the mapped region are similar to those ofnormal dark clouds.
|A distance scale from the infrared magnitude/H I velocity-width relations. V - Distance moduli to 10 galaxy clusters, and positive detection of bulk supercluster motion toward the microwave anisotropy|
The IR/H I relation is employed to derive relative distances to 10nearby galaxy clusters. A problem originally identified by van den Bergh(1981), that the surface brightnesses of galaxies in the higher redshiftclusters are in the mean found to be lower than in nearby clusters atfixed velocity width, is discussed. The extent to which this effect isaccounted for by galaxy diameter errors is investigated in detail.Cluster distance moduli and Hubble ratios are derived after firstconsidering a number of potential biases in the data. A variety of solarmotion solutions are obtained with respect to the reference frame of theclusters, and the value of the Hubble constant is discussed. The finalcluster Hubble ratios exhibit considerable scatter, signifying thepresence of an unaccounted for Local Group streaming motion. Formalsolution leads to a velocity in close agreement with the 3 K dipoleanisotropy.
|The colour-magnitude distribution of giant stars as a function of age|
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