Other Techniques Clause Samples
Other Techniques. No appropriate data are available for the Mashel watershed study area to attempt an NAIP Stereo or aerial IfSAR assessment approaches. Due to the high stand density and poor ground visibility in the riparian areas the manual stream digitization from aerial orthophotography by a technician were not attempted. Moreover, the accuracy of such manually approaches is also unknown and not believed to exceed accuracies feasible form LiDAR, with similar field data needs required to test the accuracies. Unfortunately, because of the issue of shadows in optical imagery, the utility of such data to manually clean up or improve on the features such as culvert locations in LiDAR data is unfeasible.
Other Techniques. Several other techniques for the approximation of legislation exist, and they vary according to their methods and results. Amongst these other tech- niques, two in particular have been used in international private air law. One consists in ‘cooperation’ or ‘coordination’, or even ‘convergence’, pursuant to the terminology used. Under this approach, two or more States jointly decide not to adopt conflicting legislation and, wherever 31 The EU also makes a distinction between ‘minimum’ and ‘maximum’ harmonization. The latter sets the floor or ceiling of harmonization, while the former allows Member States to adopt more stringent rules. See, ▇▇▇▇▇ ▇▇▇▇, Búrca (de) ▇▇▇▇▇▇▇, EU Law – Text, Cases and Material 661 (7th edition, Oxford University Press, 2020).
Other Techniques. Another method used to select high redshift galaxies makes use of narrow-band imaging in order to identify galaxies with a strong Lyman-α emission line, known as ▇▇▇▇▇-α Emitters (LAEs). Using photometric bandpasses, this type of galaxy can be relatively easily detected if one narrow band contains the strong emission line while the object remains undetected or relatively faint in nearby bands. Since ionizing photons are absorbed and reprocessed into ▇▇▇▇▇-α photons by the inter- stellar medium (ISM) in distant galaxies, the ▇▇▇▇▇-α line is (by definition) very strong in these sources. However, while one advantage of this technique is that both the redshift and location of the observed galaxy can be readily determined, it has disadvantages when used as an identifier for the distant galaxy population. One drawback is that the ▇▇▇▇▇-α photons can be absorbed and scattered by dust particles present within the source galaxy, reducing the observed flux from the object and complicating the interpretation. Another disadvantage is that poten- tial ambiguity remains due to other strong emission lines within galaxies, such as ▇.▇. ▇▇, [OIII], Hβ or [OII]. However, spectroscopic observations with high enough signal-to-noise of the source should be able to resolve this confusion. Lastly, due to absorption by the Earth’s atmosphere, as well as night sky emission lines in the infrared bands, only certain spectral ‘windows’ can be observed unambiguously, re- stricting observations to particular redshift ranges. While infrared satellites exist which can overcome atmospheric constraints, their use is costly and time-consuming compared to ground-based observations.