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Infrared Camera ( Cameras One and Two ) were used to make observations of the nuclear region of Seyfert galaxy NGC-4151 which will be studied in several ways : 1 ) low-resolution spectra over the entire UV and visible range will be obtained ; 2 ) slitless spectra of strong emission lines at moderate resolution and narrow-band WF / PC-2 images will be used to map the dynamics of the regions ; 3 ) Echelle spectra over the entire UV bandpass will be used to study the intrinsic absorption in the nucleus ; and 4 ) parallel imaging will be performed of the outer galaxy and other galaxies or QSOs . This process is very important as the outcome of interim emissions tests hinges upon the definition of the " Baseline " and " Action " scenarios and the results of the subsequent regional emissions analysis . Unlike CAMR , which allows facilities to emit mercury in excess of applicable emission limits by purchasing allowances , Part 246 requires facilities to achieve strict compliance with applicable emission limits . The lack of strong emission lines from gas at temperatures below 3 keV in XMM RGS and Chandra HETG spectra has become a key argument for cooling flow models which include such additional physics as AGN heating , thermal conduction , star formation , and internal absorption . Other sources of fuel-related emissions , such as those resulting from fuel leaks or seepage , and from gasoline permeation through hoses and tanks , are best controlled through proper component design and choice of hose , fuel tank , and gasket materials , as well as prompt repair of defective components . Solid blue lines indicate the location of strong emission features located by the code . Short , hair-like jets of strong emission decorate the Sun 's atmosphere to an extent not clearly seen before . The result is essentially a list of physical emissions resulting from all of the processes considered .