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there are now a number of multi-wavelength surveys that cover all but the faintest objects. the enormous increase in the number of objects detected by these surveys has resulted in great difficulties in determining the class and nature of those sources. for example, amongst the 12,000 ir-selected galaxies uncovered by the spitzer wide-area infrared extragalactic survey (swire) te{swire} only one, iras f15253-5359, was a flat-spectrum radio source and only three of these galaxies showed any evidence of an agn in x-rays te{x-ray}. we are therefore in great need of a complementary survey in the hard x-ray band to identify the nature of these sources and as a complement to the deep radio and mid-infrared surveys, such as that undertaken by the swire. we therefore propose a small survey with the satellite that will provide a great improvement over the current deep 2ms rosat survey in terms of sensitivity and field coverage from the northern hemisphere. this survey will survey the entire sky except for the celestial poles and the avoidance regions described in table 2 for a combined sensitivity down to 10^-14 erg s^-1 between 10 and 100 kev, and a minimum resolution of 2.5 arc seconds .
the debris of gas-rich galaxies usually contains a large amount of dust, which is a major target for submillimeter and millimeter observations. in this paper, we propose a sample of nearby infrared galaxies with the largest 850 and 450 micron flux densities, in the noao survey program site/sdss j0523-0030 (pi: lee), to target for a program that will observe with a segment of an x-ray mission, and determine the properties of the dust in the galaxies. the sample will be composed of all the galaxies at the distance of our lirgs (i.e., galaxies with log l/l50 > 10.5), with the reddest infrared colors. the sdss images show that their bulges are very red, which imply the existence of a very young population of stars. the 850 micron images of the galaxies show their very massive molecular complexes which are also revealed by the alma images. with these information, we will be able to study the properties of the dust emission and the star formation in these galaxies, which will provide invaluable clues to the formation and evolution of galaxies at high redshift. to demonstrate the potential value of these observations, we will present our own sample observations and estimate the noise level in the data.
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