92 CARNEGIE INSTITUTION 



minor planet, Eros, is a subject of interest at present. A vast accu- 

 mulation of photographs, together with some micrometric measure- 

 ments, has been secured. From lack of funds or other causes, little 

 progress appears to have been made in rendering the results avail- 

 able to science. What share in this work, if any, should be under- 

 taken b)^ the Carnegie Institution is a matter for future consider.a- 

 tion, after a better knowledge of the situation may have been 

 obtained. 



Piiblicaiion of Results. — 'There is reason to believe that there are 

 in existence valuable series of observations, calculations, and com- 

 pilations of great interest and prospective service to science which 

 remain in manuscript for lack of means of publication. What shall 

 be done in this connection depends, of course, upon the general 

 policy which the Trustees of the Institution may adopt in reference 

 to the matter of publication in general. * ^ * 



Astrophysical Investigations. — The principal object of astrophysical 

 research is to ascertain the physical and chemical constitution of 

 the heavenly bodies, and to trace out and explain the successive 

 stages in their evolution from nebulaae. 



One of the most important pieces of work now required in this 

 field is a systematic photographic survey of the nebulas in both 

 northern and southern heavens. Photography of the moon and 

 planets under particularly favorable instrumental and atmospheric 

 conditions, with the hope of recording details much smaller than 

 these hitherto obtained in photographs, should also be encouraged. 

 In spectroscopy there is much to be done. The measurement of 

 the radial velocities of the brighter stars is already well provided 

 for, and as soon as possible this woik should be extended to fainter 

 objects in far greater numbers. The spectra of long-period variable 

 stars, studied in connection with their light variations, offer an im- 

 portant field for research. It should be possible with suitable appa- 

 ratus to ph<jtograph stellar spectra on the scale of our present pho- 

 tographs of the solar spectrum, permitting the displacement of lines 

 due to pressure and other phenomena to be inve.stigated. In con- 

 nection with the study of stellar evolution, many new stellar spec- 

 troscopic researches are required. The spectra of nebulae, particu- 

 larly of the Andromeda and other spiral nebulae, also should receive 

 m*ore attention. 



The Sun, as the only star whose phenomena can be observed in- 

 dividually, should be thoroughly studied with the best modem 

 appliances. The law of radiation, constitution of the absorbing 



