202 ON THE OBLIQUITY 



the present, that 48 observations of the sun, when near the zenith, brought 

 out 13 4 6.484. Hence t'he difference is 6.951 not far different from Mr. 

 Le Gentil's quantity, but with a contrary sign, so that we differ in this- 

 respect by 12: but in the far more important object of the obliquity, it 

 will appear that we agree as near as could be expected. 



23. On the probable cause why the sun should so constantly give a 

 lower latitude than the stars; T can only repeat what I have said formerly 

 in the paper above referred to, namely, that from allowing too much for 

 the effects of refraction, astronomers in Europe,ass\gn probably too great a 

 zenith distance to the sun, by which excess they place their zenith too far. 

 from the ecliptic, a circumstance which tends necessarily to depress the, 

 results of observations of the sun, taken in low latitudes-. 



' JOHN WARREN, 



Honorable Company's Observatory, J 

 Ut of February, 181 1. 1 > ' 



■ - - • • '■-,.-■ 



Errata in the paper on the declination of Stars, published in the XitJi 



Volume of the Asiatick Researches. Table Vth, 3d column," 



corresponding Latitudes, 



o 1 • n 010 



N. for 13 4 2.207 read 13 4 2.879 



S. for 13 4 4.499 read 13 4 5 403 



Column 4tb. for 13 4 3.323 read 13 4 4.181 



THESE differences arise from the latitudes having been reduced, 

 without interpolating the sun's declination for the respective days ; which 

 has been done in the present correction. This alteration however, affects 

 nothing of what 1 have said in the 26th article of the paper, because 

 I only considered the observed zenith distances and not the latitudes. 



