Observations of the (then unidentified) Delta Aquariids (δ Aquariids) were recorded by
G. L. Tupman in 1870, who plotted 65 meteors observed between July 27 and August 6. He plotted the radiant's apparent beginning and ending points (RA=340°, DEC=−14°; RA=333°, DEC=−16°). This was corrected later.
Ronald A. McIntosh re-plotted the path, based on a greater number of observations made from 1926 to 1933. He determined it to begin at RA=334.9°, DEC=−19.2° and end RA=352.4°, DEC=−11.8°.
Cuno Hoffmeister and a team of German observers were the first to record the characteristics of a Northern Aquariid radiant within the stream around 1938. Canadian
D. W. R. McKinley observed both branches in 1949, but did not associate the two radiants. That was accomplished by astronomer
Mary Almond, in 1952, who determined both the accurate velocity and orbit of the δ Aquariids. She used a "more selective beamed aerial" (echo radio) to identify probable member meteors and plotted an accurate orbital plane. Her paper reported it as a broad "system of orbits" that are probably "connected and produced by one extended stream." This was confirmed in the 1952–1954
Harvard Meteor Project, via photographic observation of orbits. The Project also produced the first evidence that the stream's evolution was influenced by
Jupiter. == Viewing ==