The second IC lists a corrected RA (per Howe) of 10 13 10

Per Dreyer, NGC 3229 (= John Herschel's GC 5068, S Coolidge (#14, HN16), 1860 RA 20 16 14, NPD 89 13.8) is "faint". The 20 hours of RA is an obvious misprint (though not obvious enough to have ever been noticed by Dreyer), all other NGC listings in the same range being at 10 hours, and does not correspond to the (correct) position in the original Harvard report. Unfortunately, as for all of Coolidge's "nebulae", NGC 3229 is merely a group of (three) faint stars.

The second IC lists a corrected RA (per Howe) of 10 15 18

Per Dreyer, NGC 3234 (= John Herschel's GC 2094, 1860 RA 10 17 05, NPD 62 16.1) is "pretty bright, pretty small, round, pretty suddenly bright middle (? = 2095)", the query at the end meaning that Dreyer thought it might be the same as NGC 3225. However, the first IC notes "3234 is not = 3235; both seen by Denning". This makes the supposed equivalence between the two listings seem very odd; however Corwin points out that there is nothing at NGC 3234's supposed location, that the difference of exactly 1 degree in declination between it and NGC 3235 suggests a typographical error in Herschel's position, and feels that the two listings must represent the same object. Of course that leaves the question of what Denning saw, that led to the IC note; and Corwin makes the reasonable suggestion that he probably saw d'Arrest's preceding nebula, NGC 3232. In any event, since there is nothing at Herschel's position, the doubts that go back to the original NGC would seem to weigh heavily in favor of NGC 3234 actually being the same as NGC 3235, regardless of any subsequent uncertainties.

Per Dreyer, NGC 3235 (= John Herschel's GC 2095, d'Arrest, 1860 RA 10 17 05, NPD 61 16.6) is "faint, small, following of 2" (the preceding being NGC 3232). See NGC 3234 for a discussion of the double listing.

The second IC lists a corrected position (per DeLisle Stewart) of RA 10 18 50, NPD 147 06 and adds "h.'s place was only approximate". Also referred to as RCW49, this large emission nebula is energized by a star cluster, Westerlund 2, partially hidden within its depths. Older stars have already cleared gas and dust out of the central portions of the nebula, but younger stars are still hidden by the clouds of gas and dust out of which they recently formed. Fortunately, the fleet of space telescopes now in orbit allows us to study even those stars. The cluster is approximately 14 thousand light years away, and contains more than 2200 stars, of which 300 were previously unobservable. The cluster is only 1 or 2 million years old, so some of its stars are very massive (high-mass stars have very short lifetimes, so older clusters don't contain very massive stars). One of the cluster members consists of 82 and 83 solar mass stars which orbit each other every 3.7 days, at a distance from each other of less than 25 million miles. Note: The NASA sites (Spitzer, Chandra and APoD) all mis-state the constellation as Centaurus; but the object is in Carina, as indicated above.