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By Paul W. Hodge

A really critical blunders was once made in an past evaluation of this e-book by means of beginner astronomer Roger Raurbach. He said that 4 of the 5 globular clusters of the Fornax dwarf galaxy have been misidentified within the Atlas. that's mistaken. the 3 internal clusters have been found by means of Harlow Shapley, Walter Baade and Edwin Hubble and that i found the 2 outer clusters; their identities, as proven within the Atlas, have been released within the Astronomical magazine, quantity sixty six, web page eight, 1961. Their positions are famous to specialist astronomers and several other papers, together with a few in accordance with Hubble area Telescope photos, were released lately, overlaying either color-magnitude diagrams of the clusters' stars and spectroscopy, giving their metallicities. Please my score of this publication, that's meaningless, as i'm an writer.

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1998, prefix G). Gordon et al. (1998) cross-reference various identifications of the SNRs. d BCLMP 660 appears as a complete ring in Figure 7b of Courtès et al. (1987). We detect only a partial ring in our images. e SNR DDB 18 is contained within BCLMP 750. Gordon et al. (1998) do not identify it with G97, but we believe they are the same object.

28325 -30 28 24501 24533 24599 24798 24838 ----SC G14 28 31 28 30 28 24858 24887 25017 25060 25061 H 33 --VHK 80 -- 28 30 28 31 31 25201 25255 25615 25620 25933 ------ 28 28, 31 26 28 31 25987 26066 26163 26166 26175 ---H 35,VHK 35, SC E7 -- 28 30 31 28 28 26195 26212 26348 26414 26428 --H 32 --- 31 28 28 31 31 26477 26524 26647 26729 26788 -SC B1 ---- 30 26 31 28 30 26850 26910 --- 31 26 30 27065 27330 27544 ---- 31 31 28 27608 27639 27689 27697 27777 ------ 31 30 31 28 29 27830 27840 28021 28065 28168 -SC E34 SC E17 -VHK 58 28 26 26 28 28 28325 28367 28500 28578 28632 24472 ----- 28 31 26 31 31 28639 28664 28706 28768 28785 ----- SC F12 28 28 31 28 29 28834 28986 28988 29032 29104 SC G14 VHK 55 ---- 28 26 31 26 31 29131 29211 29250 29280 29334 ------ 31 31 31 29 31 29397 29476 --- 28 28 31 29618 29631 29799 ---- 28 31 28 29926 30001 30125 30133 30173 ------ 28 31 28 28 28 30352 30422 30459 30526 30718 ---VHK 69 -- 31 31 31 31 31 30804 31100 31267 31396 31458 ------ 29 31 31 28 31 31668 31786 31805 31929 31953 VHK 57 ---SC G6 31 28 28 26 31 31986 32023 32117 32202 32473 ----SC F9 28 31 28 28 29 33070 33350 34052 34497 35284 SC F8 ----- 29 26 31 31 31 35369 36117 --- 31 26 32 a 36568 36781 36806 ---- 31 32 32 36841 37040 --- 26 26 The variable stars are all based on the Kinman, Mould and Wood (1987) survey and are identified by the numbers in that catalog (designation: KMW), which also provided the alternate names given here (designation VHK: van den Bergh, Herbst, Kowal (1975); H: Hubble (1926); HS: Hubble and Sandage (1953); SC: Sandage and Carlson (1983)).

33 Table 4a. M33 Emission Regions Identified by Boulesteix et al. 4 30 30 30 30 30 38 32 32 32 31 43 30 32 12 45 150 71 40 76 99 535 174 109 213 354 751 752 753 756 BCLMP emission regions are labeled on the M33 charts with their number and no prefix. Separate subcomponents of complex regions are given lowercase Arabic letters and are identified on Charts 59-83. , 1997). , 1997). c SNR candidates are from Sabbadin (1979, identified with prefix S), D’Odorico, Dopita, and Benvenuti (1980, prefix DDB), and Gordon et al.

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