NGC 2030 = LMC-N59A = LH 82 = Seagull Nebula = Dragon’s Head Nebula

05 35 00.5 -67 33 18; Dor
Size 2.4’x2.0′

30″ (10/18/17 – OzSky): at 202x and 264x + NPB filter; this is the first section in the remarkable Seagull or “Dragon’s Head” Nebula, though it’s the faintest of the three connected patches extending 5.5′ from NW to SE with NGC 2032 and 2036. The brightest portion is an elongated “bar” extending ~2.0’x40″, oriented WSW-ENE, just west of a mag 12.2 O3III-type ionizing star (HD 269810 = R122). Fainter nebulosity spreads to the north in roughly an oval outline and includes a mag 14.5 star, so the total extent of NGC 2030 in the N-S direction is over 2.5′. Very faint nebulosity appears to connect NGC 2030 with brighter NGC 2032 directly SE.

24″ (4/11/08 – Magellan Observatory, Australia): this is the NW component of the Seagull Nebula; a bright, highly structured 7’x5′ emission nebula. The brightest portion of NGC 2030 is a bright streak elongated E-W that extends west from mag 12.3 HD 269810 (O3-type supergiant). A large mass of nebulosity spreads to the north from this streak in a more circular 2′ patch. This patch is incorrectly identified as NGC 2029 in modern catalogues and atlases. The Seagull Nebula is situated on the SE edge of the supergiant shell SGS LMC 4.

Notes: John Herschel discovered NGC 2030 = h2910 on 23 Dec 1834 and recorded “B; L; gradually brighter in the middle. The first of 3 neb, which run together.” On a second sweep, he logged “vF; pL; irreg R. The first of 3, which run together. See Plate III. fig 5.” The modern identities for NGC 2029 and 2030 are reversal. See historical notes for NGC 2029.

NGC 2032 = LMC-N59A = LH 82 = Seagull Nebula = Dragon’s Head Nebula

05 35 20.6 -67 34 06; Dor
Size 2’x1′

30″ (10/18/17 – OzSky): at 202x and 264x + NPB filter; NGC 2032 and 2035, separated by a dark lane, form a stunning pair of adjacent emission nebulae of comparable surface brightness, though NGC 2032 is larger. Using a narrow-band filter, NGC 2032 was extremely bright, elongated SW-NE, ~2’x1′, with a scalloped but sharply defined border at the brighter edge along the dust lane. A fairly prominent thin filament extends NE for ~1.5′, curling a bit towards the tip. A thin strip on the SE end (just beyond the lane) connects to NGC 2035. The candidate ionizing star (O5V-type) was visible unfiltered at the edge of an indentation along the eastern border, though it appeared fainter than the listed mag of 13.5. A second mag 14 star (B0-type) was also involved at 25″ to its east. A mag 11.4 star is off the SW side and a mag 12.2 star (HD 269810) is at the NE edge. The latter star (also known as RMC 122) may be the ionizing source for the surrounding nebulosity. NGC 2040 (part of same complex) is ~5′ E.

24″ (4/11/08 – Magellan Observatory, Australia): this is possibly the brightest section of the “Seagull Nebula” or “Dragon’s Head Nebula” in the LMC (similar to NGC 2035 1.6′ SE). It consists of a very bright, elongated ~SSW-NNE patch, 2’x1′, with an unusual kidney-bean shape that is indented or concave on the east side. NGC 2032 is just separated to 2035 by an elongated dark lane (oriented SSW-NNE) on the east side. A faint, thin streamer of nebulosity shoots to the north from 2032. Mag 11.4 HD 269808 is off the SW side.

Notes: James Dunlop discovered NGC 2032 = D 219 = D 194 = h2913, along with NGC 2035, on 27 Sep 1826. I assume his description of D219 applies to both numbers: “pretty bright round nebula, about 1 1/4′ diameter, bright towards the centre.” He made two observations and his position is within the Seagull Nebula complex. D 194 was described as “a pretty large faint ill defined nebula, irregular figure. It was found on 27 Sep 1834 during an LMC drift in which he misidentified the offset star (Theta Doradus). As a result, all positions in the drift (off the meridian) were reduced incorrectly. Once corrected his position (and description) is a good match with NGC 2032/2035.

John Herschel first observed the nebula on 2 Nov 1834 (sweep 508) and recorded “vB; vL. A singular figure like 3 nebulae lumped together.” On 23 Dec 1834 (sweep 522) he logged “B; L; gradually brighter in the middle. The second of 3 which run together.” A detailed sketch of the complex was published in plate III, figure 5 in the CGH observations. Herschel gave an uncertain equivalence with D 219 in his Cape catalogue. Williamina Fleming found a gaseous spectrum in 1897 on objective prism plates taken in Peru.

The Seagull Nebula contains four separate NGC designations: NGC 2030 (misidentified as NGC 2029 in GC and NGC), NGC 2032, NGC 2035 and NGC 2040 with NGC 2035 being the brightest and largest of the group. Collectively the area is known as N59A and is located at the boundary of the supershell LMC4 in the Large Magellanic Cloud. NGC 2032 and 2035, which form the bright core of the H II region N59A (B053530- 6736), belong to a single H II region that appears divided due to the presence of a heavy dust lane.

NGC 2035 = LMC-N59A = LH 82 = Seagull Nebula = Dragon’s Head Nebula

05 35 33 -67 35 11; Dor
Size 1.6’x1.2′

30″ (10/18/17 – OzSky): at 202x and 264x + NPB filter; NGC 2032 and 2035, separated by a dark lane, form a stunning pair of adjacent emission nebulae of comparable surface brightness, though NGC 2032 is larger. The two impressive regions are attached or merge at the south end by a thin strip of nebulosity. NGC 2035 was extremely bright, roughly rectangular but irregular with slightly concave eastern side and lots of complex, internal structure with brighter and darker areas. A fairly thin streamer is attached on the northeast end and extends 2′ NNE, similar (though slightly fainter) to a filament attached to NGC 2032! N59C is a detached patch ~2′ SE. It appeared moderately large, roundish, at least 1′ diameter. A mag 10.4 star is 2′ ESE.

24″ (4/11/08 – Magellan Observatory, Australia): this is the southeast section of the bright Seagull Nebula in the LMC. At 200x using a UHC filter it appeared very bright, moderately large, with a very irregular shape similar to an anvil. The very knotty, complex structure was elongated N-S, 1.6’x1.0′, with the widest part of the anvil on the south end. NGC 2032, another very bright section, is very close preceding (roughly 1.6′ between centers) and the two sections are separated by a dark lane oriented SSW-NNE. A very faint streamer attached on the NE side flows to the north (NGC 2032 has a similar but brighter streamer). A fairly small detached patch, ~1.2′ in diameter, is close SE (identified later as N59C).

Notes: James Dunlop discovered NGC 2035 = D 219 = D 194 = h2916, along with NGC 2032, on 27 Sep 1826. He described D 219 (both) as a “pretty bright round nebula, about 1 1/4′ diameter, bright towards the centre”. His position falls within the Seagull Nebula complex. D 194 was described as “a pretty large faint ill defined nebula, irregular figure. It was found on 27 Sep 1834 during an LMC drift in which he misidentified the offset star (Theta Doradus). As a result, all positions in the drift (off the meridian) were reduced incorrectly and his published position is 2.4° to the SE. Once corrected his position (and description) is a good match with NGC 2032/2035.

John Herschel first observed NGC 2035 on 23 Dec 1834 (sweep 522) and logged “B, L, bM. The 3rd of three which run together. (Plate III, fig 5)”. Herschel gave an uncertain equivalence with D 220 in the CGH.

LMC-N59C = Seagull Nebula = Dragon’s Head Nebula

05 35 38 -67 37 06; Dor
Size 1.2′

30″ (10/18/17 – OzSky): at 202x and 264x + NPB filter; fairly faint patch that is detached from NGC 2035 to its southeast. It appeared moderately large, roundish, at least 1′ diameter. A mag 10.4 star is 2′ ESE.

24″ (4/11/08 – Magellan Observatory, Australia): N59C is not plotted on the Morel close-up chart of the Seagull Nebula, but I noted a fairly small detached patch, ~1.2′ in diameter, close SE of much brighter NGC 2035. Also located 2′ W of mag 10.4 HD 269847.

NGC 2040 = ESO 056-164 = LMC-N59B = LH 88

05 36 05 -67 34 01; Dor
V = 11.5; Size 2′

30″ (10/18/17 – OzSky): at 202x and 264x + NPB filter; bright, very large, irregular nebula just east of NGC 2030/2032/2035 (Dragon’s Head or Seagull Nebula). The main portion is roughly triangular with one “vertex” on the south side and another on the northeast end. It has a sharp, contrasty edge on the east side to the south tip and some internal, irregular brightness in the interior. Unfiltered a dozen stars mag 14-15 are involved (association LH 88), with several more spreading to the south.

NGC 2040 is merged with a supernova remnant shell (SNR B0536-67.6) on the south side. On images the shell is ~2′ in diameter and weak in OIII emission, with a complex interlaced web of delicate filaments. Visually, I could see a very faint, thin curving loop, ~45″ in length, which forms the SW end of the shell (brightest part on images). A mag 13.5 star (O5III-type and high-mass X-ray binary) is in the interior of the shell, with the observed strip centered 40″ to its WSW. This star was possibly bound to the precursor star of the SNR remnant.

24″ (4/11/08 – Magellan Observatory, Australia): this is a bright, irregularly round glow, ~2′ diameter, located ~4′ ENE of the Seagull or Dragon’s Head Nebula and part of the same emission complex. The nebulosity surrounds a cluster of roughly 15 stars (LH 88). A UHC filter provided an excellent contrast gain at 200x and revealed a very irregular outline. The POSS image shows delicate filaments to the south forming a large loop (SNR shell SNR 0536-67.6) although I don’t believe this extension was recorded.

Notes: James Dunlop probably discovered NGC 2040 = D 220 = h2918 on 27 Sep 1826, along with NGC 2032/2035. He noted “a round faint nebula, about 40″ diameter.” and his position is 4′ NNW of the center.

John Herschel rediscovered NGC 2040 on 2 Nov 1834 and recorded “F; irreg R; gradually little brighter middle; r; 2′. (Pl III, fig 5).” On a later sweep he reported “vF; R; follows 3 vB L nebulae [NGC 2030, NGC 2032 and NGC 2035] which run together.” His position (from 5 sweeps) is accurate and an excellent sketch of the complex is on plate III, figure 3.