肉眼深空与双筒天文

肉眼深空与双筒天文

http://www.stargazing.net/david/eyes/neobjectsi.html

Deep Sky Objects

  • Messier’s catalog: M6, M7, M8, M13, M22, M24, M31, M35, M41, M42, M43, M44 and M47.
  • New General Catalog of Clusters and Nebulea: NGC104, NGC869, NGC884, NGC2070, NGC2247, NGC2264, NGC2362, NGC2451, NGC2516, NGC2547, NGC3114, NGC3293, NGC3372, NGC3532, NGC3766, NGC4755, NGC5139, NGC6231 and NGC6633.
  • NGC Index Catalog: IC1396, IC2391 and IC2602.
  • SMC, LMC, Coalsack, Coma Cluster,

The following deep sky objects will take very good dark skys and eye sight to be observed.

  • Messier’s catalog: M3, M5, M25, M34, M36, M37, M39 and M48.
  • New General Catalog of Clusters and Nebulea: NGC362, NGC752, NGC1981, NGC2808, NGC6067, NGC6087, NGC6752 and NGC7000.
  • NGC Index Catalog: IC4665.

双筒天文

M 31 Galaxy 4.3
NGC 3372 Bright nebula 3
IC 2944 Bright nebula 4.5
NGC 5128 Galaxy 7.6
NGC 7000 Bright nebula 4
NGC 2070 Bright nebula 5
NGC 2238 Bright nebula 6
M 42 Bright nebula 4
NGC 1499 Bright nebula 5
M 8 Bright nebula 5
M 17 Bright nebula 6
M 20 Bright nebula 6.3
NGC 253 Galaxy 8
NGC 292 Galaxy 2.8

除了几个不敢苟同，基本还需要重新看的：船底、奔鸡、5128、玫瑰

星系的话就只剩下玉夫座星系了，加油！

疏散星团的话，

宝盒、许愿井、宝石、手

类似宝盒宝石的还有小蝎NGC5281、IC2581、NGC3324、NGC3376

私藏宝藏

https://www.astronomyclub.xyz/hidden-treasure/

http://www.southastrodel.com/Page009.htm

OBSERVATIONAL COMPARISONS WITH OTHER OPEN CLUSTERS

Perhaps as our northern cousins often ellude, observers are indeed are impressed with the NGC 4755’s beauty, but they always to be hesitant to claim it is the best in the entire sky. An example of this appears in the recent book “Star Clusters” by B.A. Archinal and S.J. Hynes (2004) who states on pg. 174;

“One of the most striking and spectacular open clusters in the southern sky”

This is a bold statement indeed, but is it? Perhaps among the southern clusters I would find this almost agreeable, however, there are many other clusters have their own unique characteristics and particular charm. Two clusters that are possible usurpers to the ‘crown jewels’ of all clusters, is the almost forgotten NGC 3114 / The Gem Cluster(10027-6006) and the larger and more extensive scattered sister Carina cluster NGC 3532 / The Football Cluster (11055-5844). Both of these clusterd contain many blue stars interspersed with a few prominent yellow, orange or red stars. Often there own individual brilliance is only foreshadowed and particularly lessened by the fact that they are much larger — requiring only small apertures and/or very low magnifications to encompass all the stars in the telescopic field.

Below is a general selection of must see open clusters which can be observed during autumn (in the southern hemisphere) in March or April. I have observed all these clusters and eventually I hope to write some short text on all of them. A fuller version of this selection appears in these pages, giving the Fifty Best Clusters in both the Southern and Northern and skies, and the list of all 100 Selected Clusters.

(Also see the more general discussion can be seen in the section apecificaly on Open Clusters, if required.)

BEST SOUTHERN OPEN STAR CLUSTERS

1
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5
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7
8
9
10
11
12
13
14
15
16
17
18
19
20
21
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25
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27
28
29
30
31
32
33
34
35
36
37
38
39
40
41
42
43
44
45
46
47
48
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51
52
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  NGC No.  Other  Names     RA (2000) Dec  Con  Mag Size Class     *n   Source  
                         hh mm.m  dd mm        v    ′                     
--------------------------------------------------------------------------------
  NGC 2287 Cr 118  M41      06 46.0 -20 45  CMa  4.5  38  I 3 r     80  Lynga   
* NGC 2362 Cr 136  Mel 65   07 18.7 -24 57  CMa  3.8   6  I 3 r     60  Archinal
  NGC 2422-78      Cr 152   07 36.6 -14 29  Pup  4.4  29  I 3 m     30  Lynga   
  NGC 2439 Cr 158  Mel 74   07 40.8 -31 42  Pup  6.9  10  II 3 r    80  Lynga   
  NGC 2437 Cr 159  M46      07 41.8 -14 49  Pup  6.1  27  II 2 r   100  Lynga   

  NGC 2451 Cr 161           07 45.4 -37 57  Pup  2.8  45  II 2 m    40  Lynga   
  NGC 2477 Cr 165  Mel 78   07 52.2 -38 32  Pup  5.8  27  I 2 r    160  Lynga   
* NGC 2516 Cr 172  Mel 82   07 58.0 -60 45  Car  3.8  29  I 3 r     80          
  NGC 2547 Cr 177  Mel 84   08 10.2 -49 14  Vel  4.7  20  I 3 r     80  Lynga   
  NGC 2546 Cr 178           08 12.4 -37 37  Pup  6.3  40  III 2 m  40   Lynga   

* IC  2391 Cr 191  o Vel    08 40.3 -52 55  Vel  2.6  49  II 3 m    30  Lynga   
  NGC 2660 Cr 193  Mel 92   08 42.7 -47 12  Vel  8.8   4  I 1 r     70  Lynga   
  IC  2395 Cr 192           08 42.5 -48 08  Vel  4.6   7  II 3 m    40  Lynga   
           Cr 203  Tr 10    08 47.8 -42 30  Vel  5.0  14  II 3 m    40  Lynga   
* NGC 3114 Cr 215  Mel 98   10 02.7 -60 06  Car  4.2  35  II 3 r   171  Lynga   

  NGC 3228 Cr 218           10 21.4 -51 43  Vel  6.0  18  II 3 p    15  Lynga   
  IC  2581 Cr 222           10 27.4 -57 38  Car  4.3   7  II 2 p n  25  Lynga   
* NGC 3293 Cr 224  Mel 100  10 35.8 -58 14  Car  4.7   5  I 3 r n   93  Lynga   
* NGC 3324 Cr 225           10 37.3 -58 40  Car  6.7   5  I 3 r n   44          
* IC  2602 Cr 229  Mel 102  10 43.0 -64 24  Car  1.6  49  I 3 r     60  Lynga   

           Cr 230  Tr 14    10 44.0 -59 33  Car  5.5   5            44  Lynga   
           Cr 228           10 44.0 -60 05  Car  4.4  14            98  Lynga   
           Cr 233  Tr 16    10 45.2 -59 43  Car  5.0  10  n         90  Lynga   
* NGC 3532 Cr 238  Mel 103  11 05.5 -58 44  Car  3.0  55  II 3 r   150  Lynga   
* NGC 3572 Cr 239           11 10.3 -60 15  Car  6.6   6  II 3 m n  35  Lynga   

  NGC 3766 Cr 248  Mel 107  11 36.3 -61 37  Cen  5.3  12  I 3 r    100  Lynga   
* NGC 4755 Cr 264  Mel 114  12 53.6 -60 21  Cru  4.2  10  I 3 r    218          
  NGC 5281 Cr 276  Mel 120  13 46.6 -62 55  Cen  5.9   5  I 3 m     40  Lynga   
  NGC 5460 Cr 280  Mel 123  14 07.6 -48 18  Cen  5.6  24  I 3 m     40  Lynga   
  NGC 6067 Cr 298  Mel 140  16 13.2 -54 11  Nor  5.6  12  I 3 r    100  Lynga   

  NGC 6124 Cr 301  Mel 145  16 25.6 -40 39  Sco  5.8  29  I 3 r    100  Lynga   
  NGC 6193 Cr 310           16 41.3 -48 46  Ara  5.2  14  II 3 p n  14  Lynga   
* NGC 6231 Cr 315  Mel 153  16 54.2 -41 50  Sco  2.6  14  I 3 p     93  Archinal
  NGC 6242 Cr 317  Mel 155  16 55.5 -39 28  Sco  6.4   9  I 3 m     23  Lynga   
  NGC 6281 Cr 324  Mel 161  17 04.8 -37 53  Sco  5.4   8  II 2 p    70  Archinal

  IC  4651 Cr 327  Mel 169  17 24.7 -49 55  Ara  6.9  12  II 2 r    80  Lynga   
* NGC 6405 Cr 341  M6       17 40.7 -32 16  Sco  4.2  30  II 3 r    80  Lynga   
* NGC 6475 Cr 354  M7       17 53.9 -34 47  Sco  3.3  80  I 3 r     80  Lynga   
  NGC 6494 Cr 356  M23      17 56.9 -19 01  Sgr  5.5  27  II 2 r   150  Lynga   
  NGC 6530 Cr 362           18 04.5 -24 21  Sgr  4.6  14  II 2 m n 113  Lynga   

  IC  4725 Cr 382  M25      18 31.7 -19 07  Sgr  4.6  32  I 3 m     30  Lynga   
  NGC 6705 Cr 391  M11      18 51.1 -06 16  Sct  5.8  13  I 2 r    682  Lynga   
--------------------------------------------------------------------------------
BEST NORTHERN OPEN STAR CLUSTERS
--------------------------------------------------------------------------------
  NGC No.  Other Names      RA (2000) Dec   Con  Mag  Size Class    *n  Source  
                         hh mm.m  dd mm       v     ′                     
--------------------------------------------------------------------------------
  NGC 884  Cr 25   Mel 14   02 22.3 +57 08  Per  6.1  29  I 3 r    150  Lynga   
  NGC 869  Cr 24   Mel 13   02 19.1 +57 08  Per  5.3  29  I 3 r    200  Lynga   
  Pleiades M45              03 47.5 +24 06  Tau  1.2 110  I 3 r n  100  Sky Cat 
  Hyades                    04 26.9 +15 52  Tau  0.5 330  II 3 m   380  Archinal
  NGC 2632         M44      08 40.1 +19 59  Cnc  3.7  95  II 3 r    50  Archinal
--------------------------------------------------------------------------------
* Praesepe or the Beehive Cluster
* Description available. More will be added as time permits.

GENERAL CLUSTER DESCRIPTIONS

Of the southern clusters, three have some similar characteristics, but differ much in their comparative ages. From the brightness, compactness and mass range of each of the component stars, there is no doubt that the Jewel Box is one of the youngest of clusters. However, there a quite a few examples of clusters with similar ages and a few that are even younger.
Below I have attached some written text on these clusters so that observers might be able to compare these for themselves. (Figure B shows examples of these three 15′×15′ STScI images of clusters of similar size.)

NGC 3324

NGC 3324 / “The Second Jewel Box” / Δ322 / Cr 225 / C1035-583
Position : 10h 37.3m -58° 39′

NGC 3324 is in Carina and is of similar size (5 arcmin) and age to NGC 4755. This cluster is 1.3° NW of Eta Carinae, and it is presently speculated to be part of the enormous nebulosity complex in this region. Overall, the cluster covers about 10′, whose central 5′ area is completely embedded in nebulosity (see Figure B). Adding all the stellar magnitudes, NGC 3324 would appear as a 6.9 magnitude star. The brightest star is the O6 spectral class 8.4 mag SAO 238269 / PPM 339253* / HD 92206 that appears on the edge of the nebulosity and causes the nebulosity to shine. It is also identified as the John Herschel pair HJ 4338. (Note: Megastar 5.0 says this star is 6.9 mag. This is clearly wrong, as the combined magnitude is 8.6.) The double star’s components are listed as 8.9 and 9.6. and separated by 5.3″ along PA 91°. HJ 4338’s magnitudes to me seem slightly brighter than this, and I saw the colours were white and bluish. Since measures were first made in 1913, no change has been seen in the relative positions. Spectrally, the primary is an O6e or O5e class star, and it is likely this is the illuminator of the nebulosity.

Dunlop discovered this cluster in 1827, appearing as object Δ322 in his catalogue list. Here he says:

“A star of 7th magnitude, involved in a faint nebula.”

The faint nebulosity makes it appear more like a small globular in 15cm. Larger telescopes begin to see some faint structure to the nebula. David Frew in “March Deep-Sky Objects“ (Universe, 33, 3, p.9; March 1986) says of this nebulosity:

“This diffuse nebulosity is probably connected with the great Eta Carinae nebula, and hence lies about 7 000 ly away. It is fairly faint and amorphous, and surrounds the 8th magnitude double star h.4338. At least 15cm and rural skies are needed to see this one!”

Steve Crouch’s in his column “Southern Deep Sky” (Southern Astronomy Mar/ Apr 1994 p.55) says NGC 3324 is;

“…is a fairly large nebula in a rich star field on the north-western side of Eta Carinae. The most striking thing that I find about this nebula is its peculiar shape, having a smooth and well defined edge on the northern side but being very irregular on the opposite side. The shape is, of course, clearer with a nebula filter.”

Photographically, the cluster appears to me ‘horseshoe’ shaped, whose exit points point due east. Regarding the nebulosity, NGC 3324 has few dark globules. The Trumpler classified NGC 3324 as 1 3 r n and gave the first distance estimate of 3.3kpc, though latter-day values now favours about 3.8kpc. AOST2 gives the distance as 3kpc. Its age was first estimated to be some 2.2 million years, and this has slightly increased to about 3.5 to 3.6 million years. Overall, this is a nice cluster for medium to large apertures.

NGC 3114

Mel 98 / Cr 215 / C1001-598
Position :10h 02.7m -60° 06′

NGC 3114 is another bright Carina open cluster that shows some variations of colour in the component 120-odd stars. It is 5° W of the Eta Carinae Nebula, and its 40′ diameter appears very much larger in area than the Jewel Box. (If the Jewel Box were superimposed, it would only cover about twenty-five of the central stars of NGC 3114.) Overall this wonderful object is somewhat triangular shape, but some observers have also described NGC 3114 having six separate arms radiating from its core. Although similar in brightness to the Jewel Box (4.2 mag), NGC 3114 it is just visible in binoculars. At least 15cm telescope is required to show NGC 3114 with its hundred-odd stars shining in their full glory.

Dunlop said of this cluster (Δ297);

“A beautiful cluster of stars, arranged in curvilinear lines intersecting each other, about 40′ in diameter, extended south preceding, and north following.”

David Frew (Universe, 33, 3, p. 9; March 1986) says of NGC 3114:

“This is another large and conspicuous open cluster, that is about 4th magnitude and subtends some 35′ across. The brightest stars are about 8th magnitude, and are scattered over the face of the cluster, with no central gathering. The cluster is about 2 900 ly away.”

Quite near the centre of this cluster is the 6.18 mag HIP 49233 / SAO 237640 / PPM 357724. This is a white A6 II/III giant, and is by far the most luminous star of the cluster, and followed by about twenty-five 8th and 9th magnitude stars. It has been calculated that this cluster is 0.9kpc from us, and that the true diameter crosses about 8.5pc — about one star per parsec. Classed by Trumpler as ‘2 3 r -’. The age then estimated between 60 and 120 million years, though the higher results seem still currently preferred.

NGC 3293

Cr 224 / Mel 100 / Rb 85 / Ld 153 / C1133-579
Position : 11h 35.8m -58° 14′ (U427)

NGC 3293 is another Carina open cluster that is of a similiar age to the Jewel Box.
This cluster has an associated bright nebulosity being Gum 30 covering some 28.3′×17.4″, that is wrongly given as also NGC 3293. NGC 3293 is only the cluster. Gum 30 appears roughly triangular in shape whose longest axis is almost perfectly aligned north-south. Some ninety-three (93) components have been presently identified. In brightness, the total magnitude is 4.7, while the estimated Trumpler class is I 3 r n.

NGC 3293 is best found 40′S from the 4.5 magnitude orange K3/K4II star, HIP 51849 / SAO 238222 / HD 91942 (10356-5733). The cluster also happens to lie in quite a bright portion of the Milky Way, being some 1.6° (PA 312°) from the very centre of the bright Eta Carina nebula, NGC 3372 (10440-5930) which cover 2° of sky. The Eta Carina Nebulae is a pproximately centred on another relatively young open cluster Tr 15 / Cr 231 (10447-5921). This small and moderately bright but contains only about twenty stars. Alternatively, this cluster can be found about 32′NW of fellow cluster, NGC 3324 (10373-5839).

The brightest star lies 2.1′ NNW (PA 333°) from the observed cluster’s centre. This is the bluish-white 6.4v (6.7V) magnitude HIP 51857 / SAO 238225 / HD 91943 (10357-5781) From the B-V of +0.042 and spectral class B0.5Ib, this is the most luminous star in NGC 3293 — equal in ovrall nature to the brightest star in the Jewel Box cluster (HIP 62894) at the apex of the A-shape.
Likely the Jewel Box there is also one red-orangery supergiant that stands out. Lying 1.4°SSW (204°), this is 7.1 magnitude star does not appear in Hipparcos Catalogue but only in the Tycho one as T 8613:1280:1. Listed also as V361 Car / SAO 238228 (10357-5815) this star prodominately sticks out from the rest of the oher blue to white coloured stars and does dominates the entire cluster. The B−V is +1.443 and is placed at 10h 35m 44s -58° 14′ 42″. V361 Car is also an irrgular LC variable star which varies between 7.09V and 7.57V. This staris ideally placd for amateurs todo variable star observation with numerous comparison stars. The magnitude variations are clearly obvious, though it was certainly difficult to estimate a true magnitude because of the colour diferences — a classic example of the so-called Purkinje Effect.
A third prominent 6.5 magnitude white star at the very centre ofthe cluster. This is 6.4v magnitude HIP 51866 / SAO 238230 / HD 91969 which, like HIP 51857 above, is not a variable. An accurate position is 10h 35m 49s -58° 13′ 27″, and the star has a B−V of +0.009 and with the given spectral class of B0Ia.

The most recent age for NGC 3293 is 10.3 m.yr as stated in Dias, W.S., et al. “New Catalog of Optically Visible Open Clusters and Candidates”, A.&A., 389, 871 (2002). Distance is estimated to be 2.3 kpc.

Observational Descriptions

NGC 3293 was discovered by Abbe Nicholas Louis de la Callé from the Cape of Good Hope in 1752, who listed the cluster (L II 8);

“Small heap of 4 small stars to an lozenge.”

The early positions of this cluster remains in some dispute.

Lacaillé’ gives the 1st Jan 1752 positions as 10h 26m 32s -56° 56′ 05″ which is in 2000 coordinates is 10h 35m 57s -58° 12′ 49″. This is only about 1.2′WSW (PA 239°) from the centre of NGC 3293 — quite good considering the equipment he used. It is certainly more precise than Dunlop’s later placement, if it is indeed NGC 3293 and not NGC 3324 as concluded below;

Kenneth Glyn-Jones in “Search for the Nebulae” Pub. Alpha Academic (1975) pg.48 wrongly states;

“Class II Object 8 : Not identified: nearest object is 40′ north of Lacaillé’s position. This is IC 2581, Clust. diameter 5′, mag. 5.2”

Dunlop is stated as being the next to observed the cluster which stating he saw acluster on four seperate occassions during 1827. Here he describes DUN 321 / Δ321), as;

“A very small cluster of very bright small stars; round figure, above 4′ diameter; rich in the extremely small stars resembling faint nebula”

Dunlop’s 1827 position for NGC 3293 is 10h 27m 13s NPD 32° 37′ which translates into today’s 2000 co-ordinates of 10h 33m 45s -58° 16′ 27″ and is 17.3′E (PA 81°). This is centered only some 1.2′ENE (PA 68°) on the cluster NGC 3324 and its bright nebula, IC 2599. Both these clusters (NGC 3293 and 3324) can be matched with Dunlop’s description but NOT in the given position. Something is simply wrong here, and so we cannot conclude that Δ321 is NGC 3293.

John Herschel only describes the cluster through his small refractor describing it as; “A fine bright rich not very large cluster.”. Quite amazingly did not gaze upon NGC 3293 with his 46cm f/13 speculum mirrored telescope. Why this did not happen is a mystery, because he would have surely seen the nebulosity — not to mention such a glorious sight. I am also surprised that Dunlop’s quite accurate description was not followed up by John Herschel in his relentless pursuit of Dunlop double stars and deep-sky objects. Another problem is also with Lacaillé’s position, which Herschel certainly had in his possession during this main southern survey. This problem is simply perpetuated in many references.

For a cluster which is so comparable with the Jewel Box - of which we have copious notes. This single failure is likely the whole cause of the neglect from visual observers een today. Burnham’s Celestial Handbook says both oddly and non-descriptly, NGC 3293 is an;

“Open cluster, bright, rich, 8′ diameter, about 50 stars 6..13th mag, with dark nebulosity to the south.”

E.J. Hartung comments in AOST1;

“;Marked concentric structure is known by this beautiful open star group which is somewhat irregularly round and about 5′ across; it is bright, with stars of diferent colours. R is about 900pc.” ”

There is much to comment on this AOST1 description. The concentric structure he refers too does not seem me visible in either 20cm or 30cm — the same aperture that Hartung uses. Secondly none of the nebulosity is described at all, which is quite visible in dark skies using 30cm and averted vision. Thirdly Hartung fails to mention anything about the surrounding nebulosities at all. Another small problem is the distance, which is now estimated to be two-and-a-half times further at 2.3 kpc.

Also within AOST1’s pages are two black and white plates (Plates 3 and 4) taken by A.R. Hogg that show both the Jewel Box and NGC 3293 (Hartung Object Nos. 387 &497). These are worthy comparisons to look at. If anything, I think the stars of NGC 3293 are even more stunning than the Jewel Box. I can remember comparing these two clusters in AOST1 when I first became interested in astronomy, immediately thinking that I must look at each in succession with my own eyes. Overall I straight away thought this is a worthy and true rival to the Jewel Box.

In AOST2 this information on this cluster is vastly improved. David Frew appropriately adds ;

“Called the Gem Cluster by H.C. Russell, it is reminiscent of the Jewel Box (NGC 4755), containing abright red supergiant which contrasts nicely with the other cluster members. It is a fine object in even the smallest telescopes, and is about 2800pc. distant. ”

American J. Corder states in the Webb Society Deep Sky Observer’s Handbook; Vol.7 “The Southern Sky” pg.38; who sees NGC 3293 as;

10.5cm “Small, compact and easy cluster. 12 stars seen at 30′, Angularly round.”

While South African observer V. Hirsch in the see reference above correctly describes;

“Seems like a globular in the finder”

J. Graham Little wrote about NGC 3293 in his “Ten O’clock High” (Southern Astronomy, Mar/ Apr 1994 p.54-55);

“Another smallish but nice cluster, once again visible through ’scopes of 6cm or more. [It] has a diameter of about 6’… [and] the 50 stars being from mag. 6.5 to approx. 13.0. Visually this is a fairly condensed little cluster which stands out well from the background stars. Colours present are white, blue, green and red. There is some faint nebulosity present, with a patch of dark nebulosity to the south.”
“[H.C. Russell referred to this as the “Gem” cluster in an 1879 paper: it is now sometimes called the “Diamonds and Rubies Cluster” …Ed.]”

In April 2005 Australian Sky and Telescope (Frew, D., “The Eta Carinae Region*” *A.S&T., 1,4, p.60-61 (2005)), David Frew describes NGC 3293 as;

“A beautiful bright open cluster… A good 6cm refractor will show the nature of the group. which in my opinion is the best in the southern skies for small telescopes. Note how the bright stars are crowded into an area only about 6′ across, and arranged almost concentrically. As a bonus V361 Carinae is found… and contrasts beautifully with the other cluster members. The star is similar in mass and luminosity to Betelgeuse.”

Amazingly, the cluster also does not appear in the Jack Bennett Southern catalogue! When I first read the catalogue I was quite impressed with the neo-Messier Catalogue, but quickly dismissed it as disappointing for not containing NGC 3293 (and one or two others) since it has many other much fainter objects and some of lesser importance. Since this time I have never referred to Bennett’s Catalogue in any of my observational descriptions — mainly not wanting it to be perpetuate it any future.

Mike Inglis in “Astronomy of the Milky Way : Observer’s Guide to the Southern Sky” (2004)

“One cluster that is perhaps best suited to smaller telescopes is NGC 3114. It has about 50 stars spread over a region 35 arcseconds in diameter. The total magnitude of the cluster is 4.2, and it is interesting to compare this cluster with the previous one, NGC 2516, to see which one you find the most pleasing. The cluster NGC 3293, also called the Gem Cluster, is a very nice group to look for (see Figure 3.6). It is bright but small, at about 6 arcseconds in diameter, and has a bright red supergiant star at its center which makes a nice contrast with the other members.”

Even in the very recent (2004) book by Archinal, B., Hynes, S. “Star Clusters”, Catalogue pg.41-110 Pub. by Willmann-Bell. (2004), NGC 3293 doesn’t even rate a mention in the ‘Extended Notes’ !
[A similar problem to this is faced with one of the Top 20 brightest open cluster, the magnificent NGC 2516. This cluster is even visible in the city, appearing as a faint but largish haze.]

Double Stars in NGC 3293

1
2
3
4
5
6
7
8
Desig.     Pos.(2000)  Mag  Mag  Sep  PA   Yr  Sp
BRT 3145  (10355-5816) 10.6 12.8  4.3  40 1924   
DAW 52 BC (10357-5814)  9.5 12.5  2.3  35 1918   
DAW 51    (10358-5812)  9.4 12.0  2.3 183 1918 B1
B 2251 Aa (10358-5814)  8.5 14.0  3.0  10  --    
DAW 52 AB (10358-5814)  8.5  9.5 14.2 109 1918 B0
DAW 198   (10358-5815)  8.7  9.1 11.8 344 1918 B0
DAW 197   (10359-5813)  8.9  9.3 12.8 329 1918 B1

Variables in NGC 3293

1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
Desig     Pos.(2000)    Max   Min   Type    P(d) 
V400 Car (10348-5809)  9.76v  --    BCEP     --   
V401 Car (10355-5812)  9.56V  --    BCEP     --   
V402 Car (10355-5815)  9.91V 9.97V? GCAS     --   
V403 Car (10357-5813)  8.78V  --    BCEP     --   
V361 Car (10357-5815)  7.09V 7.57V  LC --         
V412 Car (10358-5814)  9.85V 9.88V  BCEP:    --   
V438 Car (10358-5815) 11.25V  --    ELL:     --   
V404 Car (10358-5814)  9.21V 9.23V  BCEP     --   
V405 Car (10358-5813)  9.29V  --    BCEP     --   
V439 Car (10359-5814) 13.46V  --    BE:--         
V378 Car (10359-5815)  9.22V  --    BCEP:   0.188 
V440 Car (10359-5813)  9.14B  --    BCEP     --   
V406 Car (10360-5812)  9.26V  --    BCEP     --   
V379 Car (10360-5814)  8.21V 9.34V  BCEP+E: 0.1753
V380 Car (10360-5815)  8.95V  --    BCEP:   0.236:
V381 Car (10361-5813)  9.04V 9.06V  BCEP:   0.17: 
V441 Car (10362-5814) 13.51V  --    ELL:     --

Mel 105

Cr 246 / Rb 80 / C1111-632
Position : 11h 19.7m -69° 29′

Mel 105 is the third Carina southern cluster suitable for comparison. Mel 105 in reality is likely an older version of NGC 4755 and can be found 5.9′ W from the Carina-Centaurus border. Its position is similar in declination to the multiple star Alpha (α) Crucis, some 7.5° further west. This 8.5 mag cluster has around seventy stars enclosed in its compact 4′ arcmin, and is contained in a pretty and starry field.

Small telescopes between 7.5cm and 10cm will see this object looking more like a slightly ovoid globular than an open cluster, and I still almost consider Mel 105 more as a ‘globular mimic’ (See Figure B). (I have listed some thirteen other clusters that I consider mimics). Apertures between 20cm and 25cm, and using low powers, will continue to see the cluster as unresolved. Increasing the magnification begins to see some stars. In 20cm. I could see perhaps thirty tiny points, and I was certain for the want of more telescopic aperture, I would have seen more stars. The threshold magnitude must be about 13th. Most of the stars I was seeing were certainly 13th and 14th. I still wondered why I had never read or seen much amateur information on this wonderful cluster.

Presently, distance is estimated at 2.1 to 2.2kpc, but the extinction by interstellar absorption being so high towards this region of space, makes the quoted results uncertain. Frandsen, Dreyer and Kjeldsen (A&A., 215, 287 (1989)) estimate from the CCD photometric data obtained from the 1.5-metre telescope at La Silla. Chile, an age of 150 million years. (Sky Catalogue 2000.0 suggests 59 million years, but this is likely too low.) Trumpler classes it as ‘I 2 p -’, though recently it was downgraded to ‘I 3 m -’.

NGC 6231

NGC 6231 / Mel 53 / Cr315
16h 54.0m -41° 47′

NGC 6406 / M6

NGC 6405 / The Butterfly Cluster / M6 / Mel 178 / C1736-321 (1

更配得上宝盒星团称号的宝石星团

https://www.astronomyclub.xyz/hidden-treasure/ngc-3293.html

如果天上有一个物体比卡帕（k）克鲁西斯（NGC 4755 [Caldwell 94]）更配得上Jewel Box绰号，那它就是位于Carina的疏散星团NGC 3293。这个4级宝箱在仅5’宽的区域中包裹着93级8级星和微弱的恒星-几乎是大猎户星座星云（M42）的梯形表观直径的一半。虽然Crux中的Jewel Box的大小是我们隐藏的宝藏的两倍，并且包含三倍的成员，但其恒星却无法像NGC 3293中那些明亮而紧密包装的恒星那样，特别是在小型望远镜中。

面对现实吧，Jewel Box的吸引力之一就是它的位置。它在著名的南十字星的东臂尽头像钻石戒指一样闪闪发光，它的美丽有助于照亮那个被称为科萨克星云的黑海星云的凄凉海岸。另一方面，NGC 3293的不幸之处在于，它仅位于Eta（t |）Carinae岩心的西北西北约2°处，这是一个庞大而诱人的发光气体，深色尘埃和热O-和B型星，其中许多位于星团中。NGC 3293不仅比Eta Carinae星云及其相关的星光小24倍，而且还被Carina的十几个其他开放星团包围，包括2级IC 2391（南部the宿星[Caldwell 85]） ，3幅NGC 3532（针垫簇[Caldwell 91]），

然而，NGC 3293可以说是整个地区最引人注目的对象。虽然它位于Eta Carinae建筑群的边缘，但它为该地区的气体云提供了一些照明-正如在黑暗天空下的任何照片或广角望远镜所显示的那样。星团中的一些恒星照亮了NGC 3293北部的一条反射星云，而紧靠星团东南部的是一个暗星云，它似乎是穿过Eta Carinae星云的突出尘埃带的一部分。DG特纳（David Dunlop天文台）和他的同事提出了NGC 3293可能与Carina Nebula联合体中其他物体相关联的可能性，而Carina Nebula联合体是Carina OB1联合体的核心。

NGC 3293非常年轻（约一千万年），包含大量B型巨人和超巨人，以及M型超巨人。它的年龄类似于英仙座的双星团（Caldwell 14）。特纳及其同事怀疑，NGC 3293可能与IC 2581物理相关，IC 2581是位于Carina的另一个4级星团，与西北方向成14度角。特纳和他的同事们将它们视为双星团的南半球类似物，尽管还需要收集更多数据以证实这一理论（另请参阅《隐藏的宝藏》 25和26）。

根据他们对该地区的研究，特纳和他的同事们建议，在该地区西北部发起的Carina OB1协会的恒星形成过程导致了NGC 3293和IC 2581的产生。在这两个星团的向东和向南逐渐分布的区域中，恒星形成跟随。研究人员警告说：“这张相当简单的图片并不能说明所有观察结果。”尤其是因为该地区存在一些异常星团。无论如何，似乎NGC 3293和IC 2581代表了该协会中最古老的恒星形成区域之一。但是，正如帕多瓦大学（University of Padova）的G.鲍姆（G. Baume）和他的同事在2003年的天文学和天体物理学论文中所报告的那样，在NGC 3293区域中有19颗具有H-alpha发射迹象的恒星，

尽管拉卡耶以发现星团NGC 3293（在他的1755年目录中是第八个“星云团”）而著称，但该物体是银河系裸眼背景的一部分，毫无疑问，它被许多人视作无害星Wonderstruck原住民观星者-历史上第一批天体寻宝者。当詹姆斯·邓洛普（James Dun-lop）在1826年4月29日观察到它时，他看到“一小群非常小的明亮的恒星；圆形的物体，直径约4’；富含像微弱的星云的极小恒星”。

拉卡耶和邓洛普对星云的提及都很好奇，只是因为正如前文所述，星云与它北端的星团有关。van den Bergh和Herbst在1975年的“嵌入星云中的南方恒星目录”中列出了两个反射星云：BHe 42A和BHe 42B。第一星云围绕着发光的恒星，在红色板上的距离为4’。第二个星云位于北部和西部，在最强的蓝色平板上测量为1.6’。Colin S. Gum在他的“南部H II地区调查”中也将它们列为Gum 30。他将星云的最大直径定为40’，并且相对于背景银河系，它的亮度适中。有趣的是，很少有观察者看到过这种星云，我想知道为什么。

要找到这个令人惊叹的星团和神秘的星云，请看大埃塔嘉里纳星云西北2°，以寻找两个4级的恒星，它们之间

1585381302558

大约40’。北极星是r Carinae；最南端的是NGC3293。在7 x 50双筒望远镜中，星团是模糊的椭圆形光，悬挂在4°8级恒星（如“蜘蛛嘴”）的1°长分支上-泡沫状的白色胚胎粘液，从各个角度的昆虫在野外进化。分支从东到西北呈弧形，并与一些较暗的恒星形成真实的分支或叉骨形。该星团的核心非常明亮，并带有略微膨胀的圆盘，很明显，一颗星向北分离。随着时间的流逝，中央磁盘会分裂成一群非常拥挤的太阳。避开视线，群似乎在颤抖和膨胀，好像它是由可塑粘土制成的一样，里面的东西正试图将其推出。在古董望远镜中，纤芯更清晰，看上去更拉伸，

这个星团看起来像是23倍，只是现在茧被分解成一团炽热的恒星。很难判断哪些恒星是成员，但是无论如何，随着放大倍数的增加，大约有40至50个太阳会燃烧。它们是各种色彩鲜艳的球体，令人眼花especially乱，尤其是一颗金色的星星-星团中年龄最快的M型成员。这颗星是三颗星中最南端的一颗，与星团核心处的亮星形成一条东北-西南趋势线。围绕着这颗明亮的恒星，星团的微弱成员像虫子一样蜂拥而至。一条长臂向东延伸，而另一端则粗短，向西延伸到一个明显的三角形。如果您有海盗的眼球，也许不是这个集群（具有强大的中轴，手臂，

如果看不到上述星云，请不要担心，几乎没有。但是我发现在放大倍数下它并不明显。它需要低功率和避开视线，以及区分星云和银河系的能力，这需要经验丰富但又独具慧眼的人。首先尝试双筒望远镜。如果不这样做，请将您的望远镜向东南移动30多一点，在那里您会发现一颗6级恒星沉浸在一个微小但明亮的反射星云中（NGC 3324）。邓洛普发现了星云，在原始NGC中将其描述为“相当明亮，非常大，不规则晕倒的双星参与”。注意，这里没有提到集群。但是，今天，大多数来源和星图都将NGC 3324标记为一个簇。

最后，我认为必须注意的是，尽管NGC 3293的真实物理直径为12光年（与珠宝盒的直径大致相同），但它的距离几乎是珠宝盒的两倍。如果我们可以拖曳NGC 3293并将其放置在Jewel Box旁边，我们会发现它具有大约相同的表观直径，但发出的光几乎高出了整整一倍-几乎与Delta（8）Crucis一样，这是标志着十字架的西臂。

If THERE is ONE OBJECT in the sky more deserving of the Jewel Box moniker than Kappa (k) Crucis (NGC 4755 [Caldwell 94]), it is open cluster NGC 3293 in Carina. This 4th-magnitude treasure chest packs 93 stars, 8th-magnitude and fainter, in an area only 5’-wide - almost half the apparent diameter of the Trapezium in the Great Orion Nebula (M42). And while the Jewel Box in Crux is twice as large as our hidden treasure and contains three times as many members, its stars do not punch the eye the way those bright and tightly packed ones in NGC 3293 do, especially in small telescopes.

Let’s face it, part of the Jewel Box’s attraction is its location. It shines like a diamond ring at the end of the eastern arm of the famous Southern Cross, and itsbeautyhelps to illuminate the bleak shores of that Black Sea of nebulosity known as Coalsack Nebula to its south. NGC 3293, on the other hand, suffers the misfortune of lying only about 2° north-northwest of the core of the Eta (t|) Carinae complex, a vast and alluring network of glowing gas, dark dust, and hot O- and B-type stars, many of which lie in clusters. Not only is NGC 3293 some 24 times smaller than the Eta Carinae Nebula and its associated starlight, but it is also surrounded by more than a dozen other open clusters in Carina, including 2nd-magnitude IC 2391 (the Southern Pleiades [Caldwell 85]), 3rd-magnitude NGC 3532 (the Pin Cushion Cluster [Caldwell 91]), and 4th-magnitude NGC 3114 - all dynamic objects, all vying for one’s attention, and all deserving of one’s time.

Yet NGC 3293 is arguably the most striking object in the entire region. And while it lies on the fringe of the Eta Carinae complex, it contributes some illumination to the clouds of gas in the region - as any photograph or wide-field telescope under dark skies will show. Some of the cluster’s stars illuminate a river of reflection nebulosity in the northern part of NGC 3293, while immediately to the cluster’s southeast lies a dark nebula, which appears to be part of the prominent dust lane that runs through the Eta Carinae Nebula. D. G. Turner (David Dunlop Observatory) and his colleagues have raised the possibility that NGC 3293 may be associated with other objects in the Carina Nebula complex, which is the heart of the Carina OB1 association.

NGC 3293 is very young (~10 million years) and contains a large number of B-type giants and supergiants, as well as an M-type supergiant. Its age is similar to that of the Double Cluster in Perseus (Caldwell 14). Turner and his colleagues suspect that NGC 3293 may be physically related to IC 2581, another 4th-magnitude cluster in Carina, about l4 ° to the northwest. Turner and his colleagues see them as a Southern Hemisphere analog to the Double Cluster, though more data need to be collected to confirm this theory (see also Hidden Treasures 25 and 26).

Based on their studies of the region, Turner and his colleagues suggest that the star-forming process in the Carina OB1 Association, which was initiated in the northwest section of the region, led to the creation of NGC 3293 and IC 2581. Later episodes of star formation followed in regions lying progressively eastward and southward of these two clusters. “This rather simple picture does not account for all the observations,” the researchers warn, especially since there are some anomalous clusters in the region. No matter, it appears that NGC 3293 and IC 2581 represent one of the oldest areas of star formation in the associa tion. But as G. Baume (University of Padova) and his colleagues report in a 2003 Astronomy and Astrophysics paper, 19 stars with signs of H-alpha emission in the region of NGC 3293, indicate that star formation is still active there.

Although Lacaille is credited with discovering the cluster NGC 3293 (it is the eighth “nebulous cluster” in his 1755 catalog), the object is part of the naked-eye backdrop of the Milky Way and no doubt was spied as an innocuous star by numerous wonderstruck aboriginal stargazers - history’s first celestial treasure hunters. When James Dun-lop observed it on April 29, 1826, he saw “a very small cluster of very small bright stars;round figure, about 4’ diameter;rich in extremely small stars resembling faint nebulosity.”

Both Lacaille’s and Dunlop’s reference to nebulosity is curious, only because, as stated earlier, nebulosity is involved with the cluster at its northern edge. In their 1975 “Catalogue of Southern stars embedded in nebulosity,” van den Bergh and Herbst list two reflection nebulae here: BHe 42A and BHe 42B. The firstnebula surrounds the illuminating star and measures 4’ across on red plates. The second nebula lies just to the north and west and measures 1.6’ on the blue plates, where it is strongest. Colin S. Gum, also lists them as Gum 30 in his “A survey of Southern H II regions.” He gives the nebula a maximum diameter of 40’ and rates it as being moderately bright against the background Milky Way. Interestingly, few observers have seen the nebulosity, and I have to wonder why.

To find this stunning cluster and mysterious nebulosity, look about 2° north-northwest of the Great Eta Carinae Nebula for two 4th-magnitude stars separated by

some 40’. The northern star is r Carinae; the southern one is NGC 3293. In 7 x 50 binoculars, the cluster is a fuzzy ellipse of light hanging on a 1 °-long branch of four 8th-magnitude stars like “spider spit” - that foamy white embryonic goo from which all manner of insects evolve in the wild. The branch arcs gracefully from the east to the northwest and with some fainter stars forms a true branch or wishbone pattern. The cluster’s core is very bright with a slightly swollen disk, one star is clearly separated to the north. With time the central disk breaks up into a swarm of extremely congested suns. With averted vision, the swarm seems to tremble and swell erratically, as if it were made of moldable clay, and something inside is trying to push its way out. In the antique telescope, the core is more defined and looks stretched, like taffy, from the northwest to the southeast.

The cluster looks similar at 23x, only now the cocoon breaks down into a sizzling swarm of stars. It’s hard to judge which stars are members, but no matter, some 40 to 50 suns burn into view with any increase of magnification. They are a dazzling assortment of colorful orbs, especially one golden star -the one type-M member of the cluster which has aged the fastest. This star is the southernmost of three, which form a northeast-southwest trending line from the bright star at the cluster’s core. It is around this bright star that the cluster’s fainter members swarm like bugs to a light. A long arm extending to the east, and a stubby one, end at a distinct triangle to the west. If you’ve got a pirate’s eye, might not the cluster (with its strong central axis, arms, and sharp surrounding starlight) be a sterling silver crucifix wrapped in a crystal bead rosary - a treasure well worth pocketing on the way to the gallows.

If you cannot see the nebula described above, don’t fret, few have. But I find it is not apparent under magnification. It requires low power and averted vision, as well as the ability to differentiate nebulosity from Milky Way, which takes an experienced yet discerning eye. Try first in binoculars. If you fail to do so, move your scope a little more than 30’ to the southeast, where you will find a 6th-magnitude star immersed in a tiny but bright reflection nebulosity (NGC 3324). Dunlop discovered the nebulosity, which is described in the original NGC as “pretty bright, very large, irregularly faint, double star involved.” Note that there has been no mention of a cluster. Yet, today, most sources and star charts label NGC 3324 as a cluster.

Finally, I think it’s important to note that although NGC 3293 has a true physical diameter of 12 light-years (about the same as the Jewel Box’s), it is nearly twice the distance of the Jewel Box. If we could haul in NGC 3293 and position it next to the Jewel Box, we’d find it having about the same apparent diameter but shining nearly a full magnitude brighter - almost as bright as Delta (8) Crucis, the star that marks the western arm of the Cross.

ASSA TOP 100

The Top-100 Deep-Sky Objects
N ID Other designations Ben Type Mag Size Con/td> RA Dec
1 NGC 55 LEDA 1014 1 Glxy 7.9 32’x5.6’ Scl 00 15 –39 11
2 NGC 104 47 Tucanae 2 Glcl 4.5 31’ Tuc 00 24 – 72 05
3 NGC 247 LEDA 2758 3 Glxy 8.9 18’ x 5’ Cet 00 47 – 20 46
4 NGC 246 PN G118.8-74.7 Plnb 8.5 4’ x 3.5’ Cet 00 47 – 11 53
5 NGC 253 Silver Coin 4 Glxy 7.1 22’ x 6’ Scl 00 48 – 25 17
6 NGC 288 Mel 3 5 Glcl 8.1 14’ Scl 00 53 – 26 35
7 SMC Glxy 2.3 5° x 3° Tuc 00 53 – 72 50
8 NGC 362 Mel 4 7 Glcl 6.6 13’ Tuc 01 03 – 70 51
9 NGC 1068 M 77 9 Glxy 8.9 7.1’ x 6.0’ Cet 02 43 – 00 01
10 NGC 1261 GCl 5 11 Glcl 8.4 7’ Hor 03 12 – 55 13
11 NGC 1291 NGC 1269 12 Glxy 9 11’ Eri 03 17 – 41 08
12 NGC 1316 Fornax A 14 Glxy 8.5 12‘ x 8.5’ For 03 23 – 37 12
13 NGC 1365 LEDA 13179 16 Glxy 9.5 9’ x 4’ For 03 34 – 36 08
14 NGC 1535 PN G206.4-40.5 22 Plnb 9.3 20” x 17” Eri 04 14 – 12 44
15 NGC 1851 GCl 9 32 Glcl 7.3 11’ Col 05 14 – 40 03
16 LMC Glxy 0.5 11° x 9° Dor 05 24 – 69 45
17 NGC 1904 M 79 34 Glcl 8.4 3’ Lep 05 25 – 24 33
18 NGC 1976 Orion Nebula, M 42 BrtN 2.9 1.1° x 1° Ori 05 35 – 05 27
19 NGC 1977 BrtN 4.6 20’ x 10’ Ori 05 36 – 04 52
20 NGC 2070 Tarantula Nebula 35 BrtN 40’ Dor 05 39 – 69 06
21 NGC 2287 Messier 41 OpCl 4.6 38’ CMa 06 46 – 20 46
22 NGC 2362 Tau CMa cluster OpCl 4.1 8’ CMa 07 19 – 24 57
23 NGC 2422 Messier 47 OpCl 4.5 30’ Pup 07 37 – 14 30
24 NGC 2437 Messier 46 OpCl 6.1 27’ Pup 07 42 – 14 49
25 NGC 2451 VdB-H 9 OpCl 2.8 45’ Pup 07 45 – 37 58
26 NGC 2447 M 93 OpCl 6.2 22’ Pup 07 45 – 23 52
27 NGC 2477 VdB-H 13 OpCl 5.7 27’ Pup 07 52 – 38 33
28 NGC 2516 OCl 776.0 OpCl 3.8 30 Car 07 58 – 60 52
29 NGC 2547 OpCl 4.7 20’ Vel 08 11 – 49 16
30 NGC 2548 M 48 OpCl 5.8 55’ Hya 08 14 – 05 48
31 IC 2391 omicron Vel Cluster OpCl 2.5 50’ Vel 08 40 – 53 04
32 NGC 2808 GCl 13 41 Glcl 6.3 14’ Car 09 12 – 64 52
33 NGC 2818 PN G261.9+08.5 OpCl 8.2 9’ Pyx 09 16 – 36 37
34 IC 2488 VdB-H 69 OpCl 7.4 15’ Vel 09 28 – 56 59
35 NGC 3114 VdB-H 86 OpCl 4.2 35’ Car 10 03 – 60 07
36 NGC 3115 Spindle Galaxy 42 Glxy 8.9 7.2’ x2.5’ Sex 10 05 – 07 43
37 NGC 3132 Eight-Burst Nebula 43 Plnb 8.2 84” x 53” Vel 10 08 – 40 26
38 NGC 3201 GCl 15 44 Glcl 6.8 18’ Vel 10 18 – 46 25
39 NGC 3242 Ghost of Jupiter 45 Plnb 8.6 16” Hya 10 25 – 18 38
40 IC 2581 VdB-H 97 OpCl 4.3 8’ Car 10 27 – 57 38
41 NGC 3293 Cr 224 OpCl 4.7 40 Car 10 36 – 58 14
42 NGC 3324 Ced 108 BrtN 6.7 6’ Car 10 37 – 58 38
43 IC 2602 Southern Pleiades OpCl 1.9 50’ Car 10 43 – 64 24
44 NGC 3372 eta Carinae Nebula BrtN 5 120’ Car 10 44 – 59 52
45 NGC 3532 VdB-H 109 OpCl 3 55’ Car 11 06 – 58 40
46 NGC 3766 BRAN 360, VdB-H 120 OpCl 5.3 12 Cen 11 36 – 61 37
47 NGC 3918 Blue Planetary Plnb 8.4 12 Cen 11 50 – 57 11
48 NGC 4361 PN G294.1+43.6 Plnb 10.3 45” Crv 12 25 – 18 48
49 Black Python SDC 301.0-08.6c DrkN – 80’ x 3’ Mus 12 27 – 71 25
50 NGC 4594 Sombrero, M 104 52 Glxy 8 8.7’ x 3.5’ Vir 12 40 – 11 37
51 Coalsack DrkN – 6.5° x 5° Cru 12 53 – 63 00
52 NGC 4755 Herschel’s Jewel Box OpCl 4.2 10’ Cru 12 54 – 60 20
53 NGC 4833 GCl 21 56 Glcl 7.4 14’ Mus 13 00 – 70 53
54 NGC 4945 LEDA 45279 57 Glxy 8.3 20’ x 3.8’ Cen 13 05 – 49 28
55 NGC 5128 Centaurus A 60 Glxy 7 18’ x 14’ Cen 13 26 – 43 01
56 NGC 5139 Omega Centauri 61 Glcl 3.7 36’ Cen 13 27 – 47 29
57 NGC 5189 IC 4274 62 Plnb 10.3 2.6’ Mus 13 34 – 65 59
58 NGC 5236 M 83 63 Glxy 7.5 13’ x 11’ Hya 13 37 – 29 52
59 NGC 5281 VdB-H 152 OpCl 5.9 5’ Cen 13 47 – 62 54
60 NGC 5460 C 1404-480 OpCl 5.6 25’ Cen 14 08 – 48 19
61 NGC 5662 VdB-H 162 OpCl 5.5 12’ Cen 14 35 – 56 33
62 NGC 5822 VdB-H 168, Mel 130 OpCl 6.5 40’ Lup 15 05 – 54 21
63 NGC 5823 VdB-H 169, Mel 131 OpCl 7.9 10’ Cir 15 06 – 55 36
64 Barnard 228 Be 148 DrkN – 4° x 20’ Lup 15 45 – 34 24
65 NGC 6025 VdB-H 181 OpCl 5.1 12’ TrA 16 04 – 60 30
66 NGC 6067 Mel 140 OpCl 5.6 13’ Nor 16 13 – 54 13
67 NGC 6087 S Norma Cluster OpCl 5.4 12’ Nor 16 19 – 57 54
68 NGC 6121 Me 4, GCl 41 75 Glcl 6 26’ Sco 16 24 – 26 32
69 NGC 6124 C 1622-405 OpCl 5.8 29’ Sco 16 26 – 40 40
70 NGC 6193 VdB-H 195 OpCl 5.2 15’ Ara 16 41 – 48 46
71 NGC 6218 M 12 80 Glcl 6.6 15’ Oph 16 47 – 01 57
72 NGC 6231 VdB-H 201 OpCl 2.6 15’ Sco 16 54 – 41 48
73 NGC 6254 Me 10 83 Glcl 6.6 15’ Oph 16 57 – 04 06
74 NGC 6266 Me 62, GCl 51 85 Glcl 6.6 14’ Oph 17 01 – 30 07
75 NGC 6273 M 19, GCl 52 86 Glcl 7.1 14’ Oph 17 03 – 26 16
76 NGC 6281 Cr 324 OpCl 5.4 8’ Sco 17 05 – 37 54
77 B 59-78 Pipe Nebula DrkN – 7° Oph 17 25 – 26 30
78 NGC 6405 Butterfly Cluster, M 6 OpCl 4.2 15’ Sco 17 40 – 32 13
79 NGC 6397 GCl 74 98 Glcl 5.6 26’ Ara 17 41 – 53 40
80 NGC 6475 Ptolemy’s Cluster, M 7 OpCl 3.3 80’ Sco 17 54 – 34 49
81 NGC 6494 M 23 OpCl 5.5 27’ Sgr 17 57 – 19 01
82 NGC 6514 Trifid Nebula, M 20 BrtN 8.5 29’ x 27’ Sgr 18 03 – 23 02
83 NGC 6523 Lagoon Nebula, M 8 BrtN 5.8 1.5° x 0.7° Sgr 18 04 – 24 23
84 NGC 6531 M 21 OpCl 5.9 13’ Sgr 18 05 – 22 30
85 NGC 6541 GCl 86 Glcl 6.6 13’ CrA 18 08 – 43 42
86 NGC 6584 GCl 92 107 Glcl 9.2 8’ Tel 18 19 – 52 13
87 NGC 6618 Omega Nebula, M 17 108 BrtN 7 0.8° x 0.6° Sgr 18 21 – 16 11
88 IC 4715 M 24 *cld 3.1 95’ x 35’ Sgr 18 27 – 18 23
89 IC 4725 M 25 OpCl 4.6 32’ Sgr 18 32 – 19 15
90 NGC 6656 M 22 114 Glcl 5.1 24’ Sgr 18 36 – 23 54
91 NGC 6705 Wild Duck Cluster, M 11 116 OpCl 5.8 14’ Sct 18 51 – 06 16
92 NGC 6723 ESO 396-SC010 119 Glcl 7.2 11’ Sgr 18 59 – 36 38
93 R CrA DCld359.8-17.9 DrkN – 110’ x 28’ CrA 19 02 – 37 03
94 NGC 6744 LEDA 62836 120 Glxy 9 15’ x 10’ Pav 19 10 – 63 51
95 NGC 6752 GCl 108 121 Glcl 5.4 20’ Pav 19 11 – 59 59
96 NGC 6809 M 55 122 Glcl 7 19’ Sgr 19 40 – 30 58
97 Melotte 227 Cr 411 OpCl 5.3 50’ Oct 20 12 – 79 19
98 NGC 7089 M 2 127 Glcl 6.5 13’ Aqr 21 34 – 00 49
99 NGC 7099 M 30 128 Glcl 7.5 11’ Cap 21 40 – 23 11
100 NGC 7293 Helix Nebula 129 Plnb 6.5 15’ x 12’ Aqr 22 30 – 20 48

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澳大利亚协会