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abell's planetarische nebel

 

 

 

George Abell veröffentlichte 1955 in vorläufiger und 1966 in endgültiger Form seinen Katalog Planetarischer Nebel. Dieser Katalog umfasste "alte" Planetarische Nebel,  von denen die Hälfte von Albert George Wilson und der Rest von  Robert G. Harrington,  Rudolph Minkowski und George Abell selbst auf den Platten der ersten Palomar Observatory Sky Survery (POSS I) entdeckt worden waren.

 

 

Download des Abell PN Beobachtungs-Atlas

(pdf-File 23 MByte, last update 2008)

 

Der Beobachtungsatlas umfasst den kompletten Katalog von George Abell (abzüglich der beiden ebenfalls aufgenommenen Plattenfehlern). Jeder PN ist vorgestellt mit zwei Aufsuchkarten mit einem Feld von 25° bzw. 5°. Ein 30' x 30' POSS II Bild erlaubt dann das Auffinden der exakten Position des Planetaries und gibt einen Eindruck von der zu erwartenden scheinbaren Größe.

Zusätzlich gibt zwei Detail-Abbildungen aus jeweils den blauen und den roten POSS II Platten, die hilfreich sind, die Helligkeit des PN im für uns zugänglichen Spektralbereich  zu beurteilen. Die relative spektrale Empfindlichkeit unseres Auges im Dämmerungssehen entspricht grob der der blauen POSS II Platten, die ihre maximale Empfindlichkeit zwischen 450 und 550 nm haben, während die roten POSS II Platten vor allem im Bereich von 620 bis 700 nm empfindlich sind (die POSS I Emulsionen hatten hingegen eine andere Verteilung, nämlich von 350 bis 500 nm bzw. von 620 bis 670 nm).

Der Vergleich der blauen und roten POSS II Bildern kann außerdem einen Hinweis auf den Anregungsgrad der Gas-Schalen des Planetaries geben. Die OIII-Linien des zweifach ionisierten Sauerstoffs liegen bei  501nm und 496nm (nur ein Drittel der Intensität der höheren Linie), während die HII-Linien des ionisierten Wasserstoffs bei 656 nm (H-alpha) bzw. bei 486nm (H-beta, nur ein Drittel der Intensität von H-alpha) emittiert wird. Erscheint in PN vor allem auf den blauen Platten hell, ist es in erster Linie ein Objekt für OIII-Filter. Ist er auf den roten Platten heller, so kann dies auf die H-alpha Linie und somit eine große Linienstärke in HII zurück zu führen sein. Da dies automatisch auch Emission in H-beta beinhaltet, ist in diesem Fall ein UHC-Filter, der die H-beta Linie mit beinhaltet, oftmals besser.

Einige der PN haben jedoch ihre größte Linienstärke in NII (655nm und 658nm), so dass "hell" auf den roten Platten nicht unbedingt gleichbedeutend mit hoher HII Linienstärke (in dem Fall H-alpha bei 656nm) ist! Da die meisten fotografischen H-alpha Filter (mit Ausnahme der 3nm-Filter) neben H-alpha auch NII voll durch lassen, wird selbst auf "H-alpha"-Aufnahmen meist gar nicht zwischen HII und NII differenziert. In diesen Fällen kann der OIII-Filter selbst bei auf Aufnahmen "tiefrot" erscheinenden Planetaries die bessere Wahl sein. Siehe hierzu auch hier.

 

References

 Abell GO (1955) Publ Astron Soc Pac 67: 258-261 

 Abell GO (1966) Astrophys J 144: 259-279

 

Links zu Abell PN Webseiten

Stathis Kafalis

Uwe Glahn

Steve Gottlieb und Jim Shields

Doug Snyder

 

 

Beobachtungen der Abell PN

 

Die folgenden Beobachtungen wurden seit 2006 zum größten Teil mit meinem 22" Dobson unter 6m0 bis 6m5 Bedingungen durchgeführt.

 

Abell 1 in Cepheus

00 12 54.6 +69 10 23

Even under excellent conditions no successful observation

No

DSS 12'x12'

 

Abell 2 in Cassiopeia

00 45 34.8 +57 57 35

 

At 200x, the PN appears with OIII filter as a conspicuous object and shows a small round disk.

DSS 12'x12'

 

Abell 3 in Cassiopeia

02 12 06.6 +64 09 03

 

Abell 3 is a difficult object. At 350x, the PN was suspected at times with OIII filter. Doubtful observation.

 

Francis Longstaff

DSS 12'x12'

 

Abell 4 in Perseus

02 45 23.8 +42 33 03

 

Visible without filter at 250x. At 350x with OIII filter, the PN is easy and appears as a small disk with direct vision. Responds also well to UHC. Nearby galaxy was not observed.

DSS 12'x12'

 

Abell 5 in Perseus

02 52 14.8 +50 35 54

 

Red emission is mostly NII, which is 4x stronger than HII (Frew 2013).

Not visible with either OIII, H beta, or UHC.

DSS 12'x12'

 

Abell 6 in Cassiopeia

02 58 42.0 +64 30 07

 

At 100x with OIII filter, the SE edge was visible at times, becomes more diffuse towards NW. Nearby star is disturbing.

 

David Ratledge

Stephane Zoll (with HFG 1)

DSS 12'x12'

 

Abell 7 in Lepus

05 03 07.5 -15 36 23

 

Appears as an extremely faint, large and diffuse patch N of a prominent asterism. OIII filter. Nearby galaxy is not visible.

Jim Shuder

Don Goldman

DSS 30'x30'

 

Abell 8 in Auriga

05 06 38.4 +39 08 09

 

At 200x with OIII filter, the PN is an easy object and appears as small disk superimposed to two small stars. OIII > UHC.

DSS 12'x12'

 

Abell 9 in Auriga

05 28 56.7 +36 03 05

 

Abell 9 is just at the northern edge of the OC M38 in Auriga.

 

David Ratledge

DSS 12'x12'

 

Abell 10 in Orion

05 31 45.8 +06 55 57

 

At 250x and with OIII filter, the PN is visible as a small and relatively bright disk. Easy object.

DSS 12'x12'

 

Abell 11 in Orion

05 37 22.1 +08 15 37

 

This is very likely a misclassification and rather a reflection nebula, as it shows no emission lines.

Nothing visible at 350x.

DSS 12'x12'

 

Abell 12 in Orion

06 02 20.0 +09 39 15

 

With OIII filter at 500x, it takes some time until the PN can be discerned for the first time. After that, it is a relatively easy object and appears as a small disk in the glare of µ Ori.

 

Carsten Dosche

DSS 12'x12'

 

Abell 13 in Orion

06 04 47.8 +03 56 36

 

Despite that the red color is intriguing,  this PN is strongest in NII and not in HII. According to Frew 2013 the ratio is 3.5.

For visual observers, it is therefore not necessarily an H-beta object. 

Michael Siniscalchi

Andreas Rörig

DSS 12'x12'

 

Abell 14 in Orion

06 11 08.7 +11 46 45

 

Red emission is mostly NII, which is 6x stronger than HII (Frew 2013).

 

DSS 12'x12'

 

Abell 15 in Canis Major

06 27 02.0 -25 22 50

 

This is a very low object and nothing is visible, despite relatively good transparency.

DSS 12'x12'

 

Abell 16 in Lynx

06 43 54.9 +61 47 25

 

Nothing visible.

DSS 12'x12'

 

Abell 17 in Monoceros

06 48 38.1 -09 32 43

This is likely a plate fault on a POSS I red plate. Nothing is visible on the corresponding POSS I blue plate, which was exposed 60 minutes earlier or on plates of later surveys.

Surprisingly, you  may find positive observing reports ...

 

 

 

Abell 18 in Monoceros

06 56 14.5 -02 53 09

 

Red emission is mostly NII, which is 2.5x stronger than HII (Frew 2013).

DSS 12'x12'

 

Abell 19 in Gemini

06 59 57.0 +14 36 35

 

 

DSS 12'x12'

Abell 20 in Canis Minor

07 22 57.6 +01 45 34

 

With UHC at 200x, the PN appears as a faint round disk with averted vision, quite distinct object with well defined borders.

DSS 12'x12'

 

Abell 21 in Gemini

07 29 04.5 +13 14 55

 

The most beautiful ear of the universe!

Visible already w/o filter. Responds very well to OIII filter.

E side forms filamentous crescent, which is relatively bright in OIII. Inside filled with weaker OIII emission. NW counterpart also visible as an extremely faint crescent along chain of stars, forms with E crescent a closed structure.

Don Goldman

JP Metsavainio

Ken Crawford

DSS 18'x18'

 

Abell 22 in Canis Minor

07 36 08.2 +02 42 24

 

Suspected as an extremely faint glow around star.

 

Andreas Rörig

DSS 12'x12'

 

Abell 23 in Puppis

07 43 18.0 -34 45 12

 

 

DSS 12'x12'

 

Abell 24 in Canis Minor

07 51 39.3 +03 00 29

 

This is again one of these funny red nebula that should respond well to H beta, but don't. According to Madsen et al., the red color is not due to to HII, but NII, which is about 5 times stronger than H-alpha and 7 times stronger than OIII. This makes OIII the strongest visual line, even that it doesn't look like this.

Nevertheless, even with OIII filter, the PN appears extremely faint, round and featureless.

 

Jim Misti

DSS 18'x18'

 

Abell 25 in Monoceros

08 06 46.0 -02 52 42

 

 

DSS 12'x12'

 

Abell 26 in Puppis

08 09 01.6 -32 40 25

 

 

DSS 12'x12'

 

Abell 27 in Pyxis

08 31 52.5 -32 06 10

 

Red emission is mostly NII, which is 4.6 x stronger than HII (Frew 2013).

DSS 12'x12'

 

Abell 28 in Ursa Major

08 41 35.5 +58 13 49

 

According to Madsen et al., this should be an object for the H-beta filter.

 

Martin Rusterholz

DSS 18'x18'

 

Abell 29 in Pyxis

08 40 17.0 -20 54 14

 

According to Tweedy and Kwitter, NII is stronger than HII with this PN, with some OIII being detectable. According to Frew 2013, NII is 6x stronger than HII.

DSS 18'x18'

 

Abell 30 in Cancer

08 46 53.6 +17 52 44

 

With OIII filter at 200x, the PN appears as a diffuse glow around central star, not well defined. OIII > UHC.

 

NOAO

DSS 12'x12'

 

Abell 31 in Cancer

08 54 13.2 +08 53 59

 

This is the largest Abell PN with a size of 17'x16' (of which, however, only the central part is visible) !

With OIII filter at 100x, Abell 31 is a relatively easy object and appears diffuse with no distinct boundaries. Internal structure is suspected but difficult to pin down.

Don Goldman

Capella

Adam Block

DSS 30'x30'

 

Abell 32 in Hydra

09 16 21.6 +03 53 04

 

This is likely a plate fault on a POSS I red plate. Nothing is visible on the corresponding POSS I blue plate, which was exposed 15 minutes earlier or on plates of later surveys.

 

 

 

Abell 33 in Hydra

09 39 09.1 -02 48 32

 

With OIII filter at 200x, this is a beautiful and perfect PN with distinct disk next to star. Darker center suspected. Well defined NW edge, lesser defined towards SE, appears therefore a bit oval. A bit less distinct with UHC.

 

Adam Block

Jim Misti

DSS 12'x12'

 

Abell 34 in Hydra

09 45 35.0 -13 10 10

 

With OIII filter at 100x, the PN is visible only at times as a round and extremely faint glow with relatively well defined borders.

 

Jim Misti

DSS 12'x12'

 

Abell 35 in Hydra

12 53 41.4 -22 51 42

 

This is the second largest entry in the Abell catalog with 16'x11', of which again only the central part is visible. Abell 35 is possibly a Strömgren sphere and not a true PN (Frew, thesis).

With OIII Filter, this object is immediately there as a diffuse patch around a group of three stars. The band structure in the S part was suspected. Distance of this object is about 500 LYs.

Capella

Don Goldman

DSS 30'x30'

 

Abell 36 in Virgo

13 40 41.3 -19 52 57

 

Another large and bright Abell PN with a diameter of roughly 8'..

With OIII filter at 100x, this PN (distance 800 LYs) is quite distinctly visible around its central star. It appears slightly annular with darker center.

Capella

Don Goldman

Adam Block

DSS 18'x18'

 

Abell 37 in Virgo

14 04 25.9 -17 13 40

 

With OIII filter at 250x, Abell 37 appears as a distinct small round disk. Also catalogued as IC 972.

DSS 12'x12'

 

Abell 38 in Scorpio

16 23 18.7 -31 44 58

 

Red emission is mostly NII, which is 11x (!) stronger than HII (Frew 2013).

 

DSS 12'x12'

 

Abell 39 in Hercules

16 27 33.8 +27 54 33

 

Another one of the perfectly round Abell PNs!

Appears with OIII filter as an easily visible and distinct round disk. At times, the center appeared darker. OIII > UHC.

 

Capella

Adam Block

Don Goldman

DSS 12'x12'

 

Abell 40 in Ophiuchus

16 48 34.5 -21 00 51

 

 

DSS 12'x12'

 

Abell 41 in Serpens

17 29 02.2 -15 13 07

 

Appears at 300x as a very faint little disk. Best with UHC, less pronounced with OIII.

DSS 12'x12'

 

Abell 42 in Ophiuchus

17 31 29.2 -08 19 09

 

At 300x, both with UHC and OIII suspected as an extremely faint glow with averted vision only. Uncertain observation, as the neighboring stars are interfering.

DSS 12'x12'

 

Abell 43 in Ophiuchus

17 53 32.2 +10 37 25

 

With OIII filter at 200x, Abell 43 is an easy object and appears as a filled disk with superimposed stars. Not anular. Can also be discerned without filter. There are hints to internal structure, which is, however, difficult to verify due to the superimposed small stars.

Capella

Don Goldman

NOAO

DSS 12'x12'

 

Abell 44 in Sagittarius

18 30 11.3 -16 45 24

 

Near open cluster NGC 6645, this is a small PN next to a group of stars, which are visible even with OIII filter and hamper somewhat a clear resolution of the PN.

DSS 12'x12'

 

Abell 45 in Scutum

18 30 16.1 -11 36 56

 

Not yet observed. Structure appears to be mainly NII with only little contrast to the surroundings in HII (Tweedy and Kwitter and Frew 2013).

Don Goldman

DSS 12'x12'

 

Abell 46 in Lyra

18 31 18.6 +26 56 11

 

With OIII filter at 100x, the PN is immediately visible. Somewhat more difficult at 200x, UHC filter about equally good as OIII filter. With UHC, central star is visible, while with OIII filter, the PN is a better defined round and uniform disk.

DSS 12'x12'

 

Abell 47 in Serpens

18 35 22.6 +00 13 50

 

 

DSS 12'x12'

 

Abell 48 in Aquila

18 42 46.9 -03 13 17

Unsuccessful observation.

 

Rick Johnson

DSS 12'x12'

 

Abell 49 in Scutum

18 53 28.6 -06 28 35

 

 

Capella

DSS 12'x12'

 

Abell 50 in Draco

18 59 19.9 +48 27 53

 

Abell 50 is also catalogued as NGC 6742.

Abell 50 appears as a small disk that is relatively bright. Visible even without filter.

 

Capella

NOAO

DSS 12'x12'

 

Abell 51 in Sagittarius

19 01 01.4 -18 12 14

 

 

DSS 12'x12'

 

Abell 52 in Aquila

19 04 32.4 +17 57 08

 

 

DSS 12'x12'

 

Abell 53 in Aquila

19 06 46.1 +06 23 50

 

Red emission is to a large extent NII and about 1.4x stronger than HII (Frew 2013).

With OIII filter at 200x, the PN was visible only at times as a small smudge, not anular. Difficult.

DSS 12'x12'

 

Abell 54 in Vulpecula

19 08 39.6 +22 58 59

 

 

DSS 12'x12'

 

Abell 55 in Aquila

19 10 25.8 -02 20 25

 

At 200x faintly visible even without filter, the PN becomes distinct with OIII filter. Small round blob without further structure.

DSS 12'x12'

 

Abell 56 in Aquila

19 13 06.6 +02 52 49

Even under excellent conditions no reliable observation

 

Jim Shuder

Capella

DSS 12'x12'

 

Abell 57 in Vulpecula

19 17 05.9 +25 37 33

 

With OIII filter at 200x, the PN is quite distinct. Appears as a small blob next to star. A chain of three stars is nearby.  OIII > UHC.

 

DSS 12'x12'

 

Abell 58 in Aquila

19 18 20.8 +01 46 53

 

 

DSS 12'x12'

 

Abell 59 in Sagitta

19 18 40.1 +19 34 26

 

Red emission is mostly NII, which is twice as strong as HII (Frew 2013).

Even under excellent conditions only suspected

DSS 12'x12'

 

Abell 60 in Sagittarius

19 19 17.8 -12 14 42

 

Even under excellent conditions no reliable observation

DSS 12'x12'

 

Abell 61 in Cygnus

19 19 10.3 +46 14 51

 

With OIII filter at 200x, Abell 61 can be held steadily with averted vision. Appears as a diffuse round glow, of which the W edge is somewhat better defined.

 

Capella

Don Goldman

DSS 12'x12'

 

Abell 62 in Aquila

19 33 18.3 +10 37 04

immediately visible with OIII filter as a very faint round disk with superimposed stars, less pronounced with UHC

NHAO

 

 

DSS 12'x12'

 

Abell 63 in Sagitta

19 42 10.4 +17 05 11

 

With OIII filter at 200x, this is a relatively easy PN. Appears as a subtle round and uniform glow, no structure. OIII > UHC.

DSS 12'x12'

 

Abell 64 in Aquila

19 45 35.1 -05 34 02

 

As a misclassification, Abell 64 is not a PN but the galaxy LEDA 63630.

Steadily visible at 350x (w/o filter, of course).

DSS 12'x12'

 

Abell 65 in Sagittarius

19 46 34.3 -23 08 14

 

At 200x and with OIII filter, Abell 65 is an obvious elongated patch of light. Response to OIII is better than to UHC, the PN is faintly visible even w/o filter. Nice asterism nearby.

 

Don Goldman

DSS 12'x12'

 

Abell 66 in Sagittarius

19 57 31.8 -21 36 37

At 125x and with OIII filter suspected only as a large round glow.

 

Don Goldman

 

DSS 12'x12'

 

Abell 67 in Aquila

19 58 27.0 +03 03 00

 

With OIII filter at 200x, Abell 67 is visible as a small diffuse blob. Can be held steadily with averted vision, not too difficult. Hardly visible with UHC.

DSS 12'x12'

 

Abell 68 in Vulpecula

20 00 10.5 +21 42 54

 

UHC filter better than OIII, 350x: small and round, difficult object, can be held with averted vision about 50% of the time.

DSS 12'x12'

 

Abell 69 in Cygnus

20 19 58.4 +38 23 59

 

Red emission is mostly NII, which is 5x stronger than HII (Frew 2013).

DSS 12'x12'

 

Abell 70 in Aquila

20 31 33.2 -07 05 18

 

With UHC at 350x, the PN is faint, but distinct, round, anularity not visible. Galaxy is visible at the edge of the PN only without filter.

 

NOAO

Adam Block

Capella

DSS 12'x12'

 

Abell 71 in Cygnus

20 32 23.4 +47 20 55

 

Abell 71 was observed as a very faint round glow next to two stars.

There is some, but no compelling evidence that Abell 71 is possibly an HII Strömgren sphere rather than a true PN (Pismis et al.).

 

Capella

Michael Siniscalchi

DSS 12'x12'

 

Abell 72 in Delphinus

20 50 02.1 +13 33 29

 

With OIII filter, Abell 72 is a relatively obvious object and appears at 200x as a large diffuse glow. At 350x, the interior is distinctly structured.

 

Capella

NOAO

DSS 12'x12'

 

Abell 73 in Cepheus

20 56 26.7 +57 26 00

 

Difficult, only suspected with OIII or UHC.

DSS 12'x12'

 

Abell 74 in Vulpecula

21 16 52.3 +24 08 52

 

With 7mm exit pupil and UHC, the PN was visible during two observations as a large and extremely faint glow. Some parts of the edge were well defined.

NOAO

Capella

Don Goldman

David Ratledge

DSS 30'x30'

 

Abell 75 in Cepheus

21 26 23.5 +62 53 33

 

Abell 75 is also catalogued as NGC 7076.

At 250x visible faintly without filter. UHC better than OIII, with filter well visible as a round blob, with some anularity, irregular at one side.

 

Capella

DSS 12'x12'

 

Abell 76 in Aquarius

21 30 03.5 -02 47 06

 

Abell 76 is the misclassified galaxy PGC 85185.

DSS 12'x12'

 

Abell 77 in Cepheus

21 32 10.3 +55 52 42

 

Abell 77 is possibly not a PN, but ionized ISM (Frew, thesis).

With UHC at 200x, Abell 77 is relatively easy. Appears as a faint and small smudge, slightly oval.

DSS 12'x12'

 

Abell 78 in Cygnus

21 35 29.5 +31 41 44

 

At 200x, central star immediately visible. With OIII filter, PN becomes visible as a round disk extending about halfways to the two neighboring stars. No internal structure could be discerned.

 

Capella

Adam Block

 

DSS 12'x12'

 

Abell 79 in Cygnus

22 26 17.3 +54 49 40

 

Red emission is mostly NII, which is 7x stronger than HII (Frew 2013).

Immediately visible with OIII filter at 250x as an elongated glow, no ring structure. Quite faint, but can be held steadily even with direct vision. Visible as well with UHC.

 

Tom Carrico

Capella

DSS 12'x12'

 

Abell 80 in Lacerta

22 34 45.5 +52 26 12

 

At 200x, the PN was at best suspected only with OIII filter as a round disk at the correct position. Not better with UHC.

 

Michael Breite

DSS 12'x12'

 

Abell 81 in Cepheus

22 42 25.3 +80 26 28

 

Abell 81 is also catalogued as IC 1454.

Best at 200x, this PN is visible even without filter as a small perfectly round ring with darker center. Enhanced by both UHC and OIII. Superimposed stars.

 

Rick Johnson

Maxim Usatov

DSS 12'x12'

 

Abell 82 in Cassiopeia

23 45 47.5 +57 03 56

 

Best around 150 and 250x with OIII, already with direct vision, less pronounced with UHC. Appears as a round glow placed assymetrically around star and extending about halfway to neighboring star.

 

Rick Johnson

DSS 12'x12'

 

Abell 83 in Cassiopeia

23 46 46.9 +54 44 38

 

Suspected at 200x with averted vision. The two superimposed stars on DSS print are not visible at 200x or 350x.

DSS 12'x12'

 

Abell 84 in Cassiopeia

23 47 43.9 +51 23 56

 

With OIII filter at 200x visible as a diffuse disk next to a star. Quite distinct.

 

NOAO

Michael Siniscalchi

Michael Breite

DSS 12'x12'

 

Abell 85 in Cassiopeia

23 58 53.5 +62 30 28

 

This is the supernova remnant CTB 1 and not a planetary nebula.

No reliable observation up to now even under excellent conditions. HII emission strongest along SW edge, while OIII images reveal the NE edge to be the most prominent (see image by Mischa Schirmer).

 

Mischa Schirmer

Antonio Fernandez

DSS 60'x60'

 

Abell 86 in Cepheus

00 01 30.9 +70 42 30

 

 

DSS 12'x12'

Daten der Abell PN

 

const.

RA

Dek

mag

Ø in "

other designations

notes

1

Cep

00 12 55.0

+69 10 21

18.7

46

PK 119+6.1

 

2

Cas

00 45 36

+57 57.4

14.5

33

PK 122-4.1

 

3

Cas

02 12 06.6

+64 09 01

16

60

PK 131+2.1, Sh 2-189

 

4

Per

02 45 23.7

+42 33 05

14.8

22

PK 144-15.1

 

5

Per

02 52 15.1

+50 35 54

 

134

PK 141-7.1

 

6

Cas

02 58 41.9

+64 30 06

15

188

PK 136+4.1

 

7

Lep

05 03 08.0

-15 36 13

15.5

871

PK 215-30.1

 

8

Aur

05 06 38.4

+39 08 11

17.6

62

PK 167-0.1

 

9

Aur

05 28 56.6

+36 03 05

17.8

40

PK 172+0.1

 

10

Ori

05 31 45.5

+06 56 09

14

35

PK 197-14.1, K 1-7

 

11

Ori

05 37 19.4

+08 15 45

17.1

32 

-

reflection nebula

12

Ori

06 02 20.0

+09 39 14

12.4

37

PK 198-6.1

 

13

Ori

06 04 47.9

+03 56 36

15.3

174

PK 204-8.1, YM 28

 

14

Ori

06 11 08.7

+11 46 43

17.5

40

PK 197-3.1

 

15

CMa

06 27 02.0

-25 22 50

15.8

34

PK 233-16.1

 

16

Lyn

06 43 55.5

+61 47 25

15.4

143

PK 153+22.1

 

17

-

06 48 38.0

-09 32 38.8

-

 

-

plate fault

18

Mon

06 56 14.5

-02 53 09

17

71

PK 216-0.1

 

19

Gem

06 59 56.4

+14 36 34

16.3

80

PK 200+8.1

 

20

CMi

07 22 57.4

+01 45 37

14.7

65

PK 214+7.1

 

21

Gem

07 29 02.5

+13 15 13

10.2

744

PK 205+14.1, YM 29, Sh 2-274, Medusa Nebula

 

22

CMi

07 36 07.9

+02 42 28

15.4

105

PK 215+11.1, K 1-11

 

23

Pup

07 43 18.3

-34 45 12

13.1

54

PK 249-5.1

 

24

CMi

07 51 37.6

+03 00 21

13.9

265

PK 217+14.1

 

25

Mon

08 06 46.5

-02 52 35

15.4

150

PK 224+15.1, K 1-13

 

26

Pup

08 09 01.5

-32 40 22

18.1

40

PK 250+0.1

 

27

Pyx

08 31 52.5

-32 06 09

15.6

47

PK 252+4.1, K 1-1

 

28

UMa

08 41 35.6

+58 13 48

13.5

268

PK 158+37.1

 

29

Pyx

08 40 18.9

-20 54 36

17

482

PK 244+12.1, E563-PN009

 

30

Cnc

08 46 54.4

+17 52 33

13

127

PK 208+33.1

 

31

Cnc

08 54 13.1

+08 53 59

12

970

PK 219+31.1, Sh 2-290

 

32

 -

09 16 24.8

+03 53 26

 

 

 

plate fault

33

Hya

09 39 09.0

-02 48 33

12.9

275

PK 238+34.1

 

34

Hya

09 45 35.3

-13 10 16

12.9

281

PK 248+29.1

 

35

Hya

12 53 32.9

-22 52 22

13.3

938

PK 303+40.1, Sh 2-313

possibly HII region

36

Vir

13 40 41.2

-19 52 57

11.8

478

PK 318+4.1

 

37

Vir

14 04 26.0

-17 13 41

13.6

43

PK 326+42.1, IC 972

 

38

Sco

16 23 18.5

-31 44 58

15.5

154

PK 346+12.1, K 1-3

 

39

Her

16 27 33.6

+27 54 34

12.9

170

PK 47+42.1

 

40

Oph

16 48 34.5

-21 00 51

17.8

30

PK 359+15.1

 

41

Ser

17 29 02.0

-15 12 59

15.6

16

PK 9+10.1

 

42

Oph

17 31 29.1

-08 19 10

16.5

60

PK 16+13.1

 

43

Oph

17 53 32.3

+10 37 24

14.7

80

PK 36+17.1

 

44

Sgr

18 30 11.4

-16 45 28

15.8

63

PK 15-3.1

 

45

Sct

18 30 15.4

-11 36 56

12.8

302

PK 20-0.1

 

46

Lyr

18 31 18.9

+26 56 17

13.8

63

PK 55+16.1

 

47

Ser

18 35 22.6

-00 13 50

19.5

17

PK 30+3.1

 

48

Aql

18 42 46.9

-03 13 25

17.2

43

PK 29+0.1

 

49

Sct

18 53 28.5

-06 28 33

16.2

35

PK 27-3.1

 

50

Dra

18 59 19.7

+48 27 57

13.4

31

PK 78+18.1, NGC 6742

 

51

Sgr

19 01 01.1

-18 12 15

14

64

PK 17-10.1

 

52

Aql

19 04 32.3

+17 57 07

16.5

37

PK 50+5.1

 

53

Aql

19 06 45.8

+06 23 56

16.3

30

PK 40-0.1

 

54

Vul

19 08 39.6

+22 58 58

16.8

67

PK 55+6.1

 

55

Aql

19 10 30.4

-02 21 02

13.2

47

PK 33-5.1

 

56

Aql

19 13 06.1

+02 52 48

14.1

188

PK 37-3.2

 

57

Vul

19 17 06

+25 37 30

14.4

40

PK 58+6.1

 

58

Aql

19 18 20.6

+01 47 00

17.4

44

PK 37-5.1

 

59

Sge

19 18 40.0

+19 34 33

16.4

94

PK 53+3.1

 

61

Cyg

19 19 10.1

+46 14 36

13.5

88

PK 77+14.1

 

60

Sgr

19 19 18.6

-12 14 54

16.2

201

PK 25-11.1

 

62

Aql

19 33 18.3

+10 37 01

14.7

161

PK 47-4.1

 

63

Sgr

19 42 10.4

+17 05 15

16.9

40

PK 53-3.1

 

64

Aql

19 45 34.8

+05 33 52

15.3

40

PGC 63630, CGCG 397-005

galaxy

65

Sgr

19 46 33.8

-23 08 12

13.8

134

PK 17-21.1 + several galaxy designations

 

66

Sgr

19 57 31.5

-21 36 46

14.9

295

PK 19-23.1

 

67

Aql

19 58 27.0

+03 02 52

13.6

69

PK 43-13.1

 

68

Vul

20 00 10.8

+21 42 58

15.2

40

PK 60-4.1

 

69

Cyg

20 19 58.3

+38 24 02

20.2

25

PK 76+1.1

 

70

Aql

20 31 33.2

-07 05 17

14.7

45

PK 38-25.1

 

71

Cyg

20 32 23.2

+47 21 04

14.5

165

PK 85+4.1, Sh 2-116

HII region

72

Del

20 50 02.0

+13 33 28

12.7

134

PK 59-18.1

 

73

Cep

20 56 27.0

+57 26 03

17

80

PK 95+7.1

 

74

Vul

21 16 52.3

+24 08 51

15.8

871

PK 72-17.1

 

75

Cep

21 26 23.6

+62 53 33

14.5

67

PK 101+8.1, NGC 7076

 

76

Aqr

21 30 03.8

-02 48 32

15.6

 

PK 5-036.1, PGC 85185

galaxy

77

Cep

21 32 10.2

+55 52 43

14

67

PK 97+3.1, Sh 2-128, LBN 443

HII region

78

Cyg

21 35 29.4

+31 41 45

13.4

113

PK 81-14.1

 

79

Lac

22 26 17.3

+54 49 38

15.3

59

PK 102-2.1

 

80

Lac

22 34 45.6

+52 26 06

16

161

PK 102-5.1

 

81

Cep

22 42 25.0

+80 26 32

14.4

34

PK 117+18.1, IC 1454

 

82

Cas

23 45 47.8

+57 03 59

12.7

94

PK 114-4.1

 

83

Cas

23 46 46.7

+54 44 38

15.5

42

PK 113-6.1

 

84

Cas

23 47 44.3

+51 23 56

13

147

PK 112-10.1

 

85

Cas

23 59 12.9

+62 26 13

 

2000 

CTB 1, SNR G116.9+00.1

SNR

86

Cep

00 01 31.2

+70 42 29

16.7

70

PK 118+8.2

 

 

DSS images copyright notice

The Digitized Sky Survey was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions.

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