NGC 7423 (Berkeley 57) and PK 107-2.1 (M 1-80) Open Cluster and Planetary Nebula in Cepheus

Center of field at approximately: RA 22 hours 56 minutes 20 seconds, Dec +57 degrees 09 minutes 20 seconds

Size: 5.0' and 8.0" Magnitude: 15.0 and 14.0 photographic Class: II 2 m and 2

North is up

West to the right


14.5" f5 Newtonian reflector


 ST-8XME, self-guided, binned 1x1, temp -15c, camera control MaxIm DL 4.56


Lumicon Red filter, 590 minutes (59 x 10 minute subs), 09/2/3/4/2014; 2.2-3.8 FWHM per CCDStack


CCDStack 2.81.5337.19441, Photoshop CS5.1


 Rolling Roof Observatory, Thousand Oaks, CA 91360 (+34d 13m 29s -118h 52m 20s)


There are (at least) two non-stellar objects in this field, in addition to the open cluster.

See the CDS data for these two ... just to the NNE (above left) of NGC 7423 is IRAS 22534+5653, and further to the east (left) is PK 107-2.1 (Minkowski 1-80).

See this 8" marked image. See the 8" version.

View 200% crop. The planetary is to the east (left), in this north up/west to the right, cropped image.

From the NGC / IC Project:

No Contemporary Visual Observation(s) listed ...

Historical Research Notes / Correction for NGC 7423
NGC 7423 is a nice, compressed cluster at the NGC position.  It sits between
two brighter stars, and would probably be an interesting, if faint, object at 
the eyepiece.

JH was not sure in his 1833 catalogue if this was his father's III 745 or not.
When he compiled the GC, however, he adopted his own position and his father's
description.  This is actually the best combination as both are correct.  WH's
position, however, is a minute of time east of the JH's position.  Dreyer 
noticed this when he published all of WH's papers in 1912, and wrote a short
note about it.  In that note, Dreyer also mentions "In the sweep a star 6 mag
= +56 2923 is 3m 41s f, 10' s."  Doing the math from WH's reference star
(Delta Cephei) for III 745, the BD star ends up close to its true position --
but III 745 is stubbornly 1 minute of time off.

Curiously, RNGC calls the cluster non-existent though it is clear on the POSS, 
and is included in the cluster catalogues as Berkeley 57 (that identity was
apparently first noticed by Alister Ling in 1985).  SIMBAD mistakenly equates
the cluster with a faint planetary (an infrared source) a few arcmin to the
northeast. - Dr. Harold G. Corwin, Jr.