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Winds of Aries..... LBN 762 / MBM 13 : This nice field is located in Aries. This association of gas and dust are early stellar nurseries and newborn stars.Recent studies based in PS1 photometry (April,2014) suggest this molecular cloud is about 191 parsecs away ( Astrophysycal journal, Vol 786,Number 1. E.F.Schlaly et al). The structure of LBN 762 is amazing and one must imagine what incredible kind of forces are capable to create such intrincate shapes. Larger galaxies visible in the image are PGC11152 at the right side and PGC11410 at upper left. Many other little background galaxies are visible even through the semi-translucid gas clouds.

In the March 1978 issue of Sky & Telescope magazine, in the article Deep-Sky Wonders, Walter Scott Houston referred to the "discovery" of this cluster that did not appear in any catalog or star chart of the time by an amateur astronomer, John Pazmino. Stock had referred to this cluster years earlier, going as Stock 23 in 1966, but due to the whims of fate had been forgotten until Pazmino "rediscovered" it, becoming since 1978 the objective of observation of many amateur astronomers. Stock 23 (Pazmiño's Cluster) is a cluster in the constellation Camelopardis. The cluster and dark nebulae are embedded in the extensive nebula Sh2-202. Photometric studies suggest that stock 23 is simply a random formation and not a traditional open cluster with related stars. Stock 23 is a fairly sparse and depopulated open cluster, whose nature as a real object in itself is questioned; its distance has been estimated in some studies to be around 380 parsecs (1240 light years), it has several blue stars visible in its vicinity. It should be noted, however, that in a study focusing on this association, among the stars considered to belong to it, is Camelopardalis OB1 HD 20134, a B2.5V spectral class Be star that is the brightest of Stock 23; the distance taken into consideration is 800 parsecs (about 2,600 light years), estimated for this group. The photometric studies carried out on the stars of this object, however, want to make believe that it can be more of an asterism, whose components would be therefore not physically connected to each other, but that they would be at different distances. It should be noted that at the distance of 800 parsecs extends the region H II Sh2-202, which gives that reddish appearance to the environment...

NGC 7771,7771A,7770,7969 (Pegasus) * August-September 2017 * ASA N12 astrograph (f/3.6, 1075mm) * ASA DDM85 mount * G3-16200 EC Moravian CCD* LRGB Baader filters * Subframes acquired unguided: Auotslew+ Sequence programms * L: 720 min R: 480min G::420 min B:540 min * ( Thanks to Mr. Sakib Rasool for the image suggestion). The galactic group of NGC 7771 is about 200 million light-years away in the constellation of Pegasus: NGC 7771 is the large, pebble spiral galaxy of 75,000 light-years in diameter that appears in the center of the image, which is accompanied by two small galaxies beneath it... a lenticular (NGC 7770) and a very small one in it´s border (NGC 7771A). The spiral galaxy is NGC 7769, front view. Galaxies in the NGC 7771 group interact with each other and, within a cosmological scale, are predicted to end up fused into an even larger galaxy. The history of these interactions can be described by following the faint currents of stars plucked from galaxies, distorted by the effect of the gravitational tide caused by the above-mentioned close encounters. NGC 7771 has a huge "tails" implying that the galaxies have already passed very close to each other. It is not easy to get a clear picture of this galactic group, as more detailed images also reveal the presence of dust clouds in the foreground. These faint dust nebulae, located a few hundred light-years away from us and slightly above the galactic plane, reflect the light of the stars in our own galaxy, the Milky Way. (Image information credits: APOD, Wikipedia, Michael Ryskamp )

LDN 1152,RNO 124 (" The Architeuthis Rex or Giant Squid ".This was my first impression when processing the image. An Architeuthis Rex expelling ink all around ) RNO 124 :As a whole, this nebula has a conical shape, with a star IRAS 20359+6745 at its apex. It is possible to separate two distinct reflection structures in the nebula. The former is represented by a regular cone with an opening angle of about 60 degrees and with straight walls, which are extended up to 2´. Observations confirm that RNO 124 is a system with directed outflow, which produces HH 376A as well as forms the cone reflection nebula with traces of two probable helical arms. The Ha line in the spectrum of the source star shows the presence of a high velocity component, associated with the collimated flow.HH 376A is the bow shock structure in the collimated high velocity flow, directed by the axis of the cone nebula, with shock velocity about 70-80 km s-1. Credits:"Various manifestations of the outflow connected to the cometary nebula GM 3-12 (RNO 124)*" (January 2004) T. A. Movsessian1, T. Yu. Magakian1, J. Boulesteix2 and P. Amram2 L1152 is a Lynds Opacity Class 5 cloud located in Cepheus (Lynds 1962), at an assumed distance of 325 pc (see Kirk et al. 2009). Stars form as a result of the gravitational collapse of clouds of gas and dust. This process can take place in isolated Bok globules or within fragmented giant molecular clouds . The earliest recognizable phase of the star formation process is the Class 0 phase (Andre et al. 1993), the beginning of which is marked by the formation of a hydrostatically supported protostar within an infalling cloud of gas and dust. More resolution image: http://afesan.es/Deepspace/slides/LDN%201152%20%28The%20Architeuthis%20or%20Giant%20Squid%20in%20Draco-Cepheus%29.html

Dark nebula Dobashi 2367-2365-2373-2381,TGU H466 DWB 67 -- HII (ionized) ; DWB 57 -- HII (ionized) region DR 9 -- HII (ionized) GGD 31 -- Herbig-Haro Object M 29 -- Open (galactic) Cluster Most of the atlas and catalog mainly trace relatively dense regions in dark clouds revealing a number of dense cloud cores leading to star formation, while those presented by Dobashi et al. (2005) based on the optical database are more suited to trace less dense regions and to reveal the global extents of dark cloud. Despite its impressive appearance, similar to a tiny Pleiades, the cluster M29 (NGC 6913) is a difficult object to understand. A glance at a deep exposure in blue or red filters shows that it is located in a small more transparent bay of a huge system of dark clouds known as the Great Cygnus Rift. Most prominent in the cluster are seven stars with V magnitudes 8.6–10.2 It seems that our investigation has solved the longstanding problem of the distance and age of the cluster M29. The main reason preventing determination of the cluster distance earlier is related to insufficient accuracy of the luminosity classifications of its brightest stars.The M29 cluster is usually considered to be a member of the Cyg OB1 association, along with the clusters IC 4996, Berkeley 86, and Berkeley 87; see the recent review by Reipurth & Schneider (2008). Other than the clusters, the association contains tens of O–B3 stars and cooler supergiants scattered in an area of 4° × 3 (Humphreys 1978; Garmany & Stencel 1992). The distance to this association is still controversial but is usually considered to be 1.3–1.5?kpc. The distance to the cluster M29 determined in this investigation is close to the largest of these distances.The distances to the clouds of the Great Cygnus Rift are estimated to be in the range of 700–900 pc. As a bonus.. the Herbig-Haro object GGD 31 can be seen close to the center of the image.Also the diffuse ionized HII areas DWB 57,DWB 67.