Sh2-129 emission nebula presents an irregular ring-arch form which resemble a figure of a flying bat, and according to Blitz et.Al. is situated at a distance of about 400 parsec or 1300 light-years.
According to Dobashi and collegues the region sourroundig Sh-129 is particularly rich of molecular clouds, first among all the whide obscure nebulositys system occulting the Milky Way in the direction of Cefeus; cfr. Dobahashi K. et Al., 1994 “Molecular Clouds in Cygnus. I. A Large-Scale 13CO Survey” – https://ui.adsabs.harvard.edu/abs/1994ApJS…95..419D/abstract
George Helou and collegues [ https://ui.adsabs.harvard.edu/abs/1988iras….7…..H/abstract ] studied the infrared radiation source IRAS 21168+5948 which coordinates coincide with the CO emission region, as just introduced within Avedisova Star Formation regions Catalogue; cfr. Avedisova V. S., 2002 “A Catalog of Star-Forming Regions in the Galaxy” in Astronomy Reports, vol.46 n.3: 193 – 205.
Within Sh2-129 center, recording in Oiii narrowband, is possible to enhance the vision of Ou4 nebula, whose form gave the name of squid nebula.
Discovered in 2011 by French astro-imager Nicolas Outters, the Squid Nebula’s alluring bipolar shape is distinguished by the telltale blue-green emission from doubly ionized oxygen atoms. Though apparently completely surrounded by hydrogen emission region Sh2-129, the true distance and nature of the Ou4 have been difficult to determine.
Recent investigation suggests Ou4 really does lie within Sh2-129 some 2,300 light-years away. Consistent with that scenario, Ou4 would represent a spectacular outflow driven by HR8119, a triple system of hot, massive stars seen near the center of the nebula.
The truly giant Squid Nebula would physically be nearly 50 light-years across.
This work is the result of personal SHO records using William Optics Redcat 51 and ASI1600mm Pro under Bortle 6 sky in Livorno – Italy (home balcony) with integration of records focused about Oiii signal obtained by Takahashi FSQ-106EDX4 and Proline FLI PL16083 camera retrieved from Telescopelive.
Data framelists set available:
here for WO51,
and here for Takahashi106
PixInSight cored workflow for generate 2 distinguished single channel SHO masters, linear-fit by Takahashi Oiii master, each pair blended by pixelmath within final S H and O masters, channel-combined in the SHO integration.
Normal narrowband workflow post-proccessing followed ‘till reaching an SHO starless
and SHO stars separated masters.
The same workflows I took for RGB channels, with the focus on star – separated from starless final integration to be used for final image composing.
I then integrated in Photoshop by screen blending mode after necessary fixing and adjustements.
Parallely, the same workflow I made for Oiii master, using Oiii starless for enhancing Ou4 structure, luminosity and tones, in Photoshop by adjustements and colorizing filtered layer.
Integration of Oiii starless channel within SHO master enhanced luminosity, saturation and structure of Ou4 whole nebula.
Spiral galaxy in the northern constellation of Canes Venatici belonging to M51 Group located to the southeast of the M101 Group and the NGC 5866 Group. The distances to these three groups are similar, thus the M51 Group, the M101 Group, and the NGC 5866 Group are actually considered as part of a large, loose, elongated structure; cfr.: https://arxiv.org/abs/astro-ph/9910501.
In the mid-19th century, Anglo-Irish astronomer Lord Rosse identified spiral structures within the galaxy, making this one of the first galaxies in which such structure was identified.
According to Ann, Ha et Al., 2015 [cfr.: https://arxiv.org/abs/1502.03545] catalogation of visual classified galaxies in local Universe the shape or morphology of this galaxy has a classification of SAbc where SA indicating a spiral form with no central bar feature, and bc describes a moderate to loosely wound arms, as evinced from a visible light observation with general lack of large-scale continuous spiral structure, thus M63 is considered a flocculent galaxy.
According to Thornley, 1996, when observed in the near infrared, a symmetric, two-arm structure is seen and each arm wraps 150° around the galaxy and extends out to 13,000 light-years (4,000 parsecs) from the nucleus; cfr. https://arxiv.org/abs/astro-ph/9607041.
According to Graham, 2008, the existence of a supermassive black hole (SMBH) at the nucleus is uncertain. If it’s true then its mass could be estimated as (8.5±1.9)×108 M☉, in few words around 850 million times the mass of our star the Sun; cfr.: https://arxiv.org/abs/0807.2549
Tully, Courtois and Sorce researches focused on galaxy distances measured M63 at 29.300.000 light years, alias 8.99 megaparsec. Cfr.: https://arxiv.org/abs/1605.01765
In this work I use bundle observation from Telescopelive Spain 2 CCD Officina Stellare 700mm RC.
First, by PixInSight, Cosmetic Correction was required to better recalibrate subframes, especially removing vertical couple of lines. Then the same registration, integration, bg removing, spcc, deconvolution and denoising routine to generate LRGB masterframe, while in parallel, working on Luminance master for final Photoshop image reconstruction, with starless and stars levels blending – respectively in luminosity (L) and screen (Stars) mode.
The obscuration of background objects by intervening dust towards the Galactic centre – Extinction – is generally very high, thus detailed studies of the central regions of our Galaxy are difficult.
There are small patches of sky along the line of sight to the Galactic centre that, by chance, suffer less extinction, and one of the largest and most famous of these is Baade’s Window which provides a relatively unobscured view of a region 4 degrees (~2,000 light years) south of the Galactic centre, with centre approximately located by NGC6522 star cluster.
Most of our knowledge of the stars in the bulge of the Milky Way is derived from studies in Baade’s Window.
It is named for astronomer Walter Baade, who first recognized its significance.
This area corresponds to one of the brightest visible patches of the Milky Way.
It is centered at a galactic longitude (l) of 1.02° and a galactic latitude (b) of -3.92°,[1] which corresponds to a right ascension of 18h 03m 32.14s and a declination of -30d 02m 06.96s, in the direction of the constellation Sagittarius.
According to Barbuy et Al. 2009, NGC6522 is possibly the oldest star cluster in the Milky Way, and Chiappini et Al., 2011 evaluated its age of about 12 billion years; cfr. “VLT-FLAMES Analysis of 8 giants in the Bulge Metal-poor Globular Cluster NGC 6522: Oldest Cluster in the Galaxy?” by B. Barbuy et al., 2009 [https://arxiv.org/abs/0908.3603] , and “Imprints of fast-rotating massive stars in the Galactic Bulge” by Cristina Chiappini et al., Nature 472, pp. 454–457 (28 April 2011) [https://www.nature.com/articles/nature10000]
NGC 6528 is located southwest of NGC 6522 and also presents unusually metal-richness for a globular cluster. A very similar composition with NGC 6553 suggests an origin in a similar environment; cfr.: “Chemical analysis of NGC 6528: one of the most metal-rich bulge globular cluster” by Muñoz, C.et Al., 2018 [https://arxiv.org/abs/1809.04164]
In this work I separately processed LRGB integration and L masterframe by PixInSight: after normal routine (bg removing, Spectrophotometric CC, Deconvolution and denoising) I thus preferred to separate LRGB stars from starless data, thus to proceed to the final image recomposition in Photoshop with 3 main levels group (and relative fixing and adjustments) with starless on the bottom, stars blending in screen mode, and luminance as top layer blending in luminosity.
Sh2-214 and Sh2-215 very faint practically invisible Sh2 spot within Cepheus area; starless master shows both faint nebulosity and a third spot which I wasn’t able to identify.
SH2-157, the Lobster Claw Nebula, is an emission nebula located about 11,000 light-years away in the constellation of Cassiopeia.
According to SHO palette, red/orange and predominantly yellow regions of the nebula evinced a very large H II region while the blue-colored are predominately regions featured by the emission of light from molecular oxygen.
On the top NGC 7635 – the Bubble Nebula, and on the middle the star cluster NGC 7510.
NGC 5367, also catalogued as IC 4347, a Reflection Nebula in Centaurus, lighted from two bluish components of the binary system h4636 from spectral type B4 and B7.
Nebula is associated with the cometary globule CG12, extending from bottom center to the upper right for more than 1°: dicovered in 1976 on an ESO/SRC Sky Survey plate taken with the UK Schmidt telescope, CG12 is in contrast to the most other Cometary Globules, because it is far away from the galactic disk by latitude as more than 21°.
A strong IRAS point source and a highly collimated outflow indicate that star formation is still going on. The head of the globule has been observed using NIR imaging (NTT sofi), mm continuum (SEST Simba) and sub mm (APEX) and mm (SEST) spectroscopy.
The molecular material is distributed in a 10′ North-South elongated lane with two compact maxima separated by 3′. Strong C^18O (3-2), (2-1) and (1-0) emission is detected in both maxima and both have an associated compact 1.2 mm continuum source.
The Northern core, CG 12 N, is cold and is possibly still pre-stellar. A stellar source with a NIR reflection nebulosity is observed near CG 12 N.
The observed C^18O line ratios are similar to those observed in Class 0 sources.
A remarkable C^18O (3-2) hot spot is detected in the direction of the Southern core, CG 12 S. It lies at the edge of a dense cloud core detected both in high density tracers (CS (3-2), H^13CO^+ (1-0) and DCO^+(2-1)) and in the 1.2 mm continuum.
The hot spot also lies on the axis of a highly collimated bipolar molecular outflow with a driving source most probably embedded in the dense core. This is the first detection of such a compact, warm object in a low mass star forming region.
NIR imaging reveals a bright cone-like feature with a faint counter cone in the centre of CG 12 S. The total mass (> 100 M[sun]) and the linear size of the CG 12 head (~3 pc) are similar to those of other nearby low mass star forming regions.
Even though the most evolved stars in CG 12 lie already on ZAMS the cloud contains also proto-stellar sources and a pre-stellar core.
Telescopi O Obiettivi Di Acquisizione: William Optics Redcat 51 Camere Di Acquisizione: ZWO ASI1600MM Pro Montature : Sky-Watcher EQM-35 × Filtri: Astronomik H-alpha CCD 6nm · Astronomik OIII CCD 12nm 1.25″ · Astronomik OIII CCD 6nm · Astronomik SII CCD 6nm Accessori : ZWO ASIAIR Plus · ZWO ASIAIR Pro · ZWO EAF · ZWO EFW 8 x 1.25″ / 31mm Software: Adobe Photoshop · Pleiades Astrophoto PixInsight Telescopi O Obiettivi Di Guida : QHYCCD Mini Guide Scope Camere Di Guida : ZWO ASI120MM Mini
Dettagli d’acquisizione Date: 09 Dicembre 2021 · 11 Dicembre 2021 · 12 Dicembre 2021 · 13 Dicembre 2021 · 15 Dicembre 2021 · 16 Dicembre 2021 · 17 Dicembre 2021 · 18 Dicembre 2021 · 08 Gennaio 2022 · 09 Gennaio 2022 · 10 Gennaio 2022 · 11 Gennaio 2022 · 12 Gennaio 2022 · 13 Gennaio 2022 · 14 Gennaio 2022 · 16 Gennaio 2022 · 18 Gennaio 2022 · 22 Gennaio 2022 · 23 Gennaio 2022 · 24 Gennaio 2022 · 28 Gennaio 2022 · 29 Gennaio 2022 · 31 Gennaio 2022 · 01 Febbraio 2022 · 02 Febbraio 2022 · 05 Febbraio 2022
Pose: Astronomik H-alpha CCD 12nm 1.25″: 79×180″(3h 57′) (gain: 139.00) -20°C bin 1×1 Astronomik OIII CCD 12nm 1.25″: 62×180″(3h 6′) (gain: 139.00) -20°C bin 1×1 Astronomik SII CCD 12nm 1.25″: 77×180″(3h 51′) (gain: 139.00) -20°C bin 1×1 Integrazione: 10h 54′ Dark: 33, Flat: 33, Dark dei flat: 33 Giorno lunare medio: 12.35 giorni Fase lunare media: 58.64% Scala del Cielo Scuro Bortle: 6.00
