This was just a test exposure that I used during Telescope setup, and I never intended using it. I decided to not just delete the photo but share it to give an indication of the amount of stars that is visible just out of the city in moderately light polluted skies.

A single short (unguided) 30 second test exposure at ISO 6400 of a small random section of the Carina–Sagittarius Arm of the Milky Way Galaxy through a wide field 6" Newtonian Reflector Telescope.

Photographed with the Canon 60Da DSLR (sensitive to Infra-red light at 656.28 nm in the Hydrogen Alpha wavelength), the dust and gas of the most basic and abundant element in the Universe (Hydrogen), shows up in red.

Hydrogen atoms have only 1 proton & 1 electron, and is the most basic building blocks of matter.

The variations in star colour gives us an indication of their temperature (the blue stars are hotter than the red ones).

Astrometry Info:

RA, Dec center: 269.478980362, -27.8841316586 degrees

Orientation: 1.26784149128 deg E of N

Pixel scale: 7.41620667134 arcsec/pixel

Field of view:

FOV = 2.1° x 1.4°

Food for thought...

The Milky Way Galaxy is estimated to contain over 400 billion stars. Just like our Sun (a Yellow Dwarf Star), many stars have planets and moons. The known Universe is estimated to contain over 100 billion Galaxies. This is why it is said that Astronomy can be a humbling and character building experience. It does seem to change one's perspective.

Martin

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NGC 6822 in Sagittarius

Credit: ESO/Dss2, Giuseppe Donatiello

NGC 6822 among the galactic cirrus clouds in the central bulge region. It is a purely prospective alignment since the small and isolated irregular galaxy, one of the most massive of the Local Group, is about 500 kpc (1.6 Mly) away [Cannon et al. 2006].

Having been discovered by Edward Emerson Barnard with a 6-inch telescope, it is also called Barnard's Galaxy.

The pinpoint object with a beautiful turquoise color (upper right) is the planetary nebula NGC 6818. The color is mainly due to the emission of the "forbidden" lines of doubly ionized oxygen [OIII].

Unlike a spiral or elliptical galaxy, the galaxy KK 246 looks like glitter spilled across a black velvet sheet. KK 246, also known as ESO 461-036, is a dwarf irregular galaxy residing within the Local Void, a vast region of empty space. This lonely galaxy is the only one known for certain to reside in this enormous volume, along with 15 others that have been tentatively identified.

Although the picture appears to be full of galaxies, they are actually beyond this void, and instead form part of other galaxy groups or clusters. Cosmic voids, such as this one, are the spaces within the web-like structure of the universe wherein very few or no galaxies exist.

Adjacent to the Local Group, this region of empty space is at least 150 million light-years across. For perspective, our own Milky Way galaxy is estimated to be 150,000 light-years across, making this void immense in its nothingness.

For more information: www.nasa.gov/image-feature/goddard/2020/hubble-sees-stell...

Text credit: ESA (European Space Agency)

Image credit: ESA/Hubble & NASA, E. Shaya, L. Rizzi, B. Tully, et al.

The Andromeda Galaxy family

Credit: CFHT LS-PAndAS, DESI LIS, SDSS, Giuseppe Donatiello

The complete family of M31, with all the small satellites known so far. This poster includes Pegasus V (Andromeda XXXIV) and Pisces VII (Triangulum III) discovered by me in 2020/21.

Andromeda VIII is missing because it does not exist, And XXXI and XXXII because they are not covered by the surveys used.

For convenience, the names "Andromeda"of the galaxies is indicated as "A" with the Arabic numeral instead of the Roman one.

This inverted version is in full resolution. Color version g'r'(z',i') can be provided upon reasonable request.

Last update: July 7, 2024

All 42 satellite galaxies of Andromeda (M31), including M33. The list is updated to 15 December 2025.

Andromeda – M31 (905 o 964, Abd al-Rahmān al-Sūfi)

Triangulum – M33 (1654, G.B. Hodierna)

M32 – NGC 221 - PGC 2555 (1742, G. Le Gentil)

NGC 205 – M110 – PGC 2429 (1773, C. Messier/ 1783, C. Herschel)

NGC 185 – (1787, W. Herschel)

NGC 147 – PGC 2004 (1829, J. Herschel)

Andromeda I – PGC 4666 (1970, S. V. den Bergh)

Andromeda II - PGC 4601 (1970, S. V. den Bergh)

Andromeda III – PGC 2121 (1971, S. V. den Bergh)

Andromeda V - PGC 3097824 (1998, T.E. Armandroff, J.E. Davies, G.H. Jacoby)

Andromeda VI - Pegasus dwarf (1998, T.E. Armandroff et al. / Karachentsev and Karachentseva)

Andromeda VII - Cassiopeia dwarf - PGC 2807155 (1998, Karachentsev and Karachentseva)

Andromeda VIII (2003, inesistente)

Andromeda IX - PGC 4689222 (2004, D.B. Zucker, A.Y. Kniazev, E.F. Bell, D.Martinez-Delgado)

Andromeda X – (2005, D.B. Zucker, D.Martinez-Delgado, E. F. Bell)

Andromeda XI - PGC 5056923 (2006, N.F. Martin et al.)

Andromeda XII – (2006, N.F. Martin et al.)

Andromeda XIII - Pisces III (2006, N.F. Martin et al.)

Andromeda XIV – Pisces IV (2007, S. R. Majewski et al.) isolated

Andromeda XV – (2007, R. Ibata et al.)

Andromeda XVI – Pisces V (2007, R. Ibata et al.)

Andromeda XVII – (2008, M. Irwin et al.)

Andromeda XVIII – (2008, A. W. McConnachie et al.) è considerata isolata

Andromeda XIX - (2008, A. W. McConnachie et al.)

Andromeda XX - (2008, A. W. McConnachie et al.)

Andromeda XXI – (2009, N.F. Martin et al. PAndAS)

Andromeda XXII – Pisces VI/Triangulum I ((2009, N.F. Martin et al. PAndAS)

Andromeda XXIII – (2011, J.C. Richardson et al. PAndAS)

Andromeda XXIV – (2011, J.C. Richardson et al. PAndAS)

Andromeda XXV – (2011, J.C. Richardson et al. PAndAS)

Andromeda XXVI – (2011, J.C. Richardson et al. PAndAS)

Andromeda XXVII – (2011, J.C. Richardson et al. PAndAS)

Andromeda XXVIII – (2011, C.T. Slater, E.F. Bell, N.F. Martin, Sdss)

Andromeda XXIX – (2011, E.F. Bell, C.T. Slater, N.F. Martin, Sdss)

Andromeda XXX – Cassiopeia II (2013, L.L. Watkins, N.W. Evans, G. Van de Ven)

Andromeda XXXI – Lacerta I (2013, N.F. Martin et al. Pan-STARRS)

Andromeda XXXII – Cassiopeia III (2013, N.F. Martin et al. Pan-STARRS)

Andromeda XXXIII – Perseus I (2013, N.F. Martin et al.)

Pisces VII – Triangulum III (2020, G. Donatiello et al. DESI LIS) satellite of M33

Andromeda XXXIV / Pegasus V (2021, G. Donatiello et al. DESI LIS)

Triangulum IV (I. Ogami et al. 2024) awaiting confirmation as a possible UDG satellite of M33.

Andromeda XXXV (J. M. Arias et al. 2025).

Pegasus VII (Simon E. T. Smith et al. 2025)

Andromeda (M31), Triangulum (M33) and Mirach ft NGC 404

Credit: Giuseppe Donatiello

Andromeda, like the Milky Way, is a canonical galaxy and a laboratory for examining in detail many of the astrophysical processes that are studied in the more distant field. Studying Andromeda and Triangulum in the Local Group has the advantage of offering us a view free from the problems that plague galactic studies due to our location within the Milky Way, but their location within the Local Group allows us to resolve and study individual stars and infer population properties in incomparably greater detail than is possible in distant systems.

Andromeda is the closest giant spiral galaxy to our own and the only other giant galaxy in the Local Group.

If Andromeda is the twin of the Milky Way, the Triangulum Galaxy (M33), with a mass about 10 times less than either of these two giants, is their little sister. M33 is the third brightest galaxy in the Local Group and probably also a satellite of M31. The relatively undisturbed optical appearance of M33 places strong constraints on the past interaction of these two galaxies, although it should be noted that the gaseous component is highly deformed. To study the halos of both the Andromeda and Triangulum galaxies in more detail, astronomers performed a deep photometric survey. They detected a multitude of large-scale structures of low surface brightness, including several flows and new, rather faint dwarf galaxies.

Significant variations in stellar populations due to flow-like structures are detected in the inner halo. Some previously unseen structures are present in my ultradeep wide-field survey And450.

Happy Saturday, Flickrites! To celebrate our own version of "March Madness," we'll extend our postings to the weekends this month. To start us off, here's a glowing green beauty from Chandra, taken in 2001...

(From 2001) This Chandra image shows remarkable detail and complexity in the central region of the compact galaxy group known as HCG 62. Such galaxy groups, which contain fewer galaxies than the better-known galaxy clusters, are an important class of objects because they may serve as cosmic building blocks in the large-scale structure of the universe. After galaxies themselves form in the early universe, such groups of galaxies may be the next systems to evolve. Later, it is believed, these groups of galaxies may combine with each other to form the bigger galaxy clusters. Most galaxies in the present-day universe are still in groups or poor clusters. Our own Milky Way Galaxy, along with about two dozen other galaxies, including the Andromeda Nebula (M31) and the Large and Small Magellanic Clouds, is part of a galaxy group known as the Local Group.

A team of scientists, led by Jan Vrtilek (Harvard-Smithsonian Center for Astrophysics), observed HCG 62 with Chandra for about 50,000 seconds with the Advanced CCD Imaging Spectrometer. The range of X-ray surface brightness is represented in this image by various colors: green depicts the lower-brightness regions while purple and reddish indicate increasing X-ray intensity. The image is about four minutes of arc on a side, with north to the top and east to the left.

Chandra is an excellent tool to study the intragroup gas (the material between the galaxies) since this medium is too hot (roughly ten million degrees Celsius) to emit any significant radiation at optical wavelengths, but instead radiates most strongly in X-rays. Chandra also offers by far the highest angular resolution of any X-ray telescope to date, which is essential for showing the detailed structure of a complex source such as HCG 62. Hence, this X-ray observation provides a unique window for determining the physical characteristics of the galaxy group. Perhaps the most striking features of this X-ray image of HCG 62 are the two cavities that appear nearly symmetrically opposite one another (upper left and lower right) in the hot, X-ray emitting gas. These cavities might be explained by the presence of X-ray absorbing material, but are more likely due to jets of particles recently emitted from the core of NGC 4761, the central elliptical galaxy of HCG 62, although no such jets are visible today.

Full caption/images: chandra.harvard.edu/photo/2001/hcg62/

Image credit: NASA/CfA/J. Vrtilek et al.

Read more about Chandra:

www.nasa.gov/chandra

p.s. You can see all of our Chandra photos in the Chandra Group in Flickr at: www.flickr.com/groups/chandranasa/ We'd love to have you as a member!

_____________________________________________

These official NASA photographs are being made available for publication by news organizations and/or for personal use printing by the subject(s) of the photographs. The photographs may not be used in materials, advertisements, products, or promotions that in any way suggest approval or endorsement by NASA. All Images used must be credited. For information on usage rights please visit: www.nasa.gov/audience/formedia/features/MP_Photo_Guidelin...

NGC 6822 galaxy and NGC 6818 planetary nebula

Credit: Giuseppe Donatiello

NGC 6822 among the galactic cirrus clouds in the central bulge region. It is a purely prospective alignment since the small and isolated irregular galaxy, one of the most massive of the Local Group, is about 500 kpc (1.6 Mly) away [Cannon et al. 2006].

Having been discovered by Edward Emerson Barnard with a 6-inch telescope, it is also called Barnard's Galaxy.

The pinpoint object with a beautiful turquoise color (upper right) is the planetary nebula NGC 6818. The color is mainly due to the emission of the "forbidden" lines of doubly ionized oxygen [OIII].

Regulus and Leo I (dwarf galaxy)

Credit: Giuseppe Donatiello

RA 10h 08m 22.311s Dec +11° 58′ 01.95″

Regulus , α Leonis (α Leo), is the brightest star in Leo and one of the brightest in the night sky, lying approximately 79 light-years from the Sun.

RA: 10h 08m 27.4s Dec: +12° 18′ 27″

Leo I is a dwarf spheroidal galaxy in Leo at 820,000 light-years. It is part of the Local Group of galaxies as satellite of our Milky Way (properly, Galaxy) . It was discovered in 1950 by Albert George Wilson on photographic plates of the Palomar Observatory Sky Survey (POSS). The proximity of Regulus (Alfa Leo) and the low brightness make it very difficult to observe it.

View of the Andromeda galaxy on November 10th.

Andromeda 450 kpc Survey - Deep survey of the halo of M31

Credit: Giuseppe Donatiello (Oria Amateur Astrophysical Observatory - OAAO)

doi.org/10.5281/zenodo.17622941

Deep survey of the halo of M31

The outskirts of galaxies contain vital clues to their formation history. It is in these regions that new material continues to arrive as part of their ongoing assembly, and it is also in these regions that material was deposited during violent interactions in the galaxy's past. Furthermore, the long dynamical timescales ensure that debris from accreted material takes a long time to be washed away by the merger process. This means that many formation legacies can be detected as coherent structures in space.

Andromeda is the nearest large spiral galaxy and the only other significant one in the Local Group. In many ways, Andromeda is the Milky Way, having very similar total masses, they share a common origin and, probably, the same ultimate fate when they merge. However, there are significant differences between them. M31 is slightly brighter than the Milky Way and has a higher rotation rate and a bulge with a higher velocity dispersion. M31 has a globular cluster system with ~500 members, about 3 times more than the Milky Way.

Andromeda's disk is also much more extended, but is now forming stars at a slower rate than the Galaxy. There are indications that the Milky Way has undergone an exceptionally low amount of mergers and has an unusually low specific angular momentum, while M31 appears to be a much more normal galaxy in these respects.

Andromeda has one compact elliptical galaxy (M32), three dwarf elliptical galaxies (NGC 205, NGC 147, NGC 185) among its entourage of 41 satellites, as well as no dwarf irregular (dIrr) star-forming galaxies within 200 kpc. The Milky Way has no ellipticals but two dIrr (Magellanic Clouds). However, it is perhaps in their supposed halo populations that the differences between the two galaxies are most curious and interesting.

This study of mine, based on ultra-deep imaging, highlights faint structures in the extended halo of M31, NGC 147 3 NGC 185. Some structures appear here for the first time.

This infrared image shows an outer region of the dwarf galaxy Caldwell 51 (IC 1613) and includes some even more distant background galaxies. It was captured by Hubble’s Wide Field Camera 3.

Credit: NASA, ESA, and M. Malkan (UCLA); Processing: Gladys Kober (NASA/Catholic University of America)

For Hubble's Caldwell catalog website and information on how to find these objects in the night sky, visit:

www.nasa.gov/content/goddard/hubble-s-caldwell-catalog

Ghosts and goblins around Mirach

Credit: Kees Scherer, Giuseppe Donatiello, IAC/GTC

Wide field view of the region around the star Mirach, showing the lenticular dwarf NGC 404 (the ghost) and the spheroidal dwarf Donatiello I (the goblin).

The first insert is an enlargement of the background photo, while the inset is a color processing of the galaxy taken at the GranTeCan of 10.4m diameter.

Donatiello I is a small neighboring galaxy, just 10 million light-years away (among the 120 closest to the Milky Way), was discovered on 23 September 2016 by Giuseppe Donatiello. Confirmation images were obtained by the team of the italian Telescopio Nazionale Galileo (TNG) and later captured with the spanish Gran Telescopio Canarias, the largest in the world with its 10.4m.

The announcement article was published in 2018 on Astronomy & Astrophysics [A&A 620, A126 (2018)], with first author David Martínez-Delgado.

Donatiello I is thought to form a pair with NGC 404 [ en.wikipedia.org/wiki/NGC_404], the nearest lenticular dwarf galaxy known as the Mirach's Ghost, from which it would be about 200,000 light-years away.

Messier 31 Andromeda Galaxy

Credit: Giuseppe Donatiello

This image is distributed in full-resolution as CC0 but for its use please refer to what is indicated in the info here: www.flickr.com/people/133259498@N05/

Messier 33

Credit: Giuseppe Donatiello

(J2000) RA: 01h 33m 50.02s Dec: +30° 39′ 36.7″

Messier 33 is a low-luminosity flocculent spiral galaxy at 3 million light-years in Triangulum. It is catalogued also as NGC 598 and known as Triangulum Galaxy. The galaxy is the smallest spiral galaxy in the Local Group and it is believed to be a big satellite of the Andromeda Galaxy.

M33 has two asymmetric faint arms, and an interstellar medium rich in gaseous filaments that extends for about 7 kpc. Although the inner disk is relatively undisturbed, the northern arm is less regular in shape than the southern one. M33, is a bulge-free galaxy with only two optically luminous dwarf galaxies believed to be its satellites: AndXXII (McConnachie et al., 2009; Martin et al., 2016) and Pisces VII (Martínez-Delgado et al., 2022) m discovered by me in 2020. However, given its mass, ΛCDM cosmological simulations predict that M33 should host a larger number of satellites, at least 10.

The neutral hydrogen (HI) disk is three times larger than the star-forming disk and is clearly warped. The outer disk has the same inclination as the inner one with respect to our line of sight but the position angle of the major axis changes by about 30 degrees compared to the inner disk and is more aligned with the M31 direction. While M33's undisturbed inner disk indicates that no major collisions between M31 and M33 or between M33 and a satellite have occurred in the past, the distortion could be the result of a flyby about 9 billion years ago. Timing assessments make this scenario unlikely and favor the hypothesis of a first fall of M33 in the region of influence of M31.

Full resolution image is obtainable only upon reasonable request.

Milky Way and Sagittarius DEG (SagDEG)

Credit: ESA/Gaia DR3, Giuseppe Donatiello

The Sagittarius Dwarf Elliptical Galaxy (Sag DEG or Sgr dSph) is a loop-shaped satellite galaxy of our Milky Way that lies about 70,000 light-years in Sagittarius.

Sag DEG is currently in process of being disrupted by tidal gravitational forces in this encounter. It has orbited the Milky Way, with a period of about 600 million years, at a distance of about 50,000 light-years from the galactic core, strucking our galaxy some 1.9 billion years ago and producing streams of stars out in loops, the Sagittarius Stream.

It contains four globular clusters, with the brightest of them – NGC 6715 (M54) – being known well before the discovery of the galaxy itself in 1994. At a distance from Earth of about 26.8 kpc (50,000 light-years), M54 most likely is the ancient nucleus of Sagittarius Dwarf Elliptical Galaxy.

Obtaining an image of this extremely diffuse galaxy, which is also immersed in the very rich star field of the Galactic Center, was prohibitive in the past, but now, using data from the GAIA satellite, the position and shape of Sag DEG can be revealed, creating density maps like in this image.

This one obtained by me is one of the few available of this nearby satellite that should not be confused with the almost homonymous Sag DIG at about 3.5 million light years.

Pisces VII / Triangulum III ultra faint dwarf galaxy (UFD)

Credit: TNG, Giuseppe Donatiello

Pisces VII belongs to the family of the Andromeda Galaxy (M31).

Since 2013, a new satellite of M31 had not been discovered because its minor satellites are extremely weak, in fact Pisces VII is the faintest galaxy discovered so far outside the domain of the Milky Way.

I discovered it on 1 September 2020 in the DECam images and confirmed by the Telescopio Nazionale Galileo - TNG (image).

David Martínez-Delgado, Noushin Karim, Emily J E Charles, Walter Boschin, Matteo Monelli, Michelle L M Collins, Giuseppe Donatiello, Emilio J Alfaro, Pisces VII: discovery of a possible satellite of Messier 33 in the DESI legacy imaging surveys, Monthly Notices of the Royal Astronomical Society, Volume 509, Issue 1, January 2022, Pages 16–24, doi.org/10.1093/mnras/stab2797

The Large Magellanic Cloud (LMC), an irregular satellite galaxy of the Milky Way, and one of the prime attractions of the southern hemisphere sky. At left is the Tarantula Nebula, NGC 2070, while at upper right is the second brightest nebula in the LMC, NGC 1763, aka the LMC Lagoon. In between are an amazing number of nebulas, both magenta and cyan in tint, as well as clusters of stars. The LMC is 160,000 light years away, and is gravitationally bound to the Milky Way, though there is some dispute whether it is orbiting the Milky Way or is passing by.

This field is 6° x 4°, which just encompasses the majority of the LMC's structure and features.

I shot this Monday, March 24, 2014 from the Warrumbungles Mountain Motel grounds, near Coonabarabran, NSW, Australia. This is a stack of 6 x 10 minute exposures with the Borg 77mm aperture astrographic lens, a 300mm f/4 system, and the Canon 5D MkII camera, filter modified by Hutech, at ISO 800. Shots had to dodge clouds moving through during the evening. Humidity was high from rain earlier in the day. But transparency was good when skies were clear.

Andromeda I

(11.4127, 38.0378)

Discovered by Sidney van den Bergh in 1970 with the Mount Palomar Observatory 48-inch telescope, Andromeda I is the closest known dSph companion to M31 at a projected distance of ~40 kpc.

g',r' CFHT

Pisces VII / Triangulum III

Credit: DESI LIS, G. Donatiello

I discovered it on 1 September 2020 in the DECam images and confirmed by the Telescopio Nazionale Galileo - TNG (image).

We report deep imaging observations with DOLoRes@TNG of an ultra-faint dwarf satellite candidate of the Triangulum galaxy (M33) found by visual inspection of the public imaging data release of the DESI Legacy Imaging Surveys. Pisces VII/Triangulum (Tri) III is found at a projected distance of about 1 Mpc.

We estimate an absolute magnitude of MV = −6.1 ± 0.2 if Pisces VII/Tri II is at the distance of M33, or as bright as MV = −6.8 ± 0.2 if the galaxy is isolated.

With only one potential satellite detected around M33 previously (Andromeda XXII/Tri I), it lacks a significant satellite population in stark contrast to the similarly massive Large Magellanic Cloud.

David Martínez-Delgado, Noushin Karim, Emily J E Charles, Walter Boschin, Matteo Monelli, Michelle L M Collins, Giuseppe Donatiello, Emilio J Alfaro, Pisces VII: discovery of a possible satellite of Messier 33 in the DESI legacy imaging surveys, Monthly Notices of the Royal Astronomical Society, Volume 509, Issue 1, January 2022, Pages 16–24, doi.org/10.1093/mnras/stab2797

Acknowledgment

Data from DECam Legacy Survey (g, r, z filters) obtained at the Blanco Telescope, Cerro Tololo Inter-American Observatory, NSF’s NOIRLab.

Acknowledgments: Legacy Surveys / D. Lang (Perimeter Institute)

Ultra-deep imaging of M33: exploring its stellar halo

Credit: Giuseppe Donatiello

Triangulum Galaxy Extended Halo - And450 survey (sample)

by Giuseppe Donatiello flic.kr/p/2q7MZSG

Triangulum Galaxy (M33) extends well beyond its disk in a radius of some degrees. In this region, excluding the dust cirrus clouds, there is a system of faint stellar streams and debris produced by the tidal destruction of dwarf galaxies.

Such structures are extremely weak, but they can be highlighted with an appropriate treatment of the data (it is not a simple "inverted") that enhances the latent signal.

(J2000) RA: 01h 33m 50.02s Dec: +30° 39′ 36.7″

Messier 33 is a low-luminosity flocculent spiral galaxy at 3 million light-years in Triangulum. It is catalogued also as NGC 598 and known as Triangulum Galaxy. The galaxy is the smallest spiral galaxy in the Local Group and it is believed to be a big satellite of the Andromeda Galaxy.

M33 has two asymmetric faint arms, and an interstellar medium rich in gaseous filaments that extends for about 7 kpc. Although the inner disk is relatively undisturbed, the northern arm is less regular in shape than the southern one. M33, is a bulge-free galaxy with only two optically luminous dwarf galaxies believed to be its satellites: AndXXII (McConnachie et al., 2009; Martin et al., 2016) and Pisces VII (Martínez-Delgado et al., 2022) m discovered by me in 2020. However, given its mass, ΛCDM cosmological simulations predict that M33 should host a larger number of satellites, at least 10.

The neutral hydrogen (HI) disk is three times larger than the star-forming disk and is clearly warped. The outer disk has the same inclination as the inner one with respect to our line of sight but the position angle of the major axis changes by about 30 degrees compared to the inner disk and is more aligned with the M31 direction. While M33's undisturbed inner disk indicates that no major collisions between M31 and M33 or between M33 and a satellite have occurred in the past, the distortion could be the result of a flyby about 9 billion years ago. Timing assessments make this scenario unlikely and favor the hypothesis of a first fall of M33 in the region of influence of M31.

The image is a panel from my And450 photo survey that I have been doing for a few years.

The nomenclature used is according to the PAndAS survey.

The image used as a color inset is only a short exposure layer as the processed image is much deeper with saturated luminance.

This image uses data obtained primarily with telephoto lenses. EQ5 and Avalon M-zero Obs mount.

This image is distributed in full-resolution as CC0 but for its use please refer to what is indicated in the info here: www.flickr.com/people/133259498@N05/

Full resolution image is obtainable only upon reasonable request.

Andromeda Galaxy + H-alpha clouds

credit: Giuseppe Donatiello

(J2000) RA: 00h 42m 44.3s Dec: +41° 16′ 9″ (core)

The Andromeda Galaxy, or Messier 31 (M31) and NGC 224, is a spiral galaxy approximately at 780 kiloparsecs (2.5 million light-years). It is the largest menber of the Local Group of galaxies, which also contains the Milky Way, the Triangulum Galaxy, and other smaller galaxies.

The Andromeda Galaxy, z = −0.001001, is approaching the Milky Way at about 110 Km/sec.

Composite 68MB mosaic. This image uses data taken with Tair-3S (300mm f/4.5) and custom Canon 250mm f/2.2 telephoto lenses. H-alpha data are obtained with Astronomik 12nm clip filter.

--------------------------------------------------------------

This image is distributed as CC0 but for its use please refer to what is indicated in the info here: www.flickr.com/people/133259498@N05/

Full resolution 15K px image is obtainable only upon reasonable request.

Pegasus V (Andromeda XXXIV) is a new ultra-faint satellite galaxy of Andromeda (M31) and is one of the furthest away as it is about 242 kpc (780,000 light years) from its nucleus. However, it is slightly closer to our Milky Way, in fact it is 692 kpc (about 2.25 million light years) away. The diameter is about 600 light years.

It was studied by the same international group that characterized Pisces VII (Michelle L. M. Collins, Emily J. E. Charles, David Martinez Delgado, Matteo Monelli, Noushin Karim, Giuseppe Donatiello, Erik J . Tollerud, Walter Boschin) and the results were illustrated in a paper with first author Dr. Collins of the University of Surrey.

I discovered PegV during a specific search for new M31 satellites on January 22, 2021 in the DESI LIS data. It is now my sixth galaxy discovered and the second in the Local Group.

Michelle L M Collins, Emily J E Charles, David Martínez-Delgado, Matteo Monelli, Noushin Karim, Giuseppe Donatiello, Erik J Tollerud, Walter Boschin, Pegasus V/Andromeda XXXIV–a newly discovered ultrafaint dwarf galaxy on the outskirts of Andromeda, Monthly Notices of the Royal Astronomical Society: Letters, Volume 515, Issue 1, September 2022, Pages L72–L77, doi.org/10.1093/mnrasl/slac063

Located in the constellation Andromeda, M110 was discovered in 1773 by Charles Messier. It is a satellite galaxy of the Andromeda galaxy (M31) and a member of the Local Group, which is made up of the galaxies located closest to the Milky Way (our Milky Way is considered a member of the Local Group as well). M110 is approximately 2,690,000 light-years away from Earth and has a magnitude of 8.

M110 is an elliptical galaxy, which means that it has a smooth and nearly featureless structure. Elliptical galaxies do not have arms or regions of star formation. They are oftentimes considered "dead" compared to spiral galaxies, and the stars in elliptical galaxies are often older than those in other galaxies. However, there is evidence that a population of young blue stars exists at the center of M110. This small elliptical galaxy has approximately 10 billion stars, as well as at least eight globular clusters (the brightest of which can be seen with large telescopes).

This Hubble observation was taken in visible and near-infrared light with the Wide Field and Planetary Camera 2. The core of M110 is seen toward the lower right of the image, with the galaxy's globular clusters and numerous stars shown as points of light throughout the frame. Also featured in this Hubble image are large clouds of gas and dust, seen as dark splotches (one large region is located near the middle of the image and another, smaller one appears above the galaxy's core). Hubble took these observations of M110 to study the development of globular clusters located in the galaxy.

With a telescope, M110 is fairly easy to spot near the core of the much larger and brighter Andromeda galaxy. Smaller telescopes will only reveal a faint, diffuse patch of light, while larger telescopes will unveil an oval shape with a brighter core. The best time to view M110 is during November.

Credits: NASA, ESA, STScI and D. Geisler (Universidad de Concepción)

Pisces VII/Triangulum III

Credit: Dark Energy Camera Legacy Survey (DECaLS), Gemini Observatory/NOIRLab/NSF/AURA, M.L.M. Collins et al., Giuseppe Donatiello

Pisces VII/Triangulum III (Pisc VII) was discovered in the DESI Legacy Imaging Survey and was shown to be a Local Group dwarf galaxy with follow-up imaging from the 4-m Telescopio Nazionale Galileo.

The distance bound from the red giant branch population placed Pisc VII as either an isolated ultra-faint dwarf galaxy or the second known satellite galaxy of Triangulum (M33). Using deep imaging from Gemini GMOS-N, we have resolved the horizontal branch of Pisc VII, and measure a distance of

916 kpc, making Pisc VII a likely satellite of M33.

We also discuss the presence of blue plume and helium burning stars in the colour–magnitude diagram of Pisc VII that are consistent with ages of ∼1.5 Gyr. If these are truly members of the galaxy, it would transform our understanding of how reionization affects the faintest galaxies. Future deep imaging and dynamics could allow significant insight into both the stellar populations of Pisc VII and the evolution of M33.

Reference papers:

David Martínez-Delgado, Noushin Karim, Emily J E Charles, Walter Boschin, Matteo Monelli, Michelle L M Collins, Giuseppe Donatiello, Emilio J Alfaro, Pisces VII: discovery of a possible satellite of Messier 33 in the DESI legacy imaging surveys, Monthly Notices of the Royal Astronomical Society, Volume 509, Issue 1, January 2022, Pages 16–24, doi.org/10.1093/mnras/stab2797

Michelle L M Collins, Noushin Karim, David Martinez-Delgado, Matteo Monelli, Erik J Tollerud, Giuseppe Donatiello, Mahdieh Navabi, Emily Charles, Walter Boschin, Pisces VII/Triangulum III – M33’s second dwarf satellite galaxy, Monthly Notices of the Royal Astronomical Society, Volume 528, Issue 2, February 2024, Pages 2614–2620, doi.org/10.1093/mnras/stae199

The information and annotations in the image are of scientific utility because they identify the subject and place it in a specific moment. They also indicate the subject of interest. The absence of such information makes the images useless.

Donatiello I dSph

credit: Giuseppe Donatiello

This composite image make use of data taken by CFHT, Cerro Tololo Blanco 4.2m Telescope/DECalLs DR8, 3.58m Telescopio Nazionale Galileo (TNG).

Donatiello I dSph was discovered on September 23, 2016. Discovery annunced on October 12, 2018

Martínez-Delgado et al.: Mirach’s Goblin: Discovery of a dwarf spheroidal galaxy behind the Andromeda galaxy (A&A 620, A126 (2018)) -- Full paper link: doi.org/10.1051/0004-6361/201833302

Pisces VII / Triangulum III HST

Credit: NASA/ESA/Hubble, M.G. Jones, G. Donatiello

Pisces VII / Triangulum III: What could be more exciting than seeing an object you discovered imaged by the Hubble Space Telescope?

Pisces VII / Triangulum III is an ultra-faint dwarf (UFD) galaxy that I found in September 2020 while analyzing data from the DESI LIS, a survey that was not designed to search for satellite galaxies in the Andromeda system (M31), but for dark energy.

The study, using deep images taken by our Telescopio Nazionale Galileo (TNG), confirmed that the source was in the M31 subgroup and that, indeed, it could be a strong candidate for a satellite of Triangulum (M33), the LB dwarf spiral galaxy believed to be its largest satellite. In other words, it was a satellite of another satellite, flanking Andromeda XXII.

Data analysis led to an estimate of its distance at about 3 million light-years.

Thanks to new Hubble data, the distance has now been refined to 929 ±48 kpc, essentially the same distance already estimated with TNG data (Michael G. Jones et al. 2025).

Of the 11 dwarf spheroidal and UFD galaxies I've discovered so far, HST has observed five: Donatiello II, Donatiello III, Donatiello IV, Pisces VII, and Pegasus V (image coming soon).

References on Pisces VII:

David Martínez-Delgado et al., Monthly Notices of the Royal Astronomical Society, Volume 509, Issue 1, January 2022, Pages 16–24

Michelle L M Collins et al., Monthly Notices of the Royal Astronomical Society, Volume 528, Issue 2, February 2024, Pages 2614–2620

(My elaboration from the original FITS via MAST Archive)

Sextans A [UGCA 205, DDO 75, PGC 29653]

10 11 00.5 -04 41 30 (152.7560, -4.6902)

Sex A s a dwarf irregular galaxy located at 1.32 Mpc (4.3 million light-years), in the outskirts of the Local Group as probable member.

DECam

Acknowledgments

The Dark Energy Spectroscopic Instrument (DESI) data are licensed under the Creative Commons Attribution 4.0 International License (“CC BY 4.0”, Summary, Full Legal Code). Users are free to share, copy, redistribute, adapt, transform and build upon the DESI data available through this website for any purpose, including commercially.

This image used data obtained with the Dark Energy Spectroscopic Instrument (DESI). DESI construction and operations is managed by the Lawrence Berkeley National Laboratory. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of High-Energy Physics, under Contract No. DE–AC02–05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract. Additional support for DESI was provided by the U.S. National Science Foundation (NSF), Division of Astronomical Sciences under Contract No. AST-0950945 to the NSF’s National Optical-Infrared Astronomy Research Laboratory; the Science and Technology Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Science and Technology of Mexico (CONACYT); the Ministry of Science and Innovation of Spain (MICINN), and by the DESI Member Institutions: www.desi.lbl.gov/collaborating-institutions. The DESI collaboration is honored to be permitted to conduct scientific research on Iolkam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham Nation. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the U.S. National Science Foundation, the U.S. Department of Energy, or any of the listed funding agencies.

Caldwell 51, also known as IC 1613, is an irregular dwarf galaxy located in the constellation Cetus. This member of our Local Group of galaxies is located just 2.3 million light-years from Earth and has an apparent magnitude of 9.9. Despite its relative proximity, Caldwell 51 is very difficult to spot and is one of the most elusive Caldwell objects. It appears as an extremely faint and diffuse smudge in the sky, even when viewed through moderately sized telescopes. The galaxy is visible from the Northern Hemisphere in the autumn and from the northern regions of the Southern Hemisphere in the spring. It was discovered in 1906 by the German astrophotographer Max Wolf, who also found many other astronomical objects over the course of his life, including comets, supernovae, and asteroids.

Caldwell 51 is notable for its role in improving distance measurements to more remote objects. Unlike many galaxies, Caldwell 51 is largely unobstructed by dust, and our relatively clear view of the RR Lyrae variable stars it hosts allows astronomers to make precise distance measurements. RR Lyrae variables are pulsating stars that have pulsation periods directly related to their luminosity. So, how fast they pulse tells astronomers how bright the stars truly are; then, how bright the stars actually appear tells astronomers how far away they must be. This relationship allows the stars to act as “standard candles” that can be used to determine the distances to objects within our Local Group of galaxies.

This image of a region near the center of Caldwell 51 is a composite of ultraviolet, infrared, and visible-light observations made by Hubble’s Wide Field Camera 3. The observations were taken to determine the galaxy’s chemical composition. Since most elements in the universe are formed by stars and distributed into their galaxy when the stars die, this information can help researchers learn more about the evolution of the galaxy and its star formation history.

Credit: NASA, ESA, and J. Holtzman (New Mexico State University); Processing: Gladys Kober (NASA/Catholic University of America)

For Hubble's Caldwell catalog website and information on how to find these objects in the night sky, visit:

www.nasa.gov/content/goddard/hubble-s-caldwell-catalog

Donatiello I - The Mirach's Goblin

Credit: Giuseppe Donatiello, IAC/GTC

A new wide field image around the spheroidal dwarf galaxy Donatiello I. This small neighboring galaxy, just 10 million light-years away (among the 120 closest to the Milky Way), was discovered on 23 September 2016 by Giuseppe Donatiello. Confirmation images were obtained by the team of the italian Telescopio Nazionale Galileo (TNG) and later captured with the spanish Gran Telescopio Canarias, the largest in the world with its 10.4m.

The announcement article was published in 2018 on Astronomy & Astrophysics [A&A 620, A126 (2018)], with first author David Martínez Delgado.

Donatiello I is thought to form a pair with NGC 404 [ en.wikipedia.org/wiki/NGC_404], the nearest lenticular dwarf galaxy known as the Mirach's Ghost, from which it would be about 200,000 light-years away.

Sharing on every medium is very welcome. For journalists wishing to learn more, please contact privately via this page.

References:

Mirach’s Goblin: Discovery of a dwarf spheroidal galaxy behind the Andromeda galaxy

- www.aanda.org/articles/aa/abs/2018/12/aa33302-18/aa33302-...

- arxiv.org/abs/1810.04741

- en.wikipedia.org/wiki/Donatiello_I

Nice article by Phil Plait on Bad Astronomy blog:

www.syfy.com/syfywire/an-amateur-astronomer-has-discovere...

Pisces VII with telephoto lens vs TNG

Credit: Giuseppe Donatiello

This is tough!

Stacking some sessions in the M33 region for other purposes, out of curiosity I checked if there was any trace of Pisces VII/Triangulum III in the image.

To my surprise, exactly at the expected position there is a source of a few pixels which undoubtedly is Pisces VII!

It is perhaps the first ultra-faint dwarf (UFD) galaxy to have been imaged with a telephoto lens.

The information and annotations in the image are of scientific utility because they identify the subject and place it in a specific moment. They also indicate the subject of interest. The absence of such information makes the images useless.

Draco dSph

Credit DECaLS, Giuseppe Donatiello

AR: 17h 20' 17" DEC: +57° 55' 58"

The Draco dSph is a small spheroidal dwarf galaxy discovered by Albert George Wilson of Lowell Observatory in 1954 on POSS plates. It's a satellite galaxy of the Milky Way. The Draco Dwarf is estimated to be at 80 ±10 kpc.

L- g (720 sec), r (750 sec), z (570 sec).

CTIO/NOAO 4.0m Victor M. Blanco Telescope

Acknowledgments

The Dark Energy Spectroscopic Instrument (DESI) data are licensed under the Creative Commons Attribution 4.0 International License (“CC BY 4.0”, Summary, Full Legal Code). Users are free to share, copy, redistribute, adapt, transform and build upon the DESI data available through this website for any purpose, including commercially.

This image used data obtained with the Dark Energy Spectroscopic Instrument (DESI). DESI construction and operations is managed by the Lawrence Berkeley National Laboratory. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of High-Energy Physics, under Contract No. DE–AC02–05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract. Additional support for DESI was provided by the U.S. National Science Foundation (NSF), Division of Astronomical Sciences under Contract No. AST-0950945 to the NSF’s National Optical-Infrared Astronomy Research Laboratory; the Science and Technology Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Science and Technology of Mexico (CONACYT); the Ministry of Science and Innovation of Spain (MICINN), and by the DESI Member Institutions: www.desi.lbl.gov/collaborating-institutions. The DESI collaboration is honored to be permitted to conduct scientific research on Iolkam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham Nation. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the U.S. National Science Foundation, the U.S. Department of Energy, or any of the listed funding agencies.

Pisces VII/Triangulum III - Pegasus V/Andromeda XXXIV

Credit: Gemini North, Giuseppe Donatiello

Pisces VII / Triangulum III

Pisces VII is one of the faintest dwarf galaxy detected beyond the Milky Way at 820 kpc (2.6 milion light years). Pisces VII is an ultra faint dwarf (UFD) first seen in DECam images, and followed by the TNG. It is quite close in projection to M33 so is a possible very small satellite.

It is my second discovery in this topic.

more here: arxiv.org/abs/2104.03859

arxiv.org/abs/2305.13966

Pegasus V (Andromeda XXXIV)

Pegasus V (Andromeda XXXIV) is a new ultra-faint satellite galaxy of Andromeda (M31) and is one of the furthest away as it is about 242 kpc (780,000 light years) from its nucleus. However, it is slightly closer to our Milky Way, in fact it is 692 kpc (about 2.25 million light years) away. The diameter is about 600 light years.

It was studied by the same international group that characterized Pisces VII (Michelle L. M. Collins, Emily J. E. Charles, David Martinez Delgado, Matteo Monelli, Noushin Karim, Giuseppe Donatiello, Erik J . Tollerud, Walter Boschin) and the results were illustrated in a paper with first author Dr. Collins of the University of Surrey.

I discovered PegV during a specific search for new M31 satellites on March 17, 2021 in the DESI LIS data. It is my sixth galaxy discovered and the second in the Local Group.

(Collins, M. L. M. et al 2022) : arxiv.org/abs/2204.09068

Triangulum Galaxy Extended Halo - And450 survey (sample)

Credit: Giuseppe Donatiello

M33 represents a unique opportunity to study spiral galaxies. Dwarf galaxies tend to be irregular mixtures of stars and gas, very different from the beautiful, larger spirals. Large, undisturbed dwarf spirals, like M33, are therefore environments that allow a better understanding of hierarchical formation phenomena.

Strange as it may seem, we still know little about M33. It is unclear whether or not it interacted with the larger Andromeda galaxy (M31).

Both its proximity to M31 and the distorted structure of M33's disk suggest that the galaxies already interacted tidally with each other about 2.5 billion years ago. The effect of this interaction is currently observed as a deformation of the outer part of M33's disk. A close passage between the galaxies would also have increased star formation activity in M33, according to a simulation (Semczuk et al. 2018). According to this scenario, M33 would have already encountered M31 and perhaps lost its satellites and globulars.

In a second scenario, M33 would instead be falling into the Local Group for the first time, thus retaining its entourage of satellites and globulars. According to models, a galaxy like M33 should possess at least a dozen satellite galaxies, but to date only two are suspected: Andromeda XXII (Martin et al. 2013) and Pisces VII, discovered by me (Martinez-Delgado et al. 2021). Triangulum IV remains to be confirmed.

Ultra-deep images, like this one, suggest a past of interaction as documented by two flows to the north and south. However, their formation may not be due to interaction with Andromeda but rather the consequence of the capture and destruction of one of its satellites.

The image was obtained with a telephoto lens array and is a fragment of a larger mosaic in the And450 survey program of the UAI National Deep Sky Research Section (G. Donatiello et al., in progress). The specific processing allows us to highlight the faintest regions of the halo and the associated tidal structures.

Nomenclature is according to the PAndAS survey.

To use this image please first read here: www.flickr.com/people/133259498@N05/

Located in Cassiopeia, not far from Caldwell 17, Caldwell 18 is a dwarf galaxy and a satellite of the Andromeda galaxy. Also known as NGC 185, it is a member of the Local Group of galaxies. Caldwell 17 is notable for its active galactic nucleus, a region at the center of the galaxy that emits extreme radiation over part of the electromagnetic spectrum.

Some astronomers classify Caldwell 18 as a type II Seyfert galaxy. These types of galaxies appear intensely bright when observed at infrared wavelengths despite their unremarkable brightness in visible wavelengths. Although the classification of Caldwell 18 remains up for debate within the astronomical community, if it is indeed a Seyfert galaxy, then it would be the only one known in the Local Group and the closest one to Earth.

Caldwell 18 was discovered in 1787 by the British astronomer William Herschel (who also discovered the planet Uranus). It is visible from the Northern Hemisphere in the autumn and from northern latitudes of the Southern Hemisphere in the spring. With an apparent magnitude of 9.2, this galaxy can be found with powerful binoculars. Caldwell 18 is easier to spot than the neighboring Caldwell 17, because its center appears more circular and compact than that of its neighbor.

This Hubble image combines observations taken with Hubble’s Wide Field Camera 3 in visible and infrared wavelengths. Clouds of dust appear near the galaxy’s center, and a globular star cluster appears to the left. These Hubble observations helped astronomers study the characteristics of globular clusters in nearby dwarf galaxies.

Credit: NASA, ESA, and A. Ferguson (University of Edinburgh, Institute for Astronomy); Processing: Gladys Kober (NASA/Catholic University of America)

For Hubble's Caldwell catalog website and information on how to find these objects in the night sky, visit:

www.nasa.gov/content/goddard/hubble-s-caldwell-catalog

Caldwell 17, also known as NGC 147, is a dwarf galaxy located roughly 2.5 million light-years from Earth. It is a member of the Local Group of galaxies, which is dominated by our Milky Way and the Andromeda galaxy. Caldwell 17, like its neighbor Caldwell 18, is a distant satellite of the Andromeda galaxy. Just as the planets in the solar system are gravitationally bound to the Sun, so are these smaller galaxies bound to their much more massive galactic host. While many classes of galaxies can exist as satellites, dwarf spheroidal galaxies (small, dim, spherical-shaped galaxies) like Caldwell 17 have been observed in this role more frequently than any other type of galaxy.

Dwarf satellite galaxies tend to appear very diffuse and dim, so they can be difficult to spot (especially in light-polluted or hazy skies). Caldwell 17 is no exception. It has an apparent magnitude of 9.5, and observers will need a small telescope set up in a dark location to detect the faint galaxy. Caldwell 17 is located in the southern edge of the constellation Cassiopeia, between the constellation’s “W” pattern and the Andromeda galaxy. (The neighboring Caldwell 18 is brighter and less diffuse, so it is easier to see.) The best time of year to spot Caldwell 17 from the Northern Hemisphere is the autumn. It can also be seen in northern latitudes of the Southern Hemisphere in the spring. The galaxy was discovered by the English astronomer John Herschel in September of 1829.

This image of Caldwell 17 is a composite of observations made in visible and infrared light by Hubble’s Wide Field Camera 3. The image captures an area near the core of the galaxy, which is notable for its elderly stellar population. Astronomers used Hubble’s observations to investigate the properties of Caldwell 17’s many globular star clusters.

Credit: NASA, ESA, and A. Ferguson (University of Edinburgh, Institute for Astronomy); Processing: Gladys Kober (NASA/Catholic University of America)

For Hubble's Caldwell catalog website and information on how to find these objects in the night sky, visit:

www.nasa.gov/content/goddard/hubble-s-caldwell-catalog

This image shows a globular star cluster located in the dwarf galaxy Caldwell 17 (or NGC 147). It was imaged by Hubble’s Wide Field Camera 3 (WFC3) in visible and infrared light.

Credit: NASA, ESA, and H. Bond (Pennsylvania State University); Processing: Gladys Kober (NASA/Catholic University of America)

For Hubble's Caldwell catalog website and information on how to find these objects in the night sky, visit:

www.nasa.gov/content/goddard/hubble-s-caldwell-catalog

This is the large (1/2º across) and bright (8th magnitude) edge-on galaxy NGC 55 in Sculptor. It is one of the brightest members of the Sculptor Group of galaxies near the South Galactic Pole, though some consider it a member of our own Local Group. It has an asymmetrical shape and is crossed by dark dust lanes. It is classed as a barred spiral.

The field of view is 3° by 2°.

Technical:

This is a stack of 16 x 4 minute exposures with the Askar APO120 refractor at f/5.6 (with its 0.8x Reducer) and the Canon Ra at ISO 1000. Taken from the Quailway Cottage in southeast Arizona in October 2024, with this field low in the south.

Credit: TNG/CFHT/Giuseppe Donatiello

simbad.u-strasbg.fr/simbad/sim-basic?Ident=name+donatiell...

Donatiello I, also known as Mirach's Goblin, is a dwarf spheroidal galaxy located in the constellation Andromeda, at between 8.1 and 11.4 million light-years from Earth. It is a possible satellite galaxy of the dwarf lenticular galaxy NGC 404, "Mirach's Ghost", which is located 60 arcminutes away.

It is otherwise one of the most isolated dwarf spheroidal galaxies known, being physically located around 211,000 light-years away from NGC 404.

The galaxy is named after its discoverer, amateur astrophotographer Giuseppe Donatiello, who sighted the galaxy in a 2016 review of his archival long exposures from 2010 and 2013. Follow-up observations with the Roque de los Muchachos Observatory led to a scientific paper on its discovery being published in December 2018. (Wikipedia)

en.wikipedia.org/wiki/Donatiello_I

www.aanda.org/articles/aa/abs/2018/12/aa33302-18/aa33302-...

Most galaxies are found in groups or clusters. Our own galaxy, the Milky Way, for example, is part of group of around 50 nearby galaxies dubbed the Local Group. But this galaxy, cataloged as NGC 6503, is located at the edge of a strangely empty patch of space called the Local Void.

The Local Void is a stretch of space that is at least 150 million light-years across. It seems completely empty of stars or galaxies. The galaxy's odd location on the edge of this celestial blank spot led stargazer Stephen James O'Meara to dub NGC 6503 the "Lost-In-Space galaxy."

This Hubble Space Telescope image shows NGC 6503 in striking detail and with a rich set of colors. Bright red patches of gas can be seen scattered through its swirling spiral arms, mixed with bright blue regions that contain newly forming stars. Dark brown dust lanes snake across the galaxy's bright arms and center, giving it a mottled appearance.

For more information, visit: hubblesite.org/image/3586/news_release/2015-23

Credit: NASA, ESA, D. Calzetti (University of Massachusetts), H. Ford (Johns Hopkins University), and the Hubble Heritage (STScI/AURA)-ESA/Hubble Collaboration

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The long awaited Astronomik CLS filter finally arrived, and could not wait to test it. Targeted M31, about 40 degrees from 93% moon on October 28. Gradient from either the moon's glow and/or Tromsø's city lights halo.

I tried different methods in PI and PS to eliminate the gradient, but struggled to not introduce more colour noise in the background. So left it for an overall cleaner image.

Equipment:

Canon EOS450D (astromodified)

William Optics Z61+ flatttener

Astronomik CLS-filter

Celestron AVX-mount

Orion 50mm guidescope + SAG

PHD!-guiding with dithering.

Exposures: total 1h 9 min, 23x 180sec lights ISO800, 20 darks, flats & bias.

Stacked in DSS, stretched in PI, and further edited in PS.

This Hubble image, taken by the Advanced Camera for Surveys, shows stars in the outskirts of the dwarf galaxy Caldwell 18 (NGC 185) as well as distant background galaxies (which appear as extended patches of light).

Credit: NASA, ESA, and A. Ferguson (University of Edinburgh, Institute for Astronomy); Processing: Gladys Kober (NASA/Catholic University of America)

For Hubble's Caldwell catalog website and information on how to find these objects in the night sky, visit:

www.nasa.gov/content/goddard/hubble-s-caldwell-catalog

The Triangulum galaxy is the smallest of the three spiral galaxies in the local group, being about a tenth the mass of Andromeda and the Milky Way. At 3 million light years distance, this is the farthest object from earth that can be viewed with the naked eye. I've tried from some very dark places, but can't be sure whether I saw it or just imagined it!

This is 36 minutes of exposure time, taken over 16 exposures with the modified Canon Xsi at ISO 1600 through a 500mm lens at f/4 riding piggyback on the scope. Guiding by PHD Guiding.

This Hubble image shows a small part of the dwarf galaxy Caldwell 17 (NGC 147). Near the center of the image is a globular star cluster located in the galaxy. It was imaged by Hubble’s Wide Field and Planetary Camera 2 (WFPC2) in visible and infrared light.

Credit: NASA, ESA, and J. Trauger (Jet Propulsion Laboratory); Processing: Gladys Kober (NASA/Catholic University of America)

For Hubble's Caldwell catalog website and information on how to find these objects in the night sky, visit:

www.nasa.gov/content/goddard/hubble-s-caldwell-catalog

This is a showpiece of the southern skies, the Large Magellanic Cloud, a satellite galaxy of our Milky Way and one rich in star forming nebulas and clusters.

The bright cyan Tarantula Nebula, NGC 2070, is at left, with the NGC 2014/NGC 1935 area above it. The NGC 1763 complex is at upper right.

Though short in accumulated exposure time this night, this still shows some of the faint outlying glow of outer spiral arms, and some interstellar or intergalactic dust or gas clouds at lower right.

The field is 15º by 10º.

This is a stack of just 9 x 2-minute exposures with the Canon RF135mm lens at f/2 on the Canon Ra at ISO800, tracked but not guided on the Astro-Physics AP400 mount. The lens was equipped with an 82mm URTH Night broadband filter.

Taken March 14, 2024 from the Warrumbugles Mountain Motel near Coonabarabran, NSW, Australia. Incoming clouds prevented more exposures, and some light cloud on the last frame added the slight natural star glows.

This image shows stars at the center of the dwarf galaxy Caldwell 17 (NGC 147). The image was taken in visible and infrared light by Hubble’s Wide Field and Planetary Camera 2 (WFPC2).

Credit: NASA, ESA, and J. Trauger (Jet Propulsion Laboratory); Processing: Gladys Kober (NASA/Catholic University of America)

For Hubble's Caldwell catalog website and information on how to find these objects in the night sky, visit:

www.nasa.gov/content/goddard/hubble-s-caldwell-catalog

M54, the nucleus of the dwarf galaxy SagDEG

Credit: Giuseppe Donatiello

RA/DEC: 18 55 03.330 -30 28 47.50

Some time ago, we showed you the density map of the galactic bulge obtained with Gaia data [ flic.kr/p/HQkH3Y ]. In that image we had delimited Sagittarius Dwarf Elliptical Galaxy (SagDEG) with an ellipse, highlighting how the globular cluster M54 occupied its exact center.

SagDEG is apparently enormous in the sky and occupies much of the eastern area of the constellation of Sagittarius, but it is in fact invisible. In fact, it was discovered just 30 years ago by Rodrigo Ibata, Gerry Gilmore and Mike Irwin due to the overdensity of old Population II stars [Nature 370, 194–196 (1994)].

About 10 thousand light years wide, it is estimated at about 70 thousand (21 kpc) and is still being captured by the Milky Way which is literally dismembering and sucking it. In fact, we find the majority of its stars in the so-called Sagittarius Stream which forms a double ring almost orthogonal to the disk of our Galaxy.

Four globular clusters are attributed to SagDEG, however M54 is particularly rich and compact. Occupying its geometric center, it is plausible that it represents its nucleus. In other words, observing M54 we are observing one of the approximately 70 satellites of the Milky Way.

In this image (crop), obtained over two nights (6-7 August 2024), the entire field - please enlarge - is filled with faint stars with magnitudes certainly comparable to those of M54: they are all stars belonging to SagDEG.

It has been two years since I last photographed this nearby galaxy.

31 light frames stacked with DeepSkyStacker 3.3.4.

ISO 400

Exposure 90 seconds; total exposure 46.5 min.

Prime focus through an Explore Scientific 80mm f/6 APO ED triplet refractor

Explore Scientific field flattener

Canon T3i, unmodded

Celestron Advanced VX equatorial mount.

Dark, flat, dark flat, and bias frames used to correct noise

Post-processing with Photoshop CC 2015, StarSpikes Pro 3

The first amateur image of Sextans Dwarf Spheroidal

Credit: Giuseppe Donatiello (Oria Amateur Astrophysical Observatory - OAAO)

Sextans dSph is located at the mean coordinates 10 13 03.00 -01 36 53.0

Incredibly, there is not a single image of the dwarf spheroidal galaxy Sextans (not to be confused with Sextans A and B as Wikipedia does). The object extends for no less than 4°x2° in a very rich field.

Sex dSph does not even have an exuberant density and its stars have magnitudes of about 22-23.

Was it possible to obtain an overdensity with amateur instruments?

By reprocessing the stack that I had obtained in 2024, I can say that I have detected the overdensity of Sextans.

As far as I know, this is the first and only amateur image of this satellite galaxy of the Milky Way, 320,000 light.years (90 ± 10 kpc) away.

With astrograph 110/250mm f/2.2

Edited Hubble Space Telescope image of the irregular galaxy IC 10, a mere 2.2 million light years away.

Original caption: This image shows an irregular galaxy named IC 10, a member of the Local Group — a collectiongrouping of over 50 galaxies inwithin our cosmic neighbourhood that includes the Milky Way. IC 10 is a remarkable object. It is the closest-known starburst galaxy to us, meaning that it is undergoing a furious bout of star formation fueled by ample supplies of cool hydrogen gas. This gas condenses into vast molecular clouds, which then form into dense knots where pressures and temperatures reach a point sufficient to ignite nuclear fusion, thus giving rise to new generations of stars. As an irregular galaxy, IC 10 lacks the majestic shape of spiral galaxies such as the Milky Way, or the rounded, ethereal appearance of elliptical galaxies. It is a faint object, despite its relative proximity to us — just of 2.2 million light-years. In fact, IC 10 only became known to humankind in 1887, when American astronomer Lewis Swift spotted it during an observing campaign. The small galaxy remains difficult to study even today, because it is located along a line-of-sight which is chock-full of cosmic dust and stars. A version of this image was entered into the Hubble's Hidden Treasures image processing competition by contestant Nikolaus Sulzenauer, and went on to win tenth prize.

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