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A delightful and unusual merger of galaxies, resulting in the comet-like appearance of one galaxy. Only a small amount of dust is visible, but many small dots which I presume are globular clusters are sprinkled within the pair. Edit: Upon looking at the color data, the clusters may be younger clusters, not necessarily globulars. It's bluer than I expected, which would indicate that star formation has been going on.
A color and widefield view is available in SDSS data at the Legacy Survey viewer: legacysurvey.org/viewer?ra=73.3523&dec=-4.7932&zo...
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 12.84° clockwise from up.
NGC 2146 is a disrupted barred spiral galaxy in the constellation of Camelopardalis. It was discovered in 1876 by German astronomer Friedrich Winnecke, who was known for his work on comets, asteroids, and double stars. The galaxy is classified as SB(s)ab pec, indicating a barred spiral galaxy with tightly wound arms, and no ring around the central bulge. The "pec" descriptor refers to the "peculiar" appearance of the spiral arms, one of which is markedly stretched and inclined to the galactic plane by nearly 45*. Very high star formation rate (SFR) and densities within both spiral arms resembling large stellar trails suggest the galaxy recently merged with one or two substantial dwarf satellites, and is presently reforming into a larger object. Some sources suggest that NGC 2146 may have interacted with a nearby small galaxy, NGC 2146a, however that seems unlikely because the small galaxy's spiral structure appears quite well preserved. Aside from its disrupted aspect and starburst activity, NGC 2146 is also distinctive due to its conspicuous dust lanes extending across the background glow of the galactic core. Spectroscopy of the central region reveals widening of spectral lines. This indicates a high velocity dispersion of the stars in the nucleus due to the presence of a central supermassive black hole (SMBH). Absence of an active galactic nucleus means thet the central SMBH is not presently accreting matter.
Assuming its measured redshift of 0.00298 is caused exclusively by the expansion of space (Hubble Flow), NGC 2146 would lie at a distance of 41.3 Mly. However, the median value of 16 redshift-independent distance measurements is 17.40 Mpc, or 56.72 Mly. The two distance estimates differ because the measured redshift actually results from the combined motion due to Hubble Flow and the object's "peculiar velocity" through space. When available in a statistically valid number of measurements, redshift-independent estimates are generally regarded as more accurate for nearby galaxies, closer than approximately 140 Mly. From the apparent magnitude and angular size, accepting the distance of 56.72 Mly, we can derive the galaxy's actual diameter of 97,000 ly and absolute magnitude of -20.64. NGC 2146 is some 20-30% smaller, and about 15% less bright than the Milky Way.
Chandra CXC HIPS X-ray sky survey (SIMBAD) shows numerous X-ray sources within the NGC 2146 core, in the spiral arms, and in its halo. While it is possible that some of the sources may be local to the Milky Way, clustering of the sources around NGC 2146 suggests that most are of extragalactic origin.
The most common mechanism for X-ray emission in astronomical objects involves very hot ionized gases at temperatures of millions to hundreds of millions Kelvin (K). Stellar coronas, especially in young blue giants, emit X-rays, though they are regarded as relatively weak sources. Stronger emissions come from "X-ray binaries", "cataclysmic variable stars", supernova remnants, and hot gas clouds around stellar nurseries. Still stronger localized X-ray emissions are "ultra-luminous X-ray sources" or ULX. These are produced by actively accreting intermediate mass black holes (IMBH), usually identified in galactic disks, and by central supermassive black holes (SMBH) which define "active galactic nuclei" (AGN). By far the most powerful, but very diffuse, sources of X-rays are galaxy clusters.
While it is logical to expect numerous X-ray emissions in an actively merging starburst galaxy with accelerated stellar evolution, NGC 2146 has no identified ultra-luminous X-ray sources and no active galactic nucleus. This does not imply the galaxy contains no intermediate or supermassive black holes, but merely that they are not actively accreting.
On closer inspection, the attached image records a number of small, faint background galaxies, but only two of these have identifiers associated with measurable data. Based on a subjective estimate of their angular size and apparent brightness, the rest probably lie at approximate distances between 1 and 2 Bly. The image also records a single quasar (QSO) at a light travel distance (lookback time) of 9.2 Bly.
The distinctly blue galaxy Gaia DR3 1140883127890416128 may belong to a class of special objects: "Blue Compact Dwarf" galaxies (BCDs), which are field dwarf galaxies with inexplicably high star formation rates. BCDs are rare local versions of the "Faint Blue Galaxies" (FBGs), the most common galaxy type at redshifts between 0.1 and 2, but which are undetectable with small instruments. I estimate the apparent magnitude of this object around 20.5 and angular size at 0.15 arcmin. Unfortunately, no redshift information or color photometry is available in extragalactic databases, and the suspected nature of this galaxy can not be confirmed. For additional details on BCDs and FBGs please see section 32, Dwarf Galaxies, subsections 6 and 7 here:
www.cloudynights.com/articles/cat/articles/basic-extragal...
Image Details:
Remote Takahashi TOA 150x1105 mm
OSC 31x300 sec, 2x drizzle, 40% linear crop, 26x17'
Software:
DSS, XnView, StarNet++ v2, StarTools v1.8
Extragalactic Cosmological Calculator v2
www.cloudynights.com/gallery/image/123530-extragalactic-c...
[Version Française en haut / English version below]
Lien photo d'origine : flic.kr/p/2p21GPo
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Note sur la V2 : Un grand merci à Damien Guillard, un ptit gars qu'est pas mauvais en astro, à m'avoir aidé à tirer le meilleur du signal de cette photo.
La différence est un traitement BlurXTerminator sur ma photo, fait par Damien. J'ai utilisé sa sortie affinée comme calque parmi les calques existants pour faire ressortir les nébuleuses.
Note about the V2 : A special thank to Damien Guillard,a young fella who's pretty good at astrophotography, for helping me get the most out of the signal in this photo.
The difference is a BlurXTerminator treatment on my photo, done by Damien. I used his refined output as a layer among the existing layers to bring out the nebulae.
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[Version française]
La galaxie du Triangle (Messier 33)
Il y a deux ans, j'avais fait une petite session sur la galaxie M33. Je n'en étais qu'à moitié satisfait car triop peu de poses (1h11 seulement). Voilà ce que j'écrivais à l'époque : "j'ai un peu galéré ce soir là parce que je testais ma configuration mobile (loin de la maison), avec une reprise des sessions astro avec le télescope (il fallait se réhabituer depuis le printemps), beaucoup d'humidité et je n'avais pas encore fabriqué mes résistances chauffantes, mon autoguidage ne fonctionnait pas parce que j'avais mal configuré mon wifi ... Du coup la photo n'est pas top car j'ai du jeter la moitié des poses à cause de la buée, et aussi parce que je n'ai toujours pas mis mon correcteur de coma. Elle a un goût de revanche du coup !". Eh bien ça y est ! je l'ai ma revanche. J'ai pas mal attendu ne trouvant jamais le temps ou la météo adaptée pour M33.
Cataloguée par Charles Messier en 1764, elle a du être observée avant. Sous un ciel extraimement clair, il est effectivement possible de distinguer sa tâche laiteuse à l'oeil nu. J'en ai fait l'expérience le 06/09/23 (deuxième session). Avec de bonnes jumelles, si vous savez où elle se trouve, sa détection est un peu plus facile (elle reste très sombre).
Sa distance est comprise entre 2.38 et 3.07 millions d'années lumières (elle n'est pas connue avec précision), et elle fait environ 50000 à 60000 AL de diamètre. La masse de cette galaxie est d'environ 60 milliards de masses solaires, mais seulement 17% de sa masse vient de matière ordinaire ; 83% de sa masse provient de cette composante de l'univers qu'on ne détecte pas encore, mais dont on mesure la présence, et que l'on nomme matière noire (pour signifier qu'on ne la voit pas). Les presque 12h d'exposition en HOO (Hydrogène Alpha dans le rouge + Oxygène III dans le bleu/vert) font ressortir fortement les nébuleuses, ces grandes tâches rouges et bleues qui sont des nuages denses en gaz échauffés par les étoiles environnantes. Dans notre galaxie, vous pouvez facilement observer la grande nébuleuse d'orion ou la nébuleuse de la lagune. Là, on voit leur équivalent à 2-3 millions d'années lumières. Ces nébuleuses sont des régions d'intense formation stellaire. Certaines des structures observables dans M33 ont été répertoriées dans les catalogue NGC et IC notamment, en particulier NGC 588, NGC 592, NGC 595 et NGC 604. Vous pourrez facilement les repérer en vous servant de l'astrométrie faite sur cette photo : nova.astrometry.net/annotated_full/9241132
J'ai également fait une version annotée dans laquelle j'ai repéré par des mires vertes les galaxies que j'ai repérées sur la photo. J'ai aussi fait quelques zooms sur des nébuleuses de M33 que je trouvais particulièrement jolies.
Les galaxies annotées sont :
- PGC 5648 : paire de galaxies ; magnitude 15.8 ; distance non connue ; taille apparente 0.61 min d'arc
- PGC 5575 : magnitude 15.22 ; distance 609 millions AL ; diamètre 126900 AL ; taille apparente 42.8 arcsec ; vitesse radiale d'éloignement 12944 km/s
- PGC 5899 : magnitude 14.91 ; distance estimée par redshift (0.03462) 476.7 millions d'AL / distance Hubble 490.77 millions AL ; diamètre 143200 AL ; taille apparente 59.8 arcsec ; vitesse radiale d'éloignement 10200 km/s
Je ne suis pas parvenu à trouver les références pour toutes les autres. NB: je suis à peu près certain que tous ces objets avec une mire sont des galaxies, d'une part à cause de leur forme la plupart du temps sans ambiguité, sinon parce que j'ai poussé les curseurs des courbes de luminosité pour les contraster du fond et faire ressortir leur nature, mais également parce qu'ils apparaissent de la même manière dans les images du Deep Sky Survey. Certains de ces objets ont des magnitudes comprises entre 17 et 18.
Sinon, pour les amateurs de BDs, Vinéa (fr.wikipedia.org/wiki/Vinéa), la planète aux trois soleils sur laquelle se rend plusieurs fois Yoko Tsuno dans ses aventures, est supposée se trouver dans la galaxie du triangle.
* Matériel :
Télescope Newton Skywatcher 150/750
Correcteur de coma
Monture Skywatcher AZ-EQ5
Capteur Canon 1200 D modifié (défiltré partiellement)
Filtre Optolong L-Enhance (sur 3 sessions).
Autoguidage Asi 120mm + Kepler 50/162 + Raspberry Pi3 + PhD Guiding
* Réglages :
800 iso ; poses de 90 s espacées de 5 sec.
DOFs systématiquement refaits (Darks et Flats ; Offsets conservés) et constitués de Darks>35, Offsets=30, Flats>45
* sessions et temps d'exposition :
22/08/23 : 116 brutes 90s (2h54) + DOFs - L-Enhance (H-Alpha + H-Beta + O III -> HOO)
06/09/23 : 164 brutes 90s (4h06) + DOFs - L-Enhance (H-Alpha + H-Beta + O III -> HOO)
08/09/23 : 197 brutes 90s (4h55) + DOFs - L-Enhance (H-Alpha + H-Beta + O III -> HOO)
09/09/23 : 189 brutes 90s (4h43) + DOFs - pas de filtre (spectre visible -> RVB)
Soit un cumul total de 16h39 (dont 11h55 en Ha+HB+OIII) ce qui constitue de loin mon record en temps d'exposition sur une même cible.
* Qualité du ciel : Excellente : la galaxie du triangle (M33, mag 6.27) était bien visible à l'œil nu 3 nuits sur 4. De même pour M4.
* Lune : entre 50% et 20% , seulement présente en fin de nuit.
* Traitement :
J'ai traité chaque session individuellement produisant une image Ha et une image OIII pour chaque session avec filtre, et une image RVB pour la dernière session.
Toute la phase du prétraitement jusqu'à post-traitement des sessions Ha, OIII et RVB séparées a été faite sous Siril. Le traitement complet est le suivant : 1) prétraitement des brutes par les DOFs, 2) retrait de la trame horizontale pour chaque image, 3) extraction du gradient linéaire pour chaque image, 4) extraction Ha / OIII pour les sessions avec filtre 5) alignement des images, 6) empilement, 7) retrait de la trame sur l'image empilée (il en reste un peu), 8) retrait du gradient (non linéaire), 9) déconvolution (PSF des étoiles), 10) étalonnage des couleurs (d'après catalogue pour l'image RVB) sinon manuel, 11) étirement hyperbolique généralisé, 12) histogramme, 13) suppression du bruit vert.
Les images Ha de chaque session ont été alignées puis cumulées (moyenne avec rejet) pour n'en former qu'une. De même pour les images OIII. De là, une image couleur composite HOO (RVB=Ha-OIII-OIII) a été générée.
L'image HOO et l'image RVB ont été ensuite alignées entre elles sous Siril. Pour chacune de ces images alignées, j'ai généré une starless et un starmask avec Starnet V2.
A partir de là, j'ai fait l'assemblage des quatres images alignées (2 starless et 2 starmasks) sous Gimp (en travaillant avec plusieurs calques duplicant ces images pour faire ressortir tantôt les couleurs, tantôt les contrastes).
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[English version]
The Triangulum galaxy (M33).
Two years ago, I had a small session on the M33 galaxy. I was only half satisfied because there were too few exposures (only 1 hour and 11 minutes). Here's what I wrote back then: 'I struggled a bit that evening because I was testing my mobile setup (far from home), getting back into astrophotography sessions with the telescope (had to reacquaint myself since spring), dealing with high humidity, and my autoguiding wasn't working because I had misconfigured my Wi-Fi... So, the photo isn't great because I had to discard half of the exposures due to dew, and also because I still hadn't put on my coma corrector. It feels like a rematch now!' Well, here it is! I finally got my rematch. I had to wait quite a while, never finding the right time or weather conditions for M33.
Cataloged by Charles Messier in 1764, it must have been observed before. Under an extremely clear sky, it's actually possible to distinguish its milky patch with the naked eye. I experienced this on 06/09/23 (second session). With good binoculars, if you know where to look, its detection is a bit easier (it remains quite dark).
Its distance is estimated to be between 2.38 and 3.07 million light-years (it's not precisely known), and it's about 50,000 to 60,000 light-years in diameter. The mass of this galaxy is about 60 billion solar masses, but only 17% of its mass comes from ordinary matter; 83% of its mass comes from that component of the universe that we can't yet detect but whose presence we measure, and we call it dark matter (to signify that we can't see it). The nearly 12 hours of exposure in HOO (Hydrogen Alpha in red + Oxygen III in blue/green) strongly highlight the nebulae, those large red and blue patches that are dense clouds of gas heated by surrounding stars. In our galaxy, you can easily observe the Orion Nebula or the Lagoon Nebula. Here, we see their equivalent at 2-3 million light-years. These nebulae are regions of intense star formation. Some of the structures observable in M33 have been cataloged in the NGC and IC catalogs, notably NGC 588, NGC 592, NGC 595, and NGC 604. You can easily locate them using the astrometry done on this photo: nova.astrometry.net/annotated_full/9241132 .
I also created an annotated version in which I marked galaxies I identified in the photo with green crosshairs. I also zoomed in on some nebulae in M33 that I found particularly beautiful.
The annotated galaxies are:
- PGC 5648: Pair of galaxies; magnitude 15.8; distance unknown; apparent size 0.61 arcminutes.
- PGC 5575: Magnitude 15.22; distance 609 million light-years; diameter 126,900 light-years; apparent size 42.8 arcseconds; radial velocity of recession 12,944 km/s.
- PGC 5899: Magnitude 14.91; estimated distance through redshift (0.03462) 476.7 million light-years / Hubble distance 490.77 million light-years; diameter 143,200 light-years; apparent size 59.8 arcseconds; radial velocity of recession 10,200 km/s.
I couldn't find references for all the others. Note: I'm fairly certain that all these objects with crosshairs are galaxies, either because of their unambiguous shape or because I adjusted the brightness curves to make them stand out from the background and reveal their nature. Additionally, they appear in a similar manner in Deep Sky Survey images. Some of these objects have magnitudes ranging from 17 to 18.
Otherwise, for comic book fans, Vinéa (en.wikipedia.org/wiki/Vin%C3%A9a), the planet with three suns that Yoko Tsuno visits several times in her adventures, is supposed to be located in the Triangle Galaxy.
* Equipment:
Skywatcher Newton Telescope 150/750
Coma Corrector
Skywatcher AZ-EQ5 Mount
Modified Canon 1200D Sensor (partially defiltered)
Optolong L-Enhance Filter (across 3 sessions)
Autoguiding with Asi 120mm + Kepler 50/162 + Raspberry Pi3 + PhD Guiding
* Settings:
800 ISO; 90-second exposures spaced 5 seconds apart.
Dark, Offset, and Flat frames systematically taken (Darks > 35, Offsets = 30, Flats > 45).
* Sessions and Exposure Times:
08/22/23: 116 raw 90s exposures (2h54) + Dark, Offset, and Flat frames - L-Enhance (H-Alpha + H-Beta + O III -> HOO)
09/06/23: 164 raw 90s exposures (4h06) + Dark, Offset, and Flat frames - L-Enhance (H-Alpha + H-Beta + O III -> HOO)
09/08/23: 197 raw 90s exposures (4h55) + Dark, Offset, and Flat frames - L-Enhance (H-Alpha + H-Beta + O III -> HOO)
09/09/23: 189 raw 90s exposures (4h43) + Dark, Offset, and Flat frames - No filter (visible spectrum -> RGB)
For a total cumulative exposure time of 16h39 (including 11h55 in Ha+HB+OIII), which is by far my longest exposure on a single target.
* Sky Quality: Excellent - The Triangulum Galaxy (M33, mag 6.27) was clearly visible to the naked eye on 3 out of 4 nights. The same applies to M4.
* Moon: Between 50% and 20%, only present in the late night.
* Processing:
I processed each session individually, producing an Ha and an OIII image for each filtered session and an RGB image for the last session. The entire pre-processing to post-processing phase for separate Ha, OIII, and RGB sessions was done in Siril. The complete processing is as follows: 1) Pre-processing of raw frames using Darks, 2) Removal of horizontal banding for each image, 3) Linear gradient removal for each image, 4) Ha / OIII extraction for filtered sessions, 5) Image alignment, 6) Stacking, 7) Further removal of remaining banding in the stacked image, 8) Non-linear gradient removal, 9) Deconvolution (PSF of stars), 10) Color calibration (catalog-based for the RGB image, manual otherwise), 11) Generalized hyperbolic stretch, 12) Histogram, 13) Green noise removal.
The Ha images from each session were aligned and then averaged (mean with rejection) to form one image. Likewise for the OIII images. From there, an HOO color composite image (RGB=Ha-OIII-OIII) was generated.
The HOO image and the RGB image were then aligned with each other in Siril. For each of these aligned images, I created a starless and a starmask using Starnet V2.
From there, I assembled the four aligned images (2 starless and 2 starmasks) in Gimp (working with multiple layers duplicating these images to bring out colors and contrasts as needed).
A spiral galaxy formed into a ring alongside its interacting elliptical partner. The ring may go on to become something like the Cartwheel Galaxy or Hoag's Object, or perhaps the structure is more transient than that. The Universe uses its boundless tracts of spacetime to keep its secrets from us.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 4.01° clockwise from up.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 33.11° counter-clockwise from up.
Sometimes life is just unbearably sad... and I can't do much but look at galaxies.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 56.11° counter-clockwise from up.
A color view from the Legacy Survey viewer is here: legacysurvey.org/viewer?ra=172.7533&dec=20.4686&z...
There's PANSTARRS data, too ps1images.stsci.edu/cgi-bin/ps1cutouts?pos=Apg+197&fi...
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 9.18° counter-clockwise from up.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 13.12° clockwise from up.
This is some wonderful narrowband imagery of NGC 4449 captured by Hubble back in 2005. When I first found this, I thought for sure it had already been processed somewhere along the line but all I could find was a wideband mosaic, which is here if you want to check it out. Rob Gendler did his own take as well, more strongly emphasizing the narrowband but still utilizing the wideband. The wideband imagery is nice but wow, is there a lot of amazing emission structure revealed with the narrowband data isolated. There are simple, smallish spheres, larger complex clouds, and down the center, streaming outwards like a ruptured fissure, is some massive work being done by the prodigious number of young stars radiating fiercely along the seam.
Red here represents areas of H-alpha and [N II] while slightly bluer areas show where [O III] emissions are also present. Mediumband green data (F550M) was also available and I used this to bring the stars to slightly more natural, whiter colors. Rather than maximizing differentiation between emissions, this time I applied more "realistic" colors. There's so much overlapping that it hardly matters, anyhow.
Two HST Proposals are associated with these data:
NGC 4449: a Testbed for Starbursts in the Low- and High-Redshift Universe
Calibrating Star Formation: The Link between Feedback and Galaxy Evolution
Red: HST_10522_01_ACS_WFC_F660N_sci + HST_10585_03_ACS_WFC_F658N_sci
Green: HST_10585_03_ACS_WFC_F658N_sci + HST_10522_01_ACS_WFC_F550M_sci
Blue: HST_10522_01_ACS_WFC_F502N_sci1
North is NOT up. It is 47.5° counter-clockwise from up.
One of a pair of galaxies. This one appears more disk-like (but still irregular), and is much smoother. Also apparent are many patches of star formation and associated clouds of gas, but the star formation seems less intense for this one. Its partner in the sky is here: flic.kr/p/2gtGepb
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 10.87° clockwise from up.
The 2011 Mobius Wearable Art Runway Show
Friday, May 6 · 7:00pm - 9:00pm - Boston
Created By - Mobius, Inc., Alison Safford, James Ellis Coleman
Program Order and Erratae Mobius Wearable Art 1) Inflatable Metamophosis artist: Charlie Roberts model: Liz Roncka MC talk-introduce the show 2) Liv Chaffee Students -The John Marshall School in Dorchester, MA Deandre Dewhollis, Kyshuari Santana-Everet Jose Pene Rayuana Martin-Milton Xavier Barrietos 3) Marie Ghitman – Two Group Skirts Models: Luke Burrows, Neige Christensen, Sage Dowser, Lisa Hiserodt, Sam Lanier, Jean Martin, Madelyn Medeiros, Jane Messere, Jason Picard, Q, Madelaine Ripley, and Artist 4) Jennifer Hicks - steam punk 5) Amy Keefer (SF) you all know me 6) Katie Pray-zip tease CSW 7) Becky Savitt 8) Ellla Williams- broken Record 9) Ella williams-garbage bag dress 10) Emily D’Angelo – 100% Recyclable 11) Grace Lynn Wilson – Fairy 12) Kaela Cote-Stemmermann - Pagan Sunset 13) Kaela Cote-Stemmermann - Stamp coat, model: Caroline Hickey 14) Mikaela Dalton – Mikaela Dalton – The Devil’s Tune 15) Mikaela Dalton – Untitled (cassette top), Model: Sarah Smith 16) Mikaela Joyce – Bell Jar Dress, Model: Sarah Hertel-Fernandez 17) Mikaela Joyce – Safety Pin Top 18) SeungHye Kim –The Pad Dress 19) Sonya Thorne – Apocalyptic Pieces 1-3, Model: self, Lilia Gaufberg, Zoe Cohen 20) Tess McCabe – Redshift, Model: Molly Harrison 21) William Everston (Representing Seeking Kali) -Sari Scroll for Two, Model: Artist, Karen Everston 22a) Ashley Conchieri – hand Woven and Hand Sewn, Model: Rebecca Chabot 22b) Ashley Conchieri – hand Woven and Hand Sewn, Model: 22c) Ashley Conchieri – hand Woven and Hand Sewn, Model: Monika Plioplyte 23) Julia Dusman – “Tarantula” Necklace 24) Ellen Shea - Little Red Re-Design, Model: Rebecca Woodbury 25) LeeLoo – Fallen post-apocalyptic cyber angel 26) L. Mylott Manning – Insides Out 28) Alyssa Fishenden - Plastic bag and stretch nylon halter dress 29) Robyn Giragosian and Caleb Cole – Pom Prom 30) Rachel Jayson – Dress of sheet music 31) Bethany Haeseler – Fruitloops 32) June Monteiro – “SMARTIE Dress”, Model: Chantal Lima Marquis 33) Jennifer Sherr Designs – Collage and hand painted leather vest, Model: Jess Barnett 34) Stacy A. Scibelli –Sabotage, Models: Meg Kuker, Toni Scibelli 35a) Selina Narov – Silk painted art couture clothing - Model: A. Dorian Rose 35b) Selina Narov – Silk painted art couture clothing - Model: Liz Roncka 35c) Selina Narov – Silk painted art couture clothing - Model: Jennifer Hicks 37) Albert Negredo – RECORDS (word game text) Red dress/Silver bag fabricated by Jane Wang - Model: sara june 38) Stacy A. Scibelli – plated skirt with leather head-piece (Models: tbd) 39) Stephanie Skier – Ephemeral dynamic fiberoptic fiber arts 40) the Bureau of cyberSurreal investigation international webCam Bra for Living I/O Model: Carol Susi 41) Elly Jessop – Glow Dress 42) Raphaela Riepl –Tentacles Flying Teeth, Models: Kira Lorenza Althaler as William Haugh, Florian Maria Sumerauer as Aaron Diskin Finale- 43) Word Game Design Competition Winner: June Monteiro - Model: northern sire
ONLINE BLOG for 2011 Mobius Wearable Art Runway Show: mobius-wearableart2011.blogspot.com/
@ Mobius
725 Harrison Avenue, Suite One
Boston MA 02118
Related Exhibition: A Tool Is A Mirror
A neat, compact group of galaxies. The big one at the center steals the show with its large amount of dust and star formation. Somewhat unfortunately, the little one on the right didn't quite fit onto the detector. Not much can be done about it without more Hubble time.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 51.96° clockwise from up.
the Multimedia Artist Danny "MushroomBrain" Hennesy
these are some of my eyes, I often use them when I make visional artistery but not always and not all at the same time!
Peace and Noise!
/ MushroomBrain the seer :::)
One of the more normal spiral galaxies that made it into the catalog. Looks like some past interaction just finishing up. This one happens to be overlapping a background galaxy, which might possibly (conjecture on my part) have been mistaken for part of the foreground galaxy at the time it was cataloged.
Taking a look at the catalog itself, this is noted as "RING w. I/A COMP'NS" (ring with interacting companions) and this would appear to be two mistakes: that this is a ring galaxy, and that the background galaxy is a nearby companion. I will note, however, it does look a bit like a ring in the imagery they saw (edit: actually this seems to be imagery from NED, not necessarily the original plate), and that would logically put the backgrounder as a companion based on other assumptions about ring galaxies. Uh, astronomy is based on a lot of assumptions, sometimes.
Found a color image in the DES DR1 data.
legacysurvey.org/viewer?ra=80.6775&dec=-39.0634&z...
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 55.93° counter-clockwise from up.
NGC 4535 (UGC 7727), Virgo, The Lost Galaxy of Copeland
NGC 4535 is a large galaxy in the constellation of Virgo, first documented by W. Herschel in 1785. It is classified as SAB(s)c, indicating intermediate morphology between barred and unbarred spirals, no ring, and loosely wound spiral arms. L.S. Copeland named it "The Lost Galaxy" due to its hazy, pale appearance under visual observation trough a smaller telescope. Approximately the size of the Milky Way, it is one of the larger members of the Virgo Galaxy Cluster, and appears to be moving with a "peculiar velocity" through space away from us as it orbits the cluster's center of gravity. This is suggested by the fact that its redshift is significantly higher than predicted from its redshift-independent distance measurements. Since redshift based distance estimates do not correct for peculiar motion through space, redshift-independent methods, such as the Cepheid period-luminosity relation, are regarded as more accurate for nearby galaxies closer than ~140 Mly (z < 0.01).
Based on the minor / major axis ratio of the galaxy's outline, NGC4535 is inclined to our line of sight by approximately 30*. This offers an unobstructed view of the spiral arms, dust lanes around the bulge, a short bar crossing the core, and a small, intensely bright active galactic nucleus of the Hii LINER type powered by a central supermassive black hole. The bright blue floccules within the spiral arms are "OB associations", or immense clusters of new, hot, blue giant stars. A number of curved, elongated structures in the disk strongly resemble "stellar streams", or gravitationally stretched remnants of merged dwarf galaxies. Many major galaxies in the Virgo Cluster show evidence of rapid mass assembly through the process of dwarf galaxy accretion. On the annotated image, two faint, diffuse objects which I suspect to be dwarf candidates are marked as DC.
NGC4535 has been the subject of extensive optical and radio telescope studies on the evolution of massive stars, the distribution of atomic and ionized hydrogen gas, and the interactions between the galaxy and the intergalactic medium within the Virgo Cluster.
SDSS J123421.43+081425.8, along the N perimeter of NGC4535, is identified as a small galaxy with a redshift of 0.00615, corresponding to a redshift based distance of 85.11 Mly. If this galaxy were subject to a similar peculiar velocity as NGC4535, it would actually be half the derived size, lying in the foreground. Unfortunately, redshift-independent distance measurements have not been done for this object.
Derived properties of identified faint objects are listed in the chart on the annotated image. The most remote are five quasars, three of which lie beyond the cosmic event horizon, as their recession velocities in the present cosmological epoch are superluminal. Two of them, marked with (+) appear significantly brighter than their listed apparent magnitudes. Many quasars are variable up to several magnitudes with periods ranging from days to years, depending on the inflow of matter available for accretion. The most intrinsically luminous object is LBQS 1232+0815, which is nearly 5,500 times brighter than the Milky Way. The most distant quasar is SDSS J123352.16+080527.4 (z = 2.76700), lying at the light travel distance (lookback time) of 11.33 Bly.
Image details:
-Remote Takahashi TOA 150 x 1105 mm, Paramount GT GEM
-OSC 27 x 300 sec, 2x drizzle, 50% linear crop
-Software: DSS, XnView, Starnet++ 2, StarTools 1.3 and 1.7, Cosmological Calculator 3
An irregular dwarf galaxy for today. It's kind of faint, and a bit difficult to brighten sufficiently above the noise floor, but now that I've done it I see a bit of star formation going on. I don't know why I just don't expect to see star formation in these galaxies, but it's almost always happening.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 12.44° counter-clockwise from up.
Possibly the most jumbled galaxy I've ever seen.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 31.21° clockwise from up.
Not sure there is any interaction going on, here. Looks a bit like a smooth elliptical or lenticular galaxy viewed face-on in front of a barred spiral galaxy. That doesn't mean they can't be in some early stage of interaction. I just don't see any signs of tidal tails or obvious irregularity, especially from the bottom galaxy. Whatever the case, it creates a beautiful scene.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 13.79° counter-clockwise from up.
A large tail extending from two otherwise unperturbed-looking spirals. To the left of this group is a third member apparently involved in the interaction as indicated by the much less obvious stream extending in that direction.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 68.30° clockwise from up.
A fortuitous observation of two smooth colliding galaxies which happen to host a type Ia supernova that erupted at least 5 days prior. SN 2019fkq can be seen as a bright pinpoint nestled between the cores of the two bright galaxies. Also visible in the left galaxy is a disk of dust encircling the nucleus, and numerous globular clusters are scattered about.
With the supernova measured at a redshift of .045, that puts these two galaxies at about 612 million light years away, and around 230000 light years across at the widest point. Two Milky Ways could fit across them.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 29.71° counter-clockwise from up.
–––
Crosspost by Koinup - original here
location: Redshift
"My warning meant nothing.
You're dancing in quicksand.
Why don't you watch where you're wandering?
Why don't you watch where you're stumbling?
You're wading knee deep and going in.
And you may never come back again.
This bog is thick and easy to get lost in.
cause you're a stupid, belligerent f***er.
This bog is thick and easy to get lost in.
cause you're a dumb and belligerent f***er.
I hope it sucks you down. down...down...down...
[...]" - "Swamp song", Tool
Release Date: March 10, 2010 - Distant galaxy clusters mysteriously stream at a million miles per hour along a path roughly centered on the southern constellations Centaurus and Hydra. A new study led by Alexander Kashlinsky at NASA's Goddard Space Flight Center in Greenbelt, Md., tracks this collective motion -- dubbed the "dark flow" -- to twice the distance originally reported, out to more than 2.5 billion light-years.
This all-sky view of the entire near-infrared sky reveals the distribution of galaxies beyond the Milky Way and has been desaturated to serve as the background for the dark flow plots. The image is derived from the 2MASS Extended Source Catalog, which contains more than 1.5 million galaxies, and the Point Source Catalog, which holds nearly 500 million stars within the Milky Way. The galaxies are color coded for distances obtained by various surveys. The nearest sources are blue (redshifts less than 0.01), moderately distant sources (redshifts between 0.01 and 0.04) are green, and red represents the farthest sources that 2MASS resolves (between redshifts of 0.04 and 0.1)
Credit: NASA/Goddard Space Flight Center/Scientific Visualization Studio/Dr. T.H. Jarrett/IPAC/Caltech
To learn more go to:
www.nasa.gov/centers/goddard/news/releases/2010/10-023.html
To see other visualizations of Dark Flow go to:
One of a pair of galaxies which are possibly interacting with one another. This is the more disrupted one. Many young stars and clouds of glowing gas are visible. The finger-like protrusions give this one an interesting shape. Kind of reminds me of a catcher's mitt. Its partner in the sky is here: flic.kr/p/2gtFUcc
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 0.84° counter-clockwise from up. (It my as well be up!)
An interesting field highlighting three interacting galaxies in the constellation of Pavo 190 million light years away. The tight group of three galaxies below centre frame comprises NGC 6769 (at the 6 o'clock position in the group), NGC 6770 (at the 3 o'clock position) and NGC 6771 (at the 11 o'clock position). The other two bright galaxies are IC 4842 (top of frame) and IC 4845 (at right of frame). There are also many other faint galaxies in the field worth a closer look.
Courtesy www.eso.org: It is obvious that stars and gas have been stripped off NGC 6769 and NGC 6770 are starting to form a common envelope around them, in the shape of a Devil's Mask. There is also a tenuous bridge of stars between NGC 6769 and NGC 6771. All of these features testify to strong gravitational interaction between the three galaxies. The warped appearance of the dust lane in NGC 6771 might also be interpreted as more evidence of interactions. Moreover, NGC 6769 and NGC 6770 are receding from us at a similar velocity of about 3800 km/s - a redshift just over 0.01 - while that of NGC 6771 is slightly larger, 4200 km/s.
SBIG STXL 11002M,Officina Stellare Pro RC 360
This is an 11.5 hour (L+Ls)RGB exposure ((330+90), 90, 90, 90 minutes) using 15 minute subs binned 1x1.
FOV 32.8 x 25.2 arc minutes @ 0.59 arc second/pixel.
Seeing for synthetic Luminance (Ls) and Luminance was average to poor - 2.1 to 2.7 arcsec FWHM.
only 26 shot combo, btw these stars r different in colors denoting redshift and blueshift of doppler effect
Stephan's Quintet in the constellation Pegasus is a visual grouping of five galaxies of which four form the first compact galaxy group ever discovered. The brightest member of the visual grouping is NGC7320. These galaxies are of interest because of their violent collisions. Four of the five galaxies in Stephan's Quintet form a physical association -,Hickson Compact Group 92.
NGC 7320 (to the lower left of the group) indicates a small redshift (790 km/s) while the other four exhibit large redshifts (near 6600 km/s). Since galactic redshift is proportional to distance, NGC 7320 is only a foreground projection and is ~39 million ly from Earth versus the 210-340 million ly of the other five. (Text source Wikipedia)
Planewave 17” Corrected Dall-Kirkham Astrograph f/4.5, FLI-PL6303E CCD – Remotely imaged T21 Mayhill New Mexico
35 mins Luminance, 5mins R, G & B
The incredibly distant galaxy GS-z13-1, observed just 330 million years after the Big Bang, was initially discovered with deep imaging from the NASA/ESA/CSA James Webb Space Telescope. Now, an international team of astronomers has definitively identified powerful hydrogen emission from this galaxy at an unexpectedly early period in the Universe’s history, a probable sign that we are seeing some of the first hot stars from the dawn of the Universe.
This image shows the galaxy GS-z13-1 (the red dot at centre), imaged with Webb’s Near-Infrared Camera (NIRCam) as part of the JWST Advanced Deep Extragalactic Survey (JADES) programme. These data from NIRCam allowed researchers to identify GS-z13-1 as an incredibly distant galaxy, and to put an estimate on its redshift value. Webb’s unique infrared sensitivity is necessary to observe galaxies at this extreme distance, whose light has been redshifted into infrared wavelengths during its long journey across the cosmos.
To confirm the galaxy’s redshift, the team turned to Webb’s Near-Infrared Spectrograph (NIRSpec) instrument. With new observations permitting advanced spectroscopy of the galaxy’s emitted light, the team not only confirmed GS-z13-1’s redshift of 13.0, they also revealed the strong presence of a type of ultraviolet radiation called Lyman-α emission. This is a telltale sign of the presence of newly forming stars, or a possible active galactic nucleus in the galaxy, but at a much earlier time than astronomers had thought possible. The result holds great implications for our understanding of the Universe.
[Image description: A small, zoomed-in area of deep space. Numerous galaxies in various shapes are visible, most of them small, but two are quite large and glow brightly. In the very centre is a small red dot, an extremely faraway galaxy. Two lines of light enter the left side: these are diffraction spikes, visual artefacts, caused by a nearby bright star just out of view.]
Credits: ESA/Webb, NASA, STScI, CSA, JADES Collaboration, Brant Robertson (UC Santa Cruz), Ben Johnson (CfA), Sandro Tacchella (Cambridge), Phill Cargile (CfA), J. Witstok, P. Jakobsen, A. Pagan (STScI), M. Zamani (ESA/Webb; CC BY 4.0
Well, it's been a while since I did a Prop15446 galaxy. This one was PI Julianne Dalcanton's favorite, so of course I had to. Featured are two interacting galaxies, one clearly full of star formation and dust with the other one smooth and not apparently doing much beyond participating in the interaction. The clumpy, dusty star-forming galaxy, perhaps once a spiral, now visibly being pulled into the smooth galaxy.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 8.21° clockwise from up.
A good deal of star formation going on during this conglomerative process of galactic reorganization. Lots of brightly glowing hydrogen cloud structures are visible despite the wideband filter.
Data from the following proposal is used to create this image:
Establishing HST's Low Redshift Archive of Interacting Systems
All channels: ACS/WFC F606W
North is 26.1° clockwise from up.
Two irregularly shaped galaxies, both swirling about one another in an ongoing interaction. Pockets of star formation dot both, stippling the cosmic canvas with clusters of young stars.
Establishing HST's Low Redshift Archive of Interacting Systems
All Channels: ACS/WFC F606W
North is 25.79° clockwise from up.
NASA/ESA Hubble Release Date: March 25, 2010
This image shows a smoothed reconstruction of the total (mostly dark) matter distribution in the COSMOS field, created from data taken by the NASA/ESA Hubble Space Telescope and ground-based telescopes. It was inferred from the weak gravitational lensing distortions that are imprinted onto the shapes of background galaxies. The colour coding indicates the distance of the foreground mass concentrations as gathered from the weak lensing effect. Structures shown in white, cyan, and green are typically closer to us than those indicated in orange and red. To improve the resolution of the map, data from galaxies both with and without redshift information were used.
The new study presents the most comprehensive analysis of data from the COSMOS survey. The researchers have, for the first time ever, used Hubble and the natural "weak lenses" in space to characterise the accelerated expansion of the Universe.
Credit: NASA, ESA, P. Simon (University of Bonn) and T. Schrabback (Leiden Observatory)
To learn more abou this image go to:
www.spacetelescope.org/news/html/heic1005.html
For more information about Goddard Space Flight Center go here:
Stephan's Quintet, (HCG 92, Arp 319), NGC 7320 Galaxy Group, Pegasus
This tight visual grouping of five galaxies was discovered in 1877 by Edouard Stephan at the Marseilles Observatory with the revolutionary 80 cm Foucault reflector, which was among the first to use a mirror of silvered glass, instead of speculum metal. The Quintet is the first compact group of galaxies ever documented. It has been carefully studied by numerous observatories ever since because it shows three galaxies in the process of merging, NGC7318-A, NGC7318-B, and NGC7319. All three appear to be barred spiral galaxies, severely distorted by tidal interactions. All display elongated and disrupted spiral arms, faint tidal tails of stars and gas drawn out from the galaxies into intergalactic space, and numerous bright blue regions of countless new stars ignited by gravitational perturbations of hydrogen clouds. Hubble's multi-band images in visible and infrared light reveal stellar populations of several age groups, indicating that starburst activity occurred in different epochs over hundreds of millions of years. In the long run, after billions of years, the three galaxies are destined to merge into a single giant elliptical galaxy. Based on their redshifts, and assuming Hubble Flow, the three galaxies lie at light travel distances between 267 and 312 million light years. However, they are probably much closer together. Due to strong gravitational interaction, they must have high peculiar velocities through space, which renders their distance estimates based on Hubble Flow unreliable.
www.cloudynights.com/articles/cat/articles/basic-extragal...
The fourth galaxy in the group is a modest elliptical galaxy, NGC 7317, gravitationally bound to its companions, but so far morphologically unaffected. These four galaxies are also gravitationally bound to the distant members of the Deer Lick Group, from which they are separated by only 35 arcmin.
www.cloudynights.com/topic/802766-ngc-7331-deer-lick-gala...
The most prominent galaxy in Stephan's Quintet is NGC 7320, a bright dwarf unbarred spiral which is actually 8 times closer than the other members of the visual grouping, and is gravitationally unbound to them. Based on its measurable properties (redshift, apparent magnitude, and angular size), it lies at a light travel distance of 36.4 Mly, receding at 706 km/s due to Hubble Flow (the expansion of space). Its diameter is only about 25,000 ly, five times smaller than the Milky Way's, and absolute magnitude some twenty times fainter. Blue color indicates a high star formation rate and a profusion of large, young, and very hot stars.
The most distant galaxy in the field is 2MFGC 17021, a large edge-on spiral, approximately the same size as the Milky Way, but about twice as bright. It is 784 Mly distant, receding at 17,113 km/s.
Image Details:
-Remote Takahashi TOA 150 x 1105 mm
-Paramount GT GEM
-25 x 300 sec subs, OSC, 2x drizzle, 50% linear crop
-Software: DSS, XnView, StarTools v 1.3 and 1.7, Cosmological Calculator v 2
On August 17, 2025, on the 16th anniversary of the start of my study of astronomy by self-education, I made calculations of the sky coordinates and requested shooting on remote telescopes (with parameters according to my calculations, for example, shutter speeds and number of images) to search for new astronomical objects. When I received and viewed one of the series of images, I found a star in them, which, upon checking in various information sources, turned out to be an already known supernova, but even such a find is unusual for me, because in several years of searching in images, I did not come across even a single known supernova.
When checking 5 photographs (of the sky region in the constellation Pisces) with exposures of 300 seconds taken on this date with another remote telescope, the 0.51-m f/6.8 reflector T59 of iTelescope.Net, which is located at the Siding Spring Observatory in Australia, at the very edge of the images (only 12 arcseconds from the edges of the frames!) I saw a relatively faint star (only about +20 mag), which was absent from the archival photographs: only the galaxy SDSS J004819.14+075856.8 was visible in them nearby. I assumed it was a supernova in this galaxy, and when I checked, this star was unknown, so I measured its position and brightness, then sent the information to the Transient Name Server (as of January 1, 2016 the Transient Name Server (TNS) is the official IAU mechanism for reporting new astronomical transients such as supernova candidates) with the status as a possible supernova, and it was published there: www.wis-tns.org/object/2025umq with temporary designation AT 2025umq, and as PSN J00481888+0759006 on the CBAT TOCP www.cbat.eps.harvard.edu/unconf/followups/J00481888+07590...
On August 19 I made remote observations of this star with a two-metre-aperture robotic Liverpool Telescope (LT — on the Canary island of La Palma) to confirm the reality of the object, and it worked out, I also made new measurements of its position and brightness (to refine them): about +20.3 mag. On August 23 and 24 I additionally made photometric observations with the LT to get more such information about this star. I am attaching a photo (color) for August 24 (stacked 3x60 sec. with g’, r’ and i’ filters, 9 frames in total).
On August 20, according to my calculations and request, the spectrum of this star was obtained at the Liverpool Telescope, as a result of its analysis, this star was classified as a fading Type Ia supernova at redshift of 0.159 in the galaxy SDSS J004819.14+075856.8, with assignment it the designation SN 2025umq. On August 27, the corresponding ATel #17361 www.astronomerstelegram.org/?read=17361 was published on the website «The Astronomer's Telegram» about the discovery, photometry and classification of this supernova with my name as the first author.
I will add that later I saw in one of the scientific sources on the Internet that this supernova was previously detected by ZTF sky survey (the light curve shows a maximum brightness of about +20 mag around August 10, and the first detection was on July 25), but for some reason information about it was not sent to the TNS, so I am its official discoverer.
It is important that this is the first supernova discovered by me personally (in the images obtained - at my request - from a remote telescope), because earlier I discovered two supernovae SN 2022bsi and SN 2022jhn only in the images of the CRTS sky survey, participating in the supernova search project, so I am the first co-author of those discoveries. In addition, I consider it's luck that supernova SN 2025umq was not outside the boundaries of the images, because it was very close near the edges of the frames. Also note that those two supernovae were much closer (at redshifts of 0.0369 and 0.013) to our galaxy, while this supernova is distant enough: it has a redshift of 0.159, which means it is more than 2 billion light years away, so it was a big luck that I, an amateur astronomer, was able to discover so low brightness supernova! I should add that usually such faint supernovae are rarely classified using the Liverpool Telescope (because too long exposures are needed to obtain a good signal-to-noise ratio, so it is more practical to use larger telescopes, but I did not have the opportunity to use a larger telescope to study this supernova, so I tried to do it at the Liverpool Telescope), but in this case it was possible to do so with the LT - due to the sufficient distance of this supernova from the center of the host galaxy.
Now I am the discoverer (only on the basis of self-education) of 82 variable stars, 10 planetary nebula candidates (and co-author of discovery of 5), 3 supernovae (two co-authored and one personally), 4 probably physical binaries pairs of stars, 3 novae in M31; 3 transients (possible supernovae) and 8 asteroids; author of scientific papers in astronomy, which were published in scientific journals (including peer-reviewed) and co-author of the papers, for example, the most recent «GOTO065054+593624: An 8.5 mag amplitude dwarf nova identified in real time via Kilonova Seekers» was published doi.org/10.1051/0004-6361/202553823 in Astronomy & Astrophysics (A&A). I have given online presentations during several international conferences in astronomy, for example, e-Poster during the XXXIst General Assembly of the International Astronomical Union (IAUGA 2022), my paper "The contribution of the modern amateur astronomer to the science of astronomy" (based on this my e-Poster) was published arxiv.org/abs/2212.12543 in arXiv.
Arp 130 consists of MCG+03-01-016 (PGC 178, VV 263b and others) the spiral that looks like it is interacting with IC 5378 (PGC 177, UGC 1, VV 263/a), the elliptical below it. Redshift data suggests that these galaxies are at least 20 million light-years away from each other so they just look close from our vantage point. Arp has this one in his “E and E-like galaxies – close to and perturbing spirals.” These are located in Pegasus approximately three degrees from Algenib.
The other odd irregular galaxy on the right side is IC 5377 (PGC 156, UGC 12918 and others).
Luminance – 24x600s – 240 minutes – binned 1x1
RGB – 10x300s – 50 minutes each – binned 2x2
390 minutes total exposure – 6 hours 30 minutes
Imaged August 26th and 31st and September 1st, 2019 from Dark Sky New Mexico at Rancho Hidalgo (Animas, New Mexico) with a SBIG STF-8300M on an Astro-Tech AT12RCT at f/8 2432mm.