🧵(1/2) LDN 1369 is a dark nebula located at the center of the Heart Nebula (IC 1805), also known as the "Wizard's Spire, in the constellation Cassiopeia
Taken on 26-09-24 from my backyard
🔭 William Optics Pleiades 111
📷 QHY Mini8
Exposure: 4:15 hours
#Astrophotography #Space #DeepSpace #Astronomy
![The Bubble Nebula, also known as NGC 7635, Sharpless 162, or Caldwell 11, is an H II region[1] emission nebula in the constellation Cassiopeia. It lies close to the open cluster Messier 52. The "bubble" is created by the stellar wind from a massive hot, 8.7[1] magnitude young central star, SAO 20575 (BD+60°2522).[7] The nebula is near a giant molecular cloud which contains the expansion of the bubble nebula while itself being excited by the hot central star, causing it to glow.[7] It was discovered in November 1787 by William Herschel.[5] The star BD+60°2522 is thought to have a mass of about 44 M☉.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreibfxoemd3ngle6rgov6dmm2fh46xxc6znoxdajhnpixtgb7kbnhp4)
![The Elephant's Trunk Nebula (IC 1396A) is a concentration of interstellar gas and dust within the much larger ionized gas region IC 1396 located in the constellation Cepheus about 2,400 light years away from Earth.[1] The nebula is a dark, dense globule that gets its name from its appearance at visible light wavelengths, where there is a dark patch with a bright, sinuous rim. The bright rim is the surface of the dense cloud that is being illuminated and ionized by a very bright, massive multiple star (HD 206267) that is just to the east of the Elephant's Trunk Nebula . The entire IC 1396 region is ionized by the massive star, except for dense globules that can protect themselves from the star's harsh ultraviolet rays.[citation needed]
Widefield view of the full IC 1396 nebula
The Elephant's Trunk Nebula is now thought to be a site of star formation, containing several very young (less than 100,000 yr) stars that were discovered in infrared images in 2003. Two older (but still young, a couple of million years, by the standards of stars, which live for billions of years) stars are present in a small, circular cavity in the head of the globule. Winds from these young stars may have emptied the cavity.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreib7ao6eamm54pa2lbymlgk4zk6rnjcdbskxbgn2m2ry5tjvwst4vq)
![Sh 2-129 (also known as the Flying Bat Nebula), is a large emission nebula and H II region located in the constellation Cepheus. It is part of the Cepheus molecular cloud complex and belongs to the Cep OB2 association.[1][2][3][4] Reflection nebula vdB 140 can be seen near Sh 2-129.[5][6]
Within Sh 2-129 lies a bipolar outflow nebula named Ou 4 (also known as Squid Nebula).[7] The central star of Ou4 is believed to be the massive triple star system named HD 202214](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreiaiihkuddsmcck6sv2kwusehghuwp52iz7lnezsi4grhwyykuvjry)
![NGC 281, IC 11 or Sh2-184 is a bright emission nebula and part of an H II region in the northern constellation of Cassiopeia and is part of the Milky Way's Perseus Spiral Arm. This 20×30 arcmin sized nebulosity is also associated with open cluster IC 1590, several Bok globules and the multiple star, B 1. It collectively forms Sh2-184,[4] spanning over a larger area of 40 arcmin.[5] A recent distance from radio parallaxes of water masers at 22 GHz made during 2014 is estimated it lies 2.82±0.20 kpc (9200 ly) from us.[6] Colloquially, NGC 281 is also known as the Pacman Nebula for its resemblance to the video game character.[3]
Edward Emerson Barnard discovered the nebula in August 1883, describing it as "a large faint nebula, very diffuse". Multiple star 'B 1' or β 1 was later discovered by S. W. Burnham, whose bright component is identified as the highly luminous O6 spectral class star, HD 5005 or HIP 4121. It consists of an 8th-magnitude primary with four companions at distances between 1.4 and 15.7 arcsec. There has been no appreciable change in this quintuple system since the first measures were made in 1875.
The nebula region is visible in amateur telescopes from dark sky locations. In his book Deep Sky Wonders, Walter Scott Houston describes the appearance of the nebula in small telescopes:[](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreie4f7dhzgbkshv4bjfzkie64xvtjaxsh4otwjk3x7xbeu6adbhnlu)
![NGC 7380 is a young open cluster of stars in the northern circumpolar constellation of Cepheus, discovered by Caroline Herschel in 1787. The surrounding emission nebulosity is known colloquially as the Wizard Nebula, which spans an angle of 25′. German-born astronomer William Herschel included his sister's discovery in his catalog, and labelled it H VIII.77. The nebula is known as S 142 in the 1959 Sharpless catalog (Sh2-142). It is extremely difficult to observe visually, usually requiring very dark skies and an O-III filter. The NGC 7380 complex is located at a distance of approximately 8.5 kilolight-years from the Sun, in the Perseus Arm of the Milky Way.
The cluster spans ~20 light-years (6 pc) with an elongated shape and an extended tail.[2] Age estimates range from 4[2] to 11.9[1] million years. At the center of the cluster lies DH Cephei, a close, double-lined spectroscopic binary system consisting of two massive O-type stars. This pair are the primary ionizing source for the surrounding H II region, and are driving out the surrounding gas and dust while triggering star formation in the neighboring region.[4] Of the variable stars that have been identified in the cluster, 14 have been identified as pre-main sequence stars while 17 are main sequence stars that are primarily B-type variables.[4]](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreibrgdfuy3ndlszbhi6n7pdemztutpvhr6jnsm6ix5k35fz6ebvg7i)
![Image of The Elephant's Trunk Nebula (IC 1396A) is a concentration of interstellar gas and dust within the much larger ionized gas region IC 1396 located in the constellation Cepheus about 2,400 light years away from Earth.[1] The nebula is a dark, dense globule that gets its name from its appearance at visible light wavelengths, where there is a dark patch with a bright, sinuous rim. The bright rim is the surface of the dense cloud that is being illuminated and ionized by a very bright, massive multiple star (HD 206267) that is just to the east of the Elephant's Trunk Nebula . The entire IC 1396 region is ionized by the massive star, except for dense globules that can protect themselves from the star's harsh ultraviolet rays.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreib2v3lsl3qzp523swiqicj65moeonwvtdk333pspqsftenhspvgsu)
![The Pinwheel Galaxy (also known as Messier 101, M101 or NGC 5457) is a face-on, counterclockwise intermediate spiral galaxy located 21 million light-years (6.4 megaparsecs)[5] from Earth in the constellation Ursa Major. It was discovered by Pierre Méchain in 1781[a] and was communicated that year to Charles Messier, who verified its position for inclusion in the Messier Catalogue as one of its final entries.
On February 28, 2006, NASA and the European Space Agency released a very detailed image of the Pinwheel Galaxy, which was the largest and most detailed image of a galaxy by Hubble Space Telescope at the time.[10] The image was composed of 51 individual exposures, plus some extra ground-based photos.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreibi3nlwmkw562uerqau4ba4wgzjckixvuilf7uoltxyjmhqjhblwi)
![The Whirlpool Galaxy, also known as Messier 51a (M51a) or NGC 5194, is an interacting grand-design spiral galaxy with a Seyfert 2 active galactic nucleus. It lies in the constellation Canes Venatici, and was the first galaxy to be classified as a spiral galaxy.[9] It is 31 million light-years (9.5 megaparsecs/Mpc) away and 23.58 kiloparsecs (76,900 ly) in diameter.
The galaxy and its companion, NGC 5195, are easily observed by amateur astronomers, and the two galaxies may be seen with binoculars. The Whirlpool Galaxy has been extensively observed by professional astronomers, who study it and its pair with dwarf galaxy NGC 5195 to understand galaxy structure (particularly structure associated with the spiral arms) and galaxy interactions. Its pair with NGC 5195 is among the most famous and relatively close interacting systems, and thus is a favorite subject of galaxy interaction models.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreigqfvr4mrpjkie3jipjd7hvgvgfdk5ozl77b3tcox4kyvm64rh7hi)
![The Rosette Nebula (also known as Caldwell 49) is an H II region located near one end of a giant molecular cloud in the Monoceros region of the Milky Way Galaxy. The open cluster NGC 2244 (Caldwell 50) is closely associated with the nebulosity, the stars of the cluster having been formed from the nebula's matter.The cluster and nebula lie at a distance of 5,000 light-years from Earth[7] and measure roughly 130 light years in diameter. The radiation from the young stars excites the atoms in the nebula, causing them to emit radiation themselves producing the emission nebula we see. The mass of the nebula is estimated to be around 10,000 solar masses.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreid3y7vnznj6oi2g7llz2k3nawnlmlbm7ovmdr2vtlgz5atv3s7tai)
![Bottom object in the image:
IC 405 (also known as the Flaming Star Nebula, SH 2-229, or Caldwell 31) is an emission and reflection nebula[1] in the constellation Auriga north of the celestial equator, surrounding the bluish, irregular variable star AE Aurigae. It shines at magnitude +6.0. Its celestial coordinates are RA 05h 16.2m dec +34° 28′.[2] It is located near the emission nebula IC 410, the open clusters M38 and M36, and the K-class star Iota Aurigae.
The nebula measures approximately 37.0' x 19.0', and lies about 1,500 light-years away from Earth.[2] It is believed that the proper motion of the central star can be traced back to the Orion's Belt area.[2] The nebula is about 5 light-years across.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreifpwrj3kms5qgutkgzxfszok2mumelgmxgr4ajnem6rc5524kvele)
![C/2025 A6 (Lemmon) is a non-periodic comet discovered by the Mount Lemmon Survey in images obtained on 3 January 2025. It has an inbound orbital period of about 1,350 years and will pass perihelion on 8 November 2025 when it will be 0.53 AU (79 million km; 49 million mi) from the Sun. This perihelion passage will reduce the orbital period to about 1,150 years. It makes its closest approach to Earth on 21 October 2025 and may be visible to the naked eye 42 degrees from the Sun after sunset. As of 24 October 2025, the comet is about apparent magnitude 4.2,[3] and the nucleus and coma are visible in binoculars about 12 degrees above Arcturus and near the magnitude 2.5 star Izar. (The handle of the Big Dipper points towards Arcturus.) Both Arcturus and the comet may be visible in the same field of view using low power binoculars such as 7x35s.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreigq6orjub7reelwqiugmdq2kbkoeny3pnqzhwh4jhrqm6kjnoegyu)
![C/2025 A6 (Lemmon) is a non-periodic comet discovered by the Mount Lemmon Survey in images obtained on 3 January 2025. It has an inbound orbital period of about 1,350 years and will pass perihelion on 8 November 2025 when it will be 0.53 AU (79 million km; 49 million mi) from the Sun. This perihelion passage will reduce the orbital period to about 1,150 years. It makes its closest approach to Earth on 21 October 2025 and may be visible to the naked eye 42 degrees from the Sun after sunset. As of 12 October 2025, the comet is about apparent magnitude 5.6,[6] and is visible in binoculars about 15 degrees (approximately one and a half fists) below the cup of the Big Dipper. It is currently about 2 degrees southwest of the star Psi Ursae Majoris.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreidp6cmbwr464kygmuzq2f72k6azorsjbssfjpfa5mldh22byia5su)
![IC 1396 is a large emission nebulae, a region of ionized gas, located in the constellation Cepheus about 2,400 light years away from Earth.[1]
IC 1396 is illuminated and ionized by a very bright, massive multiple star HD 206267 at its center, except for dense globules that can protect themselves from the star's harsh ultraviolet rays. This hierarchical triple star system has two members that form a spectroscopic binary that orbit each other with a period of 3.7 days, while a third member lies further away—it is unclear whether this third member is gravitationally bound to the pair. The system is emitting a stellar wind that reaches an exceptional velocity of 3,225 km/s, among the highest measured for stars of this type.[2]
Jutting from the rim of the nebula is IC 1396A, commonly called the Elephant's Trunk Nebula, a dark, dense globule with a bright, sinuous rim being illuminated by HD 206267.[3]](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreigbv6j4j3ns5ibvn4xsbzkau5lsaoe63wmy4jqgkwmplduvir6s2y)
![Westerhout 5 (Sharpless 2-199, LBN 667, Soul Nebula) is an emission nebula located in Cassiopeia. Several small open clusters are embedded in the nebula: CR 34, 632, and 634[citation needed] (in the head) and IC 1848 (in the body). The object is more commonly called by the cluster designation IC 1848.
Small emission nebula IC 1871 is present just left of the top of the head, and small emission nebulae 670 and 669 are just below the lower back area.
The galaxies Maffei 1 and Maffei 2 are both nearby the nebula, although light extinction from the Milky Way makes them very hard to see. Once thought to be part of the Local Group, they are now known to belong to their own group- the IC 342/Maffei Group.
This complex is the eastern neighbour of IC1805 (Heart Nebula) and the two are often mentioned together as the "Heart and Soul".](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreiecflvg52e6rorjtjcfrp66jd2oafhpl77n3ab7oux75ppsjsuyki)
![NGC 7380 is a young open cluster of stars in the northern circumpolar constellation of Cepheus, discovered by Caroline Herschel in 1787. The surrounding emission nebulosity is known colloquially as the Wizard Nebula, which spans an angle of 25′. German-born astronomer William Herschel included his sister's discovery in his catalog, and labelled it H VIII.77. The nebula is known as S 142 in the 1959 Sharpless catalog (Sh2-142).It is extremely difficult to observe visually, usually requiring very dark skies and an O-III filter. The NGC 7380 complex is located at a distance of approximately 8.5 kilolight-years from the Sun, in the Perseus Arm of the Milky Way.
The cluster spans ~20 light-years (6 pc) with an elongated shape and an extended tail.[2] Age estimates range from 4[2] to 11.9 million years. At the center of the cluster lies DH Cephei, a close, double-lined spectroscopic binary system consisting of two massive O-type stars. This pair are the primary ionizing source for the surrounding H II region, and are driving out the surrounding gas and dust while triggering star formation in the neighboring region. Of the variable stars that have been identified in the cluster, 14 have been identified as pre-main sequence stars while 17 are main sequence stars that are primarily B-type variables.
Shot taken on 2025-08-01 from my backyard
🔭: William Optics Pleiades 111
📷: ZWO ASI 2600
Total exposure: 26 x 300 sec (2h10)
#Astrophotography #Space #DeepSpace #Astronomy](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreice3vhh5xxnvtzjdpycyr22wpfsbi542sqqtmgyouxhtmjylfqwhu)
![The Iris Nebula (also known as NGC 7023 and Caldwell 4) is a bright reflection nebula in the constellation Cepheus. The designation NGC 7023 refers to the open cluster within the larger reflection nebula designated LBN 487.
The nebula, which shines at magnitude +6.8, is illuminated by a magnitude +7.4 star designated HD 200775.[1] It is located near the Mira-type variable star T Cephei, and near the bright magnitude +3.23 variable star Beta Cephei (Alfirk). It lies 1,300 light-years away and is six light-years across.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreievpmay3ykkqeiyjbwiaw7d75tinwpqueoeqlnpo3ofhuduligghq)
![Sharpless 101 (Sh 2-101) is a H II region[1] emission nebula located in the constellation Cygnus. It is sometimes also called the Tulip Nebula because it appears to resemble the outline of a tulip when imaged photographically. It was catalogued by astronomer Stewart Sharpless in his 1959 catalog of nebulae. It lies at a distance of about 6,000 light-years (5.7×1016 km; 3.5×1016 mi) from Earth.
Sh 2-101, at least in the field seen from Earth, is in close proximity to microquasar Cygnus X-1, site of one of the first suspected black holes. Cygnus X-1 is located about 15′ west of Sh 2-101. The companion star of Cygnus X-1 is a spectral class O9.7 Iab supergiant with a mass of 21 solar masses and 20 times the radius of the Sun. The period of the binary system is 5.8 days and the pair is separated by 0.2 astronomical units. The black hole has a mass of 15 solar masses and a Schwarzschild radius of 45 km.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:dksfsl7lygnhrmfxsxcznf3u/bafkreifdielc2mm25gh5yktm4wh6riabzxul7ddqb5ojo3iduh3ehvy4ou)
