Astronomy/DSOs

The Astronomy DSO list specifies which Deep Space Objects may be covered in the Astronomy event that year, and is roughly analogous to the Deep Sky Objects typically found in the rules for the Division B event Reach for the Stars. It is typically listed in section 3.c of the rules.

General Tips

The DSO list can seem daunting at first. A good strategy for DSOs is to take your own notes on them from various sources, and include images as well:

• Categorize the DSOs by its type or its stage in Stellar Evolution (e.g. Brown Dwarfs, Red Giants, White Dwarfs, Cepheid Variables, Supernova remnants, Globular Clusters), and take notes on each category about its stage in stellar evolution and significance in the study of Astronomy: For example, a Type Ia Supernova can either be the result of collision of two white dwarfs or accretion of matter from a stellar companion (often reaching the Red Giant stage), and its mostly uniform brightness can help Astronomers determine distance to distant galaxies using the distance modulus.
• For each Deep Space Object, take notes on what makes them unique and significant. The Chandra X-ray Observatory posts videos at the start of the competition season that briefly explain each object's significance, and the Chandra photo album and NASA's APOD are also good resources. For Variable stars, AAVSO is a helpful resource.
• Find photos (and light curves for variable stars) of the Deep Space Objects, as many as possible and across all wavelengths. Almost all tests include tasks to identify DSOs based on images or find all images of a certain DSO/category, and more difficult tests sometimes include more obscure images of the DSOs. Include the wavelength of light a certain image was taken in.
• Take notes on Miscellaneous information about each deep-star object, including, but not limited to: constellation, alternate names, magnitude, stellar classification, right ascension/declination, and color index.
• Take practice tests. They help reveal weaknesses in your notes on Deep Space Objects.
• If you are given certain information about a DSO such as the masses and the separation of the binary system, calculate the period. Use information you already have to calculate other values before the test, saving you valuable time.

2018 DSOs

2018 DSOs

Name	Images		Constellation	Magnitude		Distance	Coordinates		External Links
				Apparent	Absolute		Right Ascension	Declination
AG Carinae			Carina	6.96	~-8 (visible band)	6000 parsecs	10h 56m 11.58s	-60° 27’ 12.8056"	SIMBAD AAVSO
			One of the brightest stars in the Milky Way, surrounded by a nebula. Apparent brightness can vary drastically between 5.7 and 8.3. This star is considered in transition from a blue supergiant to a WR-star.
Alpha Orionis			Orion	0.2-1.2	Absolute	~643 ly	05h 55m 10.3053s	+07° 24' 25.426"	AAVSO, Wikipedia
			More commonly known as Betelgeuse, this semi-regular (SRc) pulsating red supergiant will likely explode as a type II supernova within the next million years.
ASASSN-15lh			Indus	16.9	-23.5 (ultraviolet band)	1,171 megaparsecs	22h 2m 15.45s	-61° 39’ 34.64”	External Links
			Supernova detected by the All Sky Automated Survey. It is either the most luminous type I supernova ever discovered, called a hypernova, or a tidal disruption event.
Circinus X-1	Image 1	Image 2	N/A	Apparent	Absolute	Distance	Right Ascension	Declination	External Links
			Neutron star orbiting a conventional super-massive star.
DEM L241	Image 1	Image 2	Constellation	Apparent	Absolute	Distance	Right Ascension	Declination	[1]
			Description of the DSO, important characteristics, etc.
Geminga			Gemini	Apparent	Absolute	815 ly	06h 33m 54.15s	+17° 46′ 12.9″	[2]
			Geminga is likely a decaying core of a Type II Supernova. It is highly visible in the gamma-ray spectrum.
HR 5171 A	Image 1	Image 2	Constellation	Apparent	Absolute	Distance	Right Ascension	Declination	External Links
			Description of the DSO, important characteristics, etc.
IC 443	Image 1	Image 2	Gemini, near Eta Geminorum	Apparent	Absolute	5000 ly, 1.5 kpc	06h 17m 13s	+22° 31′ 05′′	External Links
			IC 443 is a remnant of a supernova that likely occurred 3000-30,000 years ago. It is one of the best-studied cases of a supernova remnant interacting with the surrounding molecular clouds.
M82 X-2	Image 1	Image 2	Ursa Major	Apparent	Absolute	12 million ly, 3.5 million pc	09h 55m 51.0s	69° 40′ 45″	External Links
			M-82 X-2, an X-ray pulsar in the Messier 82 galaxy, is noted for being an ultra luminous X-ray source (ULX), shining around 100x brighter than predicted. It is part of a binary system, where it revolves around the larger star about once every 2.5 days. It rotates about once every 1.37 seconds. It was uncovered by NuSTAR and verified by the Chandra and Swift spacecraft.
NGC 6357	Image 1	Image 2	Constellation	Apparent	Absolute	Distance	Right Ascension	Declination	External Links
			Description of the DSO, important characteristics, etc.
NGC 7822	Image 1	Image 2	Cepheus	Apparent	Absolute	2900 ly, 900 pc	00h 01m 08.58s	+67° 25′ 17.0″	External Links
			NGC 7822 is a star forming region that is believed to be relatively young. It contains the star BD+66 1673, one of the hottest stars discovered within 1 kpn of the Sun, and is noted for its elephant trunk-shaped pillars of creation. Description of the DSO, important characteristics, etc.
PSR B0355+54	Image 1	Image 2	Constellation	Apparent	Absolute	Distance	Right Ascension	Declination	[3]
			Description of the DSO, important characteristics, etc.
RCW 103	Image 1	Image 2	Constellation	Apparent	Absolute	Distance	Right Ascension	Declination	External Links
			Description of the DSO, important characteristics, etc.
S Doradus			Dorado	8.6-11.5	-10.0	169000 ly, 51.8 kpc	05h 18m 14.3550s	−69° 15′ 01.151″	External Links
			First observed in 1897, S Dor is a Luminous Blue Variable (LBV) located in the Large Magellanic Cloud (LMC). It is also the brightest member of NGC 1910, an open cluster. An entire class of variable stars are named after this DSO, which have the unusual characteristic of short-term microvariations superimposed over long-term macrovariations.
SN 1987A	Image 1	Image 2	Dorado	Peaks around +2.9	Absolute	168,000 ly, 51.4 kpc	05h 35m 28.03s	−69° 16′ 11.79″	External Links
			The closest observed supernova since SN 1604, its light reached the Earth 23 February 1987. It was the first opportunity for astronomers to study the development of a supernova and learn more about core-collapse supernovae. Additionally, it detected gamma-ray radiation that proved that the post-explosion glow is radioactive. This was also the first supernova where astronomers were able to directly observe emitted neutrinos.
SN W49B	Image 1	Image 2	Aquila	Apparent	Absolute	33,000 ly, 10 kpc	19h 11m 09s	+09° 06′ 24″	Chandra Chandra (picture)
			One of the most luminous SNRs in the galaxy at gamma-ray wavelengths, SN W49B also shows Cr and Mn x-ray emissions and has asymmetrically distributed Fe and Ni. It is thought to have left a black hole at the center - possibly the most recent black hole formed in the Milky Way.

Previous Years' DSO Lists

2017 DSOs 2017 DSOs Name Images Constellation Magnitude Distance Coordinates External Links Apparent Absolute Right Ascension Declination Henize 2-428 Aquilla 19h 13m 05.239s +15° 46′ 39.80″ Space.com Heaviest known WD binary system ;Will eventually merge in 700 million years; Originally binary star system of two sun-like stars of equivalent mass; Total mass 1.8 M_sun; Nebula is asymmetric because of binary system at center instead of single star; The planetary nebula came from the outer later of the original star, from contraction/expansion during the Red Giant stages; Period is 4 hours; Emit gravitational waves resulting in loss of energy; Will eventually cause Type 1a supernova when they merge, absolute magnitude =/= -19.3 because of increased mass: will not be useful as standard candle. Henize 3-1357 (Stingray Nebula) Ara 10.75 -3.0 18kly 17h 16m 21.071s −59° 29′ 23.64″ APOD NASA Gallery Youngest known planetary nebula; Radius 0.02 pc (as large as 130 solar systems), separated by 0.3arcsec; Age 2650 yr, gases light up for no more than 40 yr; Core mass 0.59 M_sun; ionized mass (nebula mass) 0.2Msol; Star at the center was originally a asymptotic giant branch B1 supergiant, still evolving to WD; White dwarf has strong hydrogen rich Balmer lines; Luminosity 3000 L_sun. HM Cancri (RX J0806.3+1527) Cancer 21.1 ~1600 ly 08h 06m 23.20s +15° 27' 30.20" Chandra Space.com Period 321.5 seconds: shortest period known; proper motion 1.1mas/yr; separation 0.0005 A; 400,000 km/sec, approaching at 2.0ft/day and orbit decaying at 1.2 ms/yr; total mass of 1.18 M_sun assuming separation of 1.02 x 10 -6 arcseconds; Double WD system, releases gravitational wave; X-Ray binary; X-Rays originate from accretion flow crashing into magnetic poles of white dwarf. J075141/J174140 (two objects) Monceros/Draco 07h 51m 41.20s/17h 41m 40.50s -01° 41' 20.90"/+65° 26' 38.70" Chandra Binary system; white dwarf with a companion star; theoretically give off gravitational waves; Potentially may not create Type 1a Supernova, maybe a Type 1ax or .Ia Supernova, where detonation only on surface of star. M15 175px Pegasus 6.2 -9.2 ~33,600 ly 21h 29m 58.33s +12° 10′ 01.2″ Messier Catalogue UAlabama APOD M15 is one of the oldest known and closest globular clusters to Earth. It is potentially one of the densest clusters known, containing over 100,000 stars with 112 variables, 8 pulsars, and 1 double neutron star system which gives off X-rays. It contains a planetary nebula called Pease 1, which shows that stellar evolution still takes place in globular clusters. NGC 1846 Dorado 160,000ly 05h 07m 33s -67° 27' 41" NASA NGC 1846 is a globular cluster with an unusual HR diagram: there are two turn-off points. Stars in a globular clusters form at the same time, meaning that the after the turnoff point there should be few stars. There are two different populations of stars in the clusters, with calculated age difference of around 300 million years, which is suspected to be caused by a merge of 2 globular clusters. Additionally, there is a potential planetary nebula within the cluster. NGC 2392 (Eskimo Nebula) Gemini 10.1 0.4 ~3000 ly 07h 29m 10.7669s +20° 54′ 42.488″ APOD NGC 2392 is a double shell planetary nebula often called the Eskimo nebula. The rings of the nebula are formed by the collision of fast and slow moving gases. The nebula is about 10,000 years old, and will last about another 50,000 years before it cannot be seen. The high X-ray emission could be potentially due to an unseen companion star. Notable features include strong OIII lines and weak Hα lines. NGC 2440 Puppis 9.4 07h 41m 54.91s −18° 12′ 29.7″ NASA APOD Chandra NGC 2440 is a planetary nebula containing the hottest known white dwarf, HD62166. The white dwarf itself has a temperature of 200,000K, and is surrounded by cooling gas. Most light is emitted in UV, ionizing the surrounding material. Its multipolar structure could potentially be caused by the shedding of mass in different locations or precession. Omicron Ceti (Mira) Cetus 3.04 -5.04 to -5.16 ~420 ly 02h 19m 20.79210s –02° 58′ 39.4956″ Chandra NASA Science News Mira is the prototype for Mira variables, which are red giants that oscillate over long periods. It is a binary star system, with Mira A the red giant on the asymptotic giant branch that is losing mass and Mira B the white dwarf that is accreting mass. Historically, it was the first non-supernova variable star discovered. Mira A(?) is not spherical, rather it is egg shaped due to the non-radial nature of its pulsations. Additionally, it exhibits a bow shock, which was only recently discovered due to the need for high tech observatories in UV. Mira has been observed in almost all frequencies, each having seemingly different shapes and giving specific information about the star. Sirius A & B Canis Major -1.46 1.42 8.6ly 06h 45m 09s −16° 42′ Chandra APOD Sirius A and B are collectively the brightest star in the sky. Sirius A is a type A1 star, and Sirius B is a white dwarf. Sirius B was originally a bright blue star, which then shed its outer layers and became a white dwarf with broad hydrogen absorption lines. Their separation is 20 AU. Sirius A emits more radiation in the visible spectrum, while Sirius B emits more radiation in the X-ray spectrum. SN2011fe Ursa Major +9.9 -19 21 Mly 14h 03m 05.8s +54° 16′ 25″ NASA AAVSO SN 2011fe is the youngest Type 1a Supernova discovered. Discovered by the Palomar Transient Factory in 2011, it was used to test predictions and models of Type 1a supernovae. The progenitor was a carbon-oxygen white dwarf with a star no larger than the Sun. As with many type 1a supernovae, a large amount of energy was emitted through the decay of Ni-56. The location of the supernova was in the Pinwheel galaxy (M101). SNR 0509-67.5 Dorado ~52,000 pc/160 kly 05.01h 09.01m 31.01s −67.01° 31.01′ 18.2″ Chandra APOD SNR 0509-67.5 is a Type 1a supernova remnant found in the Large Magellanic Cloud. It was mostly likely a double degenerate system given the lack of companions in the vicinity. There is little doubt as to where it was a Type 1a supernovae, due to the silicon found after the explosion. It was observed through a light echo where light reflects off interstellar dust, delaying its arrival by 400 years. The outer ring is gas that has been shocked and heated by the supernova., expanding at 11,000 mph. G1.9+0.3 Sagittarius ~7665 pcs 17h 48m 45.4s -27° 10' 06" Chandra SNR G1.9+0.3 was most likely a double degenerate progenitor supernova. It is only 110 years old, the youngest Type Ia Supernova in the Milky Way. While the light would have reached the Earth in the 19th century, interstellar dust obscured it. However, the X-rays and radio waves were able to penetrate the gas. The remnant has a very asymmetric pattern, and exhibits synchrotron radiation (charged particles traveling in a curved path). SS Cygni Cygnus 7.7-12.4 2.42-7.12 114 pcs 21h 42m 42.804s 43° 35' 09.88" AAVSO Chandra A recurrent nova with a very massive white dwarf and a red dwarf-type star cooler than our sun. Often classified as U Geminorum type dwarf nova. SS Cygni is commonly thought of as the prototype dwarf nova. There are three parts to the system, the two stars and the accretion disk. The accretion disk pulsates in brightness, causing its variability. The period of the system is 6.5 hours, with outbursts every 7-8 weeks. Tycho's SNR Cassiopeia ~9000 ly 00h 25m 17s 64° 08' 37" Chandra NASA APOD A Type 1a supernova remnant that was observed in 1572 and later studied by Tycho Brahe. It remains one of the few supernovae visible to the naked eye. It was detected again using radio waves in 1952, and found that a G0-G2 star was the companion to the white dwarf progenitor. The companion star was most likely around 1.4 solar masses.

2016 DSOs 2016 DSOs Name Images Constellation Magnitude Distance Coordinates External Links 2MASSJ22282889-431026 Apparent: Absolute: Right Ascension: ; Declination: ″ 51 Pegasi b Pegasus Apparent: Absolute: 50.9 ly Right Ascension: 22h 57m 28.0s; Declination: +20° 46' 08″ 55 Cancri Cancer Apparent: Absolute: 40.3 ly Right Ascension: 08h 52m 35.81s; Declination: +28° 19' 51.0″ AB Aurigae Auriga Apparent: Absolute: ~470 ly Right Ascension: 04h 55m 45.8445s; Declination: +30° 33′ 04.292″ Barnard 68 Ophiuchus Apparent: Absolute: 500 ly Right Ascension: 17h 22m 38.2s; Declination: -23° 49′ 34″ GD 165 Bootes Apparent: Absolute: ~103 ly Right Ascension: 14h 24m 39.144s; Declination: +09° 17′ 13.98″ HAT-P-11b Cygnus Apparent: Absolute: 122 ly Right Ascension: 19h 50m 50.25s; Declination: +48° 04′ 51.1″ HD 95086 Carina Apparent: Absolute: 296 ly Right Ascension: 10h 57m 03s; Declination: -68° 40′ 02″ HD 106906b Crux Apparent: Absolute: 300 ly Right Ascension: 12h 17m 53.0s; Declination: −54° 01′ 28″ HL Tauri Taurus Apparent: Absolute: 450 ly Right Ascension: 04h 31m 38.437s; Declination: +18° 13' 57.65″ HR 8799 Pegasus Apparent: Absolute: 129 ly Right Ascension: 23h 07m 28.7150s; Declination: +21° 08′ 03.302″ Kepler-186 Cygnus Apparent: Absolute: 492 ly Right Ascension: 19h 54m 36.651s; Declination: +43° 57′ 18.06″ M42 Orion Apparent: Absolute: 1344 ly Right Ascension: 05h 35m 17.3s; Declination: −05° 23′ 28″ T Tauri Taurus Apparent: Absolute: ~600 ly Right Ascension: 04h 21m 59.43445s; Declination: +19° 32′ 06.4182″ WASP-18b Phoenix Apparent: Absolute: 325 ly Right Ascension: 01h 37m 24.95s; Declination: –45° 40′ 40.8″ WASP-43b Sextans Apparent: Absolute: ~80 pc Right Ascension: 10h 19m 38s; Declination: −09° 48′ 23″ WISE 0855-0714 Hydra Apparent: Absolute: 7.53 ly Right Ascension: 08h 55m 10.83s; Declination: –07° 14′ 42.5″

2015 DSOs 2015 DSOs Name Images Constellation Magnitude Distance Coordinates External Links FU Orionis Orion Apparent: Absolute: ~1300 ly Right Ascension: 05h 45m 22.362s; Declination: +09° 04′ 12.31″ AAVSO TW Hya Hydra Apparent: Absolute: 176 ly Right Ascension: 11h 01m 52s; Declination: −34° 42′ 17″ 2M1207 Centaurus Apparent: Absolute: 172 ly Right Ascension: 12h 07m 33.47s; Declination: −39° 32′ 54.0″ CoRoT-2 Aquila Apparent: Absolute: 930 ly Right Ascension: 19h 27m 06.496s; Declination: +01° 23′ 01.38″ HD 209458b Pegasus Apparent: Absolute: 154 ly Right Ascension: 22h 03m 10.8s; Declination: +18° 53′ 04″ HD 189733b Vulpecula Apparent: Absolute: 63.4 ly Right Ascension: 20h 00m 43.71s; Declination: +22° 42′ 39.1″ Kepler-7b Lyra Apparent: Absolute: ~3400 ly Right Ascension: 19h 14m 19.6s; Declination: +41° 5′ 23.3″ GJ 1214b Ophiuchus Apparent: Absolute: 42 ly Right Ascension: 17h 15m 18.942s; Declination: +04° 57′ 49.69″ Beta Pictoris Pictor Apparent: Absolute: 63.4 ly Right Ascension: 05h 47m 17.1s; Declination: −51° 03′ 59″ Fomalhaut Piscis Austrinus Apparent: Absolute: 25.13 ly Right Ascension: 22h 57m 39.0465s; Declination: −29° 37′ 20.050″ HR 8799 Pegasus Apparent: Absolute: 129 ly Right Ascension: 23h 07m 28.7150s; Declination: +21° 08′ 03.302″ WISE 1049-5319 Vela Apparent: Absolute: 6.6 ly Right Ascension: 10h 49m 18.723s; Declination: −53° 19′ 09.86″ Gliese 229B Lepus Apparent: Absolute: 18.8 ly Right Ascension: 06h 10m 34.6154s; Declination: −21° 51′ 52.715″ LP 944-20 Fornax Apparent: Absolute: 20.9 ly Right Ascension: 03h 39m 35.220s; Declination: –35° 25′ 44.09″ N159 Dorado Apparent: Absolute: 170000 ly Right Ascension: 05h 40m 04.2s; Declination: –69° 44′ 43″ M20 175px Sagittarius Apparent: Absolute: 5200 ly Right Ascension: 18h 02m 23s; Declination: −23° 01′ 48″

2014 DSOs 2014 DSOs Name Images Constellation Magnitude Distance Coordinates External Links Mira (Omicron Ceti) Cetus Apparent: 2.0 to 10.1 Absolute: ~-2.5 to 4.7 ~420 ly Right Ascension: 02h 19m 20.70s; Declination: -02° 58' 39.51" Chandra NASA Science News Mira is the prototype for Mira variables, which are red giants that oscillate over long periods. It is a binary star system, with Mira A the red giant that is losing mass and Mira B the white dwarf that is accreting mass. W49B Aquila Apparent: ~26,000 light years Right Ascension: 19h 11m 07s Declination: +09° 06' 00" Chandra W49B is an SNR that is theorized to have a distorted shape and a black hole from the explosion that created the remnant. It may be the most recent black hole formed in the Milky Way. Tycho's SNR (SN 1572) Cassiopeia Peak Apparent: -4 ~9000 ly Right Ascension: 00h 25m 17s; Declination: +64° 08' 37" Chandra NASA APOD A Type 1a supernova remnant that burst in early November 1572 and was later studied by Tycho Brahe. Vela SNR Vela Apparent: 12 ~800 ly Right Ascension: 08h 35m 20.66s Declination: -45° 10' 35.2" APOD The closest known supernova remnant to us with a notable pulsar and neighboring nebulae. Contains NGC 2736 or the Pencil Nebula, which is thought to have formed from part of the shock wave of the Vela SNR G1.9+0.3 Sagittarius Apparent: ~28,000 ly Right Ascension: 17h 48m 45s Declination: -27° 10' 00" Chandra NASA Possibly the most recent supernovae, specifically Type Ia, in the Milky Way. It has an extremely asymmetric pattern. Explosion was likely highly non-uniform and unusually energetic. Eta Carinae Carina Apparent: -0.8 to 7.9 ~7,500 ly Right Ascension:10h 45m 03.591s Declination:−59° 41′ 04.26″ Chandra APOD A hypergiant with a smaller companion. Massive supernova, very bright. It has a chance of exploding at any time, and will be so bright that it rivals the moon. SS Cygni Cygnus Apparent: 7.7-12.4 370 ly Right Ascension: 21h 42m 42.804s Declination: 43° 35' 09.88" AAVSO Chandra A recurrent nova with a very massive white dwarf and a red dwarf-type star cooler than our sun. Often classified as U Geminorum type dwarf nova. T Tauri Taurus Apparent: 9.3-14 462 ly Right Ascension: 04h 21m 59.43s; Declination: +19° 32′ 06.42″ NASA APOD Universe Today T Tauri is the prototype for T Tauri stars, which are the stars in the life stage between protostar and main sequence. there is a nebula located close to the star called Hind's Variable Nebula, which changes in luminosity as T Tauri varies. GRS 1915+105 Aquila Apparent: 40,000 ly Right Ascension: 19h 15m 11.60s Declination: +10° 56' 44.00 Chandra GRS 1915+105 is an x-ray binary star system containing a regular star and a black hole. It is one of the heaviest stellar black holes so far known in the Milky Way and has a self-regulating black hole. 47 Tucanae Tucana Apparent: 4.91 16,700 ly Right Ascension: 00h 24m 05.67s Declination: –72° 04′ 52.6″ Chandra APOD APOD 47 Tucanae is the second brightest globular cluster after Omega Centauri and one of the most massive globular clusters in the galaxy. The Trapezium Orion Apparent: 4 1,600 ly Right Ascension: 05h 35.4m Declination: −05° 27′ Chandra APOD APOD The Trapezium is a relatively young open cluster in the heart o the Orion Nebula. T Pyxidis Pyxis Apparent: 6.4-15.5 15,600 ly Right Ascension: 09h 04m 41.50s Declination: −32° 22′ 47.5″ AAVSO NASA APOD T Pyxidis is a recurrent nova and nova remnant containing a sun-like star and a white dwarf. It is now close to the Chandrasekhar limit and might soon explode as a type 1a supernova. Abell 30 Cancer Apparent: 15.6 5,500 ly Right Ascension: 08h 46m 53.50s Declination: +17° 52' 45.40" Chandra Abell 30 is a planetary nebula in a special, rarely-seen phase of evolution. The evolution of A30 stalled and then started up again, so the planetary nebula was reborn. RX J0806.3+1527 (HM Cnc) Cancer Apparent: 21.1 ~1600 ly Right Ascension: 08h 06m 23.20s; Declination: +15° 27' 30.20" Chandra Space.com An x-ray binary system composed of two white dwarves that are rapidly orbiting each other. Their orbits are slowly getting closer, and the stars will eventually collide. Since they are faint, they are being observed by x-ray emissions. V1647 Ori Orion Apparent: 1,300 ly Right Ascension: 05h 46m 13.10s Declination: -00° 06' 05.00" Chandra NASA V1647 Ori is a FU Orionis variable star, a low-mass protostar still partly surrounded by its birth cloud. It is spinning as fast as it can without ripping itself to pieces. V1 Andromeda Apparent: 2.5 million ly Right Ascension: 00h 41m 27s Declination: 00h 41m 27s Hubblesite NASA A Cepheid variable star in the Andromeda galaxy that began Hubble's discovery of the expansion of the universe by showing that the Andromeda galaxy was not part of our galaxy. NGC 1846 175px Doradus Apparent: 11.3 ~160,000 ly Right Ascension: 05h 07m 35.25s Declination: -67° 27' 38.9" Hubblesite NASA NGC 1846 is a globular cluster located in the outer halo of the LMC. The most intriguing object is a faint green planetary nebula, and it doesn't seem to belong in the cluster. NGC 3132 Vela Apparent: 9.87 ~2,000 ly Right Ascension: 10h 07m 01.7640s Declination: −40° 26′ 11.060″ APOD APOD NGC 3132 is a planetary nebula. There are two stars in the nebula, one of which is a white dwarf.

2013 DSOs 2013 DSOs Name Images Constellation Magnitude Distance Coordinates External Links Cassiopeia A Cassiopeia Apparent: Peak=~6 ~11,000 ly Right Ascension: 23h 23m 26.7s ; Declination: +58° 49' 3.00" Chandra Cassiopeia A is the youngest supernova remnant in the Milky Way Galaxy. IGR J17091 Scorpius Apparent: ~28,000 ly Right Ascension: 17h 09m 7.92s; Declination: -36° 24' 25.20" Chandra IGR J17091 has the highest ever known wind speed at 20 million miles per hour, which is only 3% of the speed of light. NGC 6888/ WR 136 Cygnus Apparent: +7.4 ~5,000 ly Right Ascension: 20h 12m 35.00s; Declination: +38° 26' 30.00" Chandra NGC 6888, also known as the Crescent Nebula, was created the powerful winds coming off of the Star WR 136, or HD 192163. PSR J0108-1431 Cetus Apparent: peak: 27.8 ~770 ly Right Ascension: 01h 08m 08.30s; Declination: -14° 31' 48.50" Chandra, Neutron Star Physics Blog PSR J0108-1431 is, by far, the nearest pulsar, or neutron star, to Earth. Cygnus X-1 Cygnus Apparent: 8.95 Absolute: 6.5 ~6070 ly Right Ascension: 19h 58m 21.70s; Declination: +35° 12' 05.80" Chandra, NASA Stephen Hawking lost a bet that Cynus X-1 did not contain a black hole; This black hole is 15 times the mass of the sun. SXP 1062 Tucana Apparent: ~180,000 ly Right Ascension: 01h 29m 12.40s; Declination: -73° 32' 01.70" Chandra There is evidence that there is a pulsar within this supernova remnant. Messier Object M1 (Crab Nebula) Taurus Apparent: 8.4 ~6,500 ly Right Ascension: 05h 34m 32s; Declination: +22° 0.0' 52.00" Chandra, NASA First observed in A.D. 1054, the Crab Nebula produces the equivalent of 100,000 suns in Energy and has a pulsar located in its center as well. V838 Monocerotis Monoceros Apparent: 15.74 ~20,000 ly Right Ascension: 07h 04m 04.85s ; Declination: -03° 50' 50.1" NASA, NASA, Wikipedia This object became 600,000 times more luminous than our Sun, for an instant, the brightest star in this galaxy, in January of 2002. Delta Cep (Cephei) Cepheus Apparent: 3.5-4.4 887 ly Right Ascension: 22h 29m 10.26502s; Declination: +58° 24' 54.7139" AAVSO, Wikipedia Delta Cep is located in a binary system, and is one of the closest Cepheid variable stars, with only Polaris being closer. Alpha Orionis (Betelgeuse) Orion Apparent: 0.2-1.2 ~643 ly Right Ascension: 05h 55m 10.3053s; Declination: +07° 24' 25.426" AAVSO, Wikipedia It will explode as a type II supernova within the next million years. SN 2010JL Leo Apparent: ~160 million ly Right Ascension: 09h 42m 53.33s; Declination: +09° 29' 41.80" Chandra It is the first evidence in X-rays of a supernova shock wave breaking through a cocoon of gas around the star. This discovery may help explain why some supernova explosions are more powerful than others. NGC 3582 Carina Apparent: ~6000 ly Right Ascension: 11h 12m 12s; Declination: -61° 16′ 25" NASA APOD A complex nebula where bright stars and interesting molecules are forming. LHa115-N19 Tucana Apparent: ~196,000 ly Right Ascension: 0h 47m 31s; Declination: -73° 8.3' Chandra This area is filled with ionized hydrogen gas and it is where many massive stars are expelling dust and gas through stellar winds. Antares Scorpius Apparent: 0.96 ~550 ly Right Ascension: 16h 29m 24.45970s; Declination: -26° 25' 55.2094 Wikipedia A red supergiant star in the Milky Way galaxy and the sixteenth brightest star in the nighttime sky. Rho Ophiuchi Cloud complex Ophiuchus Apparent: ~460 ly Right Ascension: 16h 28m 06s; Declination: -24° 32.5′ Wikipedia, NASA APOD One of the closest star-forming regions. IC 1396 Cepheus Apparent: ~2,400 ly Right Ascension: 21h 38m 8.7s; Declination: +57° 26' 48" Wikipedia One of the largest emission nebulae in the night sky. It contains "the Elephant's Trunk", a dark, dense globule in the nebula.

2012 DSOs 2012 DSO's Name Images Constellation Magnitude Distance Coordinates External Links Mira (Omicron Ceti) Cetus Apparent: 2.0 to 10.1 ~420 ly Right Ascension: 02h 19m 20.70s; Declination: -02° 58' 39.51" Chandra NASA Science News Mira is the prototype for Mira variables, which are red giants that oscillate over long periods. SNR 0509-67.5 Dorado ~160,000 ly Right Ascension: 05h 09m 31.7s; Declination: -67° 31' 18.01” NASA APOD Chandra A supernova remnant in the LMC (Large Magellanic Cloud). The explosion occurred 400 years ago for Earth observers. CH Cyg Cygnus Apparent: 5.6 to 10.5 ~815 ly Right Ascension: 19h 24m 33.07s; Declination: +50° 14' 29.13" Chandra AAVSO CH Cyg is a symbiotic star system between a red giant and a white dwarf. Kepler's SNR (SN 1604) Ophiuchus ~13,000 ly Right Ascension: 17h 30m 40.80s; Declination: -21° 29' 11.00" Chandra NASA APOD A Type 1a supernova remnant that was observed by Johannes Kepler in 1604. Tycho's SNR (SN 1572) Cassiopeia ~9000 ly Right Ascension: 00h 25m 17s; Declination: +64° 08' 37" Chandra NASA APOD A Type 1a supernova remnant that was observed in 1572 and later studied by Tycho Brahe. Messier 15 (NGC 7078) Pegasus Apparent: 6.2 ~33,600 ly Right Ascension: 21h 29m 58.38s; Declination: +12° 10′ 00.6″ Messier Catalogue U of Alabama M15 is one of the oldest known and closest globular clusters to Earth. Carina Nebula Carina Apparent: 1.0 ~7500 ly Right Ascension: 10h 45m 04s; Declination: -59° 41' 03" Chandra Universe Today The Carina Nebula is a very bright and large nebula. It contains Eta Carinae, which is one of the largest known stars and a prime candidate for a hypernova. T Tauri Taurus Apparent: 9.3-14 462 ly Right Ascension: 04h 21m 59.43s; Declination: +19° 32′ 06.42″ NASA APOD Universe Today T Tauri is the prototype for T Tauri stars, which are the stars in the life stage between protostar and main sequence. there is a nebula located close to the star called Hind's Variable Nebula, which changes in luminosity as T Tauri varies. Sirius B Canis Major Apparent: 8.30; Absolute: 11.18 8.6 ly Right Ascension: 06h 45m 11s; Declination: -16° 42' 05.00" Chandra NASA APOD Sirius B is the smaller, white dwarf component to the Sirius star system. RR Lyrae Lyra Apparent: 7.1 to 8.2 ~850 ly Right Ascension: 19h 25m 27.91s; Declination: +42° 47′ 03.69″ AAVSO Encyclopedia of Science RR Lyrae is the prototype for RR Lyrae variables, which are low-mass stars that pulsate regularly. U Scorpii Scorpius Apparent: 8.7 to 19.3 >15000 ly Right Ascension: 16h 22m 30.78s; Declination: -17° 52′ 42.8″ Universe Today Sky and Telescope U Scorpii is a recurrent nova, and one of ten known recurrent novae in the Milky Way. Its most recent outburst was in January 2010, and it was the best-observed outburst in history. Rosette Nebula (Caldwell 49, 3C 163) Monoceros Apparent: 9.0 4700 ly Right Ascension: 06h 31m 52.00s; Declination: +04° 55' 57.00" Atlas of the Universe Chandra A large stellar nursery that produces several O and B type stars. It has an appearance similar to a rose, hence its name. BP Psc Pisces Apparent: 11.9 ~1000 ly Right Ascension: 22h 22m 24.70s; Declination: -02° 13' 41.40" Chandra NASA NGC 2440 PDF BP Psc appears to be a red giant, but it has an accretion disc similar to that of a protostar. This has led to hypotheses that BP Psc has recently consumed a companion star or a large, gaseous planet. NGC 2440 (VV 45) Puppis Apparent: 11.5 ~4000 ly Right Ascension: 07h 41m 54.91s; Declination: -18° 12′ 29.7″ NASA APOD Hubble NGC 2440 is a planetary nebula whose star of origin is now an extremely hot white dwarf. RX J0806.3+1527 (HM Cnc) Cancer Apparent: 21.1 ~1600 ly Right Ascension: 08h 06m 23.20s; Declination: +15° 27' 30.20" Chandra Space.com An x-ray binary system composed of two white dwarves that are rapidly orbiting each other. Their orbits are slowly getting closer, and the stars will eventually collide. Since they are faint, they are being observed by x-ray emissions. DEM L238 & L249 Dorado ~160,000 ly Right Ascension: 05h 34m 08.80s; Declination: -70º 34' 28.00" Chandra Space Daily Two remnants from neighboring stars that exploded as white dwarves in the LMC.

2011 DSOs 2011 DSO's Name Images Constellation Magnitude Distance Coordinates External Links Epsilon Aurigae Auriga Apparent: 2.9 normally, 3.8 during eclipse; Absolute: -6.0 ~2000 light years (ly) Right Ascension: 05h 01m 58.1s; Declination: +43° 49’ 24” AAVSO: Epsilon Aurigae Citizen Sky: Epsilon Aurigae Epsilon Aurigae is an eclipsing binary. One part is a white giant, and the other appears to be a star shrouded by a dark cloud of dust. In the middle of this cloud, there is a clearing where the star probably is, so during an eclipse, the system appears momentarily brighter as this clearing passes over the giant. An observation project of Epsilon Aurigae took place from 2009-2011. NGC 6240 (IC 4625, UGC 10592, PGC 59186, VV 617) Ophiuchus Apparent: 12.8 ~330 million ly Right Ascension: 16h 52m 58.9s; Declination: +02° 24' 03" Chandra: NGC 6240 NASA APOD: NGC 6240 NGC 6240 is an extremely luminous infrared galaxy (ULIRG). It is the result of two smaller galaxies colliding to form one large galaxy with two nuclei and an irregular shape. Possible hypotheses for the high infrared emission are intense star formation or the presence of one or two AGNs. 3C 321 Serpens ~1.4 billion ly Right Ascension: 15h 31m 42.7s; Declination:: +24° 04’ 25.00" Chandra: 3C 321 Space.com: 3C 321 3C 321 is a binary system of galaxies. One of the galaxies is directing a large jet of energy at its companion. It is nicknamed the “Death Star Galaxy” and it is theorized that the galaxy with the jet contains a supermassive black hole. It was discovered in 2007. Centaurus A (NGC 5128, Arp 153, PGC 46957, Caldwell 77, 4U 1322-42) Centaurus Apparent: 6.84 ~15 million ly Right Ascension: 13h 25m 27.6s; Declination: -43° 01’ 09” SEDS: Centaurus A Solstation.com: Centaurus A Cen A is one of the closest radio galaxies containing an AGN to Earth. It is the fifth brightest galaxy in the sky, although it is mostly only observable from the Southern Hemisphere. It is slowly consuming another spiral galaxy, causing rapid star formation, helping the radiation coming from the nucleus. The supermassive black hole at the center sends out jets of X-rays and radio waves in which the inner parts are moving at one half of the speed of light. Stephan's Quintet (HGC 92, Arp 319, VV 288) Pegasus Apparent: 13.9 300-370 million ly Right Ascension: 22h 35m 57.5s; Declination: +33° 57’ 36” Chandra: Stephan's Quintet NASA APOD: Stephen's Quintet Stephan's Quintet is a visual grouping of five galaxies. Four of the galaxies are in a compact group, and collisions have altered the form of the galaxies. Eventually, the four will likely merge into one large galaxy. The collisions have caused emissions of both x-rays and molecular hydrogen. The four than are physically interlocked are NGC 7317, NGC 7318a, NGC 7318b, and NGC 7319. NGC 7320 is not actually part of the interacting cluster but is a foreground object in the same area as the other galaxies. The galaxies NGC 7335, NGC 7336, and NGC 7337 in the NGC 7331 group, or Deer Lick Group, was used to determine this. Occasionally, the tidal forces cause NGC 7318b to emit huge shock waves of X-rays. It is also the brightest member of the group with an apparent magnitude of 13.9. NGC 7319 is classified as a Type 2 Seyfert galaxy. MACSJ0717.5+3745 Auriga Right Ascension: 07h 17m 31.00s; Declination: +37° 45’ 39.60” Chandra: MACSJ0717.5+3745 MACSJ0717.5+3745 (MACSJ0717 for short) a galaxy cluster where four separate galaxies have been involved in a collision. The collisions are caused by a stream of hot gas known as a filament that pours into the cluster. It is one of the most complex clusters ever studied and was discovered in 2003. Bullet Cluster (1E 0657-56) Carina Right Ascension: 06h 58m 37.9s; Declination: - 55° 57’ 0” Chandra: Bullet Cluster NASA APOD: Bullet Cluster The Bullet Cluster is a system of two colliding clusters of galaxies. It is one of the best examples of evidence for the existence of dark matter. In the collision, the stars mostly did not interact, but the gases and other matter were significantly altered. This other matter is hypothesized to be dark matter, and is supported by the supposed Modified Newtonian Dynamics that explains the lensing phenomenon in the cluster. It is one of the hottest known clusters of galaxies. Perseus A (NGC 1275, PGC 12429, UGC 2669, Caldwell 24, 3C 84, QSO B0316+413) Perseus Apparent: 12.6. Right Ascension: 03h 19m 48.1s; Declination: +41° 30’ 42” NASA APOD: Perseus A Hubble Heritage: Perseus A Perseus A is a Type 1.5 Seyfert galaxy, which signifies that both broad and narrow lines on the emission spectrum are present, but there are less pronounced broad lines than a Type 1 Seyfert galaxy. It consists of two galaxies, one in the center and another that lies in front of it. Long filaments of gas stretch out from the system. SN 2006gy Perseus Peak Apparent: 14.2 Right Ascension: 03h 17m 27.10s; Declination: +41° 24’ 19.50” Chandra: SN 2006gy NASA APOD: SN 2006gy SN 2006gy was an extremely energetic supernova that reached an extremely high luminosity level. The large size of the star caused it to gain energy in its core, eventually causing it to be blown apart violently. This type of supernova is sometimes referred to a hypernova, and it compared to the star Eta Carinae in the Milky Way. SN 1996cr Circinus Right Ascension: 14h 13m 10.05 s; Declination: -65° 20’ 44.8” Chandra: SN 1996cr SN 1996cr is a powerful supernova that was noticed in a Chandra image after it was taken, and was widely studied afterward. The star exploded between 1995 and 1996, but was not discovered until 2001. It is of interest because it is located in an active galaxy with a growing supermassive black hole and rapid star formation. NGC 4603 (PGC 42510) Centaurus Apparent: 12.3 Right Ascension: 12h 40m 55.2s; Declination: -40° 58’ 35” NASA APOD: NGC 4603 HyperPhysics: NGC 4603 NGC 4603 is a large spiral galaxy. It is the most distant galaxy in which Cepheids have been used to determine the distance to the galaxy. Using this distance and determining recession velocity, it has served as a benchmark for determining the Hubble constant (70 km/sec/Mpc ±10%). NGC 7771 (VV 2002) Pegasus Apparent: 12.9 Right Ascension: 23h 51m 25.0s; Declination: +20° 06’ 49” NASA APOD: NGC 7771 a large spiral galaxy in close proximity to two other galaxies. This trio of galaxies is named the NGC 7771 group after its largest member, a spiral, the three galaxies, NGC 7769-7771, have passed by each other closely and will eventually form one huge galaxy. It is considered an accurate representation of the formation of the Milky Way. Dusty nebulae in front of the group obstruct clear viewing. NGC 2623 (Arp 243) Cancer Apparent: 13.9 Right Ascension: 08h 38m 24.1s; Declination: +25° 45’ 01” NASA APOD: NGC 2623 Hubble: NGC 2623 a system of two or more interacting galaxies. The galaxies have formed one common nucleus, but there are two strands of stars branching out from the galaxy, indicating a merger has taken place. JKCS041 Chandra: JKCS041 An extremely distant galaxy cluster, about 10.2 billion years away. This object may help scientists better understand how the universe developed at an early age. Messier 77 (NGC 1068, UGC 2188, PGC 10266, Arp 37, 3C 71) Chandra: Messier 77 Universe Today: Messier 77 One of the nearest and brightest galaxies containing a supermassive black hole. Million-mile per hour wind from the black hole shapes the galaxy. H2356-309 Chandra: H2356-309 A collection of extremely distant warm hot intergalactic medium, some of the “missing matter” in the nearby universe. Basic note sheet for the 2011 DSOs, intended for use when asked to quickly identify things, or for those new to the event.

2010 DSOs Epsilon Aurigae** AAVSO: Epsilon Aurigae Milky Way Galaxy NASA: Our Milky Way Gets a Makeover Sagittarius A* Chandra Photo Album: Sagittarius A*: 06 Jan 03 Andromeda Galaxy (M31) NASA APOD: November 14, 1999 - M31: the Andromeda Galaxy Cartwheel Galaxy Chandra Photo Album: Cartwheel Galaxy: 11 Jan 06 -**is part of a special viewing campaign this year and will be included up to at least 2011.

2009 DSOs Circinus X-1 http://www.daviddarling.info/encyclopedia/C/Circinus_X-1.html Chandra Photo Album: Circinus X-1 RU Virginis AAVSO: RU Vir Epsilon Aurigae* AAVSO: Epsilon Aurigae RX Andromedae AAVSO: RX And — a CV in transition? Z Andromedae AAVSO: Z And, October 2000 Variable Star Of The Month SN 1006 Chandra :: Photo Album:SN 1006, 15 Dec 05 Chandra :: Photo Album:SN 1006, 1 July O8 RX J0822-4300 Chandra :: Photo Album :: RX J0822-4300 in Puppis A: Chandra Discovers Cosmic Cannonball :: November 28, 2007 Chandra Press Room :: Chandra Discovers Cosmic Cannonball :: November 28, 2007 G292.0+1.8 Chandra :: Photo Album :: G292.0+1.8 :: October 23, 2007 Chandra :: Photo Album :: G292.0+1.8 :: 22 Oct 01 NASA ADS: Spitzer Spectroscopy of the Galactic Supernova Remnant G292.0+1.8: Structure and Composition of the Oxygen-Rich Ejecta NGC 2440 The colourful demise of a Sun-like star Betelgeuse AAVSO: Alpha Orionis RS Ophiuchi AAVSO: RS Ophiuchi Mira AAVSO: Mira Revisited T Tauri AAVSO: T Tauri Hind's Variable Nebula Hinds Variable Nebula APOD: 2007 December 13 - T Tauri and Hind's Variable Nebula M13 M13. RS Puppis -*is part of a special viewing campaign this year and will be included up to at least 2011.

See Also

Astronomy

Astronomy/Stellar Evolution

Astronomy/Variable Stars

Astronomy/Star and Planet Formation

Astronomy/Type Ia Supernovae

Astronomy/Type II Supernovae

Astronomy/Exoplanets

Links

Basic note sheet for the 2011 DSOs

SIMBAD Astronomy Database for DSOs