Difference between revisions of "Astronomy/DSOs"

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(2012 dso's)
(Previous Years' DSO Lists: more 2011 info)
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!rowspan="2" | 3C 321
 
!rowspan="2" | 3C 321
|rowspan="2" | [[File:3C321 wavelengths.jpg|275px]]
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|rowspan="2" | [[File:3C321 wavelengths.jpg|250px]]
 
|rowspan="2" | [[File:3c321 artist.jpg|165px]]
 
|rowspan="2" | [[File:3c321 artist.jpg|165px]]
 
|Serpens
 
|Serpens
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|Auriga
 
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|'''Right Ascension:''' 07h 17m 31.00s; '''Declination:''' +37° 45’ 39.60”
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|[http://chandra.harvard.edu/photo/2009/macs/ Chandra: MACSJ0717.5+3745]
 
|[http://chandra.harvard.edu/photo/2009/macs/ Chandra: MACSJ0717.5+3745]
 
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| colspan="5" | 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.
 
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!rowspan="2" | Bullet Cluster ''(1E 0657-56)''
 
!rowspan="2" | Bullet Cluster ''(1E 0657-56)''
 
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|Carina
 
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| '''Right Ascension:''' 06h 58m 37.9s; '''Declination:''' - 55° 57’ 0”
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|[http://chandra.harvard.edu/photo/2008/bullet/ Chandra: Bullet Cluster] [http://apod.nasa.gov/apod/ap060824.html NASA APOD: Bullet Cluster]
 
|[http://chandra.harvard.edu/photo/2008/bullet/ Chandra: Bullet Cluster] [http://apod.nasa.gov/apod/ap060824.html NASA APOD: Bullet Cluster]
 
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| colspan="5" | 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.
 
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!rowspan="2" | Perseus A ''(NGC 1275)''
 
!rowspan="2" | Perseus A ''(NGC 1275)''
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|rowspan="2" | [[File:Ngc1275 web.jpg|175px]]
 
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|Perseus
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| '''Apparent:''' 12.6.
 
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|'''Right Ascension:''' 03h 19m 48.1s; '''Declination:''' +41° 30’ 42”
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|[http://apod.nasa.gov/apod/ap080822.html NASA APOD: Perseus A] [http://heritage.stsci.edu/2003/14/supplemental.html Hubble Heritage: Perseus A]
 
|[http://apod.nasa.gov/apod/ap080822.html NASA APOD: Perseus A] [http://heritage.stsci.edu/2003/14/supplemental.html Hubble Heritage: Perseus A]
 
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| colspan="5" | 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.
 
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!rowspan="2" | SN 2006gy
 
!rowspan="2" | SN 2006gy

Revision as of 16:05, 16 September 2011

The Astronomy DSO list specifies which Deep Sky Objects may be covered in the Astronomy event that year.

2012 DSOs

2012 DSO's
Name Images Constellation Magnitude Distance Coordinates External Links
Mira
SNR 0509-67.5
CH Cyg
Kepler's SNR
Tycho's SNR
Messier 15
Carina Nebula
T Tauri
Sirius B
RR Lyrae
U Scorpii
Rosette Nebula
BP Psc
NGC 2440
RX J0806.3+1527
DEM L238 & L249

Previous Years' DSO Lists

<spoiler text="2011 DSOs">

2011 DSO's
Name Images Constellation Magnitude Distance Coordinates External Links
Epsilon Aurigae Epsilon aurigae.jpg Epsilon Auriga.jpg 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) Ngc 6240.jpg Ngc 6240 xray inset.jpg 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 3C321 wavelengths.jpg 3c321 artist.jpg 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) Ngc1275 web.jpg 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 Chandra: SN 2006gy NASA APOD: SN 2006gy
SN 1996cr Chandra: SN 1996cr
NGC 4603 NASA APOD: NGC 4603 HyperPhysics: NGC 4603
NGC 7771 NASA APOD: NGC 7771
NGC 2623 NASA APOD: NGC 2623 Hubble: NGC 2623
JKCS041 Chandra: JKCS041
Messier 77 (NGC 1068) Chandra: Messier 77 Universe Today: Messier 77
H2356-309 Chandra: H2356-309

Basic note sheet for the 2011 DSOs, intended for use when asked to quickly identify things, or for those new to the event. </spoiler> <spoiler text="2010 DSOs">

-**is part of a special viewing campaign this year and will be included up to at least 2011. </spoiler> <spoiler text="2009 DSOs">

-*is part of a special viewing campaign this year and will be included up to at least 2011. </spoiler>