Astronomy/Active Galaxies

For 2011, the Astronomy event focused on quasars, AGNs (active galactic nuclei), galaxy clusters, and groups of galaxies.

This Year's DSOs (2010-2011)

• Epsilon Aurigae**
  • AAVSO: Epsilon Aurigae
• NGC 6240
  • Chandra: NGC 6240
• 3C 321
  • Chandra: 3C 321
• Centaurus A (NGC 5128)
  • SEDS: Centaurus A
  • Solstation.com: Centaurus A
• Stephan's Quintet
  • Chandra: Stephan's Quintet
  • NASA APOD: Stephen's Quintet
• MACSJ0717.5+3745
  • Chandra: MACSJ0717.5+3745
• Bullet Cluster (1E 0657-56)
  • Chandra: Bullet Cluster
  • NASA APOD: Bullet Cluster
• Perseus A (NGC 1275)
  • NASA APOD: Perseus A
  • Hubble Heritage: Perseus A
• 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

-**Epsilon Aurigae is part of a special observing campaign through 2011 and will also be included in the DSO list for the 2011/2012 season.

Basic note sheet for the DSO, intended for use when asked to quickly identify things, or for those new to the event.

Other Information

Although these topics are the focus of this year's competition, there are other topics on which you may be tested.

Galaxies

Galaxies make up a majority of the Astronomy event not covered by the DSO list. Many of the DSO's are galaxies with interesting characteristics. Since this year's competition focuses on active galaxies, many of the DSO's are active.

Perseus A, a Type 1.5 Seyfert Galaxy

AGN's and Quasars

AGN's, or Active Galactic Nuclei, are defined as galactic nuclei that emit more electromagnetic radiation than a normal galaxy. This radiation is emitted in a large jet in one direction. In addition, a torus of gas forms around the nucleus perpendicular to the direction of the jet, which can obscure some parts of the galaxy from observers, changing their visual characteristics.

The six main characteristics that define AGN's are: compact angular size, high luminosity, continuum radiation (all types of radiation in the spectrum are emitted), emission lines, variability of emission, and strong radio emission. Quasars, or quasi-stellar radio sources, are similar, as they are galaxies that contain active nuclei. This makes them slightly different than AGN's, but closely related.

Seyfert Galaxy

Seyfert Galaxies are subclasses of active galaxies classified by emission lines of ionized gas. The two main classifications are Type 1 and Type 2. Type 1 Seyferts emit narrow and broad spectral lines, while Type 2 Seyferts only emit narrow lines. Some galaxies can also be classified as numbers between 1 and 2, like 1.5, depending on the relative sizes of the lines. Perseus A is an example of a Type 1.5 Seyfert galaxy.

A diagram showing the classifications of AGN's based on viewing angle

Other classifications

AGN's and quasars are mainly classified based on the angle that the object is viewed from by an observer on Earth. This is because the angle of the electromagnetic radiation emitted from the nucleus can change how visible the object is. If the emission jet faces away from the observer, the object will appear less active, and vice versa. The diagram at left shows how viewing angle correlates to type of AGN.

AGN's are classified into two large groups, Radio-Quiet AGN's and Radio-Loud AGN's. In Radio-Quiet AGN's, the large jet of radiation faces away from the observer. Seyfert galaxies are Radio-Quiet AGN's. In contrast, Radio-Loud AGN's occur when the jet of radiation faces the observer, and much more activity is apparent. In some cases, the radiation is pointed directly at earth, so an observer can see the radiation jet head-on. There objects are known as Blazars. BL Lacertae and OVV (optically violent variable) Quasars, which are both very variable (OVV Quasars more so), are both Blazars.

Black Holes

Black holes are supermassive objects from which nothing can escape. Since light cannot be emitted, they appear as black spots in space. They can also alter the appearance of surrounding objects because of the high gravitational pull.

Mid-mass black holes, or stellar black holes, have masses at 1.4 to 20 times the Sun. They are very dense and result from the collapse of a large star. Intermediate-mass black holes are thought to be at the center of globular clusters, and they are larger than mid-mass black holes. The largest black holes, supermassive black holes, are usually the centers of galaxies. The center of the Milky Way, Sagittarius A*, is thought to be a supermassive black hole. AGN's are usually supermassive black holes. Supermassive black holes can be over one billion solar masses and less dense than water.

They appear black because their escape velocity is greater than that of the speed of light, and nothing is faster than light.

A diagram of an eclipsing binary