ASTRO 801
Planets, Stars, Galaxies, and the Universe

Exotic Galaxies

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One technique for studying galaxies that astronomers have been using with modern, space-based observatories is to take deep fields. The longer you leave the shutter of your camera open while pointing at a particular part of the sky, the fainter the objects you will be able to see. In astronomical jargon, the fainter the faintest object in your image is, the "deeper" the image. In 1996, Hubble released the "Hubble Deep Field," which was a revolutionary image in its day. It is reproduced below.

Telescopic image of the Hubble Deep Field
Figure 9.6: The Hubble Deep Field

If you look closely, the few objects with spikes on them (a white one near the lower left and a yellow one on the center left) are stars in the Milky Way Galaxy, but every other object in this image is a distant galaxy. Thus, by taking a deep field, astronomers are presented with an excellent representative sample of the types of galaxies in the universe. We will return to the Hubble Deep Field for Lab 3.

For the most part, all of the galaxies that we observe locally, and that we find in deep fields, are normal galaxies. They contain billions of stars, clouds of gas, and dust. When we take a spectrum of the integrated light from the entire galaxy, it looks like the sum of the light from a large group of stars. Remember, stars have spectra that are very similar to blackbodies, but with absorption lines. So, for the most part, a galaxy's spectrum looks like a blackbody spectrum, but also with a lot of absorption lines.

Try this!

See for yourself the spectra of galaxies. The Sloan Digital Sky Survey has measured the spectra for many galaxies. In the window of data on each SDSS object, click on the thumbnail image of the spectrum in the lower left to bring up a full sized image of the spectrum.

  1. Bring up the SDSS Object Explorer for Object ID 587722982271090881.
  2. Bring up the SDSS Object Explorer for Object ID 588015507682230507.
  3. Bring up the SDSS Object Explorer for Object ID 587731513690095801.
How do these spectra appear? How are they similar to each other?

At the same time that astronomers were spending much of their time studying galaxies and classifying them, several astronomers were finding peculiar objects unlike many of the other galaxies. One type of peculiar galaxy, identified by astronomer Carl Seyfert, had the following properties that were unique compared to the average galaxy:

  1. The total luminosity of the galaxy is much larger (perhaps 1,000 times larger) than a normal galaxy.
  2. The spectrum of the galaxy is very different from a typical galaxy; it gives off more light at all wavelengths than a normal galaxy does, and there are many bright emission lines in its spectrum.

The extra luminosity from these “Seyfert Galaxies” comes almost entirely from the nuclear region of the galaxy, not from all areas of the galaxy equally. In general, any galaxy that shows evidence for a source of radiation that is not being created by stars is called an active galaxy. Because the non-stellar light from these galaxies is concentrated in the nucleus, they are usually called Active Galactic Nuclei or just AGN. Below is a sample image of a Seyfert galaxy, and it is a particularly nice example where it is quite obvious how much brighter the bulge region is compared to some of the other spiral galaxies you have seen previously.

Hubble image of Seyfert Galaxy NGC 7742
Figure 9.7: Hubble image of Seyfert Galaxy NGC 7742

AGN are bright radio and x-ray sources. In particular, in the radio, the galaxies show narrow jets of plasma being ejected out of the galaxy at high speeds, which end in extremely large lobes of bright radio emission. Remember, in the optical, the extent of the Milky Way is something like 30,000 parsecs in diameter. In general, the distance from lobe to lobe in a radio galaxy can be several hundred thousand parsecs, and the two largest are 4 million and 6 million parsecs from lobe to lobe! The National Radio Astronomy Observatory has spent more than 50 years studying AGN and has a large archive of images from their observations of these objects. For example, see:

There are many different types of galaxies that are called AGN, but broadly speaking, astronomers have separated them into three main classes with the following properties:

  1. Seyfert Galaxies:
    • These appear superficially to be normal spiral galaxies.
    • One clue to how they differ from normal galaxies is that the "extra" luminosity from Seyferts appears to come from an extremely bright core.
    • In some cases, the core of a Seyfert galaxy is brighter than the entire Milky Way.
    • Seyfert galaxies are particularly bright in the infrared, and this is likely due to dust surrounding the core.
    • The light from the core of a Seyfert can vary on a very short timescale, which suggests that the energy emitting region is less than 1 light-year across.
  2. Radio Galaxies:
    • Radio galaxies are often found to be associated with elliptical galaxies, but not always normal elliptical galaxies. Instead, radio galaxies tend to be associated with "disturbed" ellipticals like Centaurus A.
    • Much of the nonstellar radiation from these objects is in the radio part of the spectrum. Also, the morphology of the radio emission isn't always just a point source, instead, we often see a core, jet, lobe structure.
    • In other wavelengths (X-ray, for example), the core of the radio galaxy stands out as a bright point source.
    • The total energy output of these objects is roughly 1,000 times larger than the Milky Way, making them some of the brightest single objects in the universe.
  3. Quasars:
    • In the optical part of the spectrum, Quasars look like bright, blue stars. The name Quasar stands for "Quasi-stellar radio source," because they look like stars, but are in many ways unlike stars.
    • They are bright in the optical, x-ray, and radio portions of the spectrum, and the brightest of these objects is 100,000 times brighter than the Milky Way.

Try this!

See for yourself the spectra of active galaxies (AGN). The Sloan Digital Sky Survey had as one of its major science goals the discovery and study of a large number of quasars. Identical to the data on the normal galaxies, in the window of data on each SDSS object, click on the thumbnail image of the spectrum in the lower left to bring up a full sized image of the spectrum.

  1. Bring up the SDSS Object Explorer for Object ID 587725074457821263.
  2. Bring up the SDSS Object Explorer for Object ID 587725074995019808.

How do these spectra appear? How are they similar to each other? How do they differ from the galaxy spectra you studied above?

If you want to explore more objects beyond the few listed here, you can bring up all of the SDSS objects from a single observation with the Plate Explorer.

A question that astronomers asked, and a question you should be asking yourself now, is: What is the source of the difference between normal galaxies and active galaxies?

To answer this question, we need to return briefly to the topic of black holes. When a massive star creates a black hole, the mass of the black hole is a fraction of the mass of the star's core. We think that stellar black holes have masses of about 3 times the mass of the Sun. In the core of the Milky Way, we have found that the central black hole is several million solar masses. We think that supermassive black holes (SMBHs) like Sgr A* in the Milky Way are common in the cores of galaxies, and we are able to theorize what happens when a star or other object gets too close to the SMBH.

When matter gets close to a SMBH, it will swirl around the SMBH, and we expect this to create a disk of material around the SMBH. This is exactly analogous to the accretion disks we considered when we studied binary star systems. We believe that in many ways they look similar. As shown below, the material in this disk falls into, or accretes onto, the SMBH. As the material swirls closer and closer to the SMBH, it speeds up. Friction among the particles in the disk causes the gas to heat up, and it can reach temperatures of millions of kelvin. These disks full of hot, fast moving gas emit radiation, and the amount is large enough to power quasars and other AGN.

Image of an accretion disk in a quasar
Figure 9.8: Accretion disk in a quasar
Credit: APOD

The jets that we see in radio galaxies and quasars are likely to come from the disk, too, but these are not well understood at all. It is thought that the disk helps to “focus” the jets (see the image above for an example), but the exact mechanism of the creation of the jet and how it stays so narrow over such large distances (a few hundred thousand parsecs) is a topic of ongoing research.

The Milky Way has an SMBH in its core, but the Milky Way is not an AGN. So, clearly just the presence of an SMBH alone cannot be the only requirement for the creation of an AGN. The answer to this again rests with the accretion disk. The accretion disk fuels the central power source in AGN, and if there is no fuel or not enough fuel, then the galaxy will not be seen as an AGN. When we look at AGN in detail, it appears that many of them appear to show evidence for the host galaxy absorbing another galaxy. This act of galaxies merging with each other can funnel gas into the core, providing ample fuel to power the SMBH.  This idea does imply that AGN will "shut off" over time as they run out of fuel.  In 2016, Penn State astronomer Jessie Runnoe and her collaborators discovered a quasar that appears to have run out of fuel in between observations!