Press Release

Why Do Ionized Gas Clouds Stream Out from Galaxies?

November 19, 2010

  Using the Subaru Prime Focus Camera (Suprime-Cam) in their observations of the Coma Cluster, researchers from the National Astronomical Observatory of Japan (NAOJ), Hiroshima University, the University of Tokyo, and other institutes have discovered 14 galaxies accompanied by extended, ionized hydrogen (Note 1) clouds. The discovery marks the first time that scientists have 1) detected many galaxies with extended ionized hydrogen gas clouds in a cluster and 2) investigated their spatial and velocity distribution as well as the characteristics of their parent galaxies. The observations captured images of this cluster of galaxies during a critical moment of galaxy evolution and contribute to an understanding of how such clouds may have formed.


Figure 1:Ionized Hydrogen Gas Clouds Ejected from a Galaxy in the Coma Cluster.
Key to Figure:The figure is a pseudo-color composite of blue (B-band), green (R-band), and red (H-alpha-band). The red color shows regions with H-alpha emission without stellar light. The white bar at bottom-right represents 10 kpc (33 thousand light years). The image size is 115 x 271 arcsec².

  A cluster of galaxies is an aggregate of a few to hundreds or even thousands of galaxies. Scientists know that more elliptical (E) and lenticular (S0) galaxies exist more often in cores of clusters of galaxies than in less dense environments. The elliptical and lenticular galaxies are called as "quiescent galaxies" because they show no star formation activity. Meanwhile, spiral galaxies such as our Galaxy are still undergoing star formations, and they are likely to reside in less populated regions. These attributes of clusters raise a number of important questions about the evolution of galaxies: "What kind of mechanisms shape these variety of galaxies occurring in different environments?" and "Why do clusters of galaxies contain many galaxies that do not form stars?" The current research provides observational evidence that addresses these issues.

  The team focused their observations on the Coma Cluster, a large cluster of more than 3,000 galaxies and one of the nearest (about 300 million light years away) clusters to our Galaxy. Past observations had found several extended ionized hydrogen clouds associated with galaxies in the cluster. This group of scientists concentrated on examining these clouds and used a special filter in their observations to catch a specific spectral line (the H-alpha line) (Note 2) created by ionized hydrogen at a particular wavelength. Consequently, they detected 14 galaxies with extended ionized hydrogen clouds, examples of which are shown in Figures 1 and 2.

  Most of the ionized hydrogen gas appears as if it was ejected from the galaxy. Follow up observations with Subaru's Faint Object Camera and Spectrograph (FOCAS) confirmed that some of the gas clouds have a recession velocity (Note 3) comparable to that of adjacent galaxies. Therefore, the scientists infer that the overlap between the gas and the galaxy did not occur by chance but resulted from the gas streaming out of the galaxy.

  A more detailed investigation of the ionized hydrogen clouds and their "parent galaxies" reveals that most of the parent galaxies are currently or were recently forming stars. In addition, most parent galaxies have a relatively large velocity difference (more than 1000 km/s) when compared with the average recession velocity of the Coma Cluster. These observational results suggest that the extended ionized hydrogen gas was probably stripped from the parent galaxies by either 1) interaction with the hot gas of the cluster or 2) by the tidal force of the cluster produced when the parent galaxies are trapped by the gravity of the cluster and fall onto the cluster. This scenario predicts a difference in star formation between low and high mass galaxies. Low mass galaxies that lose all of their gas from stripping cease star formation, while higher mass galaxies retain their gas and continue to form stars. The correlation between mass and star-forming activity derived from the observations in the team's research confirms the prediction.

  In summary, this study has clarified some of the specific conditions under which extended ionized hydrogen clouds were formed as well as the relationship between the conditions and characteristics of the parent galaxies. Nevertheless, questions remain. How is the stripped gas ionized, and how does it retain the H-alpha emission? The most distant ionized gas cloud lies 300,000 light years from the parent galaxy, and it would take 100 million years or more for that cloud to travel this distance. Since the brightness of the H-alpha emission of the distant clouds is comparable to the clouds near the parent galaxy, the energy to maintain the H-alpha emission must have somehow persisted for more than 100 million years. How these H-alpha emitting structures endure this long remains a mystery. What is going on in the cluster!?

  The research group will conduct further spectroscopic observations to help solve this puzzle. They plan to estimate the temperature and density of several parts of the ionized hydrogen clouds and to tackle the question of how the galaxy and gas are evolving in the nearby cluster of galaxies.

The research on which this article is based will be published in the December 2010 issue of the Astronomical Journal (140:1814-1829): "A Dozen New Galaxies Caught in the Act: Gas Stripping and Extended Emission Line Regions in the Coma Cluster" by M. Yagi et al.

Observation Details:

  Object:A part of the central region of the Coma Cluster.
  Telescope:Subaru Telescope with an effective aperture of 8.2 meters
  Camera:Subaru Prime Focus Camera (Suprime-Cam)
  Filter:Narrow-band H-alpha (671 nm), broadband B (450 nm), broadband R (650nm)
  Observation Dates (UT):2006/04/28, 2007/05/12-15, 2009/05/25-27
  Exposure Times: 87.5 min (B), 190 min (R), 450 min (H-alpha)
  Orientation: North is up; East is left
  Coordinates: RA 13h 00m Dec. +27d 52m (J2000.0)
  Constellation: Coma Berenices

Additional notes:

1. Neutral and ionized hydrogen: A hydrogen ion (proton) becomes neutral after combining with a free electron. After the combination, the neutral hydrogen quickly loses its energy until it reaches the minimum energy level ("ground state") of the atom by emitting a number of emission lines, including H-alpha. Because neutral hydrogen at its ground state is much more stable than ionized hydrogen, energy is required to ionize a neutral hydrogen to lead another recombination and H-alpha emission. In order to maintain H-alpha emission for a long time, moderate energy sources are necessary. If the input energy to neutral hydrogen is excessive, the kinetic energy of the free electron produced by ionization of neutral hydrogen increases a lot. Such a strong energy source results in a "totally ionized hot plasma", which does not emit H-alpha, because the free electrons in it have such high energy that they cannot combine with hydrogen ions.

2. H-alpha: One of the emission lines created when a hydrogen ion (proton) combines with a free electron. Its wavelength is 656 nm, and human eyes see it as a deep red color. The H-alpha emission from the Coma Cluster is observed at around 670 nm. The expansion of the universe accounts for the shift in the appearance of the emission to the red end of the visible spectrum ("redshift").

3. Recession velocity: The apparent speed of celestial objects moving away from Earth. The expansion of the universe causes that more distant objects appear to have a larger recession velocity. Generally objects at different distances have different recession velocities.



Figure 2:Ionized Hydrogen Gas Clouds Ejected from Galaxies in the Coma Cluster. The colors in the image and the scale of the white bar are the same as those noted for Figure 1. The sizes of the fields are 145 x 87, 121 x 83, and 180 x 96 arcsec² for (a), (b) and (c), respectively.




Additional figures:The differences between the H-alpha-band and R-band images in Figure 1 and 2 (a)-(c) are as follows:
* The white structure (enclosed with a green contour) shows the region where the H-alpha emission is strong.
* The red line shows a central bright part of each parent galaxy.
The parent galaxy appears as a black color because hydrogen in the atmosphere of stars in the galaxy absorbs the light at the wavelength of H-alpha.




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