View source for MACS J0025.4-1222

{{Short description|Galaxy cluster}}
{{Galaxy cluster
| name = MACS J0025.4-1222
| image = [[Image:MACS J0025.4-1222.jpg|300px]]
| caption = Composite image of separate exposures made by Hubble Space Telescope ACS and WFPC2 detectors and the Chandra ACIS detector<ref>{{cite web
  | last = 
  | first = 
  | title = A Clash of Clusters Provides New Clue to Dark Matter
  | url=http://newswise.com/articles/view/543808/
  | access-date = 2008-10-25 }}</ref>
| ra = 00h 25m 29s.80
| dec = -12° 22' 46".99
| distance = 6.07 Gly / 1.725 Gpc
| redshift = 0.586
| constellation = [[Cetus]] 
}}

'''MACS J0025.4-1222''' is a [[galaxy cluster]] created by the collision of two galaxy clusters, and is part of the [[MAssive Cluster Survey]] (MACS). Like the earlier discovered [[Bullet Cluster]], this cluster shows a clear separation between the centroid of the intergalactic gas (of majority of the normal, or [[baryonic]], mass) and the colliding clusters.

In [[:file:MACS J0025.4-1222.jpg|the image]], intergalactic gas is shown in pink and the mass centroids of the colliding clusters in blue, showing the separation of the two, similar to the Bullet Cluster. It provides independent, direct evidence for [[dark matter]] and supports the view that dark matter particles interact with each other only very weakly.

== Details ==
The shown image is a composite of separate exposures made by [[Hubble Space Telescope]] ACS and WFPC2 detectors and the [[Chandra X-ray Observatory|Chandra]] ACIS detector.<ref>{{cite web
  | last = 
  | first = 
  | title = MACS J0025.4-1222: A Clash of Clusters Provides Another Clue to Dark Matter
  | url=http://hubblesite.org/newscenter/archive/releases/2008/32/fastfacts/
  | access-date = 2008-10-25 }}</ref> The Hubble images were taken on November 5, 2006, and June 6, 2007. The visible light images from Hubble showed  [[gravitational lensing]] which allowed astronomers to infer the distribution of total mass (both dark matter and normal matter)(colored in blue). The distribution of normal matter is mostly in the form of hot gas glowing brightly in X-rays (shown pink).  Its distribution was accurately mapped from Chandra data.<ref>{{cite web
  | last = 
  | first = 
  | title = News Release Number: STScI-2008-32
  | url=http://www.chandra.harvard.edu/photo/2008/macs/
  | access-date = 2008-10-25 }}</ref> From these it was possible to tell that most of the mass in the two blue regions was dark matter.

The international team of astronomers in this study was led by Marusa Bradac of the [[University of California, Santa Barbara]], and Steve Allen of the Kavli Institute for Particle Astrophysics and Cosmology at [[Stanford University]] and the Stanford Linear Accelerator Center ([[SLAC]]).<ref name=Brada2008>{{Cite journal|title=Revealing the Properties of Dark Matter in the Merging Cluster MACS J0025.4-1222|date = 2008 |last1=Brada|first1= M |last2=Allen|first2=S. W |last3=Ebeling|first3=H |last4=Massey|first4=R |last5=Morris|first5=R. G|last6=von der Linden|first6=A|last7=Applegate|first7=D| journal = The Astrophysical Journal|volume = 687 |issue = 2 |page = 959 |arxiv = 0806.2320|doi = 10.1086/591246 |bibcode = 2008ApJ...687..959B |s2cid = 14563896 }}</ref>

The two clusters that formed MACS J0025 are each almost a quadrillion times the mass of the Sun. They merged at speeds of millions of miles per hour, and as they did so the hot gas in each cluster collided with the hot gas in the other and slowed down. The dark matter (which interacts weakly) did not. The separation between the normal matter (pink) and dark matter (blue) therefore provides direct evidence for dark matter and supports the view that dark matter particles interact with each other almost entirely through gravity.

== References ==
{{reflist|2}}

== External links ==
*{{SIMBAD link|id=NAME+BABY+BULLET|label=MACS J0025.4-1222}}
*{{NED link|id=MACS+J0025.4-1222}}

[[Category:Galaxy clusters]]
[[Category:Cetus]]