| 词条 | MACS J0717.5+3745 |
| 释义 |
| name = MACS J0717.5+3745 | image = | caption = MACS J0717.5+3745 taken by the combination of observations from the NASA/ESA Hubble Space Telescope, the NASA Chandra X-ray Observatory, and the NRAO Jansky Very Large Array. | credit = NASA, ESA, CXC, NRAO/AUI/NSF, STScI, and R. van Weeren (Harvard-Smithsonian Center for Astrophysics) Acknowledgment: NASA, ESA, and J. Lotz (STScI), and the HFF team | epoch = J2000 | constellation = | ra = {{RA|07|17|36.50}}[1] | dec = {{DEC|+37|45|23}}[1] | brightest_member = | member_no = | richness = | bmtype = | velocity_dispersion = 1660[2] | redshift = 0.5458[1] | distance = | temperature = | mass = 0 | luminosity = | flux = | other_names = ClG J0717+3745, MCS J0717.5+3745, PLCKESZ G180.24+21.04, 1RXS J071733.8+374520, BAX 109.3900+37.7600, MCXC J0717.5+3745, RX J0717.5+3745 }} MACS J0717.5+3745 (MACS J0717 or MACS 0717 for short) is a large galaxy cluster located 5.4 billion light years away in the constellation Auriga,[3] appearing in the MAssive Cluster Survey (MACS). DescriptionThe cluster was formed by four separate galaxy clusters that have been involved in a collision. This is the first time that this phenomenon has been observed. The repeated collisions in MACSJ0717 are caused by a 13-million-light-year-long stream of galaxies, gas, and dark matter, known as a filament, pouring into a region already full of matter. When two or more of the galaxy clusters collide, the hot gas in the interstellar medium slows down, but the galaxies, composed mostly of empty space, do not slow as fast. The speed and direction of each of the clusters involved in the collision can thus be approximated through examining the offset between the galaxies and the gas.[4] Of the four subclusters, A, B, C, D, subcluster B is moving quickly relative to the other three subclusters, which are relatively at rest in relation to each other. The quick moving B exhibits kinetic Sunyaev-Zel'dovich effect (SZ effect for short), the first time this has been observed in an object, instead of statistically. The B subcluster's kinetic SZ effect was discovered due to its lack of a thermal SZ effect, unlike the other three subclusters.[5] GallerySee also
References1. ^1 2 {{cite simbad|title=ClG J0717+3745|accessdate=23 March 2016}} 2. ^{{cite web|title=A Complete Sample of 12 Very X-Ray Luminous Galaxy Clusters at z > 0.5|url=http://iopscience.iop.org/article/10.1086/518603/meta;jsessionid=32737D6FFEAE004856C90BCB189D02F8.c3.iopscience.cld.iop.org|website=The Astrophysical Journal|accessdate=23 March 2016}} 3. ^{{cite web|url=http://hubblesite.org/newscenter/archive/releases/2009/17/fastfacts/|title=Galaxy Cluster MACSJ0717|author=Hubblesite.org|accessdate=October 19, 2012|date=April 16, 2009}} 4. ^{{cite web|url=http://chandra.harvard.edu/photo/2009/macs/|title=MACSJ0717.5+3745|author=Chandra.Harvard.edu|accessdate=October 19, 2012|date=April 16, 2009}} 5. ^{{cite news |url=https://www.sciencedaily.com/releases/2014/01/140116113554.htm |title= Massive Galaxy Cluster Verifies Predictions of Cosmological Theory: First Detection of Kinetic SZ Effect in an Individual Galaxy Cluster |date= 15 January 2014 |publisher= Science Daily }} External links
2 : Galaxy clusters|Auriga (constellation) |
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