| 词条 | Perseus Cluster | ||||
| 释义 |
| name = Perseus cluster | image = | caption = Chandra X-ray Observatory observations of the central regions of the Perseus galaxy cluster. Image is 284 arcsec across. RA 03h 19m 47.60s Dec +41° 30' 37.00" in Perseus. Observation dates: 13 pointings between August 8, 2002 and October 20, 2004. Color code: Energy (Red 0.3-1.2 keV, Green 1.2-2 keV, Blue 2-7 keV). Instrument: ACIS. | credit = NASA/CXC/IoA/A.Fabian et al. | constellation = Perseus | epoch = J2000 | ra = {{RA|03h|18}}[1] | dec = {{DEC|+41|30}}[1] | redshift = 0.01790 (5 366 km/s)[1] | distance = {{convert|73.6|Mpc|Mly|2|abbr=on|lk=on}} {{hub|0.705}} [1] | richness = 2[2] | bmtype = II-III[2] | appmag_v = 13.0 | size_v = 125.9′ | member_no = >1000[1] | flux = 9.1{{e|-11}} erg s−1 cm−2 (2—10 keV)[1] | brightest_member = NGC 1275 | other_names = Abell 426,[1] NGC 1275 Cluster,[1] LGG 88 }} The Perseus cluster (Abell 426) is a cluster of galaxies in the constellation Perseus. It has a recession speed of 5,366 km/s and a diameter of 863′.[1] It is one of the most massive objects in the known universe, containing thousands of galaxies immersed in a vast cloud of multimillion-degree gas. X-radiation from the clusterThe detection of X-ray emission from Per XR-1 occurred during an Aerobee rocket flight on March 1, 1970, the source may be associated with NGC 1275 (Per A, 3C 84), and was reported in 1971.[3] If the source is NGC 1275, Lx ~4 x 1045 ergs/s.[3] More detailed observations from Uhuru confirmed the earlier detection and associated the source with the Perseus cluster.[4] Per X-1 is the galaxy cluster at 4U 0316+41 designated the Perseus cluster, Abell 426, and NGC 1275. The galaxy cluster is the brightest cluster in the sky when observed in the X-ray band.[5] The cluster contains the radio source 3C 84 that is currently blowing bubbles of relativistic plasma into the core of the cluster. These are seen as holes in an X-ray image of the cluster, as they push away the X-ray emitting gas. They are known as radio bubbles, because they appear as emitters of radio waves due to the relativistic particles in the bubble. The galaxy NGC 1275 is located at the centre of the cluster, where the X-ray emission is brightest. Perseus galaxy cluster's Cosmic music noteIn 2003 a team of astronomers led by Dr. Andrew Fabian at Cambridge University discovered one of the deepest notes ever detected, after 53 hours of Chandra observations.[6] No human will actually hear the note, because its time period between oscillations is 9.6 million years, which is 57 octaves below the keys in the middle of a piano.[6] The sound waves appear to be generated by the inflation of bubbles of relativistic plasma by the central active galactic nucleus in NGC 1275. The bubbles are visible as ripples in the X-ray band since the X-ray brightness of the intracluster medium that fills the cluster is strongly dependent on the density of the plasma. A similar case also happens in the nearby Virgo Cluster, generated by an even larger supermassive black hole in the galaxy Messier 87, also detected by Chandra. Like the former, no human will hear the note. The tone is variable, and even lower than those generated by NGC 1275, from 56 octaves below middle C on minor eruptions, to as low as 59 octaves below middle C on major eruptions.[7] Image gallerySee also
References1. ^1 2 3 4 5 6 7 8 {{cite web | title = NASA/IPAC Extragalactic Database | work = Results for Perseus Cluster | url = http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=Perseus+CLUSTER | accessdate = 2006-11-28}} 2. ^1 {{cite journal | last1 = Abell | first1 = George O. | last2 = Corwin | first2 = Harold G., Jr. | last3 = Olowin | first3 = Ronald P. |date=May 1989 | title = A catalog of rich clusters of galaxies | journal = Astrophysical Journal Supplement Series | volume = 70 | issue = May 1989 | pages = 1–138 | format = PDF | issn = 0067-0049 | bibcode = 1989ApJS...70....1A | doi = 10.1086/191333 | accessdate = March 12, 2012 | url = http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?bibcode=1989ApJS...70....1A&page_ind=0&epage_ind=137&type=PRINTER&data_type=PDF_HIGH&email=&emailsize=500&emailsplit=YES&send=GET&verified=YES}} 3. ^1 {{ cite journal |doi=10.1086/180697 |author=Fritz G |author2=Davidsen A |author3=Meekins JF |author4=Friedman H |title=Discovery of an X-ray source in Perseus |date=Mar 1971 |journal=Astrophys. J. |volume=164 |issue=3 |pages=L81–5 |bibcode=1971ApJ...164L..81F }} 4. ^{{ cite journal |volume=178|pages=309–316|author1=Forman, W.|author2=Kellogg, E.|author3=Gursky, H.|author4=Tananbaum, H.|author5=Giacconi, R.|title=Observations of the Extended X-Ray Sources in the Perseus and Coma Clusters from UHURU |date=1972 |journal=Astrophysical Journal|series=NASA/IPAC Extragalactic Database |doi=10.1086/151791|bibcode = 1972ApJ...178..309F }} 5. ^{{ cite journal |author=Edge AC |author2=Stewart GC |author3=Fabian AC |title=Properties of cooling flows in a flux limited sample of clusters of galaxies |journal=MNRAS |date=1992 |bibcode=1992MNRAS.258..177E |volume=258 |pages=177 |doi=10.1093/mnras/258.1.177}} 6. ^1 {{cite journal |last1=Fabian |first1=A.C. |last2=Sanders |first2=J.S. |last3=Allen |first3=S.W. |last4=Crawford |first4=C.S. |last5=Iwasawa |first5=K. |last6=Johnstone |first6=R.M. |last7=Schmidt |first7=R.W. |last8=Taylor |first8=G.B. |date=2003 |title=A Deep Chandra observation of the Perseus cluster: shocks and ripples |url=https://arxiv.org/abs/astro-ph/0306036 |journal=Monthly Notices of the Royal Astronomical Society |volume=344 |issue=3 |pages=L43–L47 |doi=10.1046/j.1365-8711.2003.06902.x|arxiv=astro-ph/0306036 }} 7. ^{{cite journal | last = Roy | first = Steve | last2 = Watzke | first2 = Megan | date = October 2006 | title = Chandra Views Black Hole Musical: Epic But Off-Key | url = http://chandra.harvard.edu/press/06_releases/press_100506.html | journal = Chandra X-Ray Observatory | publisher = Harvard-Smithsonian Center for Astrophysics | accessdate = 20 February 2014}} External links
6 : Galaxy clusters|Perseus Cluster|Perseus (constellation)|Perseus-Pisces Supercluster|Abell objects|Abell richness class 2 |
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