Jump to content

2MASX J07322028+3138009

Add links
From Wikipedia, the free encyclopedia
2MASX J07322028+3138009
2MASX J07322028+3138009, as seen by DESI Legacy Surveys
Observation data (J2000.0 epoch)
ConstellationGemini
Right ascension07h 32m 20.28s
Declination+31d 38m 00.8s
Redshift0.143973
Heliocentric radial velocity43,162 km/s
Distance2.514 Gly (770.8 Mpc)
Group or clusterAbell 586
Apparent magnitude (V)0.158
Apparent magnitude (B)0.208
Surface brightness15.4
Characteristics
TypeBrCLG
Size565,700 ly
Notable featuresBrightest cluster galaxy
Other designations
ABELL 586:AMI2012 0, PGC 1956691, NVSS J073220+313757, 2MASS J07322028+3138006

2MASX J07322028+3138009, known as Abell 586 Brightest Cluster Galaxy, or simply Abell 586 BCG, is a massive type-cD elliptical galaxy residing in Abell 586 galaxy cluster located in the constellation Gemini. At the redshift of 0.143973, it is 2.5 billion light-years from Earth.[1]

Characteristics[edit]

2MASX J07322028+3138009 is one of the largest galaxies. With a diameter of 565,700 light-years, it is classfied as the most luminous galaxy,[2] typically old and red lying near the center of the cluster[3] with an estimated black hole mass of 1.17 x 109 M⊙.[4]

The galaxy is uniformed in color with a well established richness correction at 0.10 magnitude/Abell richness class[5] and narrow distribution of luminosity ranging at least 5 <% N <% 500 and a luminosity evolution with a rate dM/dt = 1.09 (1 + z)H0 mag yr -1, hinting 2MASX J07322028+3138009 was brighter during the past.[6]

The galaxy is aligned with its parent cluster[7][8] and has an extended galactic halo with a mass of M500 = 2.0 × 1014 to 1.5 × 1015 M⊙,[9] which its outer component is found to be 10-40 times larger in scale. It has ~10 times of the total luminosity of the inner component, with it exhibits a steeper ⟨μ⟩-re relation than that of the elliptical fundamental plane.[10]

One possible theory for 2MASX J07322028+3138009 having special properties is the process of galactic cannibalism. As a BCG, the galaxy might have engulfed and merged with satellite galaxies thus increasing its luminosity.[11][12] Because dynamical friction is a mass-dependent process, such massive galaxies, will tend to merge quickly with the central galaxy. From major mergers, comes the building-up the mass of the central galaxy as well as reducing the number of massive satellite galaxies. It is estimated that the cannibalism rate is ∼2L* per 5 × 109 yr according to Lauer, who looked for evidence of interactions between the BCG and secondary galaxies in the study in 1988.[13] Not only to mention, as the galaxies merge with the entity, the active galactic nucleus in 2MASX J07322028+3138009 is triggered, as the accretion is sent spiraling towards its supermassive black hole.[14]

Abell 586[edit]

The galaxy cluster where 2MASX J07322028+3138009 is residing, is classfied as Bautz-Morgan type I cluster at redshift of z = 0.17, with an Abell richness class of 3. It has an X-ray emission (LX = 1.11 x 1045 h−1 50 ergs s−1 with a peak that is coincident with the position of the brightest cluster galaxy.[15] It is a massive galaxy cluster with M500 ≳ 2 × 1014 M⊙.[16] Researchers who studied the cluster found evidence of the interaction between dark matter and dark energy, whom they argued that this interaction suggests evidence of violation of the Equivalence Principle.[17]

In another study, researchers analyzed the mass content of Abell 586, through optical data obtained with Gemini Multi-Object Spectrograph (GMOS) mounted on the 8 m Gemini North telescope, and combining with the publicly available X-ray data taken by Chandra space telescope. They found, the cluster has a 68% confidence level, with velocity dispersion of 1000–1250 km s−1.[15]

From the projected mass distributions obtained through weak lensing and X-ray emission, researchers found it strikingly similar, with nearly circular geometry whom they suggested that Abell 586 is likely a truly relaxed cluster whose last major merger event occurred more than ~4 billion years ago.[15]

References[edit]

  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-06-07.
  2. ^ Postman, Marc; Lauer, Tod R. (1995-02-01). "Brightest Cluster Galaxies as Standard Candles". The Astrophysical Journal. 440: 28. doi:10.1086/175245. ISSN 0004-637X.
  3. ^ Dalal, Roohi; A Strauss, Michael; Sunayama, Tomomi; Oguri, Masamune; Lin, Yen-Ting; Huang, Song; Park, Youngsoo; Takada, Masahiro. "Brightest cluster galaxies are statistically special from z = 0.3 to z = 1". academic.oup.com. Retrieved 2024-06-07.
  4. ^ Loubser, S I; Babul, A; Hoekstra, H; Bahé, Y M; O’Sullivan, E; Donahue, M (2020-06-12). "Dynamical masses of brightest cluster galaxies I: stellar velocity anisotropy and mass-to-light ratios". Monthly Notices of the Royal Astronomical Society. 496 (2): 1857–1880. doi:10.1093/mnras/staa1682. ISSN 0035-8711.
  5. ^ Schneider, D. P.; Gunn, J. E.; Hoessel, J. G. (1983-01-01). "CCD photometry of Abell clusters. I. Magnitudes and redshifts for 84 brightest cluster galaxies". The Astrophysical Journal. 264: 337–355. doi:10.1086/160602. ISSN 0004-637X.
  6. ^ Sandage, A. (1972-11-01). "The redshift-distance relation. II. The Hubble diagram and its scatter for first-ranked cluster galaxies: A formal value for q0". The Astrophysical Journal. 178: 1–24. doi:10.1086/151763. ISSN 0004-637X.
  7. ^ Sastry, Gummuluru N. (1968-06-01). "Clusters Associated with Supergiant Galaxies". Publications of the Astronomical Society of the Pacific. 80: 252. doi:10.1086/128626. ISSN 0004-6280.
  8. ^ Niederste-Ostholt, Martin; Strauss, Michael A.; Dong, Feng; Koester, Benjamin P.; McKay, Timothy A. (April 2010). "Alignment of brightest cluster galaxies with their host clusters". Monthly Notices of the Royal Astronomical Society. doi:10.1111/j.1365-2966.2010.16597.x. ISSN 0035-8711.
  9. ^ Herbonnet, Ricardo; Sifón, Cristóbal; Hoekstra, Henk; Bahé, Yannick; van der Burg, Remco F. J.; Melin, Jean-Baptiste; von der Linden, Anja; Sand, David; Kay, Scott; Barnes, David (2020-10-01). "CCCP and MENeaCS: (updated) weak-lensing masses for 100 galaxy clusters". Monthly Notices of the Royal Astronomical Society. 497 (4): 4684–4703. doi:10.1093/mnras/staa2303. ISSN 0035-8711.
  10. ^ Gonzalez, Anthony H.; Zabludoff, Ann I.; Zaritsky, Dennis (2005-01-01). "Intracluster Light in Nearby Galaxy Clusters: Relationship to the Halos of Brightest Cluster Galaxies". The Astrophysical Journal. 618 (1): 195. doi:10.1086/425896. ISSN 0004-637X.
  11. ^ Ostriker, J. P.; Tremaine, S. D. (1975-12-01). "Another evolutionary correction to the luminosity of giant galaxies". The Astrophysical Journal. 202: L113–L117. doi:10.1086/181992. ISSN 0004-637X.
  12. ^ Hausman, M. A.; Ostriker, J. P. (1978-09-01). "Galactic cannibalism. III. The morphological evolution of galaxies and clusters". The Astrophysical Journal. 224: 320–336. doi:10.1086/156380. ISSN 0004-637X.
  13. ^ Lauer, Tod R. (1988-02-01). "The Morphology of Multiple-Nucleus, Brightest Cluster Galaxies". The Astrophysical Journal. 325: 49. doi:10.1086/165982. ISSN 0004-637X.
  14. ^ Muñoz Rodríguez, Iván; Georgakakis, Antonis; Shankar, Francesco (2022-07-01). "Incidence of AGN in massive galaxy clusters". 44: 2325. {{cite journal}}: Cite journal requires |journal= (help)
  15. ^ a b c Cypriano, E. S.; Lima Neto, G. B.; Sodre´ Jr., L.; Kneib, J. P.; Campusano, L. E. "Gemini and Chandra Observations of Abell 586, A Relaxed Strong-Lensing Cluster". The Astrophysical Journal. doi:10.1086/430661/pdf.
  16. ^ Koulouridis, E.; Gkini, A.; Drigga, E. (2024-04-01). "AGNs in massive galaxy clusters: Role of galaxy merging, infalling groups, cluster mass, and dynamical state". Astronomy & Astrophysics. 684: A111. doi:10.1051/0004-6361/202348212. ISSN 0004-6361.
  17. ^ Delliou, Morgan Le; Bertolami, O.; Pedro, F. Gil (2007). "Dark Energy-Dark Matter Interaction from the Abell Cluster A586 and violation of the Equivalence Principle". AIP Conference Proceedings. 957: 421–424. doi:10.1063/1.2823818.
Retrieved from "https://en.wikipedia.org/w/index.php?title=2MASX_J07322028%2B3138009&oldid=1227796396"