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2MASX J17201001+2637317

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2MASX J17201001+2637317
2MASX J17201001+2637317 captured by SDSS
Observation data (J2000.0 epoch)
ConstellationHercules
Right ascension17h 20m 10.04s
Declination+26d 37m 32.04s
Redshift0.160145
Heliocentric radial velocity48,010 km/s
Distance2.465 Gly (755.7 Mpc)
Group or clusterRX J1720.1+2638
Apparent magnitude (V)0.150
Apparent magnitude (B)0.198
Surface brightness16.9
Characteristics
TypeBrClG
Apparent size (V)0.43' x 0.30'
Other designations
OGC 86, PGC 1782937, NVSS J172010+263731, 2MASS J17201003+2637320, RGB J1720+266, SDSS J172010.03+263732.1

2MASX J17201001+2637317 also known as PGC 1782937, is a massive type-cD elliptical galaxy located in the constellation of Hercules. With redshift of 0.16,[1] the galaxy is located 2.4 billion light-years from Earth and the brightest cluster galaxy in the galaxy cluster, RX J1720.1+2638.[2]

Characteristics

2MASX J17201001+2637317 is classified as an optically luminous galaxy according to Sloan Digital Sky Survey.[3] It has a luminosity value of 10L* (L* = 1.0 × 1010 h2 L,[4][5] with a radio source found embedded inside its host with elliptical morphology.[6] The galaxy also has an X-ray bright,[7] radio-loud active galactic nucleus (L 1.4 GHz > 1023 W Hz−1), suggesting it contributes to energy distribution into the intergroup medium.[8] According to ROSAT and Green Bank Telescope, 2MASX J17201001+2637317 is classified as a low-excitation[9] narrow-line radio galaxy with a weak-line and also a LINER galaxy with radio power high as 1023 - 1026 W Hz−1 at 5 GHz, making it among the strongest radio emitting LINERs known so far.[10]

2MASX J17201001+2637317 is a fossil group galaxy with an estimated space density of n = (1.0 ± 0.6) × 10−6 h Mpc−3.[11] The galaxy has a central velocity dispersion between the range Ỽ ~ 300–400 km s−1[12][13] and an extended stellar envelope of excessive light with the light profile being described by a de Vaucouleurs surface brightness law, μ(r) ә r1/4, over a large range in radius.[14] It has been theorized the galaxy might have been formed from multiple galaxy mergers possibly made up of separate disk galaxies.[15] As they collided, combined efforts of dynamic friction and tidal forces redistribute the kinetic energy into random form of energy. This allows the galaxies to merge into a one amorphous, triaxial system resembling an elliptical galaxy in the case of 2MASX J17201001+2637317.[16][17]

MASX J17201001+2637317 is known to have significant ongoing star formation. Researchers who identified at least 120 early-type galaxies between redshifts of 0.1 < z < 0.4, found out the galaxy contains strong emission lines in its optical spectra, with both Hα and [O II]λ3727 line emission present.[18]

Observations of 2MASX J17201001+2637317

Researchers who investigated a connection between its star formation, the active galactic nucleus (AGN) and intracluster medium, found the sharp threshold for the star formation during the central cooling time of the hot atmosphere, is below ~5 × 108 yr or equivalent to ~30 keV cm2. This results showed the AGN feedback in 2MASX J17201001+2637317 into its hot intracluster medium is largely responsible for regulating cooling and star formation in the cores of its parent cluster, leading to the significant growth of the galaxy's supermassive black hole[19] found to actively powering an astrophysical jet.[20]

2MASX J17201001+2637317 was also observed by Spitzer Space Telescope along with 62 other brightest cluster galaxies. Through the results presented by researchers, they found the galaxy has an infrared luminosity greater than 1011 L⊙. This makes it as a luminous infrared galaxy (LIRG) showing one sign of infrared excess and a 24/8 μm flux ratio above 1.0.[21]

RX J1720.1+2638

The cluster where 2MASX J17201001+2637317 is residing, is found to be a cool-core 'relaxed-appearing' galaxy cluster and a non-fossil system.[22] It has a mini halo detected up to 8.4 GHz and confined by X-ray-detected cold fronts with its spectrum consistent with a single power law up to 18 GHz.[23] Moreover, the cluster has a luminosity of 6.20+0.04-0.02{×}1044 observed in 2-10 keV band mass profile of M500 in the range of (5–7)× 1014 M⊙. It actually displays a cool core profile, but there is evidence the galaxy cluster might have undergone a merger.[22]

According to researchers who used the caustic technique to measure cluster mass profiles from galaxy redshifts that is obtained with the Hectospec Cluster Survey (HeCS), the halo mass in RX J1720.1+2638 is estimated to be (1.99 ± 0.11)M 200. They noted it as a new observational cosmological test in essential agreement with the simulations.[24]

RX J1720.1+2638 is known to have a strong gravitational lens containing a lognormal distribution of Einstein radius, with a peak and 1σ width of <log10θE(z = 2)> = 1.16 +/- 0.28. Researchers who presented the results fromKeck Telescope detected an X-ray/lensing mass discrepancy of <MSL/MX> = 1.3 at 3σ significance showing cluster-cluster mergers do play a prominent role in shaping the properties of the cluster core, specifically causing departures from hydrostatic equilibrium, and possibly disturbing the cool core in RX J1720.1+2638.[25]

References

  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-06-15.
  2. ^ Mazzotta, P.; Markevitch, M.; Vikhlinin, A.; Forman, W. R.; David, L. P.; van Speybroeck, L. (2001-07-01). "Chandra Observation of RX J1720.1+2638: a Nearly Relaxed Cluster with a Fast-moving Core?". The Astrophysical Journal. 555: 205–214. doi:10.1086/321484. ISSN 0004-637X.
  3. ^ Ogle, Patrick M.; Lanz, Lauranne; Appleton, Philip N.; Helou, George; Mazzarella, Joseph (2019-07-01). "A Catalog of the Most Optically Luminous Galaxies at z < 0.3: Super Spirals, Super Lenticulars, Super Post-mergers, and Giant Ellipticals". The Astrophysical Journal Supplement Series. 243: 14. doi:10.3847/1538-4365/ab21c3. ISSN 0067-0049.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  4. ^ Sandage, Allan; Hardy, Eduardo (1973-08-01). "The Redshift-Distance Relation. VII Absolute Magnitudes on the First Three Ranked Cluster Galaxies as Functions of Cluster Richness and Bautz-Morgan Cluster Type: the Effect of q_{o}". The Astrophysical Journal. 183: 743–758. doi:10.1086/152263. ISSN 0004-637X.
  5. ^ Schombert, J. M. (1986-03-01). "The Structure of Brightest Cluster Members. I. Surface Photometry". The Astrophysical Journal Supplement Series. 60: 603. doi:10.1086/191100. ISSN 0067-0049.
  6. ^ Kozieł-Wierzbowska, Dorota; Goyal, Arti; Żywucka, Natalia (2020-04-01). "Radio Sources Associated with Optical Galaxies and Having Unresolved or Extended Morphologies (ROGUE). I. A Catalog of SDSS Galaxies with FIRST Core Identifications". The Astrophysical Journal Supplement Series. 247: 53. doi:10.3847/1538-4365/ab63d3. ISSN 0067-0049.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  7. ^ Brinkmann, W.; Laurent-Muehleisen, S. A.; Voges, W.; Siebert, J.; Becker, R. H.; Brotherton, M. S.; White, R. L.; Gregg, M. D. (2000-04-01). "Radio and X-ray bright AGN: the ROSAT - FIRST correlation". Astronomy and Astrophysics. 356: 445–462. ISSN 0004-6361.
  8. ^ Hess, Kelley M.; Wilcots, Eric M.; Hartwick, Victoria L. (2012-08-01). "Fresh Activity in Old Systems: Radio AGNs in Fossil Groups of Galaxies". The Astronomical Journal. 144: 48. doi:10.1088/0004-6256/144/2/48. ISSN 0004-6256.
  9. ^ Best, P. N.; Heckman, T. M. (2012-04-01). "On the fundamental dichotomy in the local radio-AGN population: accretion, evolution and host galaxy properties". Monthly Notices of the Royal Astronomical Society. 421: 1569–1582. doi:10.1111/j.1365-2966.2012.20414.x. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  10. ^ Wang, De-Liang; Wang, Jian-Guo; Dong, Xiao-Bo (2009-10-01). "Optical identification of radio-loud active galactic nuclei in the ROSAT-Green-Bank sample with SDSS spectroscopy". Research in Astronomy and Astrophysics. 9: 1078–1102. doi:10.1088/1674-4527/9/10/002. ISSN 1674-4527.
  11. ^ Santos, Walter A.; Mendes de Oliveira, Claudia; Sodré, Laerte, Jr. (2007-10-01). "Fossil Groups in the Sloan Digital Sky Survey". The Astronomical Journal. 134: 1551. doi:10.1086/521341. ISSN 0004-6256.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  12. ^ Carter, D.; Inglis, I.; Ellis, R. S.; Efstathiou, G.; Godwin, J. G. (1985-01-01). "Kinematics and dynamics of the haloes of supergiant galaxies". Monthly Notices of the Royal Astronomical Society. 212: 471–488. doi:10.1093/mnras/212.2.471. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  13. ^ Dressler, A. (1979-08-01). "The dynamics and structure of the cD galaxy in Abell 2029". The Astrophysical Journal. 231: 659–670. doi:10.1086/157229. ISSN 0004-637X.
  14. ^ Dubinski, John (1998-07-20). "The Origin of the Brightest Cluster Galaxies". The Astrophysical Journal. 502 (1): 141–149. doi:10.1086/305901. ISSN 0004-637X.
  15. ^ Barnes, Joshua E. (1988-08-01). "Encounters of Disk/Halo Galaxies". The Astrophysical Journal. 331: 699. doi:10.1086/166593. ISSN 0004-637X.
  16. ^ Hernquist, Lars (1992-12-01). "Structure of Merger Remnants. I. Bulgeless Progenitors". The Astrophysical Journal. 400: 460. doi:10.1086/172009. ISSN 0004-637X.
  17. ^ Barnes, Joshua E.; Hernquist, Lars (1992-01-01). "Dynamics of interacting galaxies". Annual Review of Astronomy and Astrophysics. 30: 705–742. doi:10.1146/annurev.aa.30.090192.003421. ISSN 0066-4146.
  18. ^ Liu, F. S.; Mao, Shude; Meng, X. M. (2012-06-01). "Star formation activities in early-type brightest cluster galaxies". Monthly Notices of the Royal Astronomical Society. 423: 422–436. doi:10.1111/j.1365-2966.2012.20886.x. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  19. ^ Rafferty, D. A.; McNamara, B. R.; Nulsen, P. E. J. (2008-11-01). "The Regulation of Cooling and Star Formation in Luminous Galaxies by Active Galactic Nucleus Feedback and the Cooling-Time/Entropy Threshold for the Onset of Star Formation". The Astrophysical Journal. 687: 899–918. doi:10.1086/591240. ISSN 0004-637X.
  20. ^ Perrott, Yvette C.; SM, Gopika; Edge, Alastair C.; Grainge, Keith J. B.; Green, David A.; Saunders, Richard D. E. (2023-03-01). "Sub-kpc radio jets in the brightest central galaxy of the cool-core galaxy cluster RXJ1720.1+2638". Monthly Notices of the Royal Astronomical Society. 520: L1–L4. doi:10.1093/mnrasl/slac160. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  21. ^ Quillen, Alice C.; Zufelt, Nicholas; Park, Jaehong; O'Dea, Christopher P.; Baum, Stefi A.; Privon, George; Noel-Storr, Jacob; Edge, Alastair; Russell, Helen; Fabian, Andy; Donahue, Megan; Bregman, Joel N.; McNamara, Brian R.; Sarazin, Craig L. (2008-05-01). "An Infrared Survey of Brightest Cluster Galaxies. I." The Astrophysical Journal Supplement Series. 176: 39–58. doi:10.1086/525560. ISSN 0067-0049.
  22. ^ a b Jiménez-Bailón, E.; Lozada-Muñoz, M.; Aguerri, J. A. L. (2013-04-01). "X-ray emission from RX J1720.1+2638 and Abell 267: A comparison between a fossil and a non-fossil system". Astronomische Nachrichten. 334: 377. doi:10.1002/asna.201211861. ISSN 0004-6337.
  23. ^ Perrott, Yvette C.; Carvalho, Pedro; Elwood, Patrick J.; Grainge, Keith J. B.; Green, David A.; Javid, Kamran; Jin, Terry Z.; Rumsey, Clare; Saunders, Richard D. E. (2021-12-01). "A 15.5 GHz detection of the galaxy cluster minihalo in RXJ1720.1+2638". Monthly Notices of the Royal Astronomical Society. 508: 2862–2880. doi:10.1093/mnras/stab2706. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  24. ^ Rines, Kenneth; Geller, Margaret J.; Diaferio, Antonaldo; Kurtz, Michael J. (2013-04-01). "Measuring the Ultimate Halo Mass of Galaxy Clusters: Redshifts and Mass Profiles from the Hectospec Cluster Survey (HeCS)". The Astrophysical Journal. 767: 15. doi:10.1088/0004-637X/767/1/15. ISSN 0004-637X.
  25. ^ Richard, Johan; Smith, Graham P.; Kneib, Jean-Paul; Ellis, Richard S.; Sanderson, A. J. R.; Pei, L.; Targett, T. A.; Sand, D. J.; Swinbank, A. M.; Dannerbauer, H.; Mazzotta, P.; Limousin, M.; Egami, E.; Jullo, E.; Hamilton-Morris, V. (2010-05-01). "LoCuSS: first results from strong-lensing analysis of 20 massive galaxy clusters at z = 0.2". Monthly Notices of the Royal Astronomical Society. 404: 325–349. doi:10.1111/j.1365-2966.2009.16274.x. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
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