4C +41.26
| 4C +41.26 | |
|---|---|
 4C +41.26 captured by SDSS | |
| Observation data (J2000.0 epoch) | |
| Constellation | Canes Venatici |
| Right ascension | 13h 35m 20.095s |
| Declination | +41d 00m 04.13s |
| Redshift | 0.228324 |
| Heliocentric radial velocity | 68,450 km/s |
| Distance | 3.15 Gly (965.8 Mpc) |
| Group or cluster | Abell 1763 |
| Apparent magnitude (V) | 0.033 |
| Apparent magnitude (B) | 0.025 |
| Surface brightness | 16.0 |
| Characteristics | |
| Type | BrClG |
| Size | 862,300 light-years (264.4 kiloparsecs) |
| Apparent size (V) | 0.24' x 0.19' |
| Other designations | |
| B3 1333+412, PGC 2174167, TXS 1333+412, RX J1335.2+410, OGC 0110, 7C 1333+4115, 2MASX J13352009+4100041, NVSS J133519+410004 | |
4C +41.26 known as PGC 2174167, is a massive elliptical galaxy of type E[1] located in the constellation of Canes Venatici. Its redshift is 0.228324, estimating the galaxy to be located 3 billion light years away from Earth.[2] It is the brightest cluster galaxy of Abell 1763 (ACO 1763).[3][4]
Characteristics
4C +41.26 is one of the largest galaxies. Spanning at least 862,300 light-years across in diameter, it is classfied as a Type-cD galaxy.[5] Not to mention, the galaxy has a high line-of-sight peculiar velocity reaching up to vpec ~ 650 km s-1. It has an active galactic nucleus, containing a powerful P1.4 ~ 1026 W Hz-1 bended double-lobed radio source, suggesting 4C +41.26 is likely shaped through its relative bulk intracluster medium (ICM) flow caused by one or several galaxy mergers.[6][7] The galaxy is estimated to have span MK = −25.7 to −27.8 mag, with the cluster halo masses of M500 up to 1.7 × 1015 M⊙.[8]
4C +41.26 is part of the rich galaxy cluster[9] with at least 181 identified galaxy members, fitted through the integrated spectral energy distributions (SEDs)[10] utilized with a set of templates built with GRASIL 3d model,[11] by astronomers.[12] The members in the cluster consists of elliptical, spiral, starburst, and poststarburst galaxies.[13] It is suggested according to observations from Spitzler MIPS Data, researchers have found traces of increased starburst activity in filament galaxies inside ACO 1763.[9]
The cluster hosts two galaxy filaments which stretches towards another neighboring galaxy cluster, Abell 1770 (ACO 1770) located ~ 13 Mpc away. The intracluster gas of ACO 1770 is elongated in the same direction, as indicated by its X-ray morphology. As the cluster is fed by the filaments, it causes 4C +41.26 to be displaced from its original location from center of the cluster (0.1 Mpc off the X-ray peak emission) by the subcluster-cluster collisions and pressure of the intracluster gas. This results the galaxy falling towards Abell 1770.[14]
See also
References
- ^ "HyperLeda -object description". atlas.obs-hp.fr. Retrieved 2024-05-26.
- ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-05-26.
- ^ "A 20 Centimeter VLA Survey of Abell Clusters of Galaxies. VII. Detailed Radio Images". THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES. doi:10.1086/312954/fulltext/.
- ^ Edwards, Louise O. V.; Fadda, Dario; Biviano, Andrea; Marleau, Francine R. (2010-02-01). "Spitzer Observations of Abell 1763. I. Infrared and Optical Photometry". The Astronomical Journal. 139: 434–446. doi:10.1088/0004-6256/139/2/434. ISSN 0004-6256.
- ^ Tonry, John L. (1987-01-01). "Properties of CD galaxies". 127: 89–98. doi:10.1007/978-94-009-3971-4_7.
{{cite journal}}: Cite journal requires|journal=(help) - ^ Douglass, E. M.; Blanton, E. L.; Randall, S. W.; Clarke, T. E.; Edwards, L. O. V.; Sabry, Z.; ZuHone, J. A. (2018-12-01). "The Megaparsec-scale Gas-sloshing Spiral in the Remnant Cool Core Cluster Abell 1763". The Astrophysical Journal. 868 (2): 121. doi:10.3847/1538-4357/aae9e7. ISSN 0004-637X.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ 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.
- ^ Loubser, S I; Hoekstra, H; Babul, A; O'Sullivan, E. "Diversity in the stellar velocity dispersion profiles of a large sample of brightest cluster galaxies z ≤ 0.3". academic.oup.com. Retrieved 2024-05-26.
- ^ a b Edwards, Louise O. V.; Fadda, D.; Frayer, D. (2009-05-01). "A Multiwavelegnth Study Of the Galaxy Cluster Abell 1763 and its Starforming Filament". 214: 307.01.
{{cite journal}}: Cite journal requires|journal=(help) - ^ "Fitting the Integrated SEDs of Galaxies - C.J. Walcher et al". ned.ipac.caltech.edu. Retrieved 2024-05-26.
- ^ Domínguez-Tenreiro, R.; Obreja, A.; Granato, G. L.; Schurer, A.; Alpresa, P.; Silva, L.; Brook, C. B.; Serna, A. "GRASIL-3D: an implementation of dust effects in the SEDs of simulated galaxies". academic.oup.com. Retrieved 2024-05-26.
- ^ Silva, Laura; Granato, Gian Luigi; Bressan, Alessandro; Danese, Luigi (1998-12-01). "Modeling the Effects of Dust on Galactic Spectral Energy Distributions from the Ultraviolet to the Millimeter Band". The Astrophysical Journal. 509: 103–117. doi:10.1086/306476. ISSN 0004-637X.
- ^ Biviano, A.; Metcalfe, L.; McBreen, B.; Altieri, B.; Coia, D.; Kessler, M. F.; Kneib, J. -P.; Leech, K.; Okumura, K.; Ott, S.; Perez-Martinez, R.; Sanchez-Fernandez, C.; Schulz, B. (2004-10-01). "An ISOCAM survey through gravitationally lensing galaxy clusters. II. The properties of infrared galaxies in the A2218 field". Astronomy and Astrophysics. 425: 33–49. doi:10.1051/0004-6361:20040385. ISSN 0004-6361.
- ^ Fadda, Dario; Biviano, Andrea; Marleau, Francine R.; Storrie-Lombardi, Lisa J.; Durret, Florence. "Starburst Galaxies in Cluster-feeding Filaments Unveiled by Spitzer". The Astrophysical Journal. doi:10.1086/526457/fulltext/22289.text.html.