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2MASX J10222849+5006200
2MASX J10222849+5006200 captured by SDSS
Observation data (J2000.0 epoch)
ConstellationUrsa Major
Right ascension10h 22m 28.44s
Declination+50d 06m 19.83s
Redshift0.158413
Heliocentric radial velocity47,491 km/s
Distance2.455 Gly (752.7 Mpc)
Group or clusterAbell 980
Apparent magnitude (V)0.031
Apparent magnitude (B)0.041
Surface brightness17.5
Characteristics
TypeBrCLG
Apparent size (V)0.44' x 0.28'
Notable featuresOldest fossil radio galaxy containing double radio lobes
Other designations
OGC 286, PGC 2362940, NVSS J102228+500620, SDSS J102228.44+500619.8, CXOGSG J102228.4+500619, RX J1022.4+5006:[ZEH2003] 04

2MASX J10222849+5006200 also known as PGC 2362940, is a massive Type-cD elliptical galaxy located in the constellation of Ursa Major. With the redshift of 0.15, the galaxy is located 2.4 billion light-years away from Earth.[1] It is the brightest cluster galaxy (BCG) inside the galaxy cluster, Abell 980.

Characteristics

2MASX J10222849+5006200 is an optically luminous galaxy with an r-band luminosity of L r > 8L*[2] with a powerful radio source.[3] It is a low-excitation radio galaxy with a 1.4 GHz luminosity range between 2 × 1023 and 3 × 1025 W Hz-1[4] featuring a hybrid of both Fanaroff-Riley (FR) I and FR II sources.[5] The galaxy is a red elliptical galaxy, known to have radio-loud active galactic nucleus with an old stellar population dominating at high stellar mass of M > 1010.5-10.8~M⊙,[6] following an fLE_RL ∝ M^{2.5_* power law of 3.[7] It also exhibits a strong, distinguishable core component correlating with its [O III] 5007 Å line emission, suggesting the galaxy's active galactic nucleus is steadily fueled over the bubble-rise time-scales.[8]

Like all giant elliptical galaxies inhabiting the center of such clusters, 2MASX J10222849+5006200 is found to have a central velocity dispersions in the range of α ~ 300-400 km s-1,[9] which is found to have a tight relation between the BCG itself and its parent cluster velocity dispersion.[10][11] The galaxy also has a light profile, over a large range in radius as described by a de Vaucouleurs surface brightness law, μ(r) α r1/4.[12] In addition, 2MASX J10222849+5006200 has an extended envelope of excess light fitted to its inner regions[13] reaching up to several hundreds of kiloparsecs.[14]

It is suggested 2MASX J10222849+5006200 was formed through mergers of smaller spiral galaxies or ellipticals.[15][16] As these galaxies collide with each other, the process of dynamic friction combined together with tidal forces, then redistributes kinetic energy into random form of energy, allowing these galaxies to form an amorphous, triaxial system resembling an elliptical galaxy like 2MASX J10222849+5006200.[17][18] Eventually the galaxy settles to become a BCG in the cluster, as the it undergoes a process of galactic cannibalism through assimilating surrounding satellite galaxies and causing it to have high luminosity.[19] As the process continues, the mass of the central galaxy is built-up, while the number of satellite galaxies becomes lesser.[20]

Radio lobes

According to Indian researchers led by Surajit Paul from the Savitribai Phule Pune University, the radio lobes in 2MASX J10222849+5006200 are the oldest of the kind they ever seen, having being formed 260 million years ago. This discovery by researchers makes 2MASX J10222849+5006200 the oldest fossil radio galaxy found. They also found a secondary pair of younger radio lobes, whom they traced to the same galaxy making 2MASX J10222849+5006200 a rare example to contain double pair of lobes, indicating its supermassive black hole is erupting episodically.[21]

Through the LoFAR Two meter Sky Survey data release 2 (LoTSS-2 at 144 MHz), Giant Meterwave radio Telescope (GMRT) and Very Large Array (VLA) observations at higher frequencies, researchers also found the double radio lobes are both produced by 2MASX J10222849+5006200 in two major episodes of radio jet activity. Lobes that were left from pervious activity, have became diffused and developed ultra-steep spectrum (USS) sources as it rises buoyantly through the confined hot intracluster medium (ICM).[22] The USS sources at point A and point B are found diffused and have moderate luminosities of ∼3.7 × 1024 W Hz−1 and ∼1.4 × 1024 W Hz−1 at 325 MHz respectively hinting the relic lobes of radio galaxies like 2MASX J10222849+5006200 are no longer active.[23][24] Concomitantly, the host galaxy has drifted towards the cluster center with a measured required drift velocity of ∼400 km s−1, not exceptional for BCGs,[25] in which it enters a new active phase manifested by a coinciding younger double radio source.[22]

From the new observational results and arguments presented by researchers, the old and young double radio sources in 2MASX J10222849+5006200 conjointly represent a `double-double' radio galaxy whose two lobe-pairs have lost their collinearity due to the lateral drift of their parent galaxy, hence making the system a plausible case of a `Detached-Double-Double Radio Galaxy' (dDDRG).[22]

In addition, the diffuse source is found to have radio mini-halo[26] of size ∼110 kpc around the BCG possessing a huge ellipsoidal stellar halo of extent ∼80 kpc and a flux density estimation of of 11.5 ± 1.3 mJy at 325 MHz, corresponding to a luminosity of 7.9 ± 0.9 × 1023 WHz−1 and a radio emissivity of 1.1 ± 0.2 × 10−40 ergs−1 cm−3 Hz−1 comparable to giant radio haloes in dying radio galaxies.[27] Looking at the cold fronts, highly aged (∼260 Myr), USS sources inside the cluster, this creates a rare system.[28]

Abell 980

The cluster where 2MASX J10222849+5006200 is residing, is found to be a rich cluster.[29] It was discovered in 1958 by George O. Abell whom he listed it as one of the original 2,712 galaxy clusters inside the Abell catalogue through retrived data from National Geographic Society - Palomar Observatory Sky Survey.[30]

Abell 980 is classified as a fossil galaxy group with an LX distribution in the 0.1-2.4 keV band, computed by using data from the ROSAT All Sky Survey[31] and located at z = 0.1582.[32] It is found to have a high Sunyaev-Zel'dovich of M SZ 500 = 4.73 +0.29 -0.32 x 1014 M⊙[33] and high X-ray luminosity of LX = 7.1 × 1044 erg s−1), with an average intracluster medium temperature of 7.1 keV.[34] By calculating the Westerbork Northern Sky Survey data at resolution of 54″ at 330 MHz, Abell 980 has a luminosity value of P330 MHz = 5.6 ± 1.3 × 1024 W Hz−1 at 330 MHz, with marginally resolved faint emission tha underlies a dominant radio peak.[35]

Furthermore, the intracluster medium in Abell 980 is said to have a quasi-relaxed appearance, with a cool core (ICM with T ∼ 4.2 keV) of size ∼100 kpc and surrounded by a large (∼500 kpc) hot gaseous halo (T ∼ 6.8 keV) with two brightness discontinuities.[28] As well, Abell 980 has a dark matter mass of 10-25-10-24 cm3 s-1 in the range of 10-100 GeV or a substructure configuration of <σv> ∼ 10-26 cm3 s-1 for a more favorable approach.[36] According to researchers who calculated the halo mass of Abell 980, it is found on average (1.99 ± 0.11)M 200, which is a new observational cosmological test in essential agreement with simulations.[37]

References

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