PKS 2338+000

PKS 2338+000
PKS 2338+000, as seen by DESI Legacy Surveys
Observation data (J2000.0 epoch)
ConstellationPisces
Right ascension23h 41m 06.91s
Declination+00d 18m 33.35s
Redshift0.276720
Heliocentric radial velocity82,959 km/s
Distance3.550 Gly (1088.4 Mpc)
Group or clusterRX J2341.1+0018
Apparent magnitude (V)0.077
Apparent magnitude (B)0.102
Surface brightness18.2
Characteristics
TypeEllip;BrCLG, NLAGN
Size667,000 ly
Apparent size (V)0.21' x 0.17'
Notable featuresRadio galaxy, brightest cluster galaxy
Other designations
NVSS JJ234106+001833, TXS 2338+000, PGC 1162543, SDSS J234106.90+001833.3, 2MASX J23410687+0018332, OGC 123, PKS J2341+0018, 87GB 233833.1+000149

PKS 2338+000 also known as PGC 1162543 and OGC 123, is a massive type-cD elliptical galaxy located in the constellation of Pisces. With a redshift of 0.276, the galaxy is located 3.5 billion light-years from Earth.[1] The galaxy is the brightest cluster galaxy inside the galaxy cluster RX J2341+0018 which is a rich cluster,[2] X-ray luminous.[3]

Characteristics

PKS 2338+000 is one of the largest galaxies. With a diameter spanning 667,000 light-years across, the galaxy is visually luminous[4] with a radio-loud nucleus scintillating than 5mJy at 1.4 GHz.[5] It is a Seyfert 2 galaxy with narrow-lines that has a measurement of ~ 102 km s−1.[6][7] PKS 2338+000 is a blazar,[8][9] an active galaxy type. Such blazars show powerful emission across its electromagnetic spectrum. It is found to the strongest active galactic nucleus (AGN) in its core.[10] The radio jet of PKS 2338+000 is accurate is below 10°parsec-scale .[11] The radio source in PKS 2338+000 on the other hand, is measured 150 GHz of 3 mJy ≈1×1023 W Hz−1[12] and of extragalactic origin.[13] Moreover, the source is of flat-spectrum type.[14][15]

A low-excitation radio galaxy with 1.4 GHz luminosity between 2 × 1023 and 3 × 1025 W Hz−1, PKS 2338+000 relies on its own halo mass.[16] Notably, the radio galaxy is quite young with an age estimated < 103 yr. When studied by Chandra and Multi-unit spectroscopic explorer (MUSE), the blistering gas are yet to meet expectations of cooled intracluster medium, of which the entropy and cooling time for the pre-feedback cluster located 20 kpc from the main cluster falls below mature-feedback clusters with a factor of ~2. As for the mechanical power of PKS 2338+000 is gauged to be ~1044 − 1045 erg s−1, suggesting entropy levels would be reinstituted within a few million years.[17]

PKS 2338+000 has a twin-peaked narrow emission line and a binary core.[18] It is theorized as the brightest cluster galaxy, PKS 2338+000 might have been formed from melding of smaller spiral and elliptical galaxies.[19] When these galaxies collide with each other, tidal forces and dynamical friction divides kinetic energy into random form of energies, allowing these galaxies to merge together into a formless, triaxial system resembling a giant elliptical galaxy like PKS 2338+000.[20][21]

Researchers found strong Hα and [O II] λ3727 emission lines inside the optical spectra.[22] Despite being red and dead galaxy, the star formation rate in PKS 2338+000 is under way, mainly being inhabited by a distinctive cluster environment that leads up to self-regulated feedback cycle between the cooling process of interstellar medium and by the activity.[23]

Rotational measure

PKS 2338+000 has a exorbitant rotational measure. When researchers used a multifrequency single-dish observation with a 100-m Effelsberg telescope, the values of the rotational measure in PKS 2338+000 is found to have a rest frame that is significant compared to rest frame 1000 rad/m2. This means a vigorous depolarisation at 21 cm and existence of dense medium encircling the galaxy with powerful magnetic fields.[24]

Molecular gas content

Researchers also evaluated the role of radio activity in PKS 2338+000. To conduct the investigation, a massive carbon oxide (CO) survey of similar radio galaxies (RGs) like PKS 2338+000, is conducted to control the galaxies' molecular gas mass at different epochs. They used a sample of 120 RGs representative of the NVSS 1.4 GHz survey, which the flux is restricted at 0.4 Jy. Through the results at all epochs, the bulk of RGs have reservoirs found unnoticeable. Researchers also saw a swift increase in the H2 mass content of the CO-detected RGs at redshifts. At 1 < z < 2.5, one-fourth of the RGs including PKS 2338+000 have a high concentration of molecular gas due to simulations indicating a particular halo mass of the epoch. Such galaxies have the likelihood of being "normal" or even starburst hosts. Overall, the estimated molecular gas reservoirs for PKS 2338+000 is 107 ≲ MH2 ≲ 1010 M⊙. This a fraction lower of ~4, in prepositional to type 1 and 2 AGN both pure and with less star formations, like the simulations.[25]

H I absorption

PKS 2338+000 has a large kpc size radio source that is ten times more than expected. The source is estimated to be in the radio-power range of 1025.7 W Hz−1-1026.5 W Hz−1 and interconnected with the H I absorption in the region. According to researchers who detected H I absorption in the radio source of PKS 2338+000, the radio continuum emission is found unresolved at ~5 to 10 kpc when observed, but has an enlarged structure. Analyzing the H I 21 cm absorption spectra of the detection to understand the morphology and kinematics of H I, researchers found the absorption profiles are compounded of widths between nulls spanning from ~60 km s−1 to 700 km s−1. The detections found, exhibits an astounding high H I column density in the range ~1021/cm2-1022/cm2 for Tspin = 100 K with a unit covering factor. The modelling of the absorption profile according to researchers, found a large part of absorption is compatible with absorption emerging from an H I disc. Despite showing strong radio power in PKS 2338+000, they failed to detect fast outflows. However, the optical emission lines shows occupancy of disturbed gas in nuclear regions that has forms of wide and high blueshifted emission-line components. Since these detections are considered low-ionisation, it is possible the interruption of gas is caused by the galaxy's own radio jets.[26]

References

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