MRC 0406-244

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MRC 0406-244
ESO image of MRC 0406-244.jpg
MRC 0406-244, as seen by ESO
Observation data (J2000.0 epoch)
Constellation Eridanus
Right ascension 04h 08m 51.47s
Declination -24d 18m 16.47s
Redshift 2.440000
Heliocentric radial velocity 731,494 km/s
Distance 10.647 Gly (light travel time distance)
Apparent magnitude  (V)0.144
Apparent magnitude  (B)0.190
Surface brightness 22.4
Notable features Radio galaxy, seyfert galaxy, galaxy merger
Other designations
TN J0408-2418, PMN J0408-2418, PGC 2823818, NVSS J040851-241815, TXS 0406-244, LQAC 062-024 001, GLEAM J040851-241817

MRC 0406-244 also known as TN J0408-2418, is a radio galaxy producing an astrophysical jet, [1] located in the constellation of Eridanus. At its redshift of 2.44, it is roughly ten billion light years from Earth. [2]

Contents

Characteristics

MRC 0406-244 is one of the most powerful radio galaxies known date-to-date; it was studied extensively by the MRC/1 Jy radio source survey. [3] MRC 0406-244 is also classified a Seyfert type 2 galaxy, [4] [5] with a complex morphology featuring several components, including a point source with an extended nebular and continuum emission. [6] Moreover, it contains an ultra-deep spectrum radio source (USS). [7]

Host galaxy

The host galaxy of MRC 0406-244 is a dusty obscured massive early-type galaxy with a star formation of (M⋆ ~ 1011 M⊙). The galaxy also has a stellar disc, within the range of 3.5 to 8.2 kpc which is similar to coeval star-forming galaxies, which is found to be smooth. [6]

Galaxy merger

From recent Hubble Space Telescope (HST) images, researchers have found several bright clumps with figure-of-eight shapes elongated along the radio jet axis of MRC 0406–244. Further images reveal there is a spatially resolved continuum. It is associated with its southeastern component that is aligned with the radio axis, with a complex morphology, including a double nucleus and tidal tail features. [8] This suggests of a tidal origin, meaning a recent galaxy merger has taken place. [9] It is believed that galaxy merger plays a dominant role in which its supermassive black hole is fueled. [10] Signs show the black hole inside the center of MRC 0406–244, is growing at an exponential rate of hundreds to thousands of solar masses per year, so as the luminosity, turning it into a quasar. [11] [12]

Observation of MRC 0406-244

According from HST and ground-based multiwavelength observations of MRC 0406–244, [13] researchers found there are two distinct components, aligned with its radio source axis. One of them has the red optical-to-IR and blue ultraviolet colors, making it a characteristic of radio galaxies, while the other is red in all colors. From the Lyα image, a nebula in MRC 0406-244 is found to be 3'' × 5'' extent, confined to the range of azimuth angles with respect to the nucleus of 60° to either side. Another component is also found extending northwest with similar morphology seen in the HST images. [14]

Researchers also found the long axis of the Lyman-alpha emission that is 130° east of north in MRC 0406–244, aligns with the radio source. They found out, the total Ly flux is 1.2 × 10−14 ergs s−1 cm−2, equivalent to a luminosity of 1 × 1045 ergs s−1. 1 40% of this flux is within the 25 × 35 area that is measured in the spectrum. The peak surface brightness of the Ly emission is found to be 9.0 × 10−16 ergs s−1 cm−2 arcsec−2, and emission is detected down to a level of 1.5 × 10−16 ergs s−1 cm−2 arcsec−2. [14]

Radio Properties

A triple radio source found in MRC 0406–244, is amongst the most power radio sources known according to researchers. They noted that the radio source reaches up to luminosity of 1.2 × 1036 ergs s−1 Hz−1 at 1 GHz and radiating at 6.3 × 1045 ergs s−1 between 100 MHz and 100 GHz. This extends over 84 kpc between the hot spots of MRC 0406–244, which found to be steep and strongly curved. The spectral index of the radio source changes from 1.21 at 1 GHz to 1.49 at 16 GHz in the rest frame to flux densities at several frequencies between 408 MHz and 8.44 GHz. This radio core contains a spectral index of 0.80 ± 0.18 (between 4.7 and 8.4 GHz, observed) that contributes the total emission at 15 GHz at 2%. [14]

The two radio lobes in MRC 0406-244 are notable for their degree of asymmetry. Given the asymmetries in arm length and the spectral indices in powerful sources, they are both related both intrinsic asymmetries and light travel-time differences. From the correlation between emission-line and radio asymmetries in other 3CR radio galaxies, [15] this suggests dominance of environmental effects, which cosmic dust plays a main role in correlation of optical and radio asymmetries. [14]

Gas and dust beyond MRC 0406-244

Further observations from researchers found, that nebular and continuum ultraviolet light extends up to 25 kpc from the nucleus of the galaxy. This is six times more than the length of the minor axis in the direction of the radio jets. Both extended components are shown to contribute to the alignment effect given their distribution is biconical along the jet axis. [16] [17] The dust at similarly large radii is known to exist, given the diffuse blue continuum is dust-scattered from active galactic nucleus light or from dust-reddened young stars. The dust must had probably originated in the galaxy, hence the outflow of both metal-rich gas and dust is important for enriching the intracluster medium.

The nebular gas can be driven out from MRC 0406–244 in two ways. One, either through expanding starburst bubbles. [18] Two, by overpressurized cocoons of material that is surrounding the expanding radio jets. [19] The dust grains are likely destroyed when interacting with powerful radio jets, so they instead transported by radiation pressure [20] or supernovae induced winds. [21]

Dust in the intergalactic medium has theorized for a long time, but detected only recently. From the study published by Ménard et al. (2010), it is suggested half of the cosmic dust lies within galaxies, whilst the other half is expelled to the intergalactic medium. [22] The extended light in MRC 0406−244 allows researchers, a rare opportunity to observe the dust in the midst of leaving the galaxy. As the host galaxy of MRC 0406−244 does not have different characteristics compared to other massive star-forming galaxies, it is possible that many highly star-forming galaxies lying at a similar redshift also expels out similar amounts of dust in bipolar outflows. The dust remains invisible unless it gets illuminated through sufficiently bright active galactic nuclei or through feedback driven star formations. If such dusty outflows in MRC 0406-244 is common, then researchers are expected to see ultraviolet-bright emission along the minor axis of stacked images of starbursting active galactic nuclei. [6]

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References

  1. ↑ Liu, F. K.; Zhang, Y. H. (2002-01-01). "A new list of extra-galactic radio jets". Astronomy and Astrophysics. 381 (3): 757–760. arXiv: astro-ph/0212477 . Bibcode:2002A&A...381..757L. doi:10.1051/0004-6361:20011572. ISSN   0004-6361.
  2. ↑ "NED Search Results for LQAC 062-024 001". NASA/IPAC Extragalactic Database.
  3. ↑ McCarthy, P. J.; van Breughel, W.; Kapahi, V. K.; Subrahmanya, C. R. (1991-08-01). "High Redshift Radio Galaxies From the Molonglo Catalogue.II". The Astronomical Journal. 102: 522. Bibcode:1991AJ....102..522M. doi:10.1086/115891. ISSN   0004-6256.
  4. ↑ Véron-Cetty, M. -P.; Véron, P. (2006-08-01). "A catalogue of quasars and active nuclei: 12th edition". Astronomy and Astrophysics. 455 (2): 773–777. Bibcode:2006A&A...455..773V. doi:10.1051/0004-6361:20065177. ISSN   0004-6361.
  5. ↑ Kruper, J. S.; Urry, C. M.; Canizares, C. R. (1990-10-01). "Soft X-Ray Properties of Seyfert Galaxies. I. Spectra". The Astrophysical Journal Supplement Series. 74: 347. Bibcode:1990ApJS...74..347K. doi:10.1086/191503. ISSN   0067-0049.
  6. 1 2 3 Hatch, N. A.; Röttgering, H. J. A.; Miley, G. K.; Rigby, E.; De Breuck, C. "The host galaxy of the z = 2.4 radio-loud AGN MRC 0406−244 as seen by HST". academic.oup.com. Retrieved 2024-05-31.
  7. ↑ De Breuck, C.; van Breugel, W.; Röttgering, H. J. A.; Miley, G. (2000-04-01). "A sample of 669 ultra steep spectrum radio sources to find high redshift radio galaxies". Astronomy and Astrophysics Supplement Series. 143 (2): 303–333. arXiv: astro-ph/0002297 . Bibcode:2000A&AS..143..303D. doi:10.1051/aas:2000181. ISSN   0365-0138.
  8. ↑ Rush, Brian; McCarthy, Patrick J.; Athreya, Ramana M.; Persson, S. E. (1997-07-20). "The High-Redshift Radio Galaxy MRC 0406−244". The Astrophysical Journal. 484 (1): 163–179. Bibcode:1997ApJ...484..163R. doi:10.1086/304307. ISSN   0004-637X.
  9. ↑ Pentericci, L.; McCarthy, P. J.; Röttgering, H. J. A.; Miley, G. K.; Breugel, W. J. M. van; Fosbury, R. (2001-07-01). "NICMOS Observations of High-Redshift Radio Galaxies:Witnessing the Formation of Bright Elliptical Galaxies?". The Astrophysical Journal Supplement Series. 135 (1): 63. arXiv: astro-ph/0102323 . Bibcode:2001ApJS..135...63P. doi:10.1086/321781. ISSN   0067-0049.
  10. ↑ Ivison, R. J.; Smail, Ian; Amblard, A.; Arumugam, V.; Breuck, C. De. "Gas-rich mergers and feedback are ubiquitous amongst starbursting radio galaxies, as revealed by the VLA, IRAM PdBI and Herschel". academic.oup.com. Retrieved 2024-05-31.
  11. ↑ Barthel, Peter; Haas, Martin; Leipski, Christian; Wilkes, Belinda (2012-10-01). "Extreme Host Galaxy Growth in Powerful Early-epoch Radio Galaxies". The Astrophysical Journal. 757 (2): L26. arXiv: 1209.0324 . Bibcode:2012ApJ...757L..26B. doi:10.1088/2041-8205/757/2/L26. ISSN   0004-637X.
  12. ↑ Seymour, N.; Altieri, B.; De Breuck, C.; Barthel, P.; Coia, D.; Conversi, L.; Dannerbauer, H.; Dey, A.; Dickinson, M.; Drouart, G.; Galametz, A.; Greve, T. R.; Haas, M.; Hatch, N.; Ibar, E. (2012-08-01). "Rapid Coeval Black Hole and Host Galaxy Growth in MRC 1138-262: The Hungry Spider". The Astrophysical Journal. 755 (2): 146. arXiv: 1206.5821 . Bibcode:2012ApJ...755..146S. doi:10.1088/0004-637X/755/2/146. ISSN   0004-637X.
  13. ↑ information@eso.org. "Radio galaxy MRC 0406-244". www.eso.org. Retrieved 2024-05-31.
  14. 1 2 3 4 Rush, Brian; J. McCarthy, Patrick; M. Athreya, Ramana; Persson, S. E. (1997). "The High-Redshift Radio Galaxy MRC 0406-244". The Astrophysical Journal. 484 (1). Bibcode:1997ApJ...484..163R. doi:10.1086/304307.
  15. ↑ McCarthy, Patrick J.; van Breugel, Wil; Kapahi, Vijay K. (1991-04-01). "Correlated Radio and Optical Asymmetries in Powerful Radio Sources". The Astrophysical Journal. 371: 478. Bibcode:1991ApJ...371..478M. doi:10.1086/169911. ISSN   0004-637X.
  16. ↑ Chambers, K. C.; Miley, G. K.; van Breugel, W. (1987). "Alignment of radio and optical orientations in high-redshift radio galaxies". Nature. 329 (6140) 329604a0: 604–606. Bibcode:1987Natur.329..604C. doi:10.1038/329604a0.
  17. ↑ McCarthy, Patrick J.; van Breugel, Wil; Spinrad, Hyron; Djorgovski, S. (1987-10-01). "A Correlation between the Radio and Optical Morphologies of Distant 3 CR Radio Galaxies". The Astrophysical Journal. 321: L29. Bibcode:1987ApJ...321L..29M. doi:10.1086/185000. ISSN   0004-637X.
  18. ↑ Humphrey, A.; Villar-Martín, M.; Vernet, J.; Fosbury, R.; di Serego Alighieri, S.; Binette, L. (2008-01-01). "Deep spectroscopy of the FUV-optical emission lines from a sample of radio galaxies at z ~ 2.5: metallicity and ionization". Monthly Notices of the Royal Astronomical Society. 383 (1): 11–40. arXiv: 0710.5324 . Bibcode:2008MNRAS.383...11H. doi: 10.1111/j.1365-2966.2007.12506.x . ISSN   0035-8711.
  19. ↑ Nesvadba, N. P. H.; Lehnert, M. D.; De Breuck, C.; Gilbert, A. M.; van Breugel, W. (2008-11-01). "Evidence for powerful AGN winds at high redshift: dynamics of galactic outflows in radio galaxies during the Quasar Era". Astronomy and Astrophysics. 491 (2): 407–424. arXiv: 0809.5171 . Bibcode:2008A&A...491..407N. doi:10.1051/0004-6361:200810346. ISSN   0004-6361.
  20. ↑ Watabe, Y.; Risaliti, G.; Salvati, M.; Nardini, E.; Sani, E.; Marconi, A. (2009-06-01). "The active galactic nuclei/starburst content in high-redshift ultraluminous infrared galaxies". Monthly Notices of the Royal Astronomical Society. 396 (1): L1–L5. arXiv: 0903.0299 . Bibcode:2009MNRAS.396L...1W. doi: 10.1111/j.1745-3933.2009.00649.x . ISSN   0035-8711.
  21. ↑ Low, Mordecai-Mark Mac; Ferrara, Andrea (1999-03-01). "Starburst-driven Mass Loss from Dwarf Galaxies: Efficiency and Metal Ejection". The Astrophysical Journal. 513 (1): 142. arXiv: astro-ph/9801237 . Bibcode:1999ApJ...513..142M. doi:10.1086/306832. ISSN   0004-637X.
  22. ↑ Ménard, Brice; Scranton, Ryan; Fukugita, Masataka; Richards, Gordon (2010-06-01). "Measuring the galaxy-mass and galaxy-dust correlations through magnification and reddening". Monthly Notices of the Royal Astronomical Society. 405 (2): 1025–1039. arXiv: 0902.4240 . Bibcode:2010MNRAS.405.1025M. doi: 10.1111/j.1365-2966.2010.16486.x . ISSN   0035-8711.
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