4C +03.10

Quasar in the constellation Orion
4C +03.10
4C +03.10 (above), as seen by DESI Legacy Surveys
Observation data (J2000.0 epoch)
ConstellationOrion
Right ascension05h 07m 36.46s
Declination+03d 07m 52.27s
Redshift2.460000
Heliocentric radial velocity737,490 km/s
Distance10.655 Gly (light travel time distance)
Apparent magnitude (V)0.180
Apparent magnitude (B)0.239
Surface brightness18.57
Other designations
PGC 2818460, NVSS J050736+030752, MRC 0504+30, OG +008, PMN J0507+0307, TXS 0504+030, 87GB 050456.7+030358, PKS J0507+307

4C +03.10 also known as PKS 0505+03 and OG +008, is a quasar located in the constellation of Orion. At a redshift of 2.46, the object is located 10.6 billion light-years away from Earth.[1][2]

Characteristics

4C +03.10 produces a powerful astrophysical jet.[3] It is an active core-dominated radio-loud quasar displaying signs of radio emission with a smaller radio morphology compared to steep-spectrum quasars and has a gamma ~ 4-7 jet axes.[4][5] But has steep-spectrum quasar characteristics with small widths of the C IV λ1549 and C III λ1909 line profiles, larger Mg II λ2800 equivalent widths, and small He II + O III/C IV intensity ratios.[6]

The quasar has an associated C IV absorbers found stronger than EWrest>=0.5 Å[7] and strong [O III] λ5007 lines.[8] It is among 20%-30% quasars that shows narrow ~1000 km s−1 emission in He II λ1640 with a special feature arising in its ionized halo associate with radio ejecta for objects or by cooling flows from clusters. In some cases, it is both.[9] Moreover, 4C +03.10, also contains a dampened Lyα absorber with a column density of NHI>=2×1020 atoms cm−2 with its frequency reaching a peak where the universe is 10%-30% of the present age with mass density of neutral gas of Ωg.[10]

The source of 4C +03.10 is known to be extremely luminous[11] according to observations by researchers who studied the Third and Fourth Cambridge Survey of radio sources between declination of -7° and +40 degrees[12] as well by Parkes Observatory.[13] It has a luminosity value of 1026 <P408 <1027 W Hz−1 and hints of an inverse correlation between the luminosity and size.[14] The source is known to flicker at 6-cm wavelength, caused by scintillation in the either interstellar or by near-source medium.[15]

Observations made by Very Large Array, found the extragalactic source is seen through a restricted celestial angular zone encompassing the Orion-Eridanus region of the Milky Way; this shows it has an extension of linear polarization with a small flux density.[16]

Observations of 4C +03.10

4C +03.10 contains a mass outflow rate of 6-700 M⊙ yr−1, which has blue-shifted velocities of a few hundred km s−1 and line widths reaching up to 1500 km s−1. According to researchers, the size of the ionized outflows is around ~2 kpc. The properties of the ionized outflows, mass outflow rate, momentum rate, and kinetic power in 4C +03.10 proves to be correlated with its luminosity from its active galactic nucleus (AGN). As the outflow increases, the AGN luminosity increases suggesting the surrounding gas is driven by fast outflows from radiation pressure, dependable by emitted luminosity.[17] Researchers theorized the outflows might be neutrino emitters.[18]

4C +03.10 has high metal enrichments. Researchers who studied Q0207-398, found out 4C +03.10 has sharp broad absorption lines allowing them to probe more in its high ionization regions. The N V λ1240/He II λ1640 ratio they measured is found to be ~1 for standard cloud properties. As for the intensity of the N V line, researchers found it sensitive to the abundance of the gas because there is plenty of nitrogen roughly the square of metallicity. The lowest metallicity capable of reproducing the N V spectrum in 4C +03.10 is Z ~ 5 Z_sun_, consistent to exist in the cores of early-type galaxies after rapid star formation. This shows similar properties in broad absorption-line quasars.[19]

The quasar was detected by Swift. Through observations, it is found X-ray bright with an average αox =1.39 ± 0.03; where αox is the power-law slope connecting the monochromatic flux at 2500 Å and at 2 keV, displaying hard X-ray spectra. Apart from that, the accretion luminosity of 4C +03.10 is between the ranges of 0.7 × 1046 erg s−1 and 5.2 × 1047 erg s−1. From its black hole mass, it is accreting at Eddington fractions of 0.1 ≲ L/LEdd ≲ 1.[20] Researchers who studied 4C +03.10, found the C iv λ 1549 broad-emission line is weak and anti-correlated with the Eddington ratio, a relation they referred it as a modified Baldwin effect (MBE). Based on MBE, it contains a high Eddington ratio.[21]

References

  1. ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-06-13.
  2. ^ Browne, L. W. A.; Savage, Ann (1977-06-01). "Redshifts of southern quasars - III". Monthly Notices of the Royal Astronomical Society. 179: 65P–68P. Bibcode:1977MNRAS.179P..65B. doi:10.1093/mnras/179.1.65P. ISSN 0035-8711.
  3. ^ 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.
  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. ^ Barthel, Peter D.; Vestergaard, Marianne; Lonsdale, Colin J. (2000-02-01). "Radio imaging of core-dominated high redshift quasars". Astronomy and Astrophysics. 354: 7–16. arXiv:astro-ph/9911474. Bibcode:2000A&A...354....7B. ISSN 0004-6361.
  6. ^ Corbin, Michael R. (1991-07-01). "The Emission-Line Properties of Steep Radio Spectrum Quasars". The Astrophysical Journal. 375: 503. Bibcode:1991ApJ...375..503C. doi:10.1086/170213. ISSN 0004-637X.
  7. ^ Vestergaard, M. (2003-12-01). "Occurrence and Global Properties of Narrow C IV λ1549 Å Absorption Lines in Moderate-Redshift Quasars". The Astrophysical Journal. 599 (1): 116–139. arXiv:astro-ph/0309550. Bibcode:2003ApJ...599..116V. doi:10.1086/379159. ISSN 0004-637X.
  8. ^ Netzer, H.; Shemmer, O.; Maiolino, R.; Oliva, E.; Croom, S.; Corbett, E.; di Fabrizio, L. (2004-10-01). "Near-Infrared Spectroscopy of High-Redshift Active Galactic Nuclei. II. Disappearing Narrow-Line Regions and the Role of Accretion". The Astrophysical Journal. 614 (2): 558–567. arXiv:astro-ph/0406560. Bibcode:2004ApJ...614..558N. doi:10.1086/423608. ISSN 0004-637X.
  9. ^ Corbin, Michael R.; Francis, Paul J. (1994-12-01). "The Emission-Line Properties of the QSO Population at z~2". The Astronomical Journal. 108: 2016. Bibcode:1994AJ....108.2016C. doi:10.1086/117214. ISSN 0004-6256.
  10. ^ Storrie-Lombardi, Lisa J.; Wolfe, Arthur M. (2000-11-10). "Surveys forz > 3 Damped Lyα Absorption Systems: The Evolution of Neutral Gas". The Astrophysical Journal. 543 (2): 552–576. arXiv:astro-ph/0006044. Bibcode:2000ApJ...543..552S. doi:10.1086/317138. ISSN 0004-637X.
  11. ^ Schneider, Donald P.; Bahcall, John N.; Saxe, David H.; Bahcall, Neta A.; Doxsey, Rodger; Golombek, Daniel; Krist, John; McMaster, Matt; Meakes, Michael; Lahav, Ofer (1992-08-01). "Accurate Positions and Finding Charts for 528 High-Redshift, Luminous Quasars". Publications of the Astronomical Society of the Pacific. 104: 678. Bibcode:1992PASP..104..678S. doi:10.1086/133037. ISSN 0004-6280.
  12. ^ Agnew, Duncan; Arp, Halton (1973-04-01). "A List of Quasi-Stellar Radio Sources and Quasi-Stellar Radio Source Candidates from the 3C and 4C Catalogs Between Declination -7° and +40°". Publications of the Astronomical Society of the Pacific. 85 (504): 162. Bibcode:1973PASP...85..162A. doi:10.1086/129427. ISSN 0004-6280.
  13. ^ McEwan, N. J.; Browne, I. W. A.; Crowther, J. H. (1975-01-01). "Accurate positions and indentifications for a complete sample of 341 radio sources from the Parkes ±4° survey". Memoirs of the Royal Astronomical Society. 80: 1. Bibcode:1975MmRAS..80....1M.
  14. ^ Singal, Ashok K. (1988-07-01). "Cosmic evolution of the physical sizes of extragalactic radio sourcesand their luminosity-size correlation". Monthly Notices of the Royal Astronomical Society. 233: 87–113. Bibcode:1988MNRAS.233...87S. doi:10.1093/mnras/233.1.87. ISSN 0035-8711.
  15. ^ Heeschen, D. S. (1984-08-01). "Flickering of extragalactic radio sources". The Astronomical Journal. 89: 1111–1123. Bibcode:1984AJ.....89.1111H. doi:10.1086/113608. ISSN 0004-6256.
  16. ^ MacLeod, J. M.; Vallee, J. P.; Broten, N. W. (1988-07-01). "Linear polarizations in selected celestial zones. The Orion-Eridanus area". Astronomy and Astrophysics Supplement Series. 74: 63–66. Bibcode:1988A&AS...74...63M. ISSN 0365-0138.
  17. ^ Carniani, S.; Marconi, A.; Maiolino, R.; Balmaverde, B.; Brusa, M.; Cano-Díaz, M.; Cicone, C.; Comastri, A.; Cresci, G.; Fiore, F.; Feruglio, C.; La Franca, F.; Mainieri, V.; Mannucci, F.; Nagao, T. (2015-08-01). "Ionised outflows in z ~ 2.4 quasar host galaxies". Astronomy and Astrophysics. 580: A102. arXiv:1506.03096. Bibcode:2015A&A...580A.102C. doi:10.1051/0004-6361/201526557. ISSN 0004-6361.
  18. ^ Padovani, P.; Turcati, A.; Resconi, E. (2018-07-01). "AGN outflows as neutrino sources: an observational test". Monthly Notices of the Royal Astronomical Society. 477 (3): 3469–3479. arXiv:1804.01386. Bibcode:2018MNRAS.477.3469P. doi:10.1093/mnras/sty877. ISSN 0035-8711.
  19. ^ Ferland, Gary J.; Baldwin, Jack A.; Korista, Kirk T.; Hamann, Fred; Carswell, R. F.; Phillips, Mark; Wilkes, Belinda; Williams, Robert E. (1996-04-01). "High Metal Enrichments in Luminous Quasars". The Astrophysical Journal. 461: 683. Bibcode:1996ApJ...461..683F. doi:10.1086/177094. ISSN 0004-637X.
  20. ^ Lawther, D.; Vestergaard, M.; Raimundo, S.; Grupe, D. (2017-06-01). "A catalogue of optical to X-ray spectral energy distributions of z ≈ 2 quasars observed with Swift - I. First results". Monthly Notices of the Royal Astronomical Society. 467 (4): 4674–4710. arXiv:1702.05444. Bibcode:2017MNRAS.467.4674L. doi:10.1093/mnras/stx423. ISSN 0035-8711.
  21. ^ Shemmer, Ohad; Lieber, Sara (2015-06-01). "Weak Emission-line Quasars in the Context of a Modified Baldwin Effect". The Astrophysical Journal. 805 (2): 124. arXiv:1503.07547. Bibcode:2015ApJ...805..124S. doi:10.1088/0004-637X/805/2/124. ISSN 0004-637X.
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