Astronomy:SDSS J2358−0009

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SDSS J2358−0009
The Type 2 quasar SDSS J2358−0009
Observation data (J2000.0 epoch)
ConstellationPisces
Right ascension 23h 58m 18.91s[1]
Declination−00° 09′ 19.10″[1]
Redshift0.402520[1]
Helio radial velocity120,672 ± 5 km/s[1]
Distance5,810.2 ± 406.7 Mly (1,781.43 ± 124.70 Mpc)[1]
Apparent magnitude (B)20.88
Characteristics
TypeType 2 quasar
Other designations
SDSS J235818.87−000919.5, QSO J2358−0009, [VV2006c] J235818.9−000919, LEDA 3420293

SDSS J2358−0009 also known as SDSS J2358−00, is a Type 2 quasar located in the constellation of Pisces. The redshift of the object is (z) 0.402[1] and it was first discovered by astronomers in November 2006 from the Sloan Digital Sky Survey (SDSS).[2]

Description

SDSS J2358−0009 is a Type 2 quasar with an estimated doubly ionized oxygen [O III] emission line luminosity of 9.96 Lʘ based on observations made by Chandra X-ray Observatory.[3][4] The host galaxy of the quasar imaged by Hubble Space Telescope (HST) is found interacting with a companion star-forming galaxy located at a projected distance of 29 kiloparsecs, with presence of tidal tails and shell-like structures east of the host's nucleus.[5][6] Further evidence also found the tidal tail of the companion is also shown linking with another companion at an unknown redshift. There is an elongated knot feature located 30 kiloparsecs east from the host, with a knotty internal substructure and mainly being dominated by continuum radio emission.[6] A tidal bridge with a surface brightness of 22.7 magnitude is seen linking between the host and the companion.[7]

A study found the quasar is compton-thick based on its [O III] luminosity ratio.[3] An extended emission-line region (EELR) is present with the extended ionized nebula shown being photoionized by the quasar. The nebula has maximum size of 64 kiloparsecs while the EELR luminosity is found to be 5.1 ± 0.1 × 1041 erg s-1.[6] There are also detections of ionized outflows from the quasar with the [O III] lines displaying a full width at half maximum of 440 ± 50. The [O III] lines are described to have no profile asymmetries, with the lines having an [O III] flux of 75 ± 6 × 1016 erg-1 s-2. The velocity shift in relative to the [O III] narrow core component is 10 ± 40 kilometers per seconds.[8] Young stellar populations has also been detected inside the quasar contributing between 88% and 95% of the flux, with the population estimated to be 0.04-0.05 billion years.[9]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 "NED Search results for SDSS J2358−0009". https://ned.ipac.caltech.edu/byname?objname=SDSS+J235818.87-000919.5&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ Zakamska, N.L.; Strauss, M.A.; Krolik, J.H.; Ridgway, S.E.; Schmidt, G.D.; Smith, P.S.; Hao, L.; Heckman, T.M. et al. (November 2006). "Hosts of type II quasars: An HST study". New Astronomy Reviews 50 (9–10): 833–836. doi:10.1016/j.newar.2006.06.048. ISSN 1387-6473. Bibcode: 2006NewAR..50..833Z. 
  3. ↑ 3.0 3.1 Vignali, C.; Alexander, D. M.; Gilli, R.; Pozzi, F. (February 2010). "Discovery of Compton-thick quasars in the Sloan Digital Sky Survey". Monthly Notices of the Royal Astronomical Society 404 (1): 48. doi:10.1111/j.1365-2966.2010.16275.x. ISSN 0035-8711. Bibcode: 2010MNRAS.404...48V. 
  4. ↑ Vignali, C.; Alexander, D. M.; Comastri, A. (2006-11-21). "The quest for Type 2 quasars: Chandra observations of luminous obscured quasars in the Sloan Digital Sky Survey". Monthly Notices of the Royal Astronomical Society 373 (1): 321–329. doi:10.1111/j.1365-2966.2006.11033.x. ISSN 0035-8711. Bibcode: 2006MNRAS.373..321V. https://articles.adsabs.harvard.edu/pdf/2006MNRAS.373..321V. 
  5. ↑ Zakamska, Nadia L.; Strauss, Michael A.; Krolik, Julian H.; Ridgway, Susan E.; Schmidt, Gary D.; Smith, Paul S.; Heckman, Timothy M.; Schneider, Donald P. et al. (2006-08-31). "Type II Quasars from the Sloan Digital Sky Survey. V. Imaging Host Galaxies with the Hubble Space Telescope". The Astronomical Journal 132 (4): 1496–1516. doi:10.1086/506986. ISSN 0004-6256. Bibcode: 2006AJ....132.1496Z. https://iopscience.iop.org/article/10.1086/506986/pdf. 
  6. ↑ 6.0 6.1 6.2 Villar-Martín, M.; Tadhunter, C.; Humphrey, A.; Encina, R. Fraga; Delgado, R. González; Torres, M. Pérez; Martínez-Sansigre, A. (June 2011). "Interactions, star formation and extended nebulae in SDSS type 2 quasars at 0.3 ≤ z ≤ 0.6". Monthly Notices of the Royal Astronomical Society: no. doi:10.1111/j.1365-2966.2011.19031.x. ISSN 0035-8711. https://academic.oup.com/mnras/article/416/1/262/1209871#20674761. 
  7. ↑ Bessiere, P. S.; Tadhunter, C. N.; Ramos Almeida, C.; Villar Martín, M. (2012-09-12). "The importance of galaxy interactions in triggering type II quasar activity". Monthly Notices of the Royal Astronomical Society 426 (1): 276–295. doi:10.1111/j.1365-2966.2012.21701.x. ISSN 0035-8711. Bibcode: 2012MNRAS.426..276B. 
  8. ↑ Villar-Martín, M.; Humphrey, A.; Delgado, R. González; Colina, L.; Arribas, S. (2011-09-29). "Ionized outflows in SDSS type 2 quasars at z ∼ 0.3-0.6". Monthly Notices of the Royal Astronomical Society 418 (3): 2032–2042. doi:10.1111/j.1365-2966.2011.19622.x. ISSN 0035-8711. Bibcode: 2011MNRAS.418.2032V. 
  9. ↑ Bessiere, P. S.; Tadhunter, C. N.; Ramos Almeida, C.; Villar Martín, M.; Cabrera-Lavers, A. (2016-12-09). "Young stellar populations in type II quasars: timing the onset of star formation and nuclear activity". Monthly Notices of the Royal Astronomical Society 466 (4): 3887–3917. doi:10.1093/mnras/stw3175. ISSN 0035-8711. https://academic.oup.com/mnras/article/466/4/3887/2666368#62746809. 



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