Astronomy:PDS 456

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PDS 456
The quasar PDS 456.
Observation data (J2000.0 epoch)
ConstellationSerpens
Right ascension 17h 28m 19.7906s
Declination−14° 15′ 55.816″
Redshift0.185000
Helio radial velocity55,462 km/s
Distance2.177 Gly
Apparent magnitude (V)14.03
Apparent magnitude (B)14.69
Characteristics
TypeQSO
Other designations
QSO B1725-142, IRAS 17254-1413, NVSS J172819-141555, 6dFGS J172819.8-141556

PDS 456 is a relatively nearby radio-quiet quasar located in the constellation of Serpens.[1] This is a luminous active galactic nucleus (AGN) with a redshift of (z) 0.184, first discovered by astronomers conducting the Pico dos Dias survey in 1997.[2][3][4] The object is known to have prototypical ionized ultra-fast X-ray outflows[5] and a bolometric luminosity value of 1047 erg s−1.[6][7][8]

Description

An extremely bright X-ray flare was detected from PDS 456 in September 2018. Based on observations, it showed a flux increase by a factor 4, including its time-scale doubling and a high level of flare energy, exceeding 1051 erg. In addition, PDS 456 also displayed X-ray emission hardening following the flare.[9] Radio images by very long baseline interferometry (VLBI) found PDS 456 has a complex nucleus described to be radio-emitting, an extended structure and a jet.[10]

In 2019, observations by the Atacama Large Millimeter Array (ALMA) found PDS 456 to contain kiloparsec-scale molecular outflows. The molecular outflows are estimated to have a mass of 2.5 x 108 Mʘ while a value of 290 Mʘ yr−1 was calculated for its outflow mass rate. Given its short depletion time, it is estimated the star-formation in PDS 456 would be quenched.[11]

Additionally, disk wind from the accretion disk[12] and signatures of highly ionized gas detected via X-ray broadband spectra of PDS 456, was also present.[13] A supermassive black hole mass of 109.2±0.2 Mʘ was estimated for the object.[10]

References

  1. ↑ Nowakowski, Tomasz; Phys.org. "Luminous quasar PDS 456 explored with MUSE" (in en). https://phys.org/news/2024-04-luminous-quasar-pds-explored-muse.html. 
  2. ↑ Behar, Ehud; Kaspi, Shai; Reeves, James; Turner, T. J.; Mushotzky, Richard; O'Brien, Paul T. (2010-02-24). "Remarkable Spectral Variability of PDS 456". The Astrophysical Journal 712 (1): 26–37. doi:10.1088/0004-637x/712/1/26. ISSN 0004-637X. Bibcode: 2010ApJ...712...26B. https://doi.org/10.1088/0004-637x/712/1/26. 
  3. ↑ A. O. Torres, Carlos; R. Quast, Germano; Coziol, Roger; Jablonski, Francisco; De La Reza, Ramiro (1997). "Discovery of a Luminous Quasar in the Nearby Universe". The Astrophysical Journal 488 (488): 19–22. doi:10.1086/310913. Bibcode: 1997ApJ...488L..19T. https://iopscience.iop.org/article/10.1086/310913/fulltext/975383.text.html. 
  4. ↑ Simpson, Chris; Ward, Martin; O'Brien, Paul; Reeves, James (February 1999). "Optical and infrared observations of the luminous quasar PDS 456: a radio-quiet analogue of 3C 273?". Monthly Notices of the Royal Astronomical Society 303 (2): L23–L28. doi:10.1046/j.1365-8711.1999.02344.x. ISSN 0035-8711. Bibcode: 1999MNRAS.303L..23S. 
  5. ↑ Hamann, Fred; Chartas, George; Reeves, James; Nardini, Emanuele (2018-01-17), "Does the X-ray outflow quasar PDS 456 have a UV outflow at 0.3c?", Monthly Notices of the Royal Astronomical Society 476: 943–953, doi:10.1093/mnras/sty043 
  6. ↑ Reeves, J. N.; O'Brien, P. T.; Vaughan, S.; Law-Green, D.; Ward, M.; Simpson, C.; Pounds, K. A.; Edelson, R. (2000-02-01). "PDS 456: an extreme accretion rate quasar?". Monthly Notices of the Royal Astronomical Society 312 (2): L17–L21. doi:10.1046/j.1365-8711.2000.03282.x. ISSN 0035-8711. Bibcode: 2000MNRAS.312L..17R. 
  7. ↑ Seebeck, Jerome; Veilleux, Sylvain; Liu, Weizhe; Rupke, David S. N.; Vayner, Andrey; Wylezalek, Dominika; Zakamska, Nadia L.; Bertemes, Caroline (2024-11-26). "Combined JWST–MUSE Integral Field Spectroscopy of the Most Luminous Quasar in the Local Universe, PDS 456". The Astrophysical Journal 976 (2): 240. doi:10.3847/1538-4357/ad815e. ISSN 0004-637X. Bibcode: 2024ApJ...976..240S. 
  8. ↑ Travascio, A.; Piconcelli, E.; Bischetti, M.; Cresci, G.; Feruglio, C.; Perna, M.; Vietri, G.; Carniani, S. et al. (June 2024). "MUSE view of PDS 456: Kiloparsec-scale wind, extended ionized gas, and close environment". Astronomy & Astrophysics 686: A250. doi:10.1051/0004-6361/202449201. ISSN 0004-6361. Bibcode: 2024A&A...686A.250T. https://doi.org/10.1051/0004-6361/202449201. 
  9. ↑ Reeves, J. N.; Braito, V.; Porquet, D.; Lobban, A. P.; Matzeu, G. A.; Nardini, E. (2021-01-01). "The flaring X-ray corona in the quasar PDS 456". Monthly Notices of the Royal Astronomical Society 500 (2): 1974–1991. doi:10.1093/mnras/staa3377. ISSN 0035-8711. Bibcode: 2021MNRAS.500.1974R. 
  10. ↑ 10.0 10.1 Yang, Jun; Paragi, Zsolt; Nardini, Emanuele; Baan, Willem A; Fan, Lulu; Mohan, Prashanth; Varenius, Eskil; An, Tao (2020-08-17). "The nearby extreme accretion and feedback system PDS 456: finding a complex radio-emitting nucleus". Monthly Notices of the Royal Astronomical Society 500 (2): 2620–2626. doi:10.1093/mnras/staa2445. ISSN 0035-8711. 
  11. ↑ Bischetti, M.; Piconcelli, E.; Feruglio, C.; Fiore, F.; Carniani, S.; Brusa, M.; Cicone, C.; Vignali, C. et al. (2019-08-01). "The gentle monster PDS 456 - Kiloparsec-scale molecular outflow and its implications for QSO feedback" (in en). Astronomy & Astrophysics 628: A118. doi:10.1051/0004-6361/201935524. ISSN 0004-6361. Bibcode: 2019A&A...628A.118B. https://www.aanda.org/articles/aa/full_html/2019/08/aa35524-19/aa35524-19.html. 
  12. ↑ Matzeu, G. A.; Reeves, J. N.; Braito, V.; Nardini, E.; McLaughlin, D. E.; Lobban, A. P.; Tombesi, F.; Costa, M. T. (2017-08-16). "Evidence for a radiatively driven disc-wind in PDS 456?". Monthly Notices of the Royal Astronomical Society: Letters 472 (1): L15–L19. doi:10.1093/mnrasl/slx129. ISSN 1745-3925. 
  13. ↑ Nardini, E.; Reeves, J. N.; Gofford, J.; Harrison, F. A.; Risaliti, G.; Braito, V.; Costa, M. T.; Matzeu, G. A. et al. (2015-02-23), "Black hole feedback in the luminous quasar PDS 456", Science 347 (6224): 860–863, doi:10.1126/science.1259202, Bibcode: 2015Sci...347..860N 



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