SDSS J150904.22+043441.8
| SDSS J150904.22+043441.8 | |
|---|---|
SDSS J150904.22+043441.8 captured by DESI Legacy Surveys | |
| Observation data (J2000.0 epoch) | |
| Constellation | Virgo |
| Right ascension | 15h 09m 04.21s[1] |
| Declination | +04° 34′ 41.79″[1] |
| Redshift | 0.111467[1] |
| Heliocentric radial velocity | 33,417 km/s ± 11[1] |
| Distance | 1.490 Gly |
| Apparent magnitude (V) | 18.90 |
| Characteristics | |
| Type | QSO2[1] |
| Size | ~159,000 ly (48.8 kpc) (estimated)[1] |
| Other designations | |
| IRAS F15065+0446, NVSS J150904+043441, LEDA 1270205, 2MASS J15090421+0434417 , 2MASX J15090422+0434415 | |
SDSS J150904.22+043441.8 is a type 2 quasar[2] located in the constellation of Virgo. The redshift of the galaxy is (z) 0.111[1][3] and it was first discovered in the IRAS survey in 1990.[4] The total doubly ionized oxygen luminosity of the galaxy is estimated to be 108.56 Lʘ and is also classified as a luminous infrared galaxy based on its total infrared luminosity of 11.6 Lʘ.[2][5]
Description
SDSS J150904.22+043441.8 is classified as a barred spiral galaxy of type SBa based on a study made by the Galaxy Zoo. The position angle of the galaxy is estimated to be 94° while the inclination is around 44°.[6] The galaxy also appears as disturbed based on broad-band optical imaging, indicating either an interaction or even a past galaxy merger.[2] The total star formation rate of the galaxy is estimated to be 34 Mʘ per year based on the infrared luminosity.[6] The supermassive black hole inside the center of the galaxy, like many others, is estimated to be 8.27 ± 0.76 Mʘ.[7]
The galaxy has a compact doubly ionized oxygen [O III] disk structure that is around three kiloparsecs in radius, with a feature described as fish-like towards the southeast from the galaxy. A kinematic map has also revealed it has gas rotations with negative velocity gradients on the eastern side while the western side has positive velocity gradients.[8] Outflows have also been detected in the galaxy, with the mass of the outflows estimated to be 9 × 105 Mʘ and around 0.46 Mʘ per year. There also molecular outflows detected, with kinetic power reaching 4.9 × 1039 erg s−1.[2] Observations made by the Atacama Large Millimeter Array (ALMA) also found the outflows are towards the northwest side of the galaxy at a position angle of 40° and by 3.8 kiloparsecs.[8]
A study published in 2022, has found the continuum emission of the galaxy has a peculiar morphology. It is known to follow in an inner structure of the molecular gas that is shaped into an oblong, but in the central region of the galaxy, there is an arc-like structure that does not follow the same path as the gas. Two spiral arms have also been discovered in the galaxy, being developed from inside the stellar bar region and extending outwards by four kiloparsecs northwest and in the position angle of -30° southeast.[6]
In 2025, carbon oxide, hydrogen and water, as well as aliphatic grain band absorption elements were detected in the galaxy. This suggests the nucleus of the galaxy is extremely obscured.[9]
References
- ^ a b c d e f g "NED Search results for SDSS J150904.22+043441.8". NASA/IPAC Extragalactic Database. Retrieved 2026-01-01.
- ^ a b c d Ramos Almeida, C; Acosta-Pulido, J A; Tadhunter, C N; González-Fernández, C; Cicone, C; Fernández-Torreiro, M (2019-05-20). "A near-infrared study of the multiphase outflow in the type-2 quasar J1509+0434". Monthly Notices of the Royal Astronomical Society: Letters. 487 (1): L18–L23. arXiv:1905.06288. doi:10.1093/mnrasl/slz072. ISSN 1745-3925.
- ^ Pierce, J. C. S.; Tadhunter, C.; Almeida, C. Ramos; Bessiere, P.; Heaton, J. V.; Ellison, S. L.; Speranza, G.; Gordon, Y.; O'Dea, C. (2023-03-27), "Galaxy interactions are the dominant trigger for local type 2 quasars", Monthly Notices of the Royal Astronomical Society, 522 (2): 1736–1751, arXiv:2303.15506, doi:10.1093/mnras/stad455
- ^ Moshir, M.; Al, Et (1990). "IRAS Faint Source Catalogue, version 2.0". IRAS Faint Source Catalogue: 0. Bibcode:1990IRASF.C......0M.
- ^ Sargsyan, Lusine; Weedman, Daniel; Lebouteiller, Vianney; Houck, James; Barry, Donald; Hovhannisyan, Ashot; Mickaelian, Areg (2011-02-24). "Infrared Spectra and Spectral Energy Distributions for Dusty Starbursts and Active Galactic Nuclei". The Astrophysical Journal. 730 (1): 19. arXiv:1101.3876. Bibcode:2011ApJ...730...19S. doi:10.1088/0004-637X/730/1/19. ISSN 0004-637X.
- ^ a b c Almeida, C. Ramos; Bischetti, M.; García-Burillo, S.; Alonso-Herrero, A.; Audibert, A.; Cicone, C.; Feruglio, C.; Tadhunter, C. N.; Pierce, J. C. S.; Pereira-Santaella, M.; Bessiere, P. S. (2022-02-01). "The diverse cold molecular gas contents, morphologies, and kinematics of type-2 quasars as seen by ALMA". Astronomy & Astrophysics. 658: A155. arXiv:2111.13578. Bibcode:2022A&A...658A.155R. doi:10.1051/0004-6361/202141906. ISSN 0004-6361.
- ^ Kong, Minzhi; Ho, Luis C. (2018-05-30). "The Black Hole Masses and Eddington Ratios of Type 2 Quasars". The Astrophysical Journal. 859 (2): 116. arXiv:1804.09852. Bibcode:2018ApJ...859..116K. doi:10.3847/1538-4357/aabe2a. ISSN 0004-637X.
- ^ a b Speranza, G.; Almeida, C. Ramos; Acosta-Pulido, J. A.; Audibert, A.; Holden, L. R.; Tadhunter, C. N.; Lapi, A.; González-Martín, O.; Brusa, M.; López, I. E.; Musiimenta, B.; Shankar, F. (2024-01-01). "Multiphase characterization of AGN winds in five local type-2 quasars". Astronomy & Astrophysics. 681: A63. arXiv:2311.10132. Bibcode:2024A&A...681A..63S. doi:10.1051/0004-6361/202347715. ISSN 0004-6361.
- ^ Almeida, C. Ramos; García-Bernete, I.; Pereira-Santaella, M.; Speranza, G.; Maiolino, R.; Ji, X.; Audibert, A.; Cezar, P. H.; Acosta-Pulido, J. A.; Alonso-Herrero, A.; García-Burillo, S.; González-Martín, O.; Rigopoulou, D.; Tadhunter, C. N.; Labiano, A. (2025-06-01). "JWST MIRI reveals the diversity of nuclear mid-infrared spectra of nearby type 2 quasars". Astronomy & Astrophysics. 698: A194. arXiv:2504.01595. Bibcode:2025A&A...698A.194R. doi:10.1051/0004-6361/202453549. ISSN 0004-6361.