PG 0052+251
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| PG 0052+251 | |
|---|---|
 HST image of PG 0052+251. The spiral host galaxy can be clearly seen. | |
| Observation data (J2000.0 epoch) | |
| Constellation | Pisces |
| Right ascension | 00h 54m 52.12s[1] |
| Declination | +25° 25′ 39.02″[1] |
| Redshift | 0.154450[1] |
| Heliocentric radial velocity | 46,303 km/s[1] |
| Distance | 2.002 Gly |
| Apparent magnitude (V) | 15.42 |
| Characteristics | |
| Type | Sb Sy1?[1] |
| Other designations | |
| 2MASS J00545212+2525391, RBS 0130, PGC 3237, RX J0054.8+2525, 2E 0217, SDSS J005452.11+252539.0, 2XMM J005452.0+252539, LAMOST J005452.09+252539.1, 1H 0048+250[1] | |
PG 0052+251 is a Seyfert type 1 galaxy located in the constellation of Pisces. Its redshift is (z) 0.154 estimating it to be two billion light-years away from Earth[1] and was first discovered in 1982 by astronomers who also classified it as a quasar albeit with low luminosity.[2] The host galaxy is particularly interesting because unlike other quasar host galaxies which are mainly ellipticals, this object is hosted by a spiral galaxy.[3] It is also radio-quiet.[4][5]
PG 0052+251 is classified as a normal barred spiral galaxy (type Sb) based on Hubble Space Telescope imaging, with several galaxy companions within its position indicating the galaxy is located in a compact group.[3][6][7][8] It is shown to have two spiral arms located both east and west from its nucleus with multiple bright H II regions located within them.[3][4] One of the arms appear to be more extended, ending in the spot where a companion object is located. There is a bright nuclear component. As a whole, the galaxy's appearance is undisturbed showing no evidence of a recent tidal event although it is facing a secondary wave of star-formation.[9][4]
The surface brightness for this galaxy is 23 magnitude arcseconds−2 with its de Vaucouleurs profile described as falling rapidly when compared to its measured profile. The major axis is estimated to be 32 kiloparsecs with its minor axis of 21 kiloparsecs. Additionally, its spheroid magnitude is 19.2 ± 0.3, making it somewhere fainter by 3.1 magnitudes comparing with its disk.[3] The radio structure of the source can be described as having a flat radio spectrum with some extended structure in the direction of south from its nucleus.[10] Observations with Very Long Baseline Array in 2025, revealed a single component at both frequencies with a flat slope between 5 and 45 GHz suggesting the radio emission is optically thick.[11]
PG 0052+251 contains a broad-line region. According to observations, the region is found to be described as a spherical shell with its depth being 600 light-days, an inner radius of 90 light-days and its outer layer being around 700 light-days long. Evidence also showed there is an inner broad component and an intermediate broad component described as being obscured within the region based on its line core properties.[12] The black hole of PG 0052+251 is estimated to be 3.69 ± 0.76 × 108 M☉ according to a study by B.M. Peterson.[13] Variations are noted in its emission lines at 8% and 7% in continuum over a measured time period of 69 days long.[14]
The galaxy is categorized as a type 1 quasar. It has a narrow-line region in additional to its broad-line region described as extended. Studies of its structure showed it has a radial extent of 0.5 kiloparsecs with a measured luminosity of 3.8 × 1042 erg s−1. There are three blob-like structures in the eastern region which in turn, are embedded inside a low-surface brightness region. One of the blobs is located 4.3 kiloparsecs away from its active nucleus.[15]
References
- 1 2 3 4 5 6 7 "NED search results for PG 0052+251". NASA/IPAC Extragalactic Database. Retrieved 2025-08-03.
- ↑ Boroson, T. A.; Oke, J. B.; Green, R. F. (December 1982). "A spectroscopic investigation of the nebulosity around low-luminosityquasars". The Astrophysical Journal. 263: 32–42. Bibcode:1982ApJ...263...32B. doi:10.1086/160477. ISSN 0004-637X.
- 1 2 3 4 Bahcall, John N.; Kirhakos, Sofia; Schneider, Donald P. (February 1996). "The Apparently Normal Galaxy Hosts for Two Luminous Quasars". The Astrophysical Journal. 457: 557. arXiv:astro-ph/9509031. Bibcode:1996ApJ...457..557B. doi:10.1086/176752. ISSN 0004-637X.
- 1 2 3 Dunlop, J. S.; McLure, R. J.; Kukula, M. J.; Baum, S. A.; O'Dea, C. P.; Hughes, D. H. (2003-04-21). "Quasars, their host galaxies and their central black holes". Monthly Notices of the Royal Astronomical Society. 340 (4): 1095–1135. arXiv:astro-ph/0108397. Bibcode:2003MNRAS.340.1095D. doi:10.1046/j.1365-8711.2003.06333.x. ISSN 0035-8711.
- ↑ McLure, R.J.; Dunlop, J.S. (October 2001). "The black hole masses of Seyfert galaxies and quasars". Monthly Notices of the Royal Astronomical Society. 327 (1): 199–207. arXiv:astro-ph/0009406. Bibcode:2001MNRAS.327..199M. doi:10.1046/j.1365-8711.2001.04709.x. ISSN 0035-8711.
- ↑ information@eso.org. "Quasar PG 0052+251". www.esahubble.org. Retrieved 2025-08-03.
- ↑ Bahcall, John N.; Kirhakos, Sofia; Saxe, David H.; Schneider, Donald P. (April 1997). "Hubble Space Telescope Images of a Sample of 20 Nearby Luminous Quasars". The Astrophysical Journal. 479 (2): 642–658. arXiv:astro-ph/9611163. Bibcode:1997ApJ...479..642B. doi:10.1086/303926. ISSN 0004-637X.
- ↑ Hutchings, J. B.; Neff, S. G. (February 1997). "JHK Imaging and Photometry of Low Z QSOs and Radio Galaxy". The Astronomical Journal. 113: 550–561. arXiv:astro-ph/9611192. Bibcode:1997AJ....113..550H. doi:10.1086/118275. ISSN 0004-6256.
- ↑ Clements, D. L. (2000-02-01). "Far-infrared-loud quasars--I. Disturbed and quiescent quasars in the PG survey". Monthly Notices of the Royal Astronomical Society. 311 (4): 833–840. arXiv:astro-ph/9909420. Bibcode:2000MNRAS.311..833C. doi:10.1046/j.1365-8711.2000.03095.x. ISSN 0035-8711.
- ↑ Kukula, Marek J.; Dunlop, James S.; Hughes, David H.; Rawlings, Steve (June 1998). "The radio properties of radio-quiet quasars". Monthly Notices of the Royal Astronomical Society. 297 (2): 366–382. arXiv:astro-ph/9802148. Bibcode:1998MNRAS.297..366K. doi:10.1046/j.1365-8711.1998.01481.x. ISSN 0035-8711.
- ↑ Chen, Sina; Laor, Ari; Behar, Ehud; Baldi, Ranieri D.; Gelfand, Joseph D.; Kimball, Amy E. (2025-01-29). "A Dichotomy in the 1–24 GHz Parsec-scale Radio Spectra of Radio-quiet Quasars". The Astrophysical Journal. 979 (2): 241. arXiv:2410.07889. Bibcode:2025ApJ...979..241C. doi:10.3847/1538-4357/ada142. ISSN 0004-637X.
- ↑ Zhang, Xue-Guang (2011-10-24). "Evidence for the Intermediate Broad-Line Region of Reverberation-Mapped Active Galactic Nucleus Pg 0052+251". The Astrophysical Journal. 741 (2): 104. Bibcode:2011ApJ...741..104Z. doi:10.1088/0004-637x/741/2/104. ISSN 0004-637X.
- ↑ Peterson, B. M.; Ferrarese, L.; Gilbert, K. M.; Kaspi, S.; Malkan, M. A.; Maoz, D.; Merritt, D.; Netzer, H.; Onken, C. A.; Pogge, R. W.; Vestergaard, M.; Wandel, A. (October 2004). "Central Masses and Broad-Line Region Sizes of Active Galactic Nuclei. II. A Homogeneous Analysis of a Large Reverberation-Mapping Database". The Astrophysical Journal. 613 (2): 682–699. arXiv:astro-ph/0407299. Bibcode:2004ApJ...613..682P. doi:10.1086/423269. ISSN 0004-637X.
- ↑ Korista, Kirk T. (July 1991). "Short Timescale Broad Emission-Line Flux Variability in High-Luminosity Active Galactic Nuclei". The Astronomical Journal. 102: 41. Bibcode:1991AJ....102...41K. doi:10.1086/115857. ISSN 0004-6256.
- ↑ Trindade Falcão, Anna; Kraemer, S B; Fischer, T C; Schmitt, H R; Feuillet, L; Crenshaw, D M; Revalski, M; Maksym, W P; Vestergaard, M; Elvis, M; Gaskell, C M; Ho, L C; Netzer, H; Storchi-Bergmann, T; Turner, T J (2024-10-22). "Hubble Space Telescope observations of nearby type 1 quasars. I. Characterization of the extended [O <scp>iii</scp>] 5007 Å emission". Monthly Notices of the Royal Astronomical Society. 535 (1): 621–633. doi:10.1093/mnras/stae2412. ISSN 0035-8711.
