Markarian 1014
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| Markarian 1014 | |
|---|---|
 SDSS image of Markarian 1014 | |
| Observation data (J2000.0 epoch) | |
| Constellation | Cetus |
| Right ascension | 01h 59m 50.24s[1] |
| Declination | +00° 23′ 40.66″[1] |
| Redshift | 0.163110[1] |
| Heliocentric radial velocity | 48,899 km/s[1] |
| Distance | 2.473 Gly (758.22 Mpc) |
| Apparent magnitude (V) | 15.87 |
| Apparent magnitude (B) | 16.08 |
| Characteristics | |
| Type | Bulge/disc, Sy 1 |
| Size | ~775,000 ly (237.62 kpc) (estimated)[1] |
| Notable features | Luminous infrared galaxy |
| Other designations | |
| PG 0157+001, UM 385, PGC 7551, IRAS 01572+0009, RBS 0264, RX J0159.8+0023, NVSS J015950+002338[1] | |
Markarian 1014 known as PG 0157+001 is a quasar located in the constellation Cetus. It is located at a distance of 2.47 billion light years from Earth and is classified as a Seyfert galaxy as well as an ultraluminous infrared galaxy (ULIRG). With a diameter of more than 770,000 light-years across, it is one of the largest galaxies known.[1]
Markarian 1014 is an active nucleus-dominated galaxy with a total far-infrared luminosity of 9.93 × 1011 erg s−1 cm−2.[2] Apart from being radio-quiet, it contains optical emission lines considered broad, measured with a full-width half maximum of Hβ > 4000 km s−1.[3] In additional to optical emission lines, Markarian 1014 shows emission features of Lyα, N v and O vi,[4] as well as polycyclic aromatic hydrocarbon.[3]
Markarian 1014 is also one of the brightest quasars classified as a warm ULIRG. It is currently in a transitional phase from a typical ULIRG to an ultraviolet-excessive quasar.[5] It has an X-ray emission measured at 2-10 KeV luminosity of 1043.80 erg s−1 when exhibiting a molecular outflow.[6] The mass of the black hole in the center of Markarian 1014 is estimated 2.5+0.6-0.6 × 108 MΘ based on an MBH measurement carried out by the Seoul National University AGN Monitoring Project.[7]
According to imaging and spectra of its host galaxy, Markarian 1014 is described as spiral-like,[8] but also has a budge + disk morphology.[9] It has a curved tidal tail found extending 60 kiloparsecs towards the north-east, suggesting it has gone through a major merger with a disk galaxy.[8] The tidal tail is known to show lengthy low surface brightness extension with another secondary tail shown faint but rotating symmetrically.[10]
Furthermore, the galaxy has twisted spiral isotopes within the 4 kiloparsec central radius hinting its spiral disk is undergoing a starburst or tidal debris caused by the merger.[11] There is also the presence of carbon monoxide (CO) emission in the galaxy. Based on the relationship between its brightness and hydrogen gas (H2) surface density, the gas mass is estimated 4 × 1010 MΘ.[12]
A 8.4 -GHz VLA image shows Markarian 1014 has a triple structure along the east–west direction. On both sides of its central core, two lobes are found with 1.1 arcsec from each other. There is also another component found faint and located at the optical nucleus position. According to the spectral index of the component, it is -1.11 ± 0.02 between 5 and 45 GHz.[5]
Stellar population
A B' - R' color map is presented for Markarian 1014. According to spectroscopy made on its regions with a steeper blue continuum spectrum, it has a young stellar population of stars aged between 180 and 290 million years old. These stars are mainly found inside a clump at the eastern region and along the north edge of its tidal tail, and both southwest and east from its nucleus. The galaxy also has other regions that are seen as redder in a B' - R' color map. This suggests much older stars aged approximately 1 billion years old but with little contribution from the old underlying population.[10]
References
- 1 2 3 4 5 6 7 "NED Search results for Markarian 1014". NASA/IPAC Extragalactic Database. Retrieved 2025-08-22.
- ↑ Boller, T.; Gallo, L. C.; Lutz, D.; Sturm, E. (2002-11-11). "Mrk 1014: an AGN-dominated ultraluminous infrared galaxy". Monthly Notices of the Royal Astronomical Society. 336 (4): 1143–1146. arXiv:astro-ph/0207378. Bibcode:2002MNRAS.336.1143B. doi:10.1046/j.1365-8711.2002.05867.x. ISSN 0035-8711.
- 1 2 Armus, L.; Charmandaris, V.; Spoon, H. W. W.; Houck, J. R.; Soifer, B. T.; Brandl, B. R.; Appleton, P. N.; Teplitz, H. I.; Higdon, S. J. U.; Weedman, D. W.; Devost, D.; Morris, P. W.; Uchida, K. I.; van Cleve, J.; Barry, D. J. (September 2004). "Observations of Ultraluminous Infrared Galaxies with the Infrared Spectrograph (IRS) on the Spitzer Space Telescope : Early Results on Markarian 1014, Markarian 463, and UGC 5101". The Astrophysical Journal Supplement Series. 154 (1): 178–183. arXiv:astro-ph/0406179. Bibcode:2004ApJS..154..178A. doi:10.1086/422915. ISSN 0067-0049.
- ↑ Liu 刘, Weizhe 伟哲; Veilleux, Sylvain; Rupke, David S. N.; Tripp, Todd M.; Hamann, Frederick; Martin, Crystal (2022-08-01). "Galactic Winds across the Gas-rich Merger Sequence. II. Lyα Emission and Highly Ionized O vi and N v Outflows in Ultraluminous Infrared Galaxies". The Astrophysical Journal. 934 (2): 160. arXiv:2206.09015. Bibcode:2022ApJ...934..160L. doi:10.3847/1538-4357/ac7a46. ISSN 0004-637X.
- 1 2 Wang, Ailing; An, Tao; Zhang, Yingkang; Cheng, Xiaopeng; Ho, Luis C; Kellermann, Kenneth I; Baan, Willem A (2023-09-02). "VLBI Observations of a sample of Palomar-Green quasars II: characterizing the parsec-scale radio emission". Monthly Notices of the Royal Astronomical Society. 525 (4): 6064–6083. doi:10.1093/mnras/stad2651. ISSN 0035-8711.
- ↑ Laha, Sibasish; Guainazzi, Matteo; Piconcelli, Enrico; Gandhi, Poshak; Ricci, Claudio; Ghosh, Ritesh; Markowitz, Alex G.; Bagchi, Joydeep (2018-11-13). "A Study of X-Ray Emission of Galaxies Hosting Molecular Outflows (MOX Sample)". The Astrophysical Journal. 868 (1): 10. arXiv:1809.07906. Bibcode:2018ApJ...868...10L. doi:10.3847/1538-4357/aae390. ISSN 0004-637X.
- ↑ Woo, Jong-Hak; Wang, Shu; Rakshit, Suvendu; Cho, Hojin; Son, Donghoon; Bennert, Vardha N.; Gallo, Elena; Hodges-Kluck, Edmund; Treu, Tommaso; Barth, Aaron J.; Cho, Wanjin; Foord, Adi; Geum, Jaehyuk; Guo, Hengxiao; Jadhav, Yashashree (2024-02-01). "The Seoul National University AGN Monitoring Project. III. Hβ Lag Measurements of 32 Luminous Active Galactic Nuclei and the High-luminosity End of the Size–Luminosity Relation". The Astrophysical Journal. 962 (1): 67. arXiv:2311.15518. Bibcode:2024ApJ...962...67W. doi:10.3847/1538-4357/ad132f. ISSN 0004-637X.
- 1 2 MacKenty, J. W.; Stockton, A. (1984-08-01). "Images and spectra of the host galaxy of the QSO Markarian 1014". The Astrophysical Journal. 283: 64–69. Bibcode:1984ApJ...283...64M. doi:10.1086/162274. ISSN 0004-637X.
- ↑ Watabe, Y.; Kawakatu, N.; Imanishi, M.; Takeuchi, T. T. (2009-12-21). "Supermassive black hole mass regulated by host galaxy morphology". Monthly Notices of the Royal Astronomical Society. 400 (4): 1803–1807. arXiv:0907.0142. Bibcode:2009MNRAS.400.1803W. doi:10.1111/j.1365-2966.2009.15345.x. ISSN 0035-8711.
- 1 2 Canalizo, Gabriela; Stockton, Alan (October 2000). "Stellar Populations in the Host Galaxies of Markarian 1014, IRAS 07598+6508, and Markarian 231". The Astronomical Journal. 120 (4): 1750–1763. arXiv:astro-ph/0007002. Bibcode:2000AJ....120.1750C. doi:10.1086/301585. ISSN 0004-6256.
- ↑ Scoville, N. Z.; S Evans, A.; Thompson, R.; Rieke, M.; Hines, D. C.; Low, F. J.; Dinshaw, N.; Surace, J. A.; Armus, L. (1999). "Scoville et al., NICMOS Imaging of IR-Luminous Galaxies". iopscience.iop.org. arXiv:astro-ph/9912246. doi:10.1086/301248. Retrieved 2024-09-28.
- ↑ Sanders, D. B.; Scoville, N. Z.; Soifer, B. T. (1988-12-01). "Detection of Abundant Molecular Gas in the UV-Excess Quasar Markarian 1014". The Astrophysical Journal. 335: L1. Bibcode:1988ApJ...335L...1S. doi:10.1086/185326. ISSN 0004-637X.
