| Markarian 1014 | |
|---|---|
 SDSS image of Markarian 1014 | |
| Observation data (J2000.0epoch) | |
| Constellation | Cetus |
| Right ascension | 01h 59m 50.24s[1] |
| Declination | +00° 23′ 40.66″[1] |
| Redshift | 0.163110[1] |
| Heliocentric radial velocity | 48,899km/s[1] |
| Distance | 2.473Gly (758.22Mpc) |
| 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 asPG 0157+001 is aquasar located in the constellationCetus. It is located at a distance of 2.47 billionlight years fromEarth and is classified as aSeyfert galaxy as well as anultraluminous infrared galaxy (ULIRG). With a diameter of more than 770,000 light-years across, it is surprising one of thelargest galaxies known.[1]
Markarian 1014 is anactive nucleus-dominated galaxy with a totalfar-infrared luminosity of 9.93 x 1011 erg s−1 cm−2.[2] Apart from being radio-quiet, it contains optical emission lines considered broad, measured with afull-width half maximum of Hβ > 4000 km s−1.[3] In additional to optical emission lines, Markarian 1014 showsemission features of Lyα, N v and O vi,[4] as well aspolycyclic 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 anultraviolet-excessive quasar.[5] It has anX-ray emission measured at 2-10 KeVluminosity of 1043.80erg s−1 when exhibiting a molecular outflow.[6] The mass of theblack hole in the center of Markarian 1014 is estimated 2.5+0.6-0.6 x 108 MΘ based on an MBH measurement carried out by theSeoul National University AGN Monitoring Project.[7]
According toimaging andspectra of its host galaxy, Markarian 1014 is described asspiral-like,[8] but also has a budge + disk morphology.[9] It has a curvedtidal tail found extending 60kiloparsecs towards the north-east, suggesting it has gone through a majormerger with adisk galaxy.[8] The tidal tail is known to show lengthy lowsurface brightness extension with another secondary tail shown faint but rotating symmetrically.[10]
Furthermore, the galaxy has twisted spiralisotopes within the 4 kiloparsec centralradius hinting its spiral disk is undergoing astarburst or tidal debris caused by the merger.[11] There is also the presence ofcarbon monoxide (CO) emission in the galaxy. Based on the relationship between its brightness andhydrogen gas (H2)surface density, the gas mass is estimated 4 x 1010MΘ.[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 1.1arcsec from each other. There is also another component found faint and located at the optical nucleus position. According to thespectral index of the component, it is -1.11 ± 0.02 between 5 and 45 GHz.[5]
A B' - R'color map is presented for Markarian 1014. According to spectroscopy made on its regions with a steeper bluecontinuum spectrum, it has a youngstellar population ofstars 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]
