| SBS 1425+606 | |
|---|---|
 Image of SBS 1425+606 taken bySloan Digital Sky Survey | |
| Observation data (J2000.0epoch) | |
| Constellation | Ursa Major |
| Right ascension | 14h 26m 56.178s |
| Declination | +60d 25m 50.87s |
| Redshift | 3.197157 |
| Heliocentric radial velocity | 958,484km/s |
| Distance | 11.4Gly (light travel time distance) |
| Apparent magnitude (V) | 0.032 |
| Apparent magnitude (B) | 0.043 |
| Surface brightness | 16.5 |
| Characteristics | |
| Type | DLA, HiBAL |
| Notable features | Quasar with highluminosity |
| Other designations | |
| 2MASS J14265618+6025508, HS 1425+6039, 2MASSi J1426561+602550, WISEA J142656.18+602550.8,PGC 4046493, KODIAQ J142656+602550,SDSS J142656.17+602550.8,QSO B1425+606 | |
SBS 1425+606 also known asHS 1425+6039 andQSO B1425+606, is aquasar located in the constellationUrsa Major. Itsredshift is 3.197157, putting the object at alight travel time distance of 11.4 billionlight years.[1]
SBS 1425+606 was first discovered in 1996 via aspectroscopy study which a team ofastronomers from the Second Byurakan Survey, found there are 76 quasars; among them is SBS 1425+606, a hundredsubdwarf stars and aBL Lac object.[2]
SBS 1425+606 is one of the mostenergetic quasars observed in theuniverse at redshift >3.[3] It has anabsolute magnitude of -31.5 or 1041watts which the intense luminosity is caused by itsaccretion disk.[4][2] Thesupermassive black hole in SBS 1425+606 propelsmatter in thespeed of light, given the speed ofgases andfriction betweenatoms, reaches up to hightemperature affecting ionization of gas and increasing its luminosity.[5]
SBS 1425+606 is classified as a broadabsorption line quasar.[6] It shows anultraviolet absorption that is hundreds of km s−1 wide,[7] with a redshifted trough extending up to avelocity ofv ≃ 12 000 km s−1. These large widths are mainly the cause by its ownaccretion process.[8] Broad absorption line quasars such as SBS 1425+606, tend to show a unique morphology which they havegas clouds absorbingfluxes atwavelengths of common quasarspectral features, although theirblueshifted velocities exceeds up to 0.1c. BAL features are interesting as they provide signatures of significantfeedback, but also compromisecosmological studies with quasars by their impact on accurate redshifts and measurements of thematter density distribution which is traced by theLyman-alpha forest.[9]
According to observations by researchers, they noted there is a strong existence of a moderately strongdamped Lyαabsorption system in SBS 1425+606, located at redshift 2.83. This is tentatively identified a possible broad absorption line, in the discoveryspectrum.Voigt profiles superposed on the data suggests the column density the "Lyα disk" is N(HI)~2.5x1020cm−2.[3] Further observations by 4 m classtelescopes fromESO inChile andObservatorio del Roque de los Muchachos inSpain, found out there is presence ofnitrogen lines of the N I λ1134 and λ1200 multiplets, offering a considerable range inoscillator strengths and the possibility of disentangling Lyα interlopers.[10]
SBS 1425+606 is shown to have an extendedLyman-α emission around its bright nucleus, which its total Ly-α luminosities corresponds to ~0.5% of the luminosities from its broad Lyαemission lines making an order ofmagnitude smaller as compared to those in radio-loudspectrum quasars. By studying SBS 1425+606, it is an important factor in determining the formation of high redshiftmassive galaxies, which they form stars through large amounts of gas, that falls in to feed the quasar. By balancing the evolution of massive galaxies between infall andfeedback mechanisms, both are equally important forgalaxy formation.[11]