QSO J0305−3150
Quasar in the constellation of Fornax
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QSO J0305−3150 or J0305−3150, is an extremely distant luminous quasar[1] located in the constellation of Fornax. It was first discovered by the VISTA Kilo-degree Infrared Galaxy survey (VIKING) in November 2013 and has a redshift of (z) 6.61, corresponding to a light travel time of 12.8 billion light-years.[2]
| QSO J0305−3150 | |
|---|---|
QSO J0305−3150 imaged by DESI Legacy Survey | |
| Observation data (J2000.0 epoch) | |
| Constellation | Fornax |
| Right ascension | 03h 05m 16.92s |
| Declination | −31° 50′ 55.92″ |
| Redshift | 6.614500 |
| Distance | 12.8 billion ly (light-travel time distance) |
| Characteristics | |
| Type | QSO |
| Other designations | |
| VIKING J030516.92−315056.0 | |
Description
QSO J0305−3150 is a quasar with an absolute magnitude of M1450 = -25.96 ± 0.06, but it is found fainter than ULAS J1120+0641.[2] Its estimated integrated line flux is 3.44 ± 0.15 Jy km s−1 making it the highest known amongst two other studied quasars, J0109−3047 and J2348−3054. When compared with another high redshift quasar SDSS J114816.64+525150.3, its emission line luminosity is found similar making the object amongst the brightest [C II] emitters.[3] A Lyman-alpha emission nebula is seen surrounding the quasar, being displaced and redshifted, with an extension of 9 kiloparsecs.[4]
The host of QSO J0305−3150 is described as massive ultraluminous inflared galaxy with a luminosity of 4.0-7.5 × 1012 L☉ and a star formation of 1500 M☉ per year. In the center like most other galaxies, lies a supermassive black hole with an estimated mass of 1 × 109 M☉. Evidence showed the black hole is accreting given the presence of complex interstellar gas located within 3 kiloparsecs with high velocity dispersion.[5] A molecular gas reservoir has been found in the host galaxy with a measured stellar mass of less than 2.1 × 1010 M☉[6] and a mass surface density of (2.0 ± 0.9) × 104 pc−2.[7]
Observations made by Atacama Large Millimeter Array in February 2025, has found the quasar is undergoing a merger with a nearby companion galaxy described as an Lyman-alpha emitter (LAE).[8][4] When observed, it is found to display a compact dust continuum emission with most recovered within 1.6 kiloparsecs and a singly ionized carbon [C II] emission profile mainly made of a central Gaussian and an extended component. Results have also shown the emission is on large-scale with an aligned velocity gradient towards the galaxy, perturbed and misaligned with small-scale emission. As there is lack of [C II] emission in physical structures of 1 kiloparsec, it is not produced in dense photodissociation regions but inside low-density regions of both diffused H I gas and interstellar medium produced from tidal stripping during the merger process.[8]
A filamentary structure has been discovered surrounding QSO J0305−3150 by James Webb Space Telescope (JWST). Based on observations, the structure is found to have a galaxy overdensity, making the structure most overdense when found in the early universe. The environment where the quasar is residing is complex with a diverse population of galaxies, among them dusty forming and ultraviolet-bright galaxies.[9]