4C +03.10

4C +03.10 also known as PKS 0505+03 and OG +008, is a quasar located in the constellation of Orion. At a redshift of 2.46, the object is located 10.6 billion light-years away from Earth.

Characteristics
4C +03.10 produces a powerful astrophysical jet. It is an active core-dominated radio-loud quasar displaying signs of radio emission with a smaller radio morphology compared to steep-spectrum quasars and has a gamma ~ 4-7 jet axes. But has steep-spectrum quasar characteristics with small widths of the C IV λ1549 and C III λ1909 line profiles, larger Mg II λ2800 equivalent widths, and small He II + O III/C IV intensity ratios.

The quasar has an associated C IV absorbers found stronger than EWrest>=0.5 Å and strong [O III] λ5007 lines. It is among 20%-30% quasars that shows narrow ~1000 km s−1 emission in He II λ1640 with a special feature arising in its ionized halo associate with radio ejecta for objects or by cooling flows from clusters. In some cases, it is both. Moreover, 4C +03.10, also contains a dampened Lyα absorber with a column density of NHI>=2×1020 atoms cm−2 with its frequency reaching a peak where the universe is 10%-30% of the present age with mass density of neutral gas of Ωg.

The source of 4C +03.10 is known to be extremely luminous according to observations by researchers who studied the Third and Fourth Cambridge Survey of radio sources between declination of -7° and +40 degrees as well by Parkes Observatory. It has a luminosity value of 1026 <P408 <1027 W Hz−1 and hints of an inverse correlation between the luminosity and size. The source is known to flicker at 6-cm wavelength, caused by scintillation in the either interstellar or by near-source medium.

Observations made by Very Large Array, found the extragalactic source is seen through a restricted celestial angular zone encompassing the Orion-Eridanus region of the Milky Way; this shows it has an extension of linear polarization with a small flux density.

Observations of 4C +03.10
4C +03.10 contains a mass outflow rate of 6-700 M⊙ yr−1, which has blue-shifted velocities of a few hundred km s−1 and line widths reaching up to 1500 km s−1. According to researchers, the size of the ionized outflows is around ~2 kpc. The properties of the ionized outflows, mass outflow rate, momentum rate, and kinetic power in 4C +03.10 proves to be correlated with its luminosity from its active galactic nucleus (AGN). As the outflow increases, the AGN luminosity increases suggesting the surrounding gas is driven by fast outflows from radiation pressure, dependable by emitted luminosity. Researchers theorized the outflows might be neutrino emitters.

4C +03.10 has high metal enrichments. Researchers who studied Q0207-398, found out 4C +03.10 has sharp broad absorption lines allowing them to probe more in its high ionization regions. The N V λ1240/He II λ1640 ratio they measured is found to be ~1 for standard cloud properties. As for the intensity of the N V line, researchers found it sensitive to the abundance of the gas because there is plenty of nitrogen roughly the square of metallicity. The lowest metallicity capable of reproducing the N V spectrum in 4C +03.10 is Z ~ 5 Z_sun_, consistent to exist in the cores of early-type galaxies after rapid star formation. This shows similar properties in broad absorption-line quasars.

The quasar was detected by Swift. Through observations, it is found X-ray bright with an average αox =1.39 ± 0.03; where αox is the power-law slope connecting the monochromatic flux at 2500 Å and at 2 keV, displaying hard X-ray spectra. Apart from that, the accretion luminosity of 4C +03.10 is between the ranges of 0.7 × 1046 erg s−1 and 5.2 × 1047 erg s−1. From its black hole mass, it is accreting at Eddington fractions of 0.1 ≲ L/LEdd ≲ 1. Researchers who studied 4C +03.10, found the C iv λ 1549 broad-emission line is weak and anti-correlated with the Eddington ratio, a relation they referred it as a modified Baldwin effect (MBE). Based on MBE, it contains a high Eddington ratio.