Deep Observations of CO and Free-Free Emission in Ultraluminous Infrared QSO IRAS F07599+6508

TL;DR

This study presents NOEMA observations of CO and free-free emission in the IR QSO IRAS F07599+6508, revealing molecular gas dynamics, potential merger features, and star formation activity, contributing to understanding ULIRG-to-QSO transition processes.

Contribution

First detailed CO and free-free emission analysis of IRAS F07599+6508, highlighting molecular gas structure, merger features, and star formation rates in an IR QSO.

Findings

Molecular gas is rotationally supported with a major axis of ~6.1 kpc.

Detected faint CO features suggest merger activity at ~11.4 and 19.1 kpc.

Estimated star formation rate of 77 solar masses per year from free-free emission.

Abstract

Infrared quasi-stellar objects (IR QSOs) are a rare subpopulation selected from ultraluminous infrared galaxies (ULIRGs) and have been regarded as promising candidates of ULIRG-to-optical QSO transition objects. Here we present NOEMA observations of the CO(1-0) line and 3 mm continuum emission in an IR QSO IRAS F07599+6508 at $z=0.1486$, which has many properties in common with Mrk 231. The CO emission is found to be resolved with a major axis of $\sim$6.1 kpc that is larger than the size of $\sim$4.0 kpc derived for 3 mm continuum. We identify two faint CO features located at a projected distance of $\sim$11.4 and 19.1 kpc from the galaxy nucleus, respectively, both of which are found to have counterparts in the optical and radio bands and may have a merger origin. A systematic velocity gradient is found in the CO main component, suggesting that the bulk of molecular gas is likely rotationally supported. Based on the radio-to-millimeter spectral energy distribution and IR data, we estimate that about 30$\%$ of the flux at 3 mm arises from free-free emission and infer a free-free-derived star formation rate of 77 $M_\odot\ {\rm yr^{-1}}$, close to the IR estimate corrected for the AGN contribution. We find a high-velocity CO emission feature at the velocity range of about -1300 to -2000 km s$^{-1}$. Additional deep CO observations are needed to confirm the presence of a possible very high-velocity CO extension of the OH outflow in this IR QSO.