IRAS F12032+1707

IRAS F12032+1707 is widely known to be the most luminous megamasers detected.^[7] Its host galaxy is found to be a part of an interacting pair of galaxies with an estimated separation of 12 kiloparsecs from each other. The estimated R-band magnitude for the host galaxy is -22.22, while the K-band magnitude is -25.79.^[8] Radio imaging made by Very Long Baseline Array (VLBA) has found it has continuum flux density of 28.7 mJy.^[7] The star formation rate is 641 M_☉ per year^[9] while the total molecular gas mass is 6.7 × 10⁹ M_☉.^[10]

A study published in 2005, has found a zero-intensive line of the radio emission of IRAS F12032+1707. When observed, the width of the line is estimated to be 2,000 kilometers per seconds, thus making this as the host of the most broadest OH megamaser lines. The H I absorption spectrum of the galaxy is shown as best fitted by two components with measured velocities of around 65,119 and 65,496 kilometers per seconds respectively. Further evidence also suggested most of the megamaser emission originates from the nucleus on the northern side of the galaxy, based on near-infrared and its optical position. Most of the emission is mainly confined to an area measuring 25 x 25 milliarcseconds, with its components positioned roughly north to south and separated.^[4]

Evidence also showed the megamaser emission has a tail feature that is highly redshifted, with the flux density estimated to be approximately 9 mJy. The lines detected at both 1,665 and 1,667 GHz frequencies are found mainly undistinguished and blended together. There is a narrow component, depicted having a bright appearance at 64,500 kilometers per seconds with the peak maximum flux density of around 16.3 mJy.^[11] A buried active galactic nucleus (AGN) is suggested to lie inside the galaxy with an intrinsic luminosity of 3.5 × 10⁴⁵ erg s⁻¹.^[12]

• IRAS F12032+1707 on SIMBAD