2M0441+2301 AabBab is a quadruple system comprised of two
pairs of binary objects with a projected separation of about 1,800 AU between
them. The more massive binary system, 2M0441+2301 Aab, consists of a low-mass
star (the "Aa" component) and a brown dwarf companion (the
"Ab" component) 33 AU away. The less massive binary system,
2M0441+2301 Bab, consists of a brown dwarf (the "Ba" component) and a
planetary-mass companion (the "Bb" component) 15 AU away. Mass
estimates indicate Aa has 200 times Jupiter's mass, Ab has 35 times Jupiter's
mass, Ba has 19 times Jupiter's mass and Bb has 9.8 times Jupiter's mass.
2M0441+2301 AabBab is currently the least massive quadruple system known.
Figure 1: Artist’s impression of a multiple system.
2M0441+2301 AabBab is a relatively young system, estimated
to be between 1 and 3 million years old. All four objects show spectroscopic
signs of low surface gravity, indicating that they are young and bloated, and
still in the process of contracting down. Additionally, Aa and Ab both show
weak emissions indicating the ongoing accretion of material. If 1,800 AU is the
true separation between Aab and Bab, then both binaries would have completed
less than 20 orbits around each other in the last 3 million years. All four
objects of this young quadruple system are believed to have formed in the same
way stars do.
Figure 2: Comparison of 2M0441+2301 AabBab with theoretical
isochrones from two models. From top to bottom, the 5 dotted lines on each
chart are the 1 Myr, 5 Myr, 10 Myr, 100 Myr and 1 Gyr isochrones (Myr - million
years; Gyr - billion years). Bowler & Hillenbrand (2015).
Reference:
Bowler & Hillenbrand (2015), "Near-Infrared Spectroscopy of 2M0441+2301 AabBab: A Quadruple System Spanning the Stellar to Planetary Mass Regimes", arXiv:1509.01658 [astro-ph.EP]
Bowler & Hillenbrand (2015), "Near-Infrared Spectroscopy of 2M0441+2301 AabBab: A Quadruple System Spanning the Stellar to Planetary Mass Regimes", arXiv:1509.01658 [astro-ph.EP]