Haro 5-2: A New Pre-main-sequence Quadruple Stellar System
: Reipurth, Bo; Briceno, C.; Geballe, T. R.; Baranec, C.; Mikkola, S.; Cody, A. M.; Connelley, M. S.; Flores, C.; Skiff, B. A.; Armstrong, J. D.; Law, N. M.; Riddle, R.
Publisher: IOP Publishing Ltd
: BRISTOL
: 2024
: The Astronomical Journal
: ASTRONOMICAL JOURNAL
: ASTRON J
: 143
: 168
: 4
: 14
: 0004-6256
: 1538-3881
DOI: https://doi.org/10.3847/1538-3881/ad5956
: https://iopscience.iop.org/article/10.3847/1538-3881/ad5956
: https://research.utu.fi/converis/portal/detail/Publication/457855518
We have discovered that the H alpha emission-line star Haro 5-2, located in the 3-6 Myr old Ori OB1b association, is a young quadruple system. The system has a 2+2 configuration, with an outer separation of 2.'' 6 and with resolved subarcsecond inner binary components. The brightest component, Aa, dominates the A-binary; it is a weak-line T Tauri star with spectral type M2.5 +/- 1. The two stars of the B component are equally bright at J, but the Bb star is much redder. Optical spectroscopy of the combined B pair indicates a rich emission-line spectrum with a M3 +/- 1 spectral type. The spectrum is highly variable and switches back and forth between a classical and a weak-line T Tauri star. In the near-IR, the spectrum shows Paschen beta and Brackett gamma in emission, indicative of active accretion. A significant mid-IR excess reveals the presence of circumstellar or circumbinary material in the system. Most multiple systems are likely formed during the protostellar phase, involving flybys of neighboring stars followed by an inspiraling phase driven by accretion from circumbinary material and leading to compact subsystems. However, Haro 5-2 stands out among young 2+2 quadruples, as the two inner binaries are unusually wide relative to the separation of the A and B pair, allowing future studies of the individual components. Assuming the components are coeval, the system could potentially allow stringent tests of pre-main-sequence evolutionary models.
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It is also based in part on observations obtained at the Southern Astrophysical Research(SOAR)telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia eInovacoes (MCTI/LNA)do Brasil, the US National Science Foundation's NOIR Lab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University(MSU).IRAF was distributed by the National Optical Astronomy Observatory, which was managed by the Association of Universities for Research in Astronomy(AURA), under acooperative agreement with the National Science Foundation.The Robo-AO system is supported by collaborating partner institutions, the California Institute of Technology, the Inter-University Centre for Astronomy and Astrophysics, the National Science Foundation under grant Nos. AST-0906060, AST-0960343, and AST1207891, a grant from the Mt. Cuba Astronomical Foundation, and a gift from Samuel OschinThis research has made use of the SIMBAD database,operated at CDS, Strasbourg, France, and of NASA'sAstrophysics Data System Bibliographic Services.
