2 July 2018 Toshinori Hayashi. Discovery of an Extraordinary Binary System
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1 2 July 2018 Toshinori Hayashi CONTENTS 1. arxiv: v1[astro-ph.he] 7 Jun 2018, Todd A. Thompson et al. Discovery of an Extraordinary Binary System 2. MNRAS 475, L15-L19 (2018) doi: /mnrasl/slx203 A detached stellar-mass black hole candidate in the globular cluster NGC 3201
2 Common introduction How to observe detached binaries including unseen objects X-ray binary(wikipedia) GW from a BH merger (Wikipedia)
3 2 4 M M e 0 P days? Non interacting -no accretion disk(noxray) Almost circular - e = ± Massive companion - a NS or a black hole?
4 : APOGEE > 10 B star in Galaxy a ΔRV Δt IJ K LMN 200 sources with highest acceleration. ASAS-SN Search for periodic photometric variations Transits, ellipsoidal variations, or starspots
5 2M l, b = , Acceleration a 2.9 km s YZ day YZ Photometric variation P [\1] days APOGEE spectrum analysis v sin i b1] 14.1 ± 0.6 kms YZ T dee 4480 ± 62K Well-fit by a single reddened template
6 TRES Best fit parameters P = ± days e = ± K = ± kms YZ f M M ij k sin k i 1b2 p M lmmn] + M ij = ± M
7 Assume that this system is tidally synchronized and circularized. i b1] = i 1b2 = i P b1] = P 1b2 = P v sin i 14.1 kms YZ R 23R / sin i L 200L / sin p i D 2.4 kpc/ sin i From Gaia parallax data s D 3.7 ± 0.8 kpc R 36 ± 8 R L 480 ± 100 L sin i 0.64 ± 0.14 L
8 With the constraint log g = 2.35 ± 0.14 from TRES L, R, T dee from Gaia and SED.ƒ M lmmn] = 3.0 Y.B M 1σ log g = 2.2 ± 0.1 Zp L = 290 Yk L Zƒ T dee = 4890 YZ K k. R = 23.8 Y.ƒ R Age = 10.B±.p Myr. p sin i = 0.97 Y.Z Z.Z M ij = 3.2 Y. M
9 log g Different analysis of spectra give different log g log g = 2.59 ± APOGEE log g = 2.2 APOGEE, lowest report log g = 2.35 ± 0.14 TRES log g might have a large systematic uncertasinty due to rapid rotation, spots, red colors? Best fitting without constraint log g Z.p M lmmn] = 2.2 Y. M 1σ pk L = 480 YZ L T dee = 4510 Ypp K.k R = 35.8 Y.ƒ R.Z sin i = 0.65 Y.Zp M ij = 5.5 Yp.p Looks match well but.p log g = 1.7 Y.k too small k.p M
10 Stars on the giant branch normally exhibit a negative correlation between [C/N] and mass, due to nuclear process. 2M may be an outlier. Due to binary interaction or previous merger in a triple system?
11 cluster NGC 3201 Non interacting - no accretion disk(no Xray) > 4.36 M? e 0.6 ~0.8 M P days Highly eccentric - e = ± Massive companion - Likely a black hole? In a globular cluster
12 Blue square: the star for reference Red cross-hairs: the object reported in this paper MUSE spectroscopy Spatial resolution 1800 < R < 3500 of some thousands stars per exposure Identified 3 stars with RV variations exceeding 100 kms YZ. One of them can be analysed. Other two need more observation.
13 Target star RA: 10 \ 17 L Dec No significant variations in magnitude No pulsation indicates RV is not due to star-intrinsic Compare NGC 3201 HST ACS CMD(Colour Magnitude Diagram) and PARSEC isochrone Best fit parameters M = 0.81 ± 0.05 M T dee = 6126 ± 20 K log g = 3.99 ± 0.05 dex M/H = 1.50 ± 0.02 dex
14 All radial velocity corrected spectra Red: Best fit PHOENIX spectra Fitting Göttingen Spectral Library of Synthetic PHOENIX spectra T dee = 6126 ± 20 K M/H = 1.50 ± 0.02 dex No emission lines indicating a cataclysmic variable or a compact binary with an illuminated low-mass star and a hot companion like a WD or NS Radial Velocity
15 Black: circular Red: Full Keplerian fit Generalized Lomb-Scargle periodgram Using likelihood function to find periodicity 167 days periodicity is likely. Phase folding & fitting RV K = 69.4 ± 2.5 kms YZ e = ± M sin i = 4.36 ± 0.41 M a M = 1.03 ± 0.03 au Companion may be a BH?
16 2M 2? a NS binary? Possibly a triple star system that consists of a compact double NS binary with a MS turn off around it But such a system never observed & actual mass of the discovered object may be higher a BH scenario is more likely?
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