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Spitzer Microlens Measurement of a Massive Remnant in a Well-Separated Binary

Shvartzvald, Y and Udalski, A and Gould, A and Han, C and Bozza, V and Friedmann, M and Hundertmark, M and Beichman, C and Bryden, G and Novati, SC and Carey, S and Fausnaugh, M and Gaudi, BS and Henderson, CB and Kerr, T and Pogge, RW and Varricatt, W and Wibking, B and Yee, JC and Zhu, W and Poleski, R and Pawlak, M and Szymanski, MK and Skowron, J and Mroz, P and Kozlowski, S and Wyrzykowski, L and Pietrukowicz, P and Pietrzynski, G and Soszynski, I and Ulaczyk, K and Choi, J-Y and Park, H and Jung, YK and Shin, I-G and Albrow, MD and Park, B-G and Kim, S-L and Lee, C-U and Cha, S-M and Kim, D-J and Lee, Y and Maoz, D and Kaspi, S and Street, RA and Tsapras, Y and Bachelet, E and Dominik, M and Bramich, DM and Horne, K and Snodgrass, C and Steele, IA and Menzies, J and Jaimes, RF and Wambsganss, J and Schmidt, R and Cassan, A and Ranc, C and Mao, S and Dong, S and D'Ago, G and Scarpetta, G and Verma, P and Jorgensen, UG and Kerins, E and Skottfelt, J (2015) Spitzer Microlens Measurement of a Massive Remnant in a Well-Separated Binary. Astrophysical Journal, 814 (2). ISSN 0004-637X

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Abstract

We report the detection and mass measurement of a binary lens OGLE-2015-BLG-1285La,b, with the more massive component having M1 > 1.35 M⊙ (80% probability). A main-sequence star in this mass range is ruled out by limits on blue light, meaning that a primary in this mass range must be a neutron star (NS) or black hole (BH). The system has a projected separation r⊥ = 6.1 ± 0.4 AU and lies in the Galactic bulge. These measurements are based on the "microlens parallax" effect, i.e., comparing the microlensing light curve as seen from Spitzer, which lay at 1.25 AU projected from Earth, to the light curves from four ground-based surveys, three in the optical and one in the near-infrared. Future adaptive optics imaging of the companion by 30 m class telescopes will yield a much more accurate measurement of the primary mass. This discovery both opens the path and defines the challenges to detecting and characterizing BHs and NSs in wide binaries, with either dark or luminous companions. In particular, we discuss lessons that can be applied to future Spitzer and Kepler K2 microlensing parallax observations.

Item Type: Article
Uncontrolled Keywords: 0201 Astronomical And Space Sciences, 0305 Organic Chemistry, 0306 Physical Chemistry (Incl. Structural)
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: American Astronomical Society; IOP Publishing
Related URLs:
Date Deposited: 09 May 2017 08:37
Last Modified: 09 May 2017 08:37
DOI or Identification number: 10.1088/0004-637X/814/2/111
URI: http://researchonline.ljmu.ac.uk/id/eprint/6381

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