IDENTIFICATION OF THE OPTICAL COUNTERPART OF FERMI BLACK WIDOW MILLISECOND PULSAR PSR J1544+4937

被引:20
作者
Tang, Sumin [1 ,2 ]
Kaplan, David L. [3 ]
Phinney, E. Sterl [1 ]
Prince, Thomas A. [1 ]
Breton, Rene P. [4 ]
Bellm, Eric [1 ]
Bildsten, Lars [2 ,5 ]
Cao, Yi [1 ]
Kong, Albert K. H. [6 ,7 ]
Perley, Daniel A. [1 ]
Sesar, Branimir [8 ]
Wolf, William M. [5 ]
Yen, T. -C. [6 ,7 ]
机构
[1] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA
[2] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA
[3] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA
[4] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England
[5] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[6] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan
[7] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan
[8] Max Planck Inst Astron, D-69117 Heidelberg, Germany
基金
美国国家科学基金会;
关键词
binaries: general; gamma rays: stars; pulsars: individual (PSR J1544+4937); white dwarfs; STELLAR ASTROPHYSICS MESA; LOW-MASS STARS; BROWN DWARFS; COMPANION; ATMOSPHERES; J1311-3430; TELESCOPE; DISCOVERY; BINARIES; PLANETS;
D O I
10.1088/2041-8205/791/1/L5
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We report the optical identification of the companion to the Fermi black widow millisecond pulsar PSR J1544+4937. We find a highly variable source on Keck Low Resolution Imaging Spectrometer images at the nominal pulsar position, with 2 mag variations over orbital period in the B, g, R, and I bands. The nearly achromatic light curves are difficult to explain with a simply irradiated hemisphere model, and suggest that the optical emission is dominated by a nearly isothermal hot patch on the surface of the companion facing the pulsar. We roughly constrain the distance to PSR J1544+4937 to be between 2 and 5 kpc. A more reliable distance measurement is needed in order to constrain the composition of the companion.
引用
收藏
页数:5
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