Locating the two black holes in NGC 6240

Science

Volumn 316, Issue 5833, 2007, Pages 1877-1880

  Max, Claire E ^a,b   Canalizo, Gabriela ^a,c   De Vries, Willem H ^a,d  

^a LAWRENCE LIVERMORE NATIONAL LABORATORY   (United States)

^b UNIVERSITY OF CALIFORNIA   (United States)

^c UNIVERSITY OF CALIFORNIA   (United States)

^d UNIVERSITY OF CALIFORNIA   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ASTRONOMY; DETECTION METHOD; INFRARED IMAGERY;

ARTICLE; ASTRONOMY; BLACK HOLE; COSMOLOGICAL PHENOMENA; GALAXY; IMAGE ANALYSIS; INFRARED RADIATION; OPTICS; PRIORITY JOURNAL; TECHNOLOGY; X RAY;

EID: 34347368778     PISSN: 00368075     EISSN: 10959203     Source Type: Journal    
DOI: 10.1126/science.1136205     Document Type: Article

References (39)

1. L. Ferrarese, D. Merritt, Astrophys. J. 539, L9 (2000).
2. K. Gebhardt et al.,, Astrophys. J. 539, L13 (2000).
3. K. Danzmann et al., Adv. Space Res. 32, 1233 (2003).
4. P. F. Hopkins et al., Astrophys. J. 625, L71 (2005).
5. B. T. Soifer et al., Astrophys. J. 278, L71 (1984).
6. Data from the HST archive (34) at http://archive.stsci.edu/hst/.
7. R. E. A. Fosbury, J. V. Wall, Mon. Not. R. Astron. Soc. 189, 79 (1979).
8. H. A. Thronson, S. Majewski, L. Descartes, M. Hereld, Astrophys. J. 364, 456 (1990).
9. S. A. Eales, E. E. Becklin, K.-W. Hodapp, D. A. Simons, C. G. Wynn-Williams, Astrophys. J. 365, 478 (1990).
10. critical parameterizes the current importance of "dark-energy" density in the universe.
11. A distance of 1 pc is approximately equal to 3 light-years.
12. P. Vignati et al., Astron. Astrophys. 349, L57 (1999).
13. S. Komossa et al., Astrophys. J. 582, L15 (2003).
14. R. J. Beswick, A. Pedlar, C. G. Mundell, J. F. Gallimore, Mon. Not. R. Astron. Soc. 325, 151 (2001).
15. J. F. Gallimore, R. Beswick, Astron. J. 127, 239 (2004).
16. E. Egami et al., Astron. J. 131, 1253 (2006).
17. M. Tecza et al., Astrophys. J. 537, 178 (2000).
18. F. Eisenhauer et al., Astron. Nachr. 325, 120 (2004).
19. We measured spatial resolution by taking the FWHM of five star clusters in the nuclear regions. These should be point sources because such clusters are only a few parsecs across, well less than the 30-pc pixel scale of the NIRC2 camera. The average FWHM for these clusters was 0.061 arc sec.
20. A. M. Koekemoer et al., in Proceedings of the 2002 HST Calibration Workshop, S. Arribas, A. Koekemoer, B. Whitmore, Eds. (Space Telescope Science Institute, Baltimore, MD, 2002), pp. 341-345.
21. C. E. Max et al., Astrophys. J. 621, 738 (2005) and references therein.
22. P. L. Wizinowich et al., Proc. SPIE 4007, 2 (2000).
23. P. L. Wizinowich et al., Publ. Astron. Soc. Pac. 112, 315 (2000).
24. E. M. Johansson et al., Proc. SPIE 4007, 600 (2000).
25. Details about NIRC2 performance can be found at the instrument Web page, www2.keck.hawaii.edu/inst/nirc2/.
26. Materials and methods are available as supporting material on Science Online.
27. L. K. Pollack, C. E. Max, G. Schneider, Astrophys. J. 660, 228 (2007).
28. B. C. Whitmore et al., Astron. J. 130, 2116 (2005) and references therein.
29. S. Komossa, personal communication.
30. L. J. Tacconi et al., Astrophys. J. 524, 732 (1999).
31. J. Binney, S. Tremaine, Galactic Dynamics (Princeton Univ. Press, Princeton, NJ, 1987).
32. A. Escala et al., Astrophys. J. 630, 152 (2005).
33. S. Kazantzidis et al., Astrophys. J. 623, L67 (2005).
34. J. Gerssen et al., Astron. J. 127, 75 (2004).
35. Chandra Proposers' Observotory Guide, version 8.0, 15 December 2005 (Chandra Science Center, Center for Astrophysics, Harvard University).
36. Chandra relative errors were measured for the "on-axis" bin (0′ to 2′), where it was found that 90% of sources have offsets <0.22″ US).
37. D. Monet et al., Astron. J. 125, 984 (2003).
38. J. Gallimore, personal communication.
39. We thank the staff of the W. M. Keck Observatory, especially D. L. Mignant and the AO team. Data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The W. M. Keck Observatory and the Keck II AO system were made possible by generous financial support from the W. M. Keck Foundation. This work was supported in part under the auspices of the U.S. Department of Energy, National Nuclear Security Administration; the University of California, Lawrence Livermore National Laboratory (under contract no. W-7405-Eng-48); and the NSF Science and Technology Center for Adaptive Optics, managed by the University of California at Santa Cruz (under cooperative agreement no. AST-9876783). The authors extend special thanks to those people of Hawaiian ancestry on whose sacred mountain we were privileged to be guests. Without their hospitality, these observations would not have been possible.