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Title:
The Optical Counterpart of M101 ULX-1
Authors:
Kuntz, K. D.; Gruendl, Robert A.; Chu, You-Hua; Chen, C.-H. Rosie; Still, Martin; Mukai, Koji; Mushotzky, Richard F.
Affiliation:
AA(Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250; ), AB(Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 West Green Street, Urbana, IL 61801; , , ), AC(Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 West Green Street, Urbana, IL 61801; , , ), AD(Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 West Green Street, Urbana, IL 61801; , , ), AE(Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Code 662, Greenbelt, MD 20771; , , ; Universities Space Research Association.), AF(Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Code 662, Greenbelt, MD 20771; , , ; Universities Space Research Association.), AG(Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Code 662, Greenbelt, MD 20771; , , )
Publication:
The Astrophysical Journal, Volume 620, Issue 1, pp. L31-L34. (ApJ Homepage)
Publication Date:
02/2005
Origin:
UCP
ApJ Keywords:
X-Rays: Binaries, X-Rays: Individual: Alphanumeric: M101 ULX-1
DOI:
10.1086/428571
Bibliographic Code:
2005ApJ...620L..31K

Abstract

We have identified the optical counterpart of the ultraluminous X-ray source M101 ULX-1 (CXOKM101 J140332.37+542102), by comparing Hubble Space Telescope Advanced Camera for Surveys images with Chandra ACIS-S images. The optical counterpart has V=23.75 and colors consistent with those for a mid-B supergiant. Archival Wide Field Planetary Camera 2 observations show that the source brightness is constant to within ~0.1 mag. The physical association of this source with the ULX is confirmed by Gemini Multi-Object Spectrograph observations that show spatially unresolved He II λ4686 and He I λ5876 emission. These results suggest that M101 ULX-1 is a high-mass X-ray binary, but deep spectroscopic monitoring observations are needed to determine the detailed properties of this system.
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