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Title: VELOCITY STRUCTURE AND VARIABILITY OF [O III] EMISSION IN BLACK HOLE HOST GLOBULAR CLUSTER RZ2109

Abstract

We present a multi-facility study of the optical spectrum of the extragalactic globular cluster RZ2109, which hosts a bright black hole X-ray source. The optical spectrum of RZ2109 shows strong and very broad [O III] {lambda}{lambda}4959, 5007 emission in addition to the stellar absorption lines typical of a globular cluster. We use observations over an extended period of time to constrain the variability of these [O III] emission lines. We find that the equivalent width of the lines is similar in all of the data sets; the change in L[O III] {lambda}5007 is {approx}<10% between the first and last observations, which were separated by 467 days. The velocity profile of the line also shows no significant variability over this interval. Using a simple geometric model, we demonstrate that the observed [O III] {lambda}5007 line velocity structure can be described by a two-component model with most of the flux contributed by a bipolar conical outflow of about 1600 km s{sup -1}, and the remainder from a Gaussian component with an FWHM of several hundred km s{sup -1}.

Authors:
; ;  [1];  [2]; ;  [3]
  1. Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824 (United States)
  2. School of Physics and Astronomy, University of Southampton, Southampton, Hampshire S017 1BJ (United Kingdom)
  3. Department of Astronomy, Indiana University, Bloomington, IN 47405 (United States)
Publication Date:
OSTI Identifier:
21587466
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 739; Journal Issue: 2; Other Information: DOI: 10.1088/0004-637X/739/2/95; Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BLACK HOLES; EMISSION; STAR CLUSTERS; VELOCITY; X-RAY GALAXIES; COSMIC RAY SOURCES; COSMIC X-RAY SOURCES; GALAXIES

Citation Formats

Steele, Matthew M., Zepf, Stephen E., Kundu, Arunav, Maccarone, Thomas J., Rhode, Katherine L., and Salzer, John J., E-mail: steele24@msu.edu. VELOCITY STRUCTURE AND VARIABILITY OF [O III] EMISSION IN BLACK HOLE HOST GLOBULAR CLUSTER RZ2109. United States: N. p., 2011. Web. doi:10.1088/0004-637X/739/2/95; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
Steele, Matthew M., Zepf, Stephen E., Kundu, Arunav, Maccarone, Thomas J., Rhode, Katherine L., & Salzer, John J., E-mail: steele24@msu.edu. VELOCITY STRUCTURE AND VARIABILITY OF [O III] EMISSION IN BLACK HOLE HOST GLOBULAR CLUSTER RZ2109. United States. doi:10.1088/0004-637X/739/2/95; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
Steele, Matthew M., Zepf, Stephen E., Kundu, Arunav, Maccarone, Thomas J., Rhode, Katherine L., and Salzer, John J., E-mail: steele24@msu.edu. Sat . "VELOCITY STRUCTURE AND VARIABILITY OF [O III] EMISSION IN BLACK HOLE HOST GLOBULAR CLUSTER RZ2109". United States. doi:10.1088/0004-637X/739/2/95; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA).
@article{osti_21587466,
title = {VELOCITY STRUCTURE AND VARIABILITY OF [O III] EMISSION IN BLACK HOLE HOST GLOBULAR CLUSTER RZ2109},
author = {Steele, Matthew M. and Zepf, Stephen E. and Kundu, Arunav and Maccarone, Thomas J. and Rhode, Katherine L. and Salzer, John J., E-mail: steele24@msu.edu},
abstractNote = {We present a multi-facility study of the optical spectrum of the extragalactic globular cluster RZ2109, which hosts a bright black hole X-ray source. The optical spectrum of RZ2109 shows strong and very broad [O III] {lambda}{lambda}4959, 5007 emission in addition to the stellar absorption lines typical of a globular cluster. We use observations over an extended period of time to constrain the variability of these [O III] emission lines. We find that the equivalent width of the lines is similar in all of the data sets; the change in L[O III] {lambda}5007 is {approx}<10% between the first and last observations, which were separated by 467 days. The velocity profile of the line also shows no significant variability over this interval. Using a simple geometric model, we demonstrate that the observed [O III] {lambda}5007 line velocity structure can be described by a two-component model with most of the flux contributed by a bipolar conical outflow of about 1600 km s{sup -1}, and the remainder from a Gaussian component with an FWHM of several hundred km s{sup -1}.},
doi = {10.1088/0004-637X/739/2/95; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 739,
place = {United States},
year = {2011},
month = {10}
}