TY - JOUR
T1 - Velocity structure and variability of [O III] emission in black hole host globular cluster RZ2109
AU - Steele, Matthew M.
AU - Zepf, Stephen E.
AU - Kundu, Arunav
AU - MacCarone, Thomas J.
AU - Rhode, Katherine L.
AU - Salzer, John J.
PY - 2011/10/1
Y1 - 2011/10/1
N2 - 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]λλ4959, 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]λ5007 is ≲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]λ5007 line velocity structure can be described by a two-component model with most of the flux contributed by a bipolar conical outflow of about 1600kms-1, and the remainder from a Gaussian component with an FWHM of several hundredkms -1.
AB - 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]λλ4959, 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]λ5007 is ≲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]λ5007 line velocity structure can be described by a two-component model with most of the flux contributed by a bipolar conical outflow of about 1600kms-1, and the remainder from a Gaussian component with an FWHM of several hundredkms -1.
KW - X-rays: binaries
KW - X-rays: galaxies: clusters
KW - galaxies: individual (NGC 4472)
KW - galaxies: star clusters: individual (NGC 4472)
KW - globular clusters: general
UR - http://www.scopus.com/inward/record.url?scp=80053463720&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/739/2/95
DO - 10.1088/0004-637X/739/2/95
M3 - Article
AN - SCOPUS:80053463720
VL - 739
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 95
ER -