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Gemini/GMOS Spectroscopy of Globular Clusters in the Merger Remnant Galaxy M85
Authors
Narae Hwang
Youkyung Ko
+4Β more
Myung Gyoon Lee
Sungsoon Lim
Hong Soo Park
Jubee Sohn
Publication date
10 May 2018
Publisher
'American Astronomical Society'
Doi
View
on
arXiv
Abstract
M85 is a peculiar S0 galaxy in Virgo and is a well-known merger remnant. In this paper, we present the first spectroscopic study of globular clusters (GCs) in M85. We obtain spectra for 21 GC candidates and the nucleus of M85 using the Gemini Multi-Object Spectrograph on the Gemini North 8.1 m telescope. From their radial velocities, 20 of the GCs are found to be members of M85. We find a strong rotation signal of the M85 GC system with a rotation amplitude of 235 km s
β
1
^{-1}
β
1
. The rotation axis of the GC system has a position angle of about 161
β
^{\circ}
β
, which is 51
.
β
\rlap{.}{^\circ}
.
β
5 larger than that of the stellar light. The rotation-corrected radial velocity dispersion of the GC system is estimated to be
Ο
r
,
c
o
r
=
\sigma_{\rm r,cor} =
Ο
r
,
cor
β
=
160 km s
β
1
^{-1}
β
1
. The rotation parameter
Ξ©
R
i
c
o
r
/
Ο
r
,
c
o
r
\Omega R_{\rm icor}/\sigma_{\rm r,cor}
Ξ©
R
icor
β
/
Ο
r
,
cor
β
of the GC system is derived to be 1.47
β
0.48
+
1.05
^{+1.05}_{-0.48}
β
0.48
+
1.05
β
, which is one of the largest among known early-type galaxies. The ages and metallicities of the GCs, which show the same trend as the results based on Lick indices, are derived from full spectrum fitting (ULySS). About a half of the GCs are an intermediate-age population of which the mean age is
βΌ
\sim
βΌ
3.7
Β±
\pm
Β±
1.9 Gyr, having a mean [Fe/H] value of --0.26. The other half are old and metal-poor. These results suggest that M85 experienced a wet merging event about 4 Gyr ago, forming a significant population of star clusters. The strong rotational feature of the GC system can be explained by an off-center major merging.Comment: 20 pages, 13 figures, 7 tables, accepted for publication in Ap
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oai:s-space.snu.ac.kr:10371/20...
Last time updated on 09/09/2024
Crossref
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info:doi/10.3847%2F1538-4357%2...
Last time updated on 11/12/2019