J/A+A/625/A50 Ultra compact dwarf galaxies catalog (Fahrion+, 2019)
Single metal-poor ultra compact dwarf galaxy at one kiloparsec distance from the
low-mass elliptical galaxy FCC 47.
Fahrion K., Georgiev I., Hilker M., Lyubenova M., van de Ven G.,
Alfaro-Cuello M., Corsini E.M., Sarzi M., McDermid R.M., de Zeeuw T.
<Astron. Astrophys. 625, A50 (2019)>
=2019A&A...625A..50F 2019A&A...625A..50F (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Radial velocities ; Morphology
Keywords: galaxies: individual: NGC 1336 - galaxies: dwarf -
galaxies: nuclei - galaxies: kinematics and dynamics
Abstract:
Photometric surveys of galaxy clusters have revealed a large number of
ultra compact dwarfs (UCDs) around predominantly massive elliptical
galaxies. Their origin is still debated as some UCDs are considered to
be the remnant nuclei of stripped dwarf galaxies while others seem to
mark the high-mass end of the star cluster population.
We aim to characterize the properties of a UCD found at very close
projected distance (rwproj=1.1kpc) from the centre of the low-mass
(M∼1010M☉) early-type galaxy FCC 47. This is a serendipitous
discovery from MUSE adaptive optics science verification data. We
explore the potential origin of this UCD as either a massive cluster
or the remnant nucleus of a dissolved galaxy.
We used archival Hubble Space Telescope data to study the photometric
and structural properties of FCC 47-UCD1. In the MUSE data, the UCD is
unresolved, but we used its spectrum to determine the radial velocity
and metallicity.
The surface brightness of FCC 47-UCD1 is best described by a single
King profile with low concentration C=Rt/Rc∼10 and large effective
radius (reff=24pc). Its integrated magnitude and blue colour
(Mg=-10.55mag, (g-z)=1.46mag) combined with a metallicity of
[M/H]=-1.12±0.10dex and an age >8Gyr obtained from the full fitting
of the MUSE spectrum suggests a stellar population mass of
M*=4.87x106M☉. The low S/N of the MUSE spectrum prevents
detailed stellar population analysis. Due to the limited spectral
resolution of MUSE, we can only give an upper limit on the velocity
dispersion (σ<17km/s), and consequently on its dynamical mass
(Mdyn<1.3x107M☉).
The origin of the UCD cannot be constrained with certainty. The low
metallicity, old age, and magnitude are consistent with a star cluster
origin, whereas the extended size is consistent with an origin as the
stripped nucleus of a dwarf galaxy with a initial stellar mass of a
few 108M☉.
Description:
File tableb1 contains a compilation of literature ultra compact dwarf
galaxies. For each UCD, name, host name, coordinates, radial velocity,
the projected distance to the host galaxy and the reference are given.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 89 381 Table of literature UCDs
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See also:
V/143 : Revised Bologna Catalog of M31 clusters, V.5 (Galleti+ 2012)
J/A+A/416/917 : Revised Bologna Catalog of M31 globular clusters
(Galleti+, 2004)
J/MNRAS/414/3699 : Study of hot stellar systems and galaxies (Misgeld+, 2011)
J/A+A/472/111 : Centaurus Compact Object Survey (Mieske+, 2007)
J/ApJ/812/34 : Properties of UCD candidates in M87/M49/M60 regions
(Liu+, 2015)
J/AJ/142/199 : Sizes and luminosities of stellar systems (Brodie+, 2011)
Byte-by-byte Description of file:tableb1.dat
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Bytes Format Units Label Explanations
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1- 19 A19 --- Name Name of the UCD
21- 35 A15 --- Host Name of the host galaxy
37- 38 I2 h RAh ? Right ascension (J2000)
40- 41 I2 min RAm ? Right ascension (J2000)
43- 47 F5.2 s RAs ? Right ascension (J2000)
49 A1 --- DE- Declination sign (J2000)
50- 51 I2 deg DEd ? Declination (J2000)
53- 54 I2 arcmin DEm ? Declination (J2000)
56- 60 F5.2 arcsec DEs ? Declination (J2000)
62- 67 F6.1 km/s RV Radial velocity
69- 74 F6.2 mag VMAG Absolute V band magnitude
76- 80 F5.1 kpc rproj Projected distance to host
82- 86 F5.2 pc reff Effective radius
88- 89 I2 --- Ref [0/13]? Reference number (1)
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Note (1): Reference as follows:
0 = This work
1 = Mieske et al. (2008A&A...487..921M 2008A&A...487..921M), some positions from
Brodie et al. (2011AJ....142..199B 2011AJ....142..199B, Cat. J/AJ/142/199) and
Misgeld & Hilker (2011MNRAS.414.3699M 2011MNRAS.414.3699M, Cat. J/AJ/142/199)
2 = Brodie et al. (2011AJ....142..199B 2011AJ....142..199B, Cat. J/AJ/142/199)
3 = Liu et al. (2015ApJ...812...34L 2015ApJ...812...34L, Cat. J/ApJ/812/34)
4 = Norris & Kannappan (2011MNRAS.414..739N 2011MNRAS.414..739N)
5 = Maraston et al. (2003IAUJD...6E..18M 2003IAUJD...6E..18M)
6 = Ma et al. (2017MNRAS.468.4513M 2017MNRAS.468.4513M)
7 = Evstigneeva et al. (2007AJ....133.1722E 2007AJ....133.1722E)
8 = Mieske et al. (2007A&A...472..111M 2007A&A...472..111M, Cat. J/A+A/472/111)
9 = Mieske et al. (2009A&A...498..705M 2009A&A...498..705M)
10 = Misgeld et al. (2011MNRAS.414.3699M 2011MNRAS.414.3699M, Cat. J/MNRAS/414/3699)
11 = Galleti et al. (2004A&A...416..917G 2004A&A...416..917G, Cat. J/A+A/416/917)
12 = Sandoval et al. (2015ApJ...808L..32S 2015ApJ...808L..32S)
13 = Janz et al. (2016MNRAS.456..617J 2016MNRAS.456..617J)
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Acknowledgements:
Katja Fahrion, kfahrion(at)eso.org
(End) Patricia Vannier [CDS] 03-Apr-2019