J/MNRAS/457/2122 Nuclear star clusters photometric masses (Georgiev+, 2016)
Masses and scaling relations for nuclear star clusters, and their co-existence
with central black holes.
Georgiev I.Y., Boker T., Leigh N., Lutzgendorf N., Neumayer N.
<Mon. Not. R. Astron. Soc., 457, 2122-2138 (2016)>
=2016MNRAS.457.2122G 2016MNRAS.457.2122G (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Associations, stellar ; Stars, masses ;
Morphology
Keywords: galaxies: nuclei - galaxies: star clusters: general
Abstract:
Galactic nuclei typically host either a nuclear star cluster (NSC,
prevalent in galaxies with masses ≲1010M☉) or a massive black
hole (MBH, common in galaxies with masses ≳1012M☉). In the
intermediate-mass range, some nuclei host both an NSC and an MBH. In
this paper, we explore scaling relations between NSC mass (M*,gal)
and host-galaxy total stellar mass (MNSC) using a large sample of
NSCs in late- and early-type galaxies, including a number of NSCs
harbouring an MBH. Such scaling relations reflect the underlying
physical mechanisms driving the formation and (co)evolution of these
central massive objects. We find ∼1.5σ significant differences
between NSCs in late- and early-type galaxies in the slopes and
offsets of the relations reff,NSC-MNSC, reff,NSC-M*,gal
and MNSC-M*,gal, in the sense that (i) NSCs in late types are
more compact at fixed MNSC and M*,gal; and (ii) the
MNSC-M*,gal relation is shallower for NSCs in late types than in
early types, similar to the MBH-M*,bulge relation. We discuss
these results in the context of the (possibly ongoing) evolution of
NSCs, depending on host-galaxy type. For NSCs with an MBH, we
illustrate the possible influence of an MBH on its host NSC, by
considering the ratio between the radius of the MBH sphere of
influence and reff,NSC. NSCs harbouring a sufficiently massive black
hole are likely to exhibit surface brightness profile deviating from a
typical King profile.
Description:
We presented an updated analysis of various scaling relations between
NSC properties (mass and size) and the stellar mass of their host
galaxies. We compared these scaling relations between late- and
early-type host galaxies, aided by the recent compilation of NSC
properties in a large sample of late-type galaxies (Georgiev & Boeker
2014, Cat. J/MNRAS/441/3570). We added literature estimates of NSC
properties in a number of other late- and early-type galaxies. Of
special relevance are data for NSCs that harbour a MBH.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 132 228 Photometric masses of Nuclear Star Clusters (NSC)
and their host galaxies
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See also:
J/MNRAS/441/3570 : Nuclear star clusters in 228 spiral gal. (Georgiev+, 2014)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Gal NSC host galaxy ID
14- 18 F5.2 mag m-M Adopted distance modulus
20- 23 F4.1 --- TType Galaxy morphological code (1)
25- 29 F5.2 pc reffNSC NSC effective radius measured in F606W or
F814W or F450W or F300W, as available in
this order (2)
31- 35 F5.2 pc e_reffNSC Error on reffNSC (lower value)
37- 40 F4.2 pc E_reffNSC Error on reffNSC (upper value)
42- 49 F8.2 10+4Msun MNSC NSC mass calculated using the M/L given
in M/Lgal (3)
51- 58 F8.2 10+4Msun e_MNSC Error on MNSC (lower value)
60- 67 F8.2 10+4Msun E_MNSC Error on MNSC (upper value)
69- 76 F8.2 10+7Msun Mgal* NSC host galaxy stellar mass (4)
78- 85 F8.2 10+7Msun e_Mgal* rms uncertainty on Mgal*
87- 94 F8.2 10+7Msun MgalHI NSC host galaxy HI mass (4)
96-103 F8.2 10+7Msun e_MgalHI rms uncertainty on MgalHI
105-109 A5 --- FNSC [UBVRI ] NSC filter used
110-114 F5.2 Msun/Lsun M/LNSC NSC mass-to-light ratio
116-119 F4.2 Msun/Lsun e_M/LNSC Error on M/LNSC (lower value)
121-124 F4.2 Msun/Lsun E_M/LNSC Error on M/LNSC (upper value)
126-127 A2 --- Fgal [BVI ] Galaxy filter used
129-132 F4.2 Msun/Lsun M/Lgal Host galaxy mass-to-light ratio
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Note (1): (1-2-3) are the same as in Georgiev and Boeker,
2014MNRAS.441.3570G 2014MNRAS.441.3570G, Cat. J/MNRAS/441/357.
Note (2): We note that differences in sizes in the different bands are <10%
(see Georgiev and Boeker, 2014MNRAS.441.3570G 2014MNRAS.441.3570G) for discussion.
Note (3): NSC mass for the F606W (V) or F814W (I) or F450W (B) or F300W (U)
filter in this priority order, e.g. if Colour is UBVI, the value is the
M/LV error weighted average from the M/LVs from the various colour combinations
containing V-band.
Note (4): NSC host galaxy stellar and HI mass, where the used colour and M/LB
are in columns Fgal and M/Lgal.
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History:
* 07-Sep-2016 : From electronic version of the journal
* 17-Jul-2017 : units of Mgal* and MgalHI corrected
(End) Patricia Vannier [CDS] 06-Sep-2016