C.D.S. - SIMBAD4 rel 1.7 - 2020.11.30CET21:24:18

1999AJ....118..831B - Astron. J., 118, 831-842 (1999/August-0)

CO band head spectroscopy of IC 342: mass and age of the nuclear star cluster.


Abstract (from CDS):

We have used the NASA Infrared Telescope Facility (IRTF) to observe the nuclear stellar cluster in the nearby, face-on, giant Scd spiral IC 342. From high-resolution (λ/Δλ=21,500) spectra of the 12CO (2-0) band head at 2.3 µm, we derive a line-of-sight stellar velocity dispersion σ=(33±3) km.s–1.

To interpret this observation we construct dynamical models based on the Jeans equation for a spherical system. The light distribution of the cluster is modeled using an archival Hubble Space Telescope (HST) V-band image and a new ground-based K-band image. Under the assumption of an isotropic velocity distribution, the observed kinematics imply a K-band mass-to-light ratio M/LK=0.05, and a cluster mass M~6x106 M. We compare the derived mass-to-light ratio with the ``Starburst99'' stellar population synthesis models of Leitherer and collaborators and infer a best-fitting cluster age in the range 106.8–7.8 yr. Although this result depends somewhat on a number of uncertainties in the modeling (e.g., the assumed extinction along the line of sight toward the nucleus, the initial mass function of the stellar population model, and the velocity dispersion anisotropy of the cluster), none of the model parameters can be plausibly modified to yield a significantly larger age. Also, the inferred age is consistent with that found in our previous study based on the near-infrared absorption-line equivalent widths of the cluster (Böker, Förster-Schreiber, & Genzel).

Recent HST observations of large samples of spiral galaxies have shown that nuclear stellar clusters are very common in intermediate- to late-type spirals. The cluster in IC 342 is more luminous than the clusters found in most other nearby spiral galaxies. If the nuclear stellar clusters in spiral galaxies all have a mass similar to that of the cluster in IC 342, then stellar population synthesis models indicate a median age for these clusters of several Gyr. This may be consistent with a scenario in which each spiral galaxy has only one episode of nuclear star cluster formation. On the other hand, the incidence of young nuclear star clusters may be high enough to indicate that the formation of these clusters is a recurring phenomenon. Age and population studies for a larger sample of galaxies are necessary to distinguish between these scenarios and to determine how these nuclear stellar clusters are related to the secular evolution of their environment.

As a by-product of our analysis, we infer that IC 342 cannot have any central black hole more massive than 5x105 M. This is ∼6 times less massive than the black hole inferred to exist in our Galaxy, consistent with the accumulating evidence that galaxies with less massive bulges harbor less massive black holes.

Abstract Copyright:

Journal keyword(s): galaxies: individual (IC 342) - Galaxies: Kinematics and Dynamics - Galaxies: Nuclei

CDS comments: Nuclear star cluster = NAME IC 342 STAR CLUSTER

Simbad objects: 9

goto Full paper

goto View the reference in ADS

Number of rows : 9

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11101 1
2 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5214 1
3 LBN 659 GiG 02 36 35.469 +59 39 16.53   17       ~ 177 2
4 UGCA 39 GiG 02 41 55.092 +59 36 14.73   16       ~ 327 1
5 IC 342 SBG 03 46 48.514 +68 05 45.98   10.5       ~ 1397 1
6 NAME IC 342 Nuclear Star Cluster Cl* 03 46 48.7 +68 05 47           ~ 3 1
7 NAME IC 342 Group GrG 03 48 42 +68 00.8           ~ 98 1
8 NGC 1560 GiG 04 32 49.087 +71 52 59.20   12.1       ~ 241 0
9 UGCA 105 GiG 05 14 15.3240822656 +62 34 47.963432681   15.3       ~ 74 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 1999AJ....118..831B and select 'bookmark this link' or equivalent in the popup menu


© Université de Strasbourg/CNRS

    • Contact