Globular Cluster Systems in Fornax

Kissler-Patig, M.; Kohle, S.; Hilker, M.; Richtler, T.; Infante, L.; Quintana, H.

doi:10.1007/978-94-009-0229-9_149

Cited by 55 publications

(126 citation statements)

References 0 publications

Supporting

Mentioning

103

Contrasting

Unclassified

Order By: Relevance

“…With regard to the globular cluster system of NGC 1399, the Washington photometry by Ostrov et al (1993) confirmed the existence of a color gradient that had been detected earlier by Bridges et al (1991), and suggested that the color distribution was multimodal, as was also supported by the V, I photometry by Kissler-Patig et al (1997). The HST imaging by Forbes et al (1998) and Grillmair et al (1999), and a refined Send offprint requests to: L. P. Bassino, e-mail: lbassino@fcaglp.fcaglp.unlp.edu.ar Based on observations obtained at Cerro Tololo Inter-American Observatory, NOAO, which is operated by AURA, Inc., under cooperative agreement with the National Science Foundation.…”

Section: Introductionsupporting

confidence: 64%

Globular cluster candidates within the Fornax Cluster: Intracluster globulars?

Bassino

Cellone

Forte

et al. 2003

A&A

View full text Add to dashboard Cite

Abstract. We present the results of a search for globular clusters in the surroundings of 15 low surface brightness dwarf galaxies belonging to the Fornax Cluster, which was carried out on CCD images obtained with the C and T 1 filters of the Washington photometric system. The globular cluster candidates show an extended and probably bimodal (C − T 1 ) color distribution, which is inconsistent with the presence of a single population of metal-poor clusters detected in several dwarf galaxies. The surface number density of these candidates shows no concentration towards the respective dwarf galaxies, in whose outskirts they have been identified. On the contrary, if we split the candidates in two groups according to their projected distances to the center of the Fornax Cluster, those located closer to the center show a higher projected density than those located farther from it. These results suggest that the potential globular clusters might not be bound to the dwarf galaxies. Alternatively, these globulars could form part of the very peripheral regions of NGC 1399 (the central galaxy of the Fornax Cluster) or even belong to the intracluster medium.

show abstract

Section: Introductionsupporting

confidence: 64%

Globular cluster candidates within the Fornax Cluster: Intracluster globulars?

Bassino

Cellone

Forte

et al. 2003

A&A

View full text Add to dashboard Cite

show abstract

“…Our estimate of N tot is consistent with the value 380±100 quoted by Harris (1996), and is 40% larger than the value 314 ± 63 estimated by Kissler-Patig et al (1997a). Our HST observations of the inner regions of the globular cluster system have reduced the uncertainty in N tot considerably over estimates from ground-based studies.…”

Section: Total Number and Specific Frequencysupporting

confidence: 87%

“…Figure 10b shows the radial profile for the sample with B < 25.5, with a background of 2.7 objects per arcmin 2 subtracted. Superposed is a curve representing the surface brightness profile of the underlying galaxy from Kissler-Patig et al (1997a), scaled arbitrarily to match the profile of the globular cluster system. The two profiles agree well at ∼ 35 − 70…”

Section: Radial Profilementioning

confidence: 99%

HSTimaging of the globular clusters in the Fornax cluster: NGC 1379

Elson¹,

Grillmair²,

Forbes³

et al. 1998

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present B and I photometry for ∼ 300 globular cluster candidates in NGC 1379, an E0 galaxy in the Fornax Cluster. Our data are from both Hubble Space Telescope (HST) and ground-based observations. The HST photometry (B only) is essentially complete and free of foreground/background contamination to ∼ 2 mag fainter than the peak of the globular cluster luminosity function. Fitting a Gaussian to the luminosity function we find B = 24.95 ± 0.30 and σ B = 1.55 ± 0.21. We estimate the total number of globular clusters to be 436 ± 30. To a radius of 70 arcsec we derive a moderate specific frequency, S N = 3.5 ± 0.4. At radii r ∼ 3 − 6 kpc the surface density profile of the globular cluster system is indistinguishable from that of the underlying galaxy light. At r ∼ < 2.5 kpc the profile of the globular cluster system flattens, and at r ∼ < 1 kpc, the number density appears to decrease. The (B − I) colour distribution of the globular clusters (from ground-based data) is similar to that for Milky Way globulars, once We stress the importance of corrections for background contamination in ground-based samples of this kind: the area covered by a globular cluster system (with radius ∼ 30 kpc) at the distance of the Virgo or Fornax cluster contains ∼ > 200 background galaxies unresolved from the ground, with magnitudes comparable to brighter globular clusters at that distance. The colour distribution of these galaxies is strongly peaked slightly bluer than the peak of a typical globular cluster distribution. Such contamination can thus create the impression of skewed colour distributions, or even of bimodality, where none exists.

show abstract

“…They are often used to constrain galaxy formation models (e.g. Harris 1991; Ashman & Zepf 1992;Forbes et al 1997;Kissler-Patig 2000;Brodie & Strader 2006;Harris 2010;Muratov & Gnedin 2010;Tonini 2013;Brodie et al 2014, and references therein).…”

Section: Introductionmentioning

confidence: 99%

Optical-near-IR analysis of globular clusters in the IKN dwarf spheroidal: a complex star formation history

Tudorica

Georgiev

Chies-Santos

2015

A&A

View full text Add to dashboard Cite

Context. Age, metallicity, and spatial distribution of globular clusters (GCs) provide a powerful tool for reconstructing major starformation episodes in galaxies. IKN is a faint dwarf spheroidal (dSph) in the M 81 group of galaxies. It contains five old GCs, which makes it the galaxy with the highest known specific frequency (S N = 126). Aims. We estimate the photometric age, metallicity, and spatial distribution of the poorly studied IKN GCs. We search SDSS for GC candidates beyond the HST/ACS field of view, which covers half of IKN. Methods. To break the age-metallicity degeneracy in the V −I colour, we used WHT/LIRIS K S -band photometry and derived photometric ages and metallicities by comparison with SSP models in the V, I, K s colour space. Results. IKN GCs' V IK s colours are consistent with old ages (≥8 Gyr) and a metallicity distribution with a higher mean than is typical for such a dSph ([Fe/H] −1.4 +0.6 −0.2 dex). Their photometric mass range (0.5 < M GC < 4 × 10 5 M ) implies an unusually high mass ratio between GCs and field stars, of 10.6%. Mixture model analysis of the RGB field stars' metallicity suggests that 72% of the stars may have formed together with the GCs. Using the most massive GC−SFR relation, we calculated a star formation rate (SFR) of ∼10 M /yr during its formation epoch. We note that the more massive GCs are closer to the galaxy photometric centre. IKN GCs also appear spatially aligned along a line close to the major axis of the IKN and nearly orthogonal to the plane of spatial distribution of galaxies in the M 81 group. We identify one new IKN GC candidate based on colour and the PSF analysis of the SDSS data. Conclusions. The evidence of i) broad and high metallicity distribution of the field IKN RGB stars and its GCs, ii) high fraction, and iii) spatial alignment of IKN GCs supports a scenario for tidally triggered, complex IKN's star formation history in the context of interactions with galaxies in the M 81 group.

show abstract

Globular Cluster Systems in Fornax

Cited by 55 publications

References 0 publications

Globular cluster candidates within the Fornax Cluster: Intracluster globulars?

Globular cluster candidates within the Fornax Cluster: Intracluster globulars?

HSTimaging of the globular clusters in the Fornax cluster: NGC 1379

Optical-near-IR analysis of globular clusters in the IKN dwarf spheroidal: a complex star formation history

Contact Info

Product

Resources

About