Wide-field imaging of NGC 4365’s globular cluster system: the third subpopulation revisited

Blom, Christina; Spitler, Lee R.; Forbes, Duncan A.

doi:10.1111/j.1365-2966.2011.19963.x

Cited by 76 publications

(141 citation statements)

References 73 publications

Supporting

Mentioning

121

Contrasting

Unclassified

Order By: Relevance

“…VUCD7 and UCD3 have effective radii on the order of 90 pc, while HUCD1 and M59cO have effective radii of 25 and 32 pc, respectively. (Blom et al 2012). The grey triangle shows the median effective radius, when these exceptionally bright compact GCs were removed in the bin at M V = −13.0 mag.…”

Section: Discussionmentioning

confidence: 99%

“…In their central HST field, Blom et al (2012) found 681 compact clusters and 30 EOs, i.e. the EOs add about 4.4% to the GC sample in the central region of NGC 4365.…”

Section: Eos In Early-type Galaxiesmentioning

confidence: 99%

“…EOs were detected in a large number of elliptical galaxies: NGC 5128 (Gomez et al 2006;McLaughlin et al 2008;Chattopadhyay et al 2009;Taylor et al 2010;Mouhcine et al 2010 (Haşegan et al 2005;Evstigneeva et al 2008;Brodie et al 2011;Chies-Santos et al 2011), M 84 (Chies-Santos et al 2011, the central galaxy of the Fornax Cluster NGC 1399 (Richtler et al 2005;Evstigneeva et al 2007;Hilker et al 2007;Evstigneeva et al 2008;Chilingarian et al 2011), NGC 3923 (Norris & Kannappan 2011), NGC 4476 (Haşegan et al 2005), NGC 5846 (Chies-Santos et al 2006), NGC 4696 (Mieske et al 2007), NGC 3311 ), IC 4041, NGC 4889, IC 3998, IC 4030, IC 4041, and NGC 4908 (Chiboucas et al 2011), NGC 4874 (Madrid et al 2010Chiboucas et al 2011), NGC 1132(Madrid 2011), NGC 1275(Penny et al 2012, NGC 4365 (Blom et al 2012), NGC 1316 (Goudfrooij 2012), NGC 1199(Da Rocha et al 2011, and ESO325-G004 (Blakeslee & Barber 2008).…”

Section: Eos In Early-type Galaxiesmentioning

confidence: 99%

“…Four EOs are found with luminosities brighter than M V = −8. Another example is the giant elliptical galaxy NGC 4365, which was covered by eight HST ACS fields (Blom et al 2012). Seven HST ACS fields provide a very good coverage and −8 mag.…”

Section: Eos In Early-type Galaxiesmentioning

confidence: 99%

See 3 more Smart Citations

A catalog of extended clusters and ultra-compact dwarf galaxies

Kroupa

2012

A&A

View full text Add to dashboard Cite

Context. In the past decade, very extended old stellar clusters with masses in the range from a few 10 4 to 10 8 M and effective radii larger than 10 pc have been found in various types of galaxies in different environments. Objects with masses comparable to normal globular clusters (GCs) are called extended clusters (ECs), while objects with masses in the dwarf galaxy regime are called ultra-compact dwarf galaxies (UCDs). Aims. The paper analyses the observational parameters total luminosity, M V , effective radius, r eff , and projected distance to the host galaxy, R proj , of all known ECs and UCDs and the dependence of these parameters on the type and the total luminosity of their host galaxy. Methods. We searched the available literature to compile a catalog of star clusters with effective radii larger than 10 pc. As there is no clear distinction between ECs and UCDs, both types of objects will be called extended stellar objects -abbreviated "EOs" -in this paper.Results. In total, we found 813 EOs of which 171 are associated with late-type galaxies and 642 EOs associated with early-type galaxies. EOs cover a luminosity range from about M V = −4 to −14 mag. However, the vast majority of EOs brighter than M V = −10 mag are associated with giant elliptical galaxies. At each magnitude extended objects are found with effective radii between 10 pc and an upper size limit, which shows a clear trend: the more luminous the object the larger is the upper size limit. For EOs associated with early-and late-type galaxies, the EO luminosity functions peak at −6.40 mag and −6.47 mag, respectively, which is about one magnitude fainter than the peak of the GC luminosity function. EOs and GCs form a coherent structure in the r eff vs. M V parameter space, while there is a clear gap between EOs and early-type dwarf galaxies. However, there is a small potential overlap at the high-mass end, where the most extended EOs are close to the parameters of some compact elliptical galaxies. We compare the EO sample with the numerical models of a previous paper and conclude that the parameters of the EO sample as a whole can be very well explained by a star cluster origin, where EOs are the results of merged star clusters of cluster complexes.

show abstract

Section: Discussionmentioning

confidence: 99%

“…In their central HST field, Blom et al (2012) found 681 compact clusters and 30 EOs, i.e. the EOs add about 4.4% to the GC sample in the central region of NGC 4365.…”

Section: Eos In Early-type Galaxiesmentioning

confidence: 99%

Section: Eos In Early-type Galaxiesmentioning

confidence: 99%

Section: Eos In Early-type Galaxiesmentioning

confidence: 99%

See 2 more Smart Citations

A catalog of extended clusters and ultra-compact dwarf galaxies

Kroupa

2012

A&A

View full text Add to dashboard Cite

show abstract

“…Blom, Spitler & Forbes (2012) presented the (g − i) colour profiles obtained from Subaru/Suprime-Cam photometry for the three subpopulations. For the purposes of a spectroscopic/photometric metallicity comparison, we consider only the rGC and the bGC colour profiles in their work and exclude the central "green" GCs.…”

Section: 6mentioning

confidence: 99%

The SLUGGS survey: combining stellar and globular cluster metallicities in the outer regions of early-type galaxies

Pastorello

Forbes

Usher

et al. 2015

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

The outer halo regions of early-type galaxies carry key information about their past accretion history. However, spectroscopically probing the stellar component at such galactocentric radii is still challenging. Using Keck/DEIMOS, we have been able to measure the metallicities of the stellar and globular cluster components in 12 early-type galaxies out to more than 10 R e . We find similar metallicity gradients for the metalpoor and metal-rich globular cluster subpopulations, suggesting a common formation process for the two subpopulations. This is in conflict with most current theoretical predictions, where the metal-poor globular clusters are thought to be purely accreted and metal-rich globular clusters mostly formed in-situ. Moreover, we find that the globular cluster metallicity gradients show a trend with galaxy mass, being steeper in lower-mass galaxies than in higher-mass galaxies. This is similar to what we find for the outermost galaxy stars and suggests a more active accretion history, with a larger role played by major mergers, in the most massive galaxies. This conclusion is qualitatively consistent with expectations from two-phase galaxy assembly models. Finally, we find that the small difference in metallicity between galaxy stars and metal-rich globular clusters at 1 R e may correlate with galaxy mass. The origin of this difference is not currently clear.

show abstract

Globular Cluster Systems and Galaxy Formation

Beasley

2020

Reviews in Frontiers of Modern Astrophysics

View full text Add to dashboard Cite

Wide-field imaging of NGC 4365’s globular cluster system: the third subpopulation revisited

Cited by 76 publications

References 73 publications

A catalog of extended clusters and ultra-compact dwarf galaxies

A catalog of extended clusters and ultra-compact dwarf galaxies

The SLUGGS survey: combining stellar and globular cluster metallicities in the outer regions of early-type galaxies

Globular Cluster Systems and Galaxy Formation

Contact Info

Product

Resources

About