Globular Clusters and Spur Clusters in NGC 4921, the Brightest Spiral Galaxy in the Coma Cluster

Lee, Myung Gyoon; Jang, In Sung

doi:10.3847/0004-637x/819/1/77

Cited by 21 publications

(25 citation statements)

References 59 publications

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“…5 with a Sérsic law (Sérsic 1963), we obtain the Sérsic index values, n AGC = 1.41 ± 0.34 for all globular clusters, n BGC = 1.07±0.28 for the blue globular clusters, and n RGC = 1.89±0.83 for the red globular clusters. These values are similar to those of NGC 4921 (Lee & Jang 2016). The corresponding effective radii of the globular cluster systems are R eff,AGC = 0.…”

Section: Radial Distributions Of the Globular Clusterssupporting

confidence: 79%

“…We derived F 814W aperture correction values for the sources including star cluster candidates following the method as used in Lee & Jang (2016). The steps are as follows.…”

Section: Data Reductionmentioning

confidence: 99%

“…Although the Sérsic index value for the blue globular clusters is slightly smaller than that for the red globular clusters, the difference is within errors. In most massive galaxies, the blue globular clusters have a shallower density profile than the red globular clusters (Lee et al (1998); Brodie & Strader (2006) and references therein; see also Lee & Jang (2016); Cho et al (2016); Harris et al (2017)). Therefore, NGC 4589 is a rare example that shows both blue and red subpopulations that have similar radial profiles.…”

Section: Radial Distributions Of the Globular Clustersmentioning

confidence: 99%

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Star Clusters in the Elliptical Galaxy NGC 4589 Hosting a Calcium-rich SN Ib (SN 2005cz)

Lee

Jang

Kang

2019

ApJ

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NGC 4589, a bright E2 merger-remnant galaxy, hosts the peculiar fast and faint calcium-rich Type Ib supernova (SN) SN 2005cz. The progenitor of Ca-rich SNe Ib has been controversial: it could be a) a young massive star with 6-12 M in a binary system, or b) an old low-mass star in a binary system that was kicked out from the galaxy center. Moreover, previous distance estimates for this galaxy have shown a large spread, ranging from 20 Mpc to 60 Mpc. Thus, using archival Hubble Space T elescope/ACS F 435W , F 555W , and F 814W images, we search for star clusters in NGC 4589 in order to help resolve these issues. We find a small population of young star clusters with 25 < V ≤ 27 (−7.1 < M V ≤ −5.1) mag and age < 1 Gyr in the central region at R < 0. 5 (< 3.8 kpc), thus supporting the massive-star progenitor scenario for SN 2005cz. In addition to young star clusters, we also find a large population of old globular clusters. In contrast to previous results in the literature, we find that the color distribution of the globular clusters is clearly bimodal. The turnover (Vega) magnitude in the V -band luminosity functions of the blue (metal-poor) globular clusters is determined to be V 0 (max) = 24.40 ± 0.10 mag. We derive the total number of globular clusters, N GC = 640 ± 50, and the specific frequency, S N = 1.7 ± 0.2. Adopting a calibration for the metal-poor globular clusters, M V (max) = −7.66 ± 0.14 mag, we derive a distance to this galaxy: (m − M ) 0 = 32.06 ± 0.10(ran) ± 0.15(sys) (d = 25.8 ± 2.2 Mpc).

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Section: Radial Distributions Of the Globular Clusterssupporting

confidence: 79%

“…We derived F 814W aperture correction values for the sources including star cluster candidates following the method as used in Lee & Jang (2016). The steps are as follows.…”

Section: Data Reductionmentioning

confidence: 99%

Section: Radial Distributions Of the Globular Clustersmentioning

confidence: 99%

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Star Clusters in the Elliptical Galaxy NGC 4589 Hosting a Calcium-rich SN Ib (SN 2005cz)

Lee

Jang

Kang

2019

ApJ

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“…At the distance of the Coma cluster ( -» m M 35), a GC system with a standard Gaussian luminosity function for a low-mass earlytype galaxy (with mean M V = −7.3 mag; Miller & Lotz 2007) has a peak whose measurement is within the reach of these observations (V 0 ≈ 27.7 mag). Lee & Jang (2016) showed that GCLF distances to the Coma cluster can be obtained with HST imaging. For this analysis, we use our "deep" sample, which extends to V 606 = 29 mag.…”

Section: The Gc Luminosity Function and The Distance To Df17mentioning

confidence: 99%

A Rich Globular Cluster System in Dragonfly 17: Are Ultra-Diffuse Galaxies Pure Stellar Halos?*

Peng

Lim

2016

ApJL

123

141

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Observations of nearby galaxy clusters at low surface brightness have identified galaxies with low luminosities, but sizes as large as L å galaxies, leading them to be dubbed "ultra-diffuse galaxies" (UDGs). The survival of UDGs in dense environments like the Coma cluster suggests that UDGs could reside in much more massive dark halos. We report the detection of a substantial population of globular clusters (GCs) around a Coma UDG, Dragonfly 17 (DF17). We find that DF17 has a high GC specific frequency of S N = 26 ± 13. The GC system is extended, with an effective radius of 12″ ± 2″, or 5.6 ± 0.9 kpc at Coma distance, 70% larger than the galaxy itself. We also estimate the mean of the GC luminosity function to infer a distance of -+ 97 14 17 Mpc, providing redshift-independent confirmation that one of these UDGs is in the Coma cluster. The presence of a rich GC system in DF17 indicates that, despite its low stellar density, star formation was intense enough to form many massive star clusters. If DF17ʼs ratio of total GC mass to total halo mass is similar to those in other galaxies, then DF17 has an inferred total mass of ∼1011 M e , only ∼10% the mass of the Milky Way, but extremely dominated by dark matter, with M/L V ≈ 1000. We suggest that UDGs like DF17 may be "pure stellar halos," i.e., galaxies that formed their stellar halo components, but then suffered an early cessation in star formation that prevented the formation of any substantial central disk or bulge.

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“…In the CDF, two modes (MP and MR) are clearly present, and the MP mode is much more dominant for the IGC. Color-magnitude diagrams for the GC populations around both NGC 4874 and 4889 from HST ACS imaging are presented and briefly discussed by Lee & Jang (2016a), while Cho et al (2016) complete a more comprehensive discussion specifically for the NGC 4874 system, now including threecolor ( ) g I H , , photometry. A structural feature held in common by all four of the Galaxy clusters discussed here (Coma, A2052, A2147, and A2199 from Paper II) is a prominent X-ray halo gas component.…”

Section: Metallicity and Color Distributionsmentioning

confidence: 99%

Globular Cluster Systems in Brightest Cluster Galaxies. Iii. Beyond Bimodality

Harris

Ciccone

Eadie

et al. 2017

ApJ

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We present new deep photometry of the rich globular cluster (GC) systems around the Brightest Cluster Galaxies UGC 9799 (Abell 2052) and UGC 10143 (Abell 2147), obtained with the Hubble Space Telescope (HST) ACS and WFC3 cameras. For comparison, we also present new reductions of similar HST/ACS data for the Coma supergiants NGC 4874 and 4889. All four of these galaxies have huge cluster populations (to the radial limits of our data, comprising from 12,000 to 23,000 clusters per galaxy). The metallicity distribution functions (MDFs) of the GCs can still be matched by a bimodal-Gaussian form where the metal-rich and metalpoor modes are separated by 0.8 dex, but the internal dispersions of each mode are so large that the total MDF becomes very broad and nearly continuous from [Fe/H];−2.4 to solar. There are, however, significant differences between galaxies in the relative numbers of metal-rich clusters, suggesting that they underwent significantly different histories of mergers with massive gas-rich halos. Last, the proportion of metal-poor GCs rises especially rapidly outside projected radii  R R 4 eff , suggesting the importance of accreted dwarf satellites in the outer halo. Comprehensive models for the formation of GCs as part of the hierarchical formation of their parent galaxies will be needed to trace the systematic change in structure of the MDF with galaxy mass, from the distinctly bimodal form in smaller galaxies up to the broad continuum that we see in the very largest systems.

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Globular Clusters and Spur Clusters in NGC 4921, the Brightest Spiral Galaxy in the Coma Cluster

Cited by 21 publications

References 59 publications

Star Clusters in the Elliptical Galaxy NGC 4589 Hosting a Calcium-rich SN Ib (SN 2005cz)

Star Clusters in the Elliptical Galaxy NGC 4589 Hosting a Calcium-rich SN Ib (SN 2005cz)

A Rich Globular Cluster System in Dragonfly 17: Are Ultra-Diffuse Galaxies Pure Stellar Halos?*

Globular Cluster Systems in Brightest Cluster Galaxies. Iii. Beyond Bimodality

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