Detailed surface photometry of the cD galaxies NGC 4839 and NGC 4874

Ali, Gamal B.; Shaban, Eman A.; Amin, Mohamed; Rassem, M.

doi:10.1007/s10509-014-1991-y

Cited by 2 publications

(3 citation statements)

References 24 publications

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“…1 = 11.6 ± 0.5 kpc. The surface brightness profile of NGC 4839 shows a slight excess over the fitting line at R > 1 , which is a cD envelope, consistent with the previous results in Schombert (1988); Ali et al (2014). On the other hand, this excess is much weaker in the case of NGC 4816.…”

Section: Radial Number Density Profiles Of the Gcssupporting

confidence: 90%

Globular Clusters in NGC 4839 Falling into Coma: Evidence for the Second Infall?

Oh¹,

Lee²,

Jang³

2023

Preprint

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NGC 4839 is the brightest galaxy (cD) of the NGC 4839 group at R ≈ 1 Mpc in the south-west of the Coma cluster, which is known to be falling into Coma. However, it has been controversial whether it is in the first phase of infall or in the second phase of infall after passing the Coma center. We present a wide field study of globular clusters (GCs) in NGC 4839 and its environment based on Hyper Suprime-Cam gr images in the Subaru archive. We compare the GC system of NGC 4839 with that of NGC 4816, which is the brightest member (S0) of the nearby group and lies at a similar distance in the west from the Coma center. Interestingly the spatial distribution of the GCs in NGC 4839 is significantly more compact than that of the GCs in NGC 4816. In addition, the radial number density profile of the GCs in NGC 4839 shows an abrupt drop at R N 4839 ≈ 80 kpc, while that of the GCs in NGC 4816 shows a continuous slow decline even in the outer region at 80 < R N 4816 < 500 kpc. The effective radius of the NGC 4839 GC system is about three times smaller than that of the NGC 4816 GC system. This striking difference can be explained if NGC 4839 lost a significant fraction of the GCs in its outskirt when it passed through Coma. This supports strongly the second infall scenario where the NGC 4839 passed the Coma center about 1.6 Gyr ago, and began the second infall after reaching the apocenter in the south-west recently.

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Section: Radial Number Density Profiles Of the Gcssupporting

confidence: 90%

Globular Clusters in NGC 4839 Falling into Coma: Evidence for the Second Infall?

Oh¹,

Lee²,

Jang³

2023

Preprint

View full text Add to dashboard Cite

show abstract

“…The effective radius of the NGC 4839 galaxy light, R eff,N4839 = 23 5 ± 0 7 = 11.4 ± 0.3 kpc, is similar to that of the NGC 4816 galaxy light, R eff,N4816 = 23 9 ± 1 1 = 11.6 ± 0.5 kpc. The surface brightness profile of NGC 4839 shows a slight excess over the fitting line at > ¢ R 1 , which is a cD envelope, consistent with the previous results in Schombert (1988), Ali et al (2014). On the other hand, this excess is much weaker in the case of NGC 4816.…”

Section: Radial Number Density Profiles Of the Gcssupporting

confidence: 89%

“…The main host of the NGC 4839 group is NGC 4839 (M V = − 23.1 mag, v h = 7338 km s −1 ), which is an elongated cD galaxy (Schombert 1988;Ali et al 2014). There are only two previous studies of the GCs in NGC 4839.…”

Section: Previous Studies Of Ngc 4839 Gcsmentioning

confidence: 99%

Globular Clusters in NGC 4839 Falling into Coma: Evidence for the Second Infall?

Oh¹,

Lee²,

Jang

2023

ApJ

View full text Add to dashboard Cite

NGC 4839 is the brightest galaxy (cD) of the NGC 4839 group at R ≈ 1 Mpc in the southwest of the Coma cluster, which is known to be falling into Coma. However, it has been controversial whether it is in the first phase of infall or in the second phase of infall after passing the Coma center. We present a wide field study of globular clusters (GCs) in NGC 4839 and its environment based on Hyper Suprime-Cam gr images in the Subaru archive. We compare the GC system of NGC 4839 with that of NGC 4816, which is the brightest member (S0) of the nearby group and lies at a similar distance in the west from the Coma center. Interestingly the spatial distribution of the GCs in NGC 4839 is significantly more compact than that of the GCs in NGC 4816. In addition, the radial number density profile of the GCs in NGC 4839 shows an abrupt drop at R N4839 ≈ 80 kpc, while that of the GCs in NGC 4816 shows a continuous slow decline even in the outer region at 80 < R N4816 < 500 kpc. The effective radius of the NGC 4839 GC system is about 3 times smaller than that of the NGC 4816 GC system. This striking difference can be explained if NGC 4839 lost a significant fraction of the GCs in its outskirt when it passed through Coma. This supports strongly the second-infall scenario where the NGC 4839 passed the Coma center about 1.6 Gyr ago, and began the second infall after reaching the apocenter in the southwest recently.

show abstract

Detailed surface photometry of the cD galaxies NGC 4839 and NGC 4874

Cited by 2 publications

References 24 publications

Globular Clusters in NGC 4839 Falling into Coma: Evidence for the Second Infall?

Globular Clusters in NGC 4839 Falling into Coma: Evidence for the Second Infall?

Globular Clusters in NGC 4839 Falling into Coma: Evidence for the Second Infall?

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