The globular cluster system of NGC 1399

Schuberth, Y.; Richtler, T.; Hilker, M.; Dirsch, B.; Bassino, L. P.; Romanowsky, Aaron J.; Infante, L.

doi:10.1051/0004-6361/200912482

Cited by 188 publications

(386 citation statements)

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“…The most extended stellar kinematics for NGC1399 reaches a distance of R=97 arcsec (∼9.4 kpc) (Saglia et al 2000), so it does not map the regions of the exponential component. At these large radii, the kinematics is traced by GCs and PNe out to ∼13 arcmin (McNeil et al 2010;Schuberth et al 2010), thus almost out to the region of the break. The kinematics of red and blue GCs are distinct.…”

Section: Which Kind Of Physical Structure Is the Outer Exponential Comentioning

confidence: 97%

“…This galaxy has been studied in detail over a wide wavelength range, from radio to X-ray. NGC1399 is characterized by a large number of compact stellar systems (GCs and UCDs), for which several studies have provided the number-density distribution and stellar population estimates (Dirsch et al 2003;Mieske et al 2004;Bassino et al 2006;Schuberth et al 2010;Puzia et al 2014;Voggel et al 2016).…”

Section: Introductionmentioning

confidence: 99%

“…The most extended kinematics of the stars (out to ∼90 arcsec) was derived by Saglia et al (2000): it shows a small rotation (∼30 km s −1 ) and a high stellar velocity dispersion in the center (∼370 km s −1 ), which decreases at larger radii and remains constant at 250-270 km s −1 . At larger radii, out to ∼13 arcmin, the kinematics is traced by GCs and PNe (McNeil et al 2010;Schuberth et al 2010). The kinematics of red and blue GCs are distinct, with red GCs having velocity dispersions consistent with that of stars, while blue GCs are more erratic, showing a higher velocity dispersion, 300 σ 400 km s −1 (Schuberth et al 2010).…”

Section: Introductionmentioning

confidence: 99%

“…At larger radii, out to ∼13 arcmin, the kinematics is traced by GCs and PNe (McNeil et al 2010;Schuberth et al 2010). The kinematics of red and blue GCs are distinct, with red GCs having velocity dispersions consistent with that of stars, while blue GCs are more erratic, showing a higher velocity dispersion, 300 σ 400 km s −1 (Schuberth et al 2010). The velocity dispersions of the PNe are consistent with the values derived by the star's kinematics and with those for the red GCs (Napolitano et al 2002;McNeil et al 2010).…”

Section: Introductionmentioning

confidence: 99%

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THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

Iodice

Capaccioli

Grado

et al. 2016

ApJ

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We have started a new, deep multi-imaging survey of the Fornax cluster, dubbed the Fornax Deep Survey (FDS), at the VLT Survey Telescope (VST). In this paper we present the deep photometry inside two square degrees around the bright galaxy NGC1399 in the core of the cluster. We found that the core of the Fornax cluster is characterized by a very extended and diffuse envelope surrounding the luminous galaxy NGC1399: we map the surface brightness out to 33 arcmin (∼192 kpc) from the galaxy center and down to μ g ∼31 mag arcsec −2 in the g band. The deep photometry allows us to detect a faint stellar bridge in the intracluster region on the west side of NGC1399 and toward NGC1387. By analyzing the integrated colors of this feature, we argue that it could be due to the ongoing interaction between the two galaxies, where the outer envelope of NGC1387 on its east side is stripped away. By fitting the light profile, we found that there exists a physical break radius in the total light distribution at R=10 arcmin (∼58 kpc) that sets the transition region between the bright central galaxy and the outer exponential halo, and that the stellar halo contributes 60% of the total light of the galaxy (Section 3.5). We discuss the main implications of this work on the build-up of the stellar halo at the center of the Fornax cluster. By comparing with the numerical simulations of the stellar halo formation for the most massive bright cluster galaxies (i.e., M M 13 log 14, we find that the observed stellar halo mass fraction is consistent with a halo formed through the multiple accretion of progenitors with stellar mass in the range 10 8 -10 11 M e . This might suggest that the halo of NGC1399 has also gone through a major merging event. The absence of a significant number of luminous stellar streams and tidal tails out to 192 kpc suggests that the epoch of this strong interaction goes back to an early formation epoch. Therefore, different from the Virgo cluster, the extended stellar halo around NGC1399 is characterized by a more diffuse and well-mixed component, including the intracluster light.

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Section: Which Kind Of Physical Structure Is the Outer Exponential Comentioning

confidence: 97%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

Iodice

Capaccioli

Grado

et al. 2016

ApJ

Self Cite

170

342

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show abstract

“…Moreover, in a number of nearby ETGs the kinematics of bGCs have been found to be significantly distinct from those of the stellar component and the rGCs (e.g. Schuberth et al 2010;Pota et al 2013).…”

Section: What Is the Origin Of Gc Metallicity Bimodality?mentioning

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

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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.

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The isolated elliptical galaxy NGC 5812–MOND or dark matter?

Richtler,

Salinas,

Lane

et al. 2023

Astron Nachr

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There exist isolated elliptical galaxies, whose dynamics can be modeled without resorting to dark matter or MOND, for example, NGC 7507. Such objects lack understanding within the current framework of galaxy formation. The isolated elliptical NGC 5812 is another object to investigate a possible role of isolation. We use globular clusters (GCs) and the galaxy light itself as dynamical tracers to constrain its mass profile. We employ Gemini/GMOS mask spectroscopy, apply the GMOS reduction procedures provided within IRAF, measure GC velocities by cross correlation methods and extract the line‐of‐sight kinematics of galaxy spectra using the tool pPXF. We identify 28 GCs with an outermost galactocentric distance of 20 kpc, for which velocities could be obtained. Furthermore, 16 spectra of the integrated galaxy light out to 6 kpc have been used to model the central kinematics. These spectra provide evidence for a disturbed velocity field, which is plausible given the disturbed morphology of the galaxy. We construct spherical Jeans models for the galaxy light and apply tracer mass estimators for the globular clusters. With the assumptions inherent to the mass estimators, MOND is compatible with the mass out to 20 kpc. However, a dark matter free galaxy is not excluded, given the uncertainties related to a possible nonsphericity and a possible nonequilibrium state. We find one globular cluster with an estimated mass of , the first Ultra Compact Dwarf in an isolated elliptical. We put NGC 5812 into the general context of dark matter or alternative ideas in elliptical galaxies. The case for a MONDian phenomenology also among early‐type galaxies has become so strong that deviating cases appear astrophysically more interesting than agreements. The baryonic Tully Fisher relation (BTFR) as predicted by MOND is observed in some samples of early‐type galaxies, in others not. However, in cases of galaxies that deviate from the MONDian prediction, data quality and data completeness are often problematic.

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The globular cluster system of NGC 1399

Cited by 188 publications

References 100 publications

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

THE FORNAX DEEP SURVEY WITH VST. I. THE EXTENDED AND DIFFUSE STELLAR HALO OF NGC 1399 OUT TO 192 kpc

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

The isolated elliptical galaxy NGC 5812–MOND or dark matter?

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