Counter-dispersed slitless-spectroscopy technique: planetary nebula velocities in the halo of NGC 1399

McNeil, Emily; Arnaboldi, M.; Freeman, K. C.; Gerhard, Ortwin; Coccato, L.; Das, Payel

doi:10.1051/0004-6361/201014428

Cited by 39 publications

(73 citation statements)

References 50 publications

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“…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). The X-ray data have shown the presence of a hot gaseous halo associated with NGC1399, which extends out to about 90 kpc (Paolillo et al 2002).…”

Section: Introductionsupporting

confidence: 81%

“…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%

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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

174

342

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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: Introductionsupporting

confidence: 81%

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

confidence: 97%

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

174

342

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show abstract

“…The kinematics of the ICL contains the fossil records of past interactions, due to the long dynamical timescale, and thus helps in reconstructing the processes that dominate the evolution of galaxies in clusters and the formation of the ICL (Napolitano et al 2003;Rudick et al 2006;Gerhard et al 2007;Murante et al 2007;. The kinematics in the cD halos can be used to separate cluster from galaxy components, as shown in simulations ; so far, however, the observational results are not unanimous: in both NGC 6166 in Abell 2199 (Kelson et al 2002) as well as NGC 3311 in Abell 1060 (Ventimiglia et al 2010b) the velocity dispersion profile in the outer halo rises to nearly cluster values, whereas in the Fornax cD galaxy NGC 1399 (McNeil et al 2010) and in the central Coma BCGs (Coccato et al 2010) the velocity dispersion profiles remain flat, and in M 87 in Virgo (Doherty et al 2009) it appears to fall steeply to the outer edge. Evidently, more work is needed both to enlarge the sample and to link the results to the evolutionary state of the host clusters.…”

Section: Introductionmentioning

confidence: 99%

The unmixed kinematics and origins of diffuse stellar light in the core of the Hydra I cluster (Abell 1060)

Ventimiglia

Arnaboldi

Gerhard

2011

A&A

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Context. Diffuse intracluster light (ICL) and cD galaxy halos are believed to stem from galaxy evolution and disruption in clusters. Aims. The processes involved may be constrained by studying the dynamical state of the ICL and the galaxies in the cluster core. Here we present a kinematic study of diffuse light in the Hydra I (Abell 1060) cluster core, using planetary nebulas (PNs) as tracers. Methods. We used multi-slit imaging spectroscopy with FORS2 on VLT-UT1 to detect 56 PNs associated with diffuse light in the central 100 × 100 kpc 2 of the Hydra I cluster, at a distance of ∼50 Mpc. We measured their [OIII] m 5007 magnitudes, sky positions, and line-of-sight velocity distribution (LOSVD), and compared them with the phase-space distribution of nearby galaxies.Results. The luminosity function of the detected PNs is consistent with that expected at a distance of ∼50 Mpc. Their number density is ∼4 times lower for the light seen than expected, and we discuss ram pressure stripping of the PNs by the hot intracluster medium as one of the possible explanations. The LOSVD histogram of the PNs is highly non-Gaussian and multipeaked: it is dominated by a broad central component with σ ∼ 500 km s −1 at around the average velocity of the cluster, and shows two additional narrower peaks at 1800 km s −1 and 5000 km s −1 . The main component is broadly consistent with the outward continuation of the intracluster halo of NGC 3311, which was earlier shown to have a velocity dispersion of ∼470 km s −1 at radii of > ∼ 50 . Galaxies with velocities in this range are absent in the central 100 × 100 kpc 2 and may have been disrupted earlier to build this component. The PNs in the second peak in the LOSVD at 5000 km s −1 are coincident spatially and in velocities with a group of dwarf galaxies in the MSIS field. They may trace the debris from the ongoing tidal disruption of these galaxies. Conclusions. Most of the diffuse light in the core of Abell 1060 is still not phase-mixed. The build-up of ICL and the dynamically hot cD halo around NGC 3311 are ongoing, through the accretion of material from galaxies falling into the cluster core and tidally interacting with its potential well.

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“…The use of PNe radial velocity measurements has revealed the following kinematic properties for the halos of early-type galaxies (e.g., Douglas et al 2007;Coccato et al 2009;Teodorescu et al 2010;McNeil et al 2010, and references therein):…”

Section: Early-typesmentioning

confidence: 99%

Planetary nebulae as kinematic tracers of galaxy stellar halos

Coccato

2016

Proc. IAU

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Abstract. The kinematic and dynamical properties of galaxy stellar halos are difficult to measure because of the faint surface brightness that characterizes these regions. Spiral galaxies can be probed using the radio Hi emission; on the contrary, early-type galaxies contain less gas, therefore alternative kinematic tracers need to be used. Planetary nebulae (PNe) can be easily detected far out in the halo thanks to their bright emission lines. It is therefore possible to map the halo kinematics also in early-type galaxies, typically out to 5 effective radii or beyond. Thanks to the recent spectroscopic surveys targeting extra-galactic PNe, we can now rely on a few tens of galaxies where the kinematics of the stellar halos are measured. Here, I will review the main results obtained in this field in the last decades.

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Counter-dispersed slitless-spectroscopy technique: planetary nebula velocities in the halo of NGC 1399

Cited by 39 publications

References 50 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 unmixed kinematics and origins of diffuse stellar light in the core of the Hydra I cluster (Abell 1060)

Planetary nebulae as kinematic tracers of galaxy stellar halos

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