The SLUGGS survey: multipopulation dynamical modelling of the elliptical galaxy NGC 1407 from stars and globular clusters

Pota, Vincenzo; Romanowsky, Aaron J.; Brodie, Jean P.; Peñarrubia, Jorge; Forbes, Duncan A.; Napolitano, N. R.; Foster, Caroline; Walker, Matthew G.; Strader, Jay; Roediger, Joel

doi:10.1093/mnras/stv831

Cited by 31 publications

(117 citation statements)

References 121 publications

(212 reference statements)

Supporting

Mentioning

103

Contrasting

Order By: Relevance

“…And we also note that their age for the bulge component (13.5 ± 1.4 Gyr) agrees well with the age derived by McDermid et al (2015) of 13.4 Gyr. Here we tentatively assign the same class D to NGC 4649 as Pota et al (2015) using SLUGGS data.…”

Section: Discussionmentioning

confidence: 83%

The SLUGGS survey: the assembly histories of individual early-type galaxies

Forbes¹,

Romanowsky²,

Pastorello³

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

Early-type (E and S0) galaxies may have assembled via a variety of different evolutionary pathways. Here we investigate these pathways by comparing the stellar kinematic properties of 24 early-type galaxies from the SLUGGS survey with the hydrodynamical simulations of Naab et al. (2014). In particular, we use the kinematics of starlight up to 4 effective radii (R e ) as diagnostics of galaxy inner and outer regions, and assign each galaxy to one of six Naab et al. assembly classes.The majority of our galaxies (14/24) have kinematic characteristics that indicate an assembly history dominated by gradual gas dissipation and accretion of many gas-rich minor mergers. Three galaxies, all S0s, indicate that they have experienced gas-rich major mergers in their more recent past. One additional elliptical galaxy is tentatively associated with a gas-rich merger which results in a remnant galaxy with low angular momentum. Pathways dominated by gas-poor (major or minor) mergers dominate the mass growth of six galaxies. Most SLUGGS galaxies appear to have grown in mass (and size) via the accretion of stars and gas from minor mergers, with late major mergers playing a much smaller role.We find that the fraction of accreted stars correlates with the stellar mean age and metallicity gradient, but not with the slope of the total mass density profile. We briefly mention future observational and modelling approaches that will enhance our ability to accurately reconstruct the assembly histories of individual present day galaxies.

show abstract

Section: Discussionmentioning

confidence: 83%

The SLUGGS survey: the assembly histories of individual early-type galaxies

Forbes¹,

Romanowsky²,

Pastorello³

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

View full text Add to dashboard Cite

show abstract

“…It would also be interesting to study samples of galaxies with extended (in radius) kinematical datasets, such as Planetary Nebulae and Globular Clusters. With such galaxies, it is possible to probe the mass distribution in the external regions, where DM effects should be dominant (e.g., Coccato et al 2009;Napolitano et al 2009Napolitano et al , 2011Pota et al 2013Pota et al , 2015Alabi et al 2016). We plan to test the EG formalism with these datasets, probing the apparent mass in Eq.…”

Section: Discussionmentioning

confidence: 99%

Testing Verlinde's emergent gravity in early-type galaxies

Tortora

Koopmans

Napolitano

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Verlinde derived gravity as an emergent force from the information flow, through two-dimensional surfaces and recently, by a priori postulating the entanglement of information in three-dimensional space, he derived the effect of the gravitational potential from dark matter (DM) as the entropy displacement of dark energy by baryonic matter. In Emergent Gravity (EG) this apparent DM depends only on the baryonic mass distribution and the present-day value of the Hubble parameter. In this paper we test the EG proposition, formalized by Verlinde for a spherical and isolated mass distribution, using the central dynamics (SDSS velocity dispersion, σ) and the K-band light distribution in a sample of 4260 massive (M > ∼ 10 10 M ) and local early-type galaxies (ETGs) from the SPIDER datasample. Our results remain unaltered if we consider the sample of 807 roundest field galaxies. Using these observations we derive the predictions by EG for the stellar mass-to-light ratio (M/L) and the Initial Mass Function (IMF), and compare them with the same inferences derived from a) the standard DM-based models, b) an alternative description of the missing mass (i.e. MOND) and c) stellar population models. We demonstrate that, consistently with a classical Newtonian framework with a DM halo component, or alternative theories of gravity as MOND, the central dynamics can be fitted if the IMF is assumed non-universal. The results can be interpreted with a IMF lighter than a standard Chabrier at low-σ, and bottom-heavier IMFs at larger σ. We find lower, but still acceptable, stellar M/L in EG theory, if compared with the DM-based NFW model and with MOND. The results from EG are comparable to what is found if the DM haloes are adiabatically contracted and also with expectations from spectral gravity-sensitive features. If the strain caused by the entropy displacement would be not maximal, as adopted in the current formulation, then the dynamics of ETGs could be reproduced with larger M/L.

show abstract

“…As stressed by Bender et al (2015a), deep photometry alone is not enough to recognize the structure of the stellar halo, and kinematics measurements are necessary when possible. In particular, the possibility to infer the variation of the orbital distribution of stars, PNe, and GCs (e.g., Gerhard et al 2001;Napolitano et al 2009Napolitano et al , 2011Napolitano et al , 2014Romanowsky et al 2009;Pota et al 2015) in the galaxy halos is a strong observational test for galaxy-formation scenarios that can be compared with predictions of hydrodynamical simulations (e.g., Wu et al 2014).…”

Section: Introductionmentioning

confidence: 99%

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

View full text Add to dashboard Cite

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.

show abstract

The SLUGGS survey: multipopulation dynamical modelling of the elliptical galaxy NGC 1407 from stars and globular clusters

Cited by 31 publications

References 121 publications

The SLUGGS survey: the assembly histories of individual early-type galaxies

The SLUGGS survey: the assembly histories of individual early-type galaxies

Testing Verlinde's emergent gravity in early-type galaxies

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

Contact Info

Product

Resources

About