Stellar populations in the bulges of S0s and the formation of S0 galaxies

Aragón-Salamanca, Alfonso

doi:10.1017/s1743921308017924

Cited by 6 publications

(5 citation statements)

References 13 publications

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“…Figure 6 shows the resulting Tully-Fisher relation for the S0 galaxies analyzed here, compared to the relation for spiral galaxies (Tully & Pierce 2000;Rothberg et al 2000), calibrated to the same absolute magnitude scale. As found previously by Aragón-Salamanca (2008), there is clearly an offset between the S0 and spiral relations, in the sense that the S0s are systematically fainter. This offset fits straightforwardly with a picture in which the S0 galaxies ceased forming stars at some point in the past, leading to a steady fading of their stellar populations.…”

Section: Tully-fisher Relationsupporting

confidence: 82%

Planetary Nebula Spectrograph survey of S0 galaxy kinematics – II. Clues to the origins of S0 galaxies

Cortesi¹,

Merrifield²,

Coccato³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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The stellar kinematics of the spheroids and discs of S0 galaxies contain clues to their formation histories. Unfortunately, it is difficult to disentangle the two components and to recover their stellar kinematics in the faint outer parts of the galaxies using conventional absorption line spectroscopy. This paper therefore presents the stellar kinematics of six S0 galaxies derived from observations of planetary nebulae (PNe), obtained using the Planetary Nebula Spectrograph. To separate the kinematics of the two components, we use a maximum-likelihood method that combines the discrete kinematic data with a photometric component decomposition. The results of this analysis reveal that: the discs of S0 galaxies are rotationally supported; however, the amount of random motion in these discs is systematically higher than in comparable spiral galaxies; and the S0s lie around one magnitude below the Tully-Fisher relation for spiral galaxies, while their spheroids lie nearly one magnitude above the Faber-Jackson relation for ellipticals. All of these findings are consistent with a scenario in which spirals are converted into S0s through a process of mild harassment or "pestering," with their discs somewhat heated and their spheroid somewhat enhanced by the conversion process. In such a scenario, one might expect the properties of S0s to depend on environment. We do not see such an effect in this fairly small sample, although any differences would be diluted by the fact that the current location does not necessarily reflect the environment in which the transformation occurred. Similar observations of larger samples probing a broader range of environments, coupled with more detailed modelling of the transformation process to match the wide range of parameters that we have shown can now be measured, should take us from these first steps to the definitive answer as to how S0 galaxies form.

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Section: Tully-fisher Relationsupporting

confidence: 82%

Planetary Nebula Spectrograph survey of S0 galaxy kinematics – II. Clues to the origins of S0 galaxies

Cortesi¹,

Merrifield²,

Coccato³

et al. 2013

Monthly Notices of the Royal Astronomical Society

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“…One proposed scenario is that S0 galaxies may form from spiral galaxies which underwent some form of environment-related process and lost most of their gas and spiral structures. These processes therefore would leave behind a disc structure alongside the spheroidal structure of the bulge and halo (Gunn & Gott 1972;Aragón-Salamanca 2008;Quilis et al 2000;Byrd & Valtonen 1990;Bekki et al 2005;Bournaud et al 2005). Such scenario would leave the stellar kinematics of the resulting S0 galaxy almost unperturbed, in comparison with the kinematics of the progenitor spiral galaxy (Aragón-Salamanca et al 2006;Buta et al 2010;Cortesi et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Chromodynamical analysis of lenticular galaxies using globular clusters and planetary nebulae

Zanatta

Cortesi

Chies-Santos

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Recovering the origins of lenticular galaxies can shed light on the understanding of galaxy formation and evolution, since they present properties that can be found in both elliptical and spiral galaxies. In this work we study the kinematics of the globular cluster (GC) systems of three lenticular galaxies located in low density environments (NGC 2768, NGC 3115 and NGC 7457), and compare them with the kinematics of planetary nebulae (PNe). The PNe and GC data come from the Planetary Nebulae Spectrograph and the SLUGGS Surveys. Through photometric spheroid-disc decomposition and PNe kinematics we find the probability for a given GC to belong to either the spheroid or the disc of its host galaxy or be rejected from the model. We find that there is no correlation between the components that the GCs are likely to belong to and their colours. Particularly, for NGC 2768 we find that its red GCs display rotation preferentially at inner radii (Re < 1). In the case of the GC system of NGC 3115 we find a group of GCs with similar kinematics that are not likely to belong to either its spheroid nor disc. For NGC 7457 we find that 70% of its GCs are likely to belong to the disc. Overall, our results suggest that these galaxies assembled into S0s through different evolutionary paths. Mergers seem to have been very important for NGC 2768 and NGC 3115 while NGC 7457 is more likely to have experienced secular evolution.

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“…The mechanism responsible for transforming a spiral into an S0 galaxy has to stop star formation in the disk and enhance arXiv:1512.01185v1 [astro-ph.GA] 3 Dec 2015 the spheroidal component (Dressler & Sandage 1983). Interestingly, S0 galaxies are found in all environments, from high density clusters to the field, allowing for a variety of evolutionary paths (gas stripping, strangulation, harassment, minor mergers, pestering, secular evolution) and raising the question of whether S0 galaxies are a unique class, or a collection of objects whose formation mechanisms are environment dependent (Gunn & Gott 1972;Aragón-Salamanca 2008;Quilis et al 2000;Kronberger et al 2008;Byrd & Valtonen 1990;Bournaud et al 2005). Recent work, moreover, suggests the possibility of creating S0s through major mergers under specific initial conditions (Borlaff et al 2014;Naab et al 2014).…”

Section: Introductionmentioning

confidence: 99%

The SLUGGS survey: chromodynamical modelling of the lenticular galaxy NGC 1023

Cortesi¹,

Chies-Santos²,

Pota³

et al. 2015

Mon. Not. R. Astron. Soc.

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Globular clusters (GCs) can be considered discrete, long-lived, dynamical tracers that retain crucial information about the assembly history of their parent galaxy. In this paper, we present a new catalogue of GC velocities and colours for the lenticular galaxy NGC 1023, we study their kinematics and spatial distribution, in comparison with the underlying stellar kinematics and surface brightness profile, and we test a new method for studying GC properties. Specifically, we decompose the galaxy light into its spheroid (assumed to represent the bulge + halo components) and disk components and use it to assign to each GC a probability of belonging to one of the two components. Then we model the galaxy kinematics, assuming a disk and spheroidal component, using planetary nebulae (PNe) and integrated stellar light. We use this kinematic model and the probability previously obtained from the photometry to recalculate for each GC its likelihood of being associated with the disk, the spheroid, or neither. We find that the reddest GCs are likely to be associated with the disk, as found for faint fuzzies in this same galaxy, suggesting that the disk of this S0 galaxy originated at z 2. The majority of blue GCs are found likely to be associated with the spheroidal (hot) component. The method also allows us to identify objects that are unlikely to be in equilibrium with the system. In NGC 1023 some of the rejected GCs form a substructure in phase space that is connected with NGC 1023 companion galaxy.

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Stellar populations in the bulges of S0s and the formation of S0 galaxies

Cited by 6 publications

References 13 publications

Planetary Nebula Spectrograph survey of S0 galaxy kinematics – II. Clues to the origins of S0 galaxies

Planetary Nebula Spectrograph survey of S0 galaxy kinematics – II. Clues to the origins of S0 galaxies

Chromodynamical analysis of lenticular galaxies using globular clusters and planetary nebulae

The SLUGGS survey: chromodynamical modelling of the lenticular galaxy NGC 1023

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