Stellar content of NGC 404 – The nearest S0 Galaxy

Тихонов, Н. А.; Galazutdinova, O. A.; Aparicio, A.

doi:10.1051/0004-6361:20021819

Cited by 21 publications

(43 citation statements)

References 42 publications

(39 reference statements)

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“…As expected, we found no traces of any young population (SSP and CST), no emission lines were seen in the spectra at that location. Our results for the old population are in good agreement with those from HST stellar photometry ([Fe/H] = −1.11 dex, Tikhonov et al 2003).…”

Section: Star Formation Historysupporting

confidence: 88%

“…Tikhonov et al (2003) reached a similar conclusion from their optical photometry studies. In that respect, NGC 404 is similar to the elliptical galaxy NGC 205 where the central cluster, HubbleV, is younger and more metal-rich than the surrounding fields.…”

Section: Star Formation Historysupporting

confidence: 61%

“…To accomplish this, the age and metallicity of each component were fixed to the values found in the core of NGC 404 (Table 2), leaving only the relative fraction to vary with radius. These mass and light fractions resulting from the various fits were then converted to an absolute distribution by scaling our results to the values measured by Tikhonov et al (2003) and Dalcanton et al (2009), i.e., μ V,0 = 16.6, D = 3.05 Mpc, respectively, and the stellar mass-to-light ratio derived from the fitted models (on average M/L V = 0.7).…”

Section: Star Formation Historymentioning

confidence: 99%

“…At ∼3.4 Mpc (Tonry et al 2001;Karachentsev et al 2002;Tikhonov et al 2003), NGC 404 is the closest dS0 galaxy to the Local Group (see Table 1 for a summary of the targets' properties). It is also fairly isolated, the nearest neighbour being over 1 Mpc away (Karachentsev & Makarov 1999).…”

Section: Introductionmentioning

confidence: 99%

“…(1) Tikhonov et al (2003); (2) has also a low-ionisation nuclear emission line region (LINER, Pogge et al 2000). By comparison, NGC 404 is only about 0.8 mag brighter than NGC 205 or the other dEs in nearby clusters presented in Koleva et al (2009a).…”

Section: Introductionmentioning

confidence: 99%

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Stellar population and kinematics of NGC 404

Bouchard

Prugniel

Koleva

et al. 2010

A&A

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Context. NGC 404 is a nearly face-on, nearby low-luminosity lenticular galaxy. Probing its characteristics provides a wealth of information on the details of the possible evolution processes of dS0 galaxies, which may not be possible in other, more distant objects. Aims. We study the internal kinematics and the spatial distribution of the star formation history in NGC 404. Methods. We obtained long-slit spectroscopy at the OHP 1m93 telescope along the major and minor axes of NGC 404. The spectra had a resolution R = 3600 covering a wavelength range from 4600 to 5500 Å. The data were fitted against the Pegase. HR stellar population models to derive the internal stellar kinematics, ages, and metallicities simultaneously. All this was done while taking any instrumental contamination to the line-of-sight velocity distribution into account. First, the global properties of the galaxy were analysed by fitting a single model to the data and looking at the kinematic variations and SSP equivalent age and metallicities as a function of radius. Afterwards, the stellar populations were decomposed into 4 individually analysed components.Results. NGC 404 clearly shows two radial velocity inversions along its major axis. The kinematically decoupled core rotates in the same direction as the neutral hydrogen shell that surrounds the galaxy. We resolved the star formation history in the core of the galaxy into 4 events Conclusions. We conclude that NGC 404 had a spiral morphology about 1 Gyr ago and that one or many merger events has triggered a morphological transition. The interstellar medium in the galaxy has two components, the cold molecular gas is most probably a remnant from its past spiral incarnation and the outer neutral hydrogen layer that has probably been acquired in one of the latest mergers.

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Section: Star Formation Historysupporting

confidence: 88%

Section: Star Formation Historysupporting

confidence: 61%

Section: Star Formation Historymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Stellar population and kinematics of NGC 404

Bouchard

Prugniel

Koleva

et al. 2010

A&A

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On the Origin of S0 Galaxies

Alvensleben

2004

Astrophysics and Space Science Library

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I will review the basic properties of S0 galaxies in the local Universe in relation to both elliptical and spiral galaxies, their neighbours on the Hubble sequence, and also in relation to dwarf spheroidal (dSph) galaxies. This will include colours, luminosities, spectral features, information about the age and metallicity composition of their stellar populations and globular clusters, about their ISM content, as well as kinematic signatures and their implications for central black hole masses and past interaction events, and the number ratios of S0s to other galaxy types in relation to environmental galaxy density. I will point out some caveats as to their morphological discrimination against other classes of galaxies, discuss the role of dust and the wavelength dependence of bulge/disk light ratios. These effects are of importance for investigations into the redshift evolution of S0 galaxies -both as individual objects and as a population. The various formation and transformation scenarios for S0 and dSph galaxies will be presented and confronted with the available observations.

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Resolved Stellar Populations as Tracers of Outskirts

Crnojević

2017

Astrophysics and Space Science Library

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Galaxy haloes contain fundamental clues about the galaxy formation and evolution process: hierarchical cosmological models predict haloes to be ubiquitous, and to be (at least in part) the product of past merger and/or accretion events. The advent of wide-field surveys in the last two decades has revolutionized our view of our own Galaxy and its closest "sister", Andromeda, revealing copious tidal streams from past and ongoing accretion episodes, as well as doubling the number of their known faint satellites. The focus shall now be shifted to galaxy haloes beyond the Local Group: resolving individual stars over significant areas of galaxy haloes will enable estimates of their ages, metallicities and gradients. The valuable information collected for galaxies with a range of masses, morphologies and within diverse environments will ultimately test and quantitatively inform theoretical models of galaxy formation, and shed light onto the many challenges faced by simulations on galactic scales.Comment: Invited review, Book chapter in "Outskirts of Galaxies", Eds. J. H. Knapen, J. C. Lee and A. Gil de Paz, Astrophysics and Space Science Library, Springer, in pres

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Stellar content of NGC 404 – The nearest S0 Galaxy

Cited by 21 publications

References 42 publications

Stellar population and kinematics of NGC 404

Stellar population and kinematics of NGC 404

On the Origin of S0 Galaxies

Resolved Stellar Populations as Tracers of Outskirts

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