Study of the stellar line-strength indices and kinematics along bars

Pérez, I.; Sánchez‐Blázquez, P.; Zurita, A.

doi:10.1051/0004-6361:200811084

Cited by 65 publications

(113 citation statements)

References 73 publications

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“…Yoachim & Dalcanton 2008;MacArthur et al 2009;Sánchez-Blázquez et al 2011). The stellar metallicity gradients along the bars of the 20 early-type galaxies presented here were derived in previous works (Pérez et al 2009, hereinafter, Paper I) and provided interesting results about the radial distribution of the stellar parameters in the bar region.…”

Section: Introductionsupporting

confidence: 61%

“…In previous works (Pérez et al , 2009Pérez & Sánchez-Blázquez 2011), we derived the radial distribution of the stellar ages and metallicities along the bar and the bulges of the galaxies presented in this work. Line strength indices were measured and used to derive age and metallicity gradients in the bulge and bar region by comparing with stellar population models.…”

Section: Comparison Of the Nebular Gas Abundances With The Distributimentioning

confidence: 99%

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Ionised gas abundances in barred spiral galaxies

Florido

Pérez

Zurita

et al. 2012

A&A

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Aims. This is the third paper of a series devoted to studying the properties of bars from long-slit spectroscopy to understand their formation, evolution, and influence on the evolution of disk galaxies. In this paper, we aim to determine the gas metallicity distribution of a sample of 20 barred early-type galaxies. We compare the nebular and stellar metallicity distributions to attempt to infer the origin of the warm gas. Methods. We performed long-slit spectroscopy along the bar and obtained metallicities derived using different calibrations. We compare the nebular emission metallicities derived using different semi-empirical methods. We carry out AGN diagnostic diagrams for data at different radii to determine the radius of influence of the AGN and the nature of the galactic nuclei. We then derive the gas metallicities along the bars and compare our results to the distribution of stellar metallicities in the same regions. Results. Most of the gas emission is centrally concentrated, although 15 galaxies also show emission along the bar. In the central regions, gas oxygen abundances are in the range 12 + log(O/H) = 8.4−9.1. The nebular metallicity gradients are very shallow in the bulge and bar regions. For three galaxies (one of them a low-ionization nuclear emission-line region), the gas metallicities lie well below the stellar ones in the bulge region. These results do not depend on the choice of semi-empirical calibration used to calculate the abundances. We see that the galaxies with the lowest metallicities are those with the largest rotational velocities. Unlike our stellar metallicities, we find no correlation between the nebular abundances and the central velocity dispersion. In most galaxies, the gradient in the gas nebular metallicities in the bulge region is shallower than that for the stellar metallicity. Conclusions. The presence of gas of significantly lower metallicity than the stellar abundances in three of our galaxies, suggests that the gas has an external origin that fuels the present star formation at the center of some early-type barred galaxies. That the bar/disk nebular metallicities are higher than the central ones might indicate that the gas could be accreted via cooling flows instead of radial accretion from gas sitting in the outer parts of the disk.

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Section: Introductionsupporting

confidence: 61%

Section: Comparison Of the Nebular Gas Abundances With The Distributimentioning

confidence: 99%

Ionised gas abundances in barred spiral galaxies

Florido

Pérez

Zurita

et al. 2012

A&A

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“…Following the results from Pérez et al (2009) for the stellar linestrength indices and the age and metallicity distribution along the bars of a sample of 20 galaxies, we carried out a detailed study of the populations of the central regions of those galaxies. We compared the results with the bulge properties of a similar sample of unbarred galaxies (Moorthy et al 2006), deriving ; i.e., empty symbols represent unbarred galaxies, while filled symbols represent barred galaxies with the crosses our galaxies and the diamonds Moorthy's galaxies for which a reliable gradient could be obtained.…”

Section: Summary and Discussionmentioning

confidence: 99%

Study of stellar populations in the bulges of barred galaxies

Pérez

Sánchez‐Blázquez

2011

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Aims. We wish to determine the influence of bars on the building of galaxy bulges through analysis of ages and metallicities derived from stellar absorption line-strength indices. Methods. Long-slit spectroscopy was obtained for a sample of 20 early-type barred galaxies. Line-strength indices were measured and used to derive age and metallicity gradients in the bulge region by comparing them with stellar population models. The same analysis was carried out with similar data for unbarred galaxies taken from the literature. Results. The bulges of barred galaxies seem to be more metal rich, at a given velocity dispersion (σ), than the bulges of unbarred galaxies, as measured by a few metallicity sensitive indices. There are indications that the ratio of relative abundance of alpha elements with respect to iron, [E/Fe], derived for the bulges of barred galaxies tend to lie above the values of the unbarred galaxies at a given σ. The metallicity gradients for the majority of the bulges are negative so less metal-rich towards the end of the bulge. The gradient values show a large scatter for galaxies with σ below 150 km s −1 . The age distribution is related to the presence of a bulge substructure, such as a nuclear ring or an inner disk. The metallicity of both the bulge and the bar are very well correlated, indicating a close link between the enrichment histories of both components. Conclusions. Bulges of barred early type galaxies might have experienced a different chemical enrichment than do the bulges of unbarred galaxies of the same morphological type, the same central velocity dispersion, and low inclination angles. The hinted stellar populations differences separating the bulges of barred and unbarred galaxies and the strong link between the metallicity of the bulge and the presence of a bar points to scenarios where they both form simultaneously in processes that lead to rapid and massive episodes of star formation, possibly linked to the bar formation. To confirm and generalise the results found here, it would be useful to extend the data set to a larger number of unbarred galaxies and a wider range of morphological types

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“…Given these difficulties, progress has been slow from an observational viewpoint (see e.g. Gadotti & de Souza 2005Pérez et al 2007Pérez et al , 2009Sánchez-Blázquez et al 2011;Seidel et al 2015). 2 In addition, different studies have uncovered diverse results, possibly because of differences in sample selection (Cacho et al 2014;Zhou et al 2015).…”

Section: Introductionmentioning

confidence: 99%

MUSE tells the story of NGC 4371: The dawning of secular evolution

Gadotti¹,

Seidel²,

Sánchez‐Blázquez³

et al. 2015

A&A

134

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We use data from the Multi-Unit Spectroscopic Explorer (MUSE), recently commissioned at the Very Large Telescope (VLT), to study the kinematics and stellar population content of NGC 4371, an early-type massive barred galaxy in the core of the Virgo cluster. We integrate this study with a detailed structural analysis using imaging data from the Hubble and Spitzer Space Telescopes, which allows us to perform a thorough investigation of the physical properties of the galaxy. We show that the rotationally supported inner components in NGC 4371, i.e. an inner disc and a nuclear ring -which, according to the predominant scenario, are built with stars formed from gas brought to the inner region by the bar -are vastly dominated by stars older than 10 Gyr. Our results thus indicate that the formation of the bar occurred at a redshift of about z = 1.8 +0.5 −0.4 (error bars are derived from 100 Monte Carlo realisations). NGC 4371 thus testifies to the robustness of bars. In addition, the mean stellar age of the portion of the major disc of the galaxy that is covered by our MUSE data is above 7 Gyr with a small contribution from younger stars. This suggests that the quenching of star formation in NGC 4371, which is very likely an environmental effect, was already occurring at a redshift of about z = 0.8 +0.2 −0.1 . Our results suggest that bar-driven secular evolution processes may have an extended impact on the evolution of galaxies, and thus on the properties of galaxies as observed today, and not necessarily be restricted to more recent cosmic epochs.

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Study of the stellar line-strength indices and kinematics along bars

Cited by 65 publications

References 73 publications

Ionised gas abundances in barred spiral galaxies

Ionised gas abundances in barred spiral galaxies

Study of stellar populations in the bulges of barred galaxies

MUSE tells the story of NGC 4371: The dawning of secular evolution

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