The environmental dependence of the Mg2 correlations for elliptical galaxies

Guzmán, R.; Lucey, J. R.; Carter, D.; Terlevich, Elena

doi:10.1093/mnras/257.2.187

Cited by 63 publications

(91 citation statements)

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“…Guzmán et al (1992) found systematic variations in the zeropoint of the Mg 2 -σ relation for a sample of Coma galaxies as a function of their distance to the cluster centre. Jørgensen et al (1996Jørgensen et al ( , 1997, examining a sample of eleven clusters, detected a weak correlation between the intensity of the Mg line and the local density within the clusters, in agreement with the Guzmán et al result.…”

Section: Differences In the Line-strength Indices Between Ldegs And Hmentioning

confidence: 89%

“…The relations between the central velocity dispersion and the strength of the integrated stellar Mg and MgH features around 5100 Å have been studied in numerous works (e.g., Terlevich et al 1981;Gorgas et al 1990;Guzmán et al 1992;Bender et al 1993;Jørgensen et al 1996;Bender et al 1998;Bernardi et al 1998;Colless et al 1999;Jørgensen 1999;Concannon et al 2000;Kuntschner 2000;Poggianti et al 2001a;Proctor & Sansom 2002;Worthey & Collobert 2003;Mehlert et al 2003;Thomas et al 2004). Although, classically, the Mg 2 -σ relation has been interpreted as the interplay between mass and metallicity (Forbes et al 1998;Kobayashi & Arimoto 1999;Terlevich et al 1999), nowadays there is still much debate as to whether this relation reflects trends in stellar ages, in metallicities, or in the relative abundance of different heavy elements (e.g., T98; Jørgensen 1999; Trager et al 2000b;K01;Poggianti et al 2001a;Mehlert et al 2003;Caldwell et al 2003;Thomas et al 2005).…”

Section: The Index-velocity Dispersion Relationsmentioning

confidence: 99%

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Stellar populations of early-type galaxies in different environments

Sánchez‐Blázquez

Gorgas

Cardiel

et al. 2006

A&A

120

163

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Aims. This paper commences a series devoted to the study of the stellar content of early-type galaxies. The goal of the series is to set constraints on the evolutionary status of these objects. Methods. In this paper we describe the details of the galaxy sample, the observations, and the data reduction. Line-strength indices and velocity dispersions (σ) are measured in 98 early-type galaxies drawn from different environments, and the relation of the indices with the velocity dispersion analysed in detail.Results. The present sample indicates that some of the index-σ relations depend on galaxy environment. In particular, the slope of the relation between Balmer lines and σ is steeper for galaxies in the Virgo cluster, small groups, and in the field than for galaxies in the Coma cluster. In several indices there is also a significant offset in the zero point between the relations defined by the different subsamples. The slopes of the index-σ relation for the Virgo and low-density environment galaxies are explained by a variation of both age and metallicity, with velocity dispersion, as previously noted in other studies. For the galaxies in the Coma cluster, however, the relation of the indices with σ only requires a variation of the abundance along the σ sequence. In agreement with other studies, we find that the models that better reproduce the slopes are those in which the α elements vary more than the Fe-peak elements along the σ sequence, while, at a given σ, older galaxies show an higher α/Fe ratio. Conclusions. The results can be explained assuming that galaxies in the Coma cluster have experienced a truncated star formation and chemical enrichment history compared to a more continuous time-extended history for their counterparts in lower density environments.

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Section: Differences In the Line-strength Indices Between Ldegs And Hmentioning

confidence: 89%

Section: The Index-velocity Dispersion Relationsmentioning

confidence: 99%

Stellar populations of early-type galaxies in different environments

Sánchez‐Blázquez

Gorgas

Cardiel

et al. 2006

A&A

120

163

View full text Add to dashboard Cite

show abstract

“…Several authors have tried to measure systematic differences in the FP built with ETGs populating different clustering scales (e.g., De Carvalho and Djorgovski, 1992; Guzmán et al, 1992;Zepf and Whitmore, 1993). Zepf and Whitmore (1993) first measured the FP for ETGs in compact groups (CGs), deriving tentative evidences of systematic differences.…”

Section: The Fp and The Environmentmentioning

confidence: 99%

Toward understanding the origin of the fundamental plane for early-type galaxies

D’Onofrio

Valentinuzzi

Secco

et al. 2006

New Astronomy Reviews

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We present a panoramic review of several observational and theoretical aspects of the modern astrophysical research about the origin of the Fundamental Plane (FP) relation for Early-Type Galaxies (ETGs). The discussion is focused on the problem of the tilt and the tightness of the FP, and on the attempts to derive the luminosity evolution of ETGs with redshift. Finally, a number of observed features in the FP are interpreted from the standpoint of a new theoretical approach based on the two-component tensor virial theorem.

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“…Measured UBV colors and spectral line-strength indices suggest that this is indeed the case, with ages of field ellipticals ranging between about 2 Gyr and 12 Gyr (Schweizer & Seitzer 1992;González 1993;Faber et al 1995;Davies 1996;Trager et al 2000). In cluster ellipticals, the colors and line strengths vary less and the inferred ages are more uniformly old (de Carvalho & Djorgovski 1992), especially near the cluster centers (Guzmán et al 1992). These observations all agree with the notion that-on average-major mergers occurred earliest in high-density regions now at the centers of rich clusters, significantly later in cluster outskirts where galaxies are still falling in, and at the slowest rate in the field.…”

Section: Ellipticals From Wrecked Disksmentioning

confidence: 99%

Interactions as a driver of galaxy evolution

Schweizer

2000

Philosophical Transactions of the Royal Society of London. Seri

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Gravitational interactions and mergers are shaping and reshaping galaxies throughout the observable universe. While observations of interacting galaxies at low redshifts yield detailed information about the processes at work, observations at high redshifts suggest that interactions and mergers were much more frequent in the past. Major mergers of nearby disk galaxies form remnants that share many properties with ellipticals and are, in essence, present-day protoellipticals. There is also tantalizing evidence that minor mergers of companions may help build bulges in disk galaxies. Gas plays a crucial role in such interactions. Because of its dissipative nature, it tends to get crunched into molecular form, turning into fuel for starbursts and active nuclei. Besides the evidence for ongoing interactions, signatures of past interactions and mergers in galaxies abound: tidal tails and ripples, counterrotating disks and bulges, polar rings, systems of young globular clusters, and aging starbursts. Galaxy formation and transformation clearly is a prolonged process occurring to the present time. Overall, the currently available observational evidence points towards Hubble's morphological sequence being mainly a sequence of decreasing merger damage.

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The environmental dependence of the Mg2 correlations for elliptical galaxies

Cited by 63 publications

References 0 publications

Stellar populations of early-type galaxies in different environments

Stellar populations of early-type galaxies in different environments

Toward understanding the origin of the fundamental plane for early-type galaxies

Interactions as a driver of galaxy evolution

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