Group, field and isolated early-type galaxies - I. Observations and nuclear data

Denicoló, Glenda; Terlevich, R.; Terlevich, Elena; Forbes, Duncan A.; Terlevich, A. I.; Carrasco, L.

doi:10.1111/j.1365-2966.2005.08583.x

Cited by 80 publications

(118 citation statements)

References 61 publications

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“…However, other studies show that the structural relations depend on wavelength (Jørgensen et al 1996;Hudson et al 1997;Pahre et al 1998;Scodeggio et al 1998;Jun & Im 2008). -As far as the environment is concerned, several studies imply that the structural relations and/or the structural parameters of galaxies are affected by the environment (Bender et al 1992(Bender et al , 1998Trujillo et al 2001Trujillo et al , 2002Bernardi et al 2003b;Aguerri et al 2004;Gutiérrez et al 2004;Denicoló et al 2005;Jørgensen et al 2005), although other studies reach exactly the opposite conclusion (de la Rosa et al 2001;Treu et al 2001;Evstigneeva et al 2002;Gonzáles-García & van Albada 2003;Reda et al 2004Reda et al , 2005Nigoche-Netro et al 2007). …”

Section: Discussionmentioning

confidence: 99%

“…Several studies have also discovered that the structural relations and/or the structural parameters of galaxies are affected by the environment (Bender et al 1992(Bender et al , 1998Trujillo et al 2001Trujillo et al , 2002Bernardi et al 2003b;Aguerri et al 2004;Gutiérrez et al 2004;Denicoló et al 2005;Jørgensen et al 2005), although other studies have reached exactly the opposite conclusion (de la Rosa et al 2001;Treu et al 2001;Evstigneeva et al 2002;Gonzáles-García & van Albada 2003;Reda et al 2004Reda et al , 2005Nigoche-Netro et al 2007). This second set of results suggest that galaxies very quickly absorb the changes caused by gravitational interactions, not keeping memory of these changes in regard to the structural relations.…”

Section: Introductionmentioning

confidence: 99%

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The Faber-Jackson relation for early-type galaxies: dependence on the magnitude range

Nigoche-Netro

Aguerri

Lagos

et al. 2010

A&A

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Aims. Previous studies have found that the coefficients and intrinsic dispersions of both the Kormendy relation and the Fundamental Plane depend on the magnitude range within which the galaxies are contained. We study whether this type of behaviour is also present for the Faber-Jackson relation. Methods. We take a sample of early-type galaxies from the Sloan Digital Sky Survey (SDSS-DR7, ∼90 000 galaxies) spanning a range of approximately 7 mag in both g and r filters and analyse the behaviour of the Faber-Jackson relation parameters as functions of the magnitude range. We calculate the parameters in two ways: i) we consider the faintest (brightest) galaxies in each sample and we progressively increase the width of the magnitude interval by inclusion of the brighter (fainter) galaxies (increasing-magnitudeintervals); and ii) we consider narrow-magnitude intervals of the same width (ΔM = 1.0 mag) over the whole magnitude range available (narrow-magnitude-intervals). Results. Our main results are that: i) in both increasing and narrow-magnitude-intervals the Faber-Jackson relation parameters change systematically, ii) non-parametric tests show that the fluctuations in the values of the slope of the Faber-Jackson relation are not products of chance variations. Conclusions. We conclude that the values of the Faber-Jackson relation parameters depend on the width of the magnitude range and the luminosity of galaxies within the magnitude range. This dependence is caused, to a great extent by the selection effects and because the geometrical shape of the distribution of galaxies on the M − log(σ 0 ) plane depends on luminosity. We therefore emphasize that if the luminosity of galaxies or the width of the magnitude range or both are not taken into consideration when comparing the structural relations of galaxy samples for different wavelengths, environments, redshifts and luminosities, any differences found may be misinterpreted.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Faber-Jackson relation for early-type galaxies: dependence on the magnitude range

Nigoche-Netro

Aguerri

Lagos

et al. 2010

A&A

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“…A comparison of the emission corrections derived from the [OIII]λ5007 and Hα lines, respectively, is also performed by Denicoló et al (2005a) for their sample of early-type galaxies. The authors show that the differences in the emission corrections derived through the two methods are small for the majority of galaxies, but argue that it is very dangerous to rely on the use of the [OIII]λ5007 alone because the [OIII]λ5007/Hβ ratio may be very different from galaxy to galaxy.…”

Section: Hβ Correction For Emission Infillingmentioning

confidence: 99%

“…Denicoló et al (2005a) adopt an absorption value on the basis of the Hα EW measured for their sample of stars (mainly K). Differently, as described in Papers I and II, we computed the emitted flux in the Hα line using, as a reference, the spectrum of an elliptical galaxy (NGC 1426) lacking emission lines or dust.…”

Section: Hβ Correction For Emission Infillingmentioning

confidence: 99%

Nearby early-type galaxies with ionized gas

Annibali

Bressan

Rampazzo

et al. 2006

A&A

146

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Aims. The paper is devoted to the study of the underlying stellar population of a sample of 65 nearby early-type galaxies, predominantly located in low density environments, a large fraction of which show emission lines. Methods. Ages, metallicities, and [α/Fe] ratios have been derived through the comparison of Lick indices measured at different galacto-centric distances (7 apertures and 4 gradients) with new simple stellar population (SSP) models that account for the presence of α/Fe-enhancement. The SSPs cover a wide range of ages (10 9 −16 × 10 9 yr), metallicities (0.0004 ≤ Z ≤0.05), and [α/Fe] ratios (0-0.8). To derive the stellar population parameters, we use an algorithm that provides, together with the most likely solution in the (age, Z, [α/Fe]) space, the probability density function along the age-metallicity degeneracy. Results. We derive a large spread in age, with SSP-equivalent ages ranging from a few to 15 Gyr. Age does not show any significant trend with central velocity dispersion σ c , but E galaxies appear on average older than lenticulars. On the contrary, a significant increasing trend of metallicity and [α/Fe] with σ c is observed, testifying that the chemical enrichment was more efficient and the duration of the star formation shorter in more massive galaxies. These latter two relations do not depend on galaxy morphological type. We have also sought possible correlations with the local galaxy density ρ xyz , but neither metallicity nor α-enhancement show clear trends. However, we find that while low density environments (LDE) (ρ xyz ≤ 0.4) contain very young objects (from 1 Gyr to 4 Gyr), none of the galaxies in the higher density environments (HDE) (40% of galaxies with a measured density) is younger than 5 Gyr. Considering the lack of environmental effect on the [α/Fe] ratio and the high value of [α/Fe] in some young massive objects, we argue that young galaxies in LDE are more likely due to recent rejuvenation episodes. By comparing the number of "rejuvenated" objects with the total number of galaxies in our sample, and by means of simple two-SSP component models, we estimate that, on average, the rejuvenation episodes do not involve more than 25% of the total galaxy mass. The good quality of the data also allow us to analyze the gradients of stellar populations. An average negative metallicity gradient ∆ log Z/∆ log(r/r e ) ∼ −0.21 is firmly detected, while the age and α-enhancement spatial distributions within r e /2 appear quite flat. These observations suggest that, in a given galaxy, the star formation proceeded on similar timescales all across the central r e /2 region, but with an increasing efficiency toward the center.

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“…Some papers have found that this dispersion depends on both luminosity (Bender et al 1992;Jørgensen et al 1996;Hyde & Bernardi 2009) and the environment (Bernardi et al 2003b;Denicoló et al 2005). The behaviour of the intrinsic dispersions in the FJR and the KR have not been studied thoroughly because a third variable is believed to cause most of the intrinsic dispersion in both these relations.…”

Section: Introductionmentioning

confidence: 99%

The intrinsic dispersion in the Faber-Jackson relation for early-type galaxies as function of the mass and redshift

Nigoche-Netro

Aguerri

Lagos

et al. 2011

A&A

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Context. It has been reported that the intrinsic dispersion at constant magnitude in the structural relations of early-type galaxies is a useful tool to study the universality of these structural relations, that is to say, to study whether the structural relations depend on luminosity, wavelength, redshift, and/or environment. Aims. We study the intrinsic dispersion at approximately constant magnitude in the Faber-Jackson relation as a function of luminosity, mass, and redshift. Methods. We use a sample of approximately 90 000 early-type galaxies from the Sloan Digital Sky Survey (SDSS-DR7) spanning a magnitude range of 7 mag in both g and r filters. We calculate the intrinsic dispersion in the Faber-Jackson relation at approximately constant magnitude and compare this at different luminosities, masses, and redshifts. Results. The main results are the following: i) the intrinsic dispersion in the Faber-Jackson relation depends on the luminosity, mass, and redshift; ii) the distribution for brighter and more massive galaxies has smaller intrinsic dispersion than that for fainter and less massive galaxies; iii) the distribution of bright and massive galaxies at higher redshift has smaller intrinsic dispersion than similar galaxies at low redshift. Conclusions. Comparisons of the results found in this work with recent studies from the literature make us conclude that the intrinsic dispersion in the Faber-Jackson relation could depend on the history of galaxies, in other words, the intrinsic dispersion could depend on the number and nature of transformation events that have affected the galaxies during their life times, such as collapse, accretion, interaction, and merging.

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Group, field and isolated early-type galaxies - I. Observations and nuclear data

Cited by 80 publications

References 61 publications

The Faber-Jackson relation for early-type galaxies: dependence on the magnitude range

The Faber-Jackson relation for early-type galaxies: dependence on the magnitude range

Nearby early-type galaxies with ionized gas

The intrinsic dispersion in the Faber-Jackson relation for early-type galaxies as function of the mass and redshift

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