On the Invariant Distribution of Galaxies in there‐〈μ〉ePlane out toz = 0.64

Barbera, F. La; Busarello, G.; Merluzzi, P.; Massarotti, M.; Capaccioli, M.

doi:10.1086/377250

Cited by 51 publications

(99 citation statements)

References 45 publications

(40 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The low value of the Pearson correlation coefficient (ρ = 0.3) reflects the large scatter of the relation when all the comparison galaxies are considered together. The rms deviation in µ e from the fitted relation (rms = 0.7 mag arcsec −2 ) is slightly larger than values quoted in earlier works (e.g., Hamabe & Kormendy 1987;La Barbera et al 2003) making it difficult to observe a clear trend, contrary to previous findings (e.g., Aguerri et al 2004;Ravikumar et al 2006). However, comparing galaxies with different absolute magnitudes could be misleading because of the strong bias caused by selecting systems with different stellar masses (Nigoche-Netro et al 2008).…”

Section: Kormendy Relationcontrasting

confidence: 77%

No evidence for small disk-like bulges in a sample of late-type spirals

Costantin

Méndez-Abreu

Corsini

et al. 2017

A&A

View full text Add to dashboard Cite

Context. About 20% of low-redshift galaxies are late-type spirals with a small or no bulge component. Although they are the simplest disk galaxies in terms of structure and dynamics, the role of the different physical processes driving their formation and evolution is not yet fully understood. Aims. We investigated whether small bulges of late-type spirals follow the same scaling relations traced by ellipticals and large bulges and if they are disk-like or classical bulges. Methods. We derived the photometric and kinematic properties of 9 nearby late-type spirals. To this aim, we analyzed the surfacebrightness distribution from the i-band images of the Sloan Digital Sky Survey and obtained the structural parameters of the galaxies from a two-dimensional photometric decomposition. We found a bulge component in 7 galaxies of the sample, while the remaining 2 resulted to be pure disk galaxies. We measured the line-of-sight stellar velocity distribution within the bulge effective radius from the long-slit spectra taken with high spectral resolution at the Telescopio Nazionale Galileo. We used the photometric and kinematic properties of the sample bulges to study their location in the Fundamental Plane, Kormendy, and Faber-Jackson relations defined for ellipticals and large bulges. Results. We found that our sample bulges satisfy some of the photometric and kinematic prescriptions for being considered disk-like bulges such as small sizes and masses with nearly exponential light profiles, small bulge-to-total luminosity ratios, low stellar velocity dispersions, and ongoing star formation. However, each of them follows the same scaling relations of ellipticals, massive bulges, and compact early-type galaxies so they cannot be classified as disk-like systems. Conclusions. We found a single population of galaxy spheroids that follow the same scaling relations, where the mass seems to lead to a smooth transition in the photometric and kinematic properties from less massive bulges to more massive bulges and ellipticals.

show abstract

Section: Kormendy Relationcontrasting

confidence: 77%

No evidence for small disk-like bulges in a sample of late-type spirals

Costantin

Méndez-Abreu

Corsini

et al. 2017

A&A

View full text Add to dashboard Cite

show abstract

“…On the other hand, some studies have also claimed that the data are consistent with the hierarchical evolutionary scenario (e.g., Kauffmann and Charlot, 1993;Kauffmann, 1996). Working with a large sample of ETGs in three clusters at different redshifts, La Barbera et al (2003) concluded that the slope of the µ e -log(r e ) relation is almost invariant up to z ∼ 0.64 (a KR ∼ 2.91 ± 0.08).…”

Section: The Kormendy Relation (Kr)mentioning

confidence: 99%

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

D’Onofrio

Valentinuzzi

Secco

et al. 2006

New Astronomy Reviews

View full text Add to dashboard Cite

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.

show abstract

“…When the structural relations are constructed for galaxy samples at different redshifts, several studies report similarly (Barger et al 1998;Ziegler et al 1999;La Barbera et al 2003;Barr et al 2006) that only the zero point of these relations depends on the redshift and this dependence may be caused by the passive evolution of the stellar populations that form at high redshift (z form > 2). Nevertheless, their results conflict with those of other authors.…”

Section: Introductionmentioning

confidence: 95%

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

Nigoche-Netro

Aguerri

Lagos

et al. 2010

A&A

View full text Add to dashboard Cite

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.

show abstract

On the Invariant Distribution of Galaxies in ther_e‐〈μ〉_ePlane out toz = 0.64

Cited by 51 publications

References 45 publications

No evidence for small disk-like bulges in a sample of late-type spirals

No evidence for small disk-like bulges in a sample of late-type spirals

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

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

Contact Info

Product

Resources

About