A Comparison of Coma Cluster S0 Galaxies with the Tully-Fisher Relation for Late-Type Spirals

2001 ◽  
Vol 121 (2) ◽  
pp. 683-691 ◽  
Author(s):  
Joannah L. Hinz ◽  
Hans-Walter Rix ◽  
Gary M. Bernstein
Keyword(s):  
Coma Cluster ◽  
Late Type ◽  
Fisher Relation ◽  
S0 Galaxies

scholarly journals S0 galaxies in the Coma cluster: environmental dependence of the S0 offset from the Tully–Fisher relation

2013 ◽  
Vol 433 (3) ◽  
pp. 2667-2692 ◽  
Author(s):  
T. D. Rawle ◽  
John R. Lucey ◽  
Russell J. Smith ◽  
J. T. C. G. Head
Keyword(s):  
Coma Cluster ◽  
Fisher Relation ◽  
S0 Galaxies ◽  
Environmental Dependence

scholarly journals Supernova Rates

1996 ◽  
Vol 145 ◽  
pp. 1-9 ◽  
Author(s):  
Sidney Van Den Bergh
Keyword(s):  
Luminosity Function ◽  
Historical Data ◽  
Starburst Galaxies ◽  
Early Type ◽  
Late Type ◽  
Interstellar Absorption ◽  
Blue Galaxies ◽  
S0 Galaxies ◽  
Intermediate Redshifts ◽  
Parent Galaxy

Extragalactic supernova rates are reviewed. The main uncertainties in calculated rates are due to (1) the influence of the (still poorly known) luminosity function of supernova of a given type on “control times”, to (2) uncertain corrections for possible inclination - dependent bias in supernova discovery probabilities, and (3) interstellar absorption. The total supernova rate in late-type galaxies is found to be ∼ 2(H0/75)2 supernovae (SNe) per century per 1010LB(ʘ) This is consistent with the rate of 3 SNe per century that is derived from the historical data on Galactic supernovae. It is, however, a source of some concern that none of the three Galactic SNe expected to have occurred during the last century was actually observed!The expansion velocities of SNe Ia are found to correlate strongly with parent galaxy Hubble type. This relation is in the sense that low expansion velocities are only observed for those SNe Ia that occur in early-type galaxies. This suggests that V(exp) correlates with the ages of SNe Ia progenitors. It is speculated that the progenitors of a few SNe Ia with high V(exp) values in E and S0 galaxies were formed during recent starbursts.SNe Ia rates appear to be enhanced in post-starburst galaxies. It is suggested that supernova rates might be quite high in the recently discovered population of faint blue galaxies at intermediate redshifts.

scholarly journals Ultimate merging at z ∼ 0.1

2019 ◽  
Vol 627 ◽  
pp. L3 ◽  
Author(s):  
Daniel Maschmann ◽  
Anne-Laure Melchior
Keyword(s):  
Small Groups ◽  
The Other ◽  
Late Type ◽  
Star Forming ◽  
Rotating Discs ◽  
Stellar Velocity ◽  
High Fraction ◽  
Emission Line Galaxies ◽  
Two Peaks ◽  
S0 Galaxies

We present a study of 58 double-peaked emission line galaxies for which one of the components is suppressed in [OIII]λ5008 or is significantly weaker than the other one. Accordingly, the two components are classified differently in the BPT diagram. We show that the strong [OIII] component coincides with the stellar velocity and the suppressed component is off-centred in 66% of the galaxies, while in 12% of them it is the opposite. The analysis of their morphology reveals that about half of the sample is composed of S0, and the rest is composed of mergers and late-type galaxies in equal measure. We discuss the hypothesis that these characteristics exclude rotating discs and suggest different stages of merging. It is possible that the number of mergers is underestimated if the double nuclei are not resolved. Tidal features are detected in the outskirts of some S0 galaxies. This high fraction of S0 is surprising, as in addition most of the galaxies are isolated and the others are in small groups. All these galaxies that host an AGN component are massive, lie on the star forming sequence, and exhibit an enhanced star formation at their centre. While we cannot exclude outflows, these galaxies exhibit spectra that do not correspond to usual outflow observations characterised by high gas velocities, and the standard deviations of the two peaks are comparable. In parallel, these characteristics are compatible with ultimate stages of galaxy merging, where the two nuclei are either too close to be detected, or dynamical disturbances might be present in post-mergers like massive S0 galaxies.

scholarly journals Barred S0 galaxies in the Coma cluster

2014 ◽  
Vol 439 (2) ◽  
pp. 1749-1764 ◽  
Author(s):  
G. B. Lansbury ◽  
J. R. Lucey ◽  
R. J. Smith
Keyword(s):  
Coma Cluster ◽  
S0 Galaxies

The Tully-Fisher Relation in Coma and Virgo Cluster S0 Galaxies

2003 ◽  
Vol 126 (6) ◽  
pp. 2622-2634 ◽  
Author(s):  
J. L. Hinz ◽  
G. H. Rieke ◽  
N. Caldwell
Keyword(s):  
Virgo Cluster ◽  
Fisher Relation ◽  
S0 Galaxies

The distribution of early- and late-type galaxies in the Coma cluster

1995 ◽  
Vol 109 ◽  
pp. 1490 ◽  
Author(s):  
M. Doi ◽  
M. Fukugita ◽  
S. Okamura ◽  
E. L. Turner
Keyword(s):  
Coma Cluster ◽  
Late Type

scholarly journals Properties of E & S0 Galaxies in the Coma Cluster

1996 ◽  
Vol 171 ◽  
pp. 419-419
Author(s):  
Dörte Mehlert ◽  
Ralf Bender ◽  
Roberto Saglia ◽  
Gary Wegner ◽  
Inger Jørgensen
Keyword(s):  
Kinetic Energy ◽  
Stellar Population ◽  
Velocity Dispersion ◽  
Low Density ◽  
Coma Cluster ◽  
Measured Velocity ◽  
The Mean ◽  
Velocity Dispersions ◽  
S0 Galaxies ◽  
Mean Kinetic Energy

As one of the richest nearby clusters, Coma is the ideal place to study the structure of galaxies as a function of environmental density, thus to constrain the theories of galaxy formation and evolution. For a magnitude limited sample of ≈ 40 E and S0 galaxies we want to obtain spectra with sufficient S/N and spatial resolution, that we can derive the rotation curves, the velocity dispersions profiles and the radial gradients of the line indices of Mg, Fe and Hβ. Following questions will be addressed: •Are the radial velocity dispersion profiles and the rotation of galaxies in high density environments similar to those in low density environments? Data for galaxies in low density environment are available from Bender et al. (1994, MNRAS, 269, 785). Are the centrally measured velocity dispersions representative for the mean kinetic energy of the galaxy?•Can the scatter in the Fundamental Plane (FP) - which tightly correlates the radii, surface brightnesses and (central) velocity dispersions (Djorgovski & Davis, 1987, ApJ, 313, 59; Dressier et al. 1987, ApJ, 313, 42) - for the Coma cluster be reduced if the mean kinetic energy is used instead of the central velocity dispersion? Can we derive stronger constraint on the variations in the M/L ratio than already implied by the FP?•The radial gradients of the line indices can be used to test the hypothesis that the metallicity gradient depends on the so-called “escape velocity” of the stars introduced by Franx & Illingworth (1990, ApJ, 359, L41). Also we can check whether the age of the stellar population varies with radius. Ages and metallicities can be estimated from the data with the use of stellar population models (Worthey 1994, ApJS, 95, 105; Bruzual & Chariot 1993, ApJ, 405, 538).•How does the radial variation of stellar populations and kinematics within the galaxies vary as a function of the clusters density profile?

scholarly journals Double-peak emission line galaxies in the SDSS catalogue

2020 ◽  
Vol 641 ◽  
pp. A171
Author(s):  
Daniel Maschmann ◽  
Anne-Laure Melchior ◽  
Gary A. Mamon ◽  
Igor V. Chilingarian ◽  
Ivan Yu. Katkov
Keyword(s):  
Star Formation ◽  
Emission Line ◽  
Control Sample ◽  
Host Galaxy ◽  
Late Type ◽  
Double Peak ◽  
Two Samples ◽  
Emission Line Galaxies ◽  
S0 Galaxies ◽  
Peak Emission

Double-peak narrow emission line galaxies have been studied extensively in the past years, in the hope of discovering late stages of mergers. It is difficult to disentangle this phenomenon from disc rotations and gas outflows with the sole spectroscopic measurement of the central 3″. We aim to properly detect such galaxies and distinguish the underlying mechanisms with a detailed analysis of the host-galaxy properties and their kinematics. Relying on the Reference Catalogue of Spectral Energy Distribution, we developed an automated selection procedure and found 5663 double-peak emission line galaxies at z <  0.34 corresponding to 0.8% of the parent database. To characterise these galaxies, we built a single-peak no-bias control sample (NBCS) with the same redshift and stellar mass distributions as the double-peak sample (DPS). These two samples are indeed very similar in terms of absolute magnitude, [OIII] luminosity, colour-colour diagrams, age and specific star formation rate, metallicity, and environment. We find an important excess of S0 galaxies in the DPS, not observed in the NBCS, which cannot be accounted for by the environment, as most of these galaxies are isolated or in poor groups. Similarly, we find a relative deficit of pure discs in the DPS late-type galaxies, which are preferentially of Sa type. In parallel, we observe a systematic central excess of star formation and extinction for double peak (DP) galaxies. Finally, there are noticeable differences in the kinematics: The gas velocity dispersion is correlated with the galaxy inclination in the NBCS, whereas this relation does not hold for the DPS. Furthermore, the DP galaxies show larger stellar velocity dispersions and they deviate from the Tully-Fisher relation for both late-type and S0 galaxies. These discrepancies can be reconciled if one considers the two peaks as two different components. Considering the morphological biases in favour of bulge-dominated galaxies and the star formation central enhancement, we suggest a scenario of multiple, sequential minor mergers driving the increase of the bulge size, leading to larger fractions of S0 galaxies and a deficit of pure disc galaxies.

scholarly journals A Tully-Fisher Relation for S0 Galaxies

1999 ◽  
Vol 117 (6) ◽  
pp. 2666-2675 ◽  
Author(s):  
Eyal Neistein ◽  
Dan Maoz ◽  
Hans-Walter Rix ◽  
John L. Tonry
Keyword(s):  
Fisher Relation ◽  
S0 Galaxies
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