Extragalactic database

Paturel, G.; Andernach, H.; Nella, H. Di; Durand, N.; Garnier, R.; Gouguenheim, L.; Lanoix, P.; Marthinet, M. C.; Petit, C.; Rousseau, Judith; Theureau, G.; Vauglin, I.

doi:10.1051/aas:1997354

Cited by 145 publications

(161 citation statements)

References 27 publications

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“…All these galaxies have concordant redshift (Hickson et al 1992), up to z = 0.045, and are members of groups with a surface brightness μ g ≥ 24 mag arcsec 2 . All morphologies for the galaxies in our sample were extracted from the online compilation HYPERCAT 2 (Paturel et al 1994(Paturel et al , 1997.…”

Section: Compact Group Galaxiesmentioning

confidence: 99%

The star formation histories of Hickson compact group galaxies

Plauchu-Frayn

Olmo

Coziol

et al. 2012

A&A

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Aims. We study the star formation fistory (SFH) of 210 galaxy members of 55 Hickson compact groups (HCG) and 309 galaxies from the Catalog of Isolated Galaxies (CIG). The SFH traces the variation of star formation over the lifetime of a galaxy, and consequently yields a snapshot picture of its formation. Comparing the SFHs in these extremes in galaxy density allows us to determine the main effects of compact groups (CG) on the formation of galaxies. Methods. We fit our spectra using the spectral synthesis code STARLIGHT and obtained the stellar population contents and mean stellar ages of HCG and CIG galaxies in three different morphological classes: early-type galaxies (EtG), early-type spirals (EtS), and late-type spirals (LtS). Results. We find that EtG and EtS galaxies in HCG show higher contents of old and intermediate stellar populations as well as an important deficit of the young stellar population, which clearly implies an older average stellar age in early galaxies in HCG. For LtS galaxies we find similar mean values for the stellar content and age in the two samples. However, we note that LtS can be split into two subclasses, namely old and young LtS. In HCG we find a higher fraction of young LtS than in the CIG sample, in addition, most of these galaxies belong to groups in which most of the galaxies are also young and actively forming stars. The specific star formation rate (SSFR) of spiral galaxies in the two samples differ. The EtS in HCG show lower SSFR values, while LtS peak at higher values compared with their counterparts in isolation. We also measured the shorter star formation time scale (SFTS) in HCG galaxies, which indicates that they have a shorter star formation activity than CIG galaxies. We take these observations as evidence that galaxies in CG have evolved more rapidly than galaxies in isolation, regardless of their morphology. Our observations are consistent with the hierarchical galaxy formation model, which states that CGs are structures that formed recently from primordial small-mass density fluctuations. From the systematic difference in SFTS we deduce that the HCG have most probably formed ∼3 Gyr in the past. The galaxies in the HCG are not in equilibrium state, but merging without gas (i.e., under dissipationless conditions), which may explain their relatively long lifetime.

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Section: Compact Group Galaxiesmentioning

confidence: 99%

The star formation histories of Hickson compact group galaxies

Plauchu-Frayn

Olmo

Coziol

et al. 2012

A&A

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“…In most cases, however, a di †erent Ðlter was used than for the data presented here. Global properties of the 67 galaxies in our sample, taken from the LEDA (see Paturel et al 1997), are listed in Table 1. Absolute magnitudes (col. [2]) are based on the distances listed in column (4) and based on the Virgo-centric infall corrected heliocentric velocities assuming km s~1 H 0 \ 80 Mpc~1 (see Paturel et al 1997 for details).…”

Section: The Samplementioning

confidence: 99%

“…Col. (7) : Logarithm of the apparent diameter (in of the galaxy according to k B \ 25 0@ .1) the convention of the Second Reference Catalogue of Bright Galaxies (de Vaucouleurs et al 1976). Col. (8) : The radial velocity (in km s~1) of the galaxy corrected for Virgocentric infall (see Paturel et al 1997 for the infall model). Col. (9) : Total B[V color, corrected for galactic extinction and redshift e †ects.…”

Section: Introductionmentioning

confidence: 99%

WFPC2 Images of the Central Regions of Early-Type Galaxies. I. The Data

Rest

Bosch

Jaffe

et al. 2001

The Astronomical Journal

207

377

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We present high-resolution R-band images of the central regions of 67 early-type galaxies obtained with the Wide Field and Planetary Camera 2 (WFPC2) aboard the Hubble Space T elescope (HST ). This homogeneously selected sample roughly doubles the number of early-type galaxies that have now been imaged at HST resolution and complements similar data on the central regions of radio galaxies and the bulges of spiral galaxies. Our sample strikingly conÐrms the complex morphologies of the central regions of early-type galaxies which have become apparent from previous studies with HST . In particular, we detect dust, either in the form of nuclear disks or with a Ðlamentary distribution, in 43% of all galaxies, in good agreement with previous estimates. In addition, we Ðnd evidence for embedded stellar disks in a remarkably large fraction of 51%. In 14 of those galaxies the disklike structures are misaligned with the main galaxy, suggesting that they correspond to stellar bars in S0 galaxies. We analyze the luminosity proÐles of the galaxies in our sample and classify galaxies according to their central cusp slope. To a large extent we conÐrm the results from previous HST surveys in that early-type galaxies reveal a clear dichotomy : the bright ellipticals are generally boxy and have luminosity proÐles that (M B [ [20.5) break from steep outer power laws to shallow inner cusps (referred to as "" core ÏÏ galaxies). The fainter ellipticals, on the other hand, typically have disky isophotes and luminosity proÐles that lack a clear break and have a steep central cusp (referred to as "" power-law ÏÏ galaxies). The advantages and shortcomings of classiÐcation schemes utilizing the extrapolated central cusp slope c are discussed, and it is shown that c might be an inadequate representation for galaxies whose luminosity proÐle slope changes smoothly with radius rather than resembling a broken power law. Thus, we introduce a new, alternative parameter and show how this a †ects the classiÐcation. In fact, we Ðnd evidence for an "" intermediate ÏÏ class of galaxies that cannot unambiguously be classiÐed as either core or power-law galaxies and that have central cusp slopes and absolute magnitudes intermediate between those of core and power-law galaxies. It is unclear at present, however, whether these galaxies make up a physically distinct class or whether distance and/or resolution e †ects cause them to lose their distinct core or power-law characteristics.

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“…All these quantities are corrected for the contribution of the point source (see Govoni et al 2000b), for cosmological dimming and for K-correction according to Poggianti (1997). The distance/systemic velocities used to derive r e and <µ e > are relative to the Cosmic Microwave Background (CMB) reference frame and come from the Lyon Meudon Extragalactic Database (LEDA, Paturel et al 1997). …”

Section: Observations and Data Analysismentioning

confidence: 99%

The fundamental plane of radio galaxies

Bettoni

Falomo

Fasano

et al. 2001

A&A

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Abstract.We collected photometrical and dynamical data for 73 low red-shift (z < 0.2) Radio Galaxies (LzRG) in order to study their Fundamental Plane (FP). For 22 sources we also present new velocity dispersion data that complement the photometric data given in our previous study of LzRG (Govoni et al. 2000a). It is found that the FP of LzRG is similar to the one defined by non-active elliptical galaxies, with LzRG representing the brightest end of the population of early type galaxies. Since the FP mainly reflects the virial equilibrium condition, our result implies that the global properties of early-type galaxies (defining the FP) are not influenced by the presence of gas accretion in the central black hole. This is fully in agreement with the recent results in black hole demography, showing that virtually all luminous spheroidal galaxies host a massive black hole and therefore may potentially become active. We confirm and extend to giant ellipticals the systematic increase of the mass-to-light ratio with galaxy luminosity.

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Extragalactic database

Cited by 145 publications

References 27 publications

The star formation histories of Hickson compact group galaxies

The star formation histories of Hickson compact group galaxies

WFPC2 Images of the Central Regions of Early-Type Galaxies. I. The Data

The fundamental plane of radio galaxies

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