Detailed Morphological Classification of Early-Type Galaxies in the Perseus Cluster

Poulain, P.; Nieto, J. L.; Davoust, E.

doi:10.1007/978-94-011-2522-2_30

Cited by 10 publications

(27 citation statements)

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“…In order to derive effective radii and total luminosities (to be used later for deriving the galaxy mass) we fit the galaxy isophotes, precisely as done for galaxies in different environments at low and intermediate redshift (e.g., Michard 1985;Poulain et al 1992;Michard & Marshall 1993, 1994Andreon 1994;Andreon et al 1996Andreon et al , 1997.…”

Section: Morphology Size and Stellar Massmentioning

confidence: 99%

Size growth of red-sequence early-type galaxies in clusters in the last 10 Gyr

Andreon

Dong

Raichoor

2016

A&A

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We carried out a photometric and structural analysis in the rest-frame V band of a mass-selected (log M/M > 10.7) sample of red-sequence galaxies in 14 galaxy clusters, 6 of which are at z > 1.45, namely JKCS041, IDCS J1426.5+3508, SpARCS104922.6+564032.5, SpARCSJ021524-034331, XDCPJ0044.0-2033, and SPT-CLJ2040-4451. To this end, we reduced/analyzed about 300 orbits of multicolor images taken with the Advanced Camera for Survey and the Wide Field Camera 3 on the Hubble Space Telescope. We uniformly morphologically classified galaxies from z = 0.023 to z = 1.803, and we homogeneously derived sizes (effective radii) for the entire sample. Furthermore, our size derivation allows, and therefore is not biased by, the presence of the usual variety of morphological structures seen in early-type galaxies, such as bulges, bars, disks, isophote twists, and ellipiticy gradients. By using such a mass-selected sample, composed of 244 red-sequence early-type galaxies, we find that the log of the galaxy size at a fixed stellar mass, log M/M = 11, has increased with time at a rate of 0.023 ± 0.002 dex per Gyr over the last 10 Gyr, in marked contrast with the threefold increase found in the literature for galaxies in the general field over the same period. This suggests, at face value, that secular processes should be excluded as the primary drivers of size evolution because we observed an environmental dependent size growth. Using spectroscopic ages of Coma early-type galaxies we also find that recently quenched early-type galaxies are a numerically minor population not different enough in size to alter the mean size at a given mass, which implies that the progenitor bias is minor, i.e., that the size evolution measured by selecting galaxies at the redshift of observation is indistinguishable from the one that compares ancestors and descendents.

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Section: Morphology Size and Stellar Massmentioning

confidence: 99%

Size growth of red-sequence early-type galaxies in clusters in the last 10 Gyr

Andreon

Dong

Raichoor

2016

A&A

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“…Significantly refined morphological information were derived by Poulain et al (1992) for 91 early-type galaxies of this list from a detailed isophotal shape analysis. Thanks to the high resolution of their CCD images, a variety of fine details in the structure of the galaxy images could be uncovered.…”

Section: Introductionmentioning

confidence: 99%

“…Andreon (1994) studied morphological segregations in A 426 from a BGP subsample of 96 galaxies with B ≤ 15.7 in the inner ∼30 region. He took the morphological type information from Poulain et al (1992) for most galaxies and from a visual inspection of Schmidt plates taken at Palomar and Calern, respectively, in the remaining cases. Andreon et al (1997a) extended the isophotal analysis and provided morphological data for a complete sample of galaxies with m Zwicky < 15.7 in a region of 5.…”

Section: Introductionmentioning

confidence: 99%

The galaxy cluster Abell 426 (Perseus). A catalogue of 660 galaxy positions, isophotal magnitudes and morphological types

Brunzendorf

Meusinger

1999

Astron. Astrophys. Suppl. Ser.

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Abstract. We present a homogeneous catalogue of galaxies in the field of the nearby galaxy cluster A 426 (Perseus) based on a survey of digitised Schmidt plates taken with the Tautenburg 2 m telescope in the B band. Accurate positions, morphological types, B 25 isophotal magnitudes, angular radii and position angles are given for 660 galaxies within a field of about 10 square-degrees, centred on α = 3 h 21 min , δ = 41• 33 (J2000). When available, the radial velocity and the most common name taken from NED or PGC are included. The catalogue comprises galaxies brighter than B 25 ≈ 19.5. The estimated limit of completeness is B 25 ≈ 18. Two thirds of the galaxies are published for the first time. The galaxy positions are measured with a mean accuracy of 0. 5, the photometric accuracy is of the order of 0.1 to 0.2 mag depending on image crowding and galaxy shape. Morphological properties were evaluated from the visual inspections of both deep images obtained from the digital co-addition of a large number of plates and higher-resolution images from single plates taken under good seeing conditions. The superimposed images unveil faint structures down to µ B ≈ 27 mag arcsec −2 . The catalogue is applied to a study of statistical properties of the galaxies in A 426: projected distribution of morphological types, segregation of morphological types, position of the cluster centre, distribution of galaxy position angles, type-dependent luminosity functions, and total B-luminosity of the the cluster. In agreement withThe catalogue is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html Based on observations made with the 2 m telescope of the Thüringer Landessternwarte Tautenburg, Germany, and with the 2.2 m telescope of the German-Spanish Astronomical Centre, Calar Alto, Spain.Visiting Astronomer, German-Spanish Astronomical Centre, Calar Alto, operated by the Max-Planck-Institute for Astronomy, Heidelberg, jointly with the Spanish National Comission for Astronomy.previous studies, we find a relative spiral-deficiency in the central region (r < ∼ 30 ). The percentage of identified S+Irr increases, however, increases from 30% in the centre to more than 50% in the outer parts. The projected distributions of early-and late-type galaxies are not co-centred. The total luminosity of all supposed member galaxies in the surveyed area is estimated to (6.5 ± 0.9) 10 12 × h −2 50 blue solar luminosities. We do not analyse in detail possible substructures in the projected distribution of galaxies. However, we found a pronounced clump of galaxies at α(J2000.0) = 3 h 20. m 4, δ(J2000.0) = 43 • 4 , which is shown to be a background cluster at z ≈ 0.050.

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“…We contributed to this effort by two series of papers, one series presenting the isophote shapes of selected samples of ellipticals (Nieto et al 1991;Poulain et al 1992), and their analysis (Nieto et al 1994;Andreon 1994), and the other presenting the quantitative morphology of E-S0 galaxies (Michard & Marchal 1993, 1994a and their analysis (Michard 1994).…”

Section: Introductionmentioning

confidence: 99%

Morphological classification and structural parameters for early-type galaxies in the Coma cluster

Andreon

Davoust

Michard

et al. 1996

Astron. Astrophys. Suppl. Ser.

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Abstract. -We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than mB = 17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to mB = 17.00 falling in a circular region of 50 arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to mR = 16.05 (or mB 17.5), also in a region of 50 arcmin diameter, but centered 2.6 degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.

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Detailed Morphological Classification of Early-Type Galaxies in the Perseus Cluster

Cited by 10 publications

References 1 publication

Size growth of red-sequence early-type galaxies in clusters in the last 10 Gyr

Size growth of red-sequence early-type galaxies in clusters in the last 10 Gyr

The galaxy cluster Abell 426 (Perseus). A catalogue of 660 galaxy positions, isophotal magnitudes and morphological types

Morphological classification and structural parameters for early-type galaxies in the Coma cluster

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