The Morphologies of Distant Galaxies. II. Classifications from the Hubble Space Telescope Medium Deep Survey

Abraham, Roberto; Bergh, Sidney van den; Glazebrook, Karl; Ellis, Richard S.; Santiago, B.; Surma, P.; Griffiths, R. E.

doi:10.1086/192352

Cited by 363 publications

(543 citation statements)

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“…Conventional asymmetry parameters, computed by subtracting the 180 rotated image from the original image (Abraham et al 1996;Conselice et al 2000;Wu 2000), would measure the galaxy to be '' symmetric,'' with no information whatsoever about spiral arms. With R, one is able to quantify the prominent features caused by spiral arms in the residual image.…”

Section: Residual Parameter Rmentioning

confidence: 99%

“…Currently, the determination of redshifts of I $ 22 early-type galaxies is feasible with ground-based telescopes of aperture e4 m (Koo et al 1996;Lilly et al 1995;Cowie et al 1996;Cohen et al 1996Cohen et al , 2000. Moreover, previous studies have shown that morphological classification of faint galaxies is possible down to I ' 22:5 using Hubble Space Telescope (HST) images with exposure times e1 hr (Griffiths et al 1994a(Griffiths et al , 1994bDriver, Windhorst, & Griffiths 1995;Glazebrook et al 1995;Im et al 1996Im et al , 1995aAbraham et al 1996;Brinchmann et al 1998;Schade et al 1999;Im, Griffiths, & Ratnatunga 2000;Roche et al 1996Roche et al , 1998. Thus, in principle, a combination of HST imaging and spectroscopy using large ground-based telescopes can provide the data to constrain the number-density evolution of E/ S0's at z < 1.…”

Section: Introductionmentioning

confidence: 99%

“…For example, Menanteau et al (1999) study galaxies in deep HST archive exposures, supplemented by ground-based infrared H+K 0 near-infrared imaging. They classify galaxies morphologically using both quantitative (AC method; Abraham et al 1996) and qualitative (visual) methods. Lacking redshifts, they model galaxy counts versus color and conclude that the number density of distant spheroids has not changed substantially since z $ 1.…”

Section: Introductionmentioning

confidence: 99%

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The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

Simard

Faber

et al. 2002

ApJ

142

132

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We present the luminosity function and color-redshift relation of a magnitude-limited sample of 145 mostly red field E/S0 galaxies at zd1 from the DEEP Groth Strip Survey (GSS). Using nearby galaxy images as a training set, we develop a quantitative method to classify E/S0 galaxies based on smoothness, symmetry, and bulge-to-total light ratio. Using this method, we identify 145 E/S0's at 16:5 < I < 22 within the GSS, for which 44 spectroscopic redshifts (z spec ) are available. Most of the galaxies with spectroscopic redshifts (86%) form a '' red envelope '' in the redshift-color diagram, consistent with predictions of spectral synthesis models in which the dominant stellar population is formed at redshifts ze1:5. We use the tight correlation between VÀI and z spec for this red subset to estimate redshifts of the remaining E/S0's to an accuracy of $10%, with the exception of a small number (16%) of blue interlopers at low redshift that are quantitatively classified as E/S0's but are not contained within the red envelope. Constructing a luminosity function of the full sample of 145 E/S0's, we find that there is about 1.1-1.9 mag brightening in rest-frame B-band luminosity back to z ' 0:8 from z ¼ 0, consistent with other studies. Together with the red colors, this brightening is consistent with models in which the bulk of stars in red field E/S0's formed before z for e1:5 and have been evolving rather quiescently, with few large starbursts since then. Evolution in the number density of field E/ S0 galaxies is more difficult to measure, and uncertainties in the raw counts and their ratio to local samples might amount to as much as a factor of 2. Within that uncertainty, the number density of red E/S0's to z ' 0:8 seems relatively static, being comparable to or perhaps moderately less than that of local E/S0's, depending on the assumed cosmology. A doubling of E/S0 number density since z ¼ 1 can be ruled out with high confidence (97%) if m ¼ 1. Taken together, our results are consistent with the hypothesis that the majority of luminous field E/S0's were already in place by z $ 1, that the bulk of their stars were already fairly old, and that their number density has not changed by large amounts since then.

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Section: Residual Parameter Rmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

Simard

Faber

et al. 2002

ApJ

142

132

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“…Kinemetry has similarities to non-parametric measures used in quantitative image morphology, especially in its use of an asymmetry measure which is similar to that used in morphology (Abraham et al 1996b;Conselice 2003). However, model-fitting is still performed in order to determine a best fit inclination and PA before calculating the kinemetry coefficients.…”

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confidence: 99%

The Dawes Review 1: Kinematic Studies of Star-Forming Galaxies Across Cosmic Time

Glazebrook

2013

Publ. Astron. Soc. Aust.

Self Cite

129

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The last seven years have seen an explosion in the number of Integral Field galaxy surveys, obtaining resolved 2D spectroscopy, especially at high-redshift. These have taken advantage of the mature capabilities of 8-10 m class telescopes and the development of associated technology such as AO. Surveys have leveraged both high spectroscopic resolution enabling internal velocity measurements and high spatial resolution from AO techniques and sites with excellent natural seeing. For the first time, we have been able to glimpse the kinematic state of matter in young, assembling starforming galaxies and learn detailed astrophysical information about the physical processes and compare their kinematic scaling relations with those in the local Universe. Observers have measured disc galaxy rotation, merger signatures, and turbulence-enhanced velocity dispersions of gas-rich discs. Theorists have interpreted kinematic signatures of galaxies in a variety of ways (rotation, merging, outflows, and feedback) and attempted to discuss evolution vs. theoretical models and relate it to the evolution in galaxy morphology. A key point that has emerged from this activity is that substantial fractions of high-redshift galaxies have regular kinematic morphologies despite irregular photometric morphologies and this is likely due to the presence of a large number of highly gas-rich discs. There has not yet been a review of this burgeoning topic. In this first Dawes review, I will discuss the extensive kinematic surveys that have been done and the physical models that have arisen for young galaxies at high-redshift.

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“…Early work from the Medium Deep Survey (MDS) reported an excess of faint peculiar systems (Griffiths et al 1994), but the excess become much more convincing with the extension of this work to include number counts as a function of magnitude (Glazebrook et al 1995;Abraham et al 1996). Worries with regard to bulk misclassification of peculiar galaxies have been eased by the incorporation of objective machinebased classifications, which are now routinely being used to supplement (and in some cases replace) visual morphological classifications from a number of different surveys Odewahan et al 1996;Brinchmann et al 1997).…”

Section: Hst Field Surveys With Morphological Informationmentioning

confidence: 71%

A Review of High-Redshift Merger Observations

Abraham

1999

Galaxy Interactions at Low and High Redshift

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Abstract. Evolution in the merger rate as a function of redshift is in principle the key observable testing hierarchical models for the formation and evolution of galaxies. However, in practice, direct measurement of this quantity has proven difficult. In this opening review I outline the current best estimates for the merger rate as a function of cosmic epoch, focussing mostly upon recent advances made possible by deep ground-based redshift surveys and morphological studies undertaken with HST. I argue that a marriage of these techniques, in an attempt to determine the space density of mergers amongst the abundant morphologically peculiar population at high redshifts, is probably the most promising currently-available avenue for determining the prevalence of mergers at high redshifts. However, resolved kinematical studies, which seem set to become available in the next few years, are probably the best hope for a definitive determination of the space density of mergers at high redshifts. Observational Techniques:Three observational techniques have been used to probe changes in the merger rate as a function of cosmic epoch. These are (a) studies of angular and physical correlation functions, (b) pair counts, and (c) morphological studies. The advantages (+) and disadvantages (−) of each of these approaches for studying high-redshift mergers can be crudely summarized as follows.

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The Morphologies of Distant Galaxies. II. Classifications from the Hubble Space Telescope Medium Deep Survey

Cited by 363 publications

References 0 publications

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

The Dawes Review 1: Kinematic Studies of Star-Forming Galaxies Across Cosmic Time

A Review of High-Redshift Merger Observations

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