Spectral energy distributions of galaxies in high-redshift clusters - III. Abell 370 at z = 0.37

MacLaren, Iain; Ellis, Richard S.; Couch, Warrick J.

doi:10.1093/mnras/230.2.249

Cited by 29 publications

(18 citation statements)

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“…As such, they play an important part in understanding the evolutionary history of galaxy populations. Evidence for these (and related) galaxies have been found both locally (Caldwell et al 1993 ;Zabludo † et al 1996) and at moderate redshift (e.g., Sharples et al 1985 ;Lavery & Henry 1986 ;Couch & Sharples 1987 ;MacLaren, Ellis, & Couch 1988 ;Broadhurst et al 1988 ;Fabricant, McClintock, & Bautz 1991 ;Abraham et al 1996 ;Fisher et al 1998 ;Morris et al 1998 ;Dressler et al 1999), in both cluster and Ðeld environments. Many authors have interpreted the presence of these galaxies as evidence that a large percentage of cluster galaxies recently underwent strong starbursts (e.g., Dressler & Gunn 1983 ;Couch & Sharples 1987 ;Barger et al 1996 ;Poggianti & Barbaro 1996 ;Couch et al 1998 ;Poggianti et al 1999).…”

Section: Introductionmentioning

confidence: 95%

Differential Galaxy Evolution in Cluster and Field Galaxies at \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr

Balogh

Morris

Yee

et al. 1999

ApJ

881

581

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Section: Introductionmentioning

confidence: 95%

Differential Galaxy Evolution in Cluster and Field Galaxies at \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr

Balogh

Morris

Yee

et al. 1999

ApJ

881

581

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“…However, these galaxies do not show any sign of on‐going star formation as non‐detection in the [O ii ] emission line indicates. Therefore, E+A galaxies have been interpreted as post‐starburst galaxies, that is, galaxies which truncated the starburst suddenly (Dressler & Gunn 1983, 1992; Couch & Sharples 1987; MacLaren, Ellis & Couch 1988; Newberry, Boroson & Kirshner 1990; Fabricant, McClintock & Bautz 1991; Abraham et al 1996). A recent study found that E+A galaxies have an α‐element excess (Goto 2007a), which also supported the post‐starburst interpretation of E+A galaxies.…”

Section: Introductionmentioning

confidence: 99%

Spatially resolved medium resolution spectroscopy of an interacting E+A (post-starburst) system with the Subaru Telescope^★

Goto

Yagi

Yamauchi

2008

Monthly Notices of the Royal Astronomical Society

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We have performed spatially resolved medium resolution long‐slit spectroscopy of a nearby E+A (post‐starburst) galaxy system, SDSS J161330.18+510335.5, with the FOCAS spectrograph mounted on the Subaru Telescope. This E+A galaxy has an obvious companion galaxy 14 kpc in front with the velocity difference of 61.8 km s−1. Both galaxies have obviously disturbed morphology. Thus, this E+A system provides us with a perfect opportunity to investigate the relation between the post‐starburst phenomena and galaxy–galaxy interaction. We have found that the Hδ equivalent width (EW) of the E+A galaxy is greater than 7 Å galaxy wide (8.5 kpc) with no significant spatial variation. The E+A galaxy has a weak [O iii] emission (EW ∼ 1 Å) offset by ∼2.6 kpc from the peak of the Balmer absorption lines. We detected a rotational velocity in the companion galaxy of >175 km s−1. The progenitor of the companion may have been a rotationally supported, but yet passive S0 galaxy. We did not detect significant rotation on the E+A galaxy. A metallicity estimate based on the r−H colour suggests Z= 0.008 and 0.02, for the E+A and the companion galaxies, respectively. Assuming these metallicity estimates, the age of the E+A galaxy after quenching the star formation is estimated to be 100–500 Myr, with its centre having a slightly younger stellar population. The companion galaxy is estimated to have an older stellar population of >2 Gyr of age with no significant spatial variation. These findings are inconsistent with a simple picture where the dynamical interaction creates infall of the gas reservoir that causes the central starburst/post‐starburst. Instead, our results present an important example where the galaxy–galaxy interaction can trigger a galaxy‐wide post‐starburst phenomenon.

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“…However, these galaxies do not show any sign of ongoing star formation as non‐detection in the [O ii ] emission line indicates. Therefore, E+A galaxies have been interpreted as post‐starburst galaxies, that is, galaxies that truncated starburst suddenly (Dressler & Gunn 1983, 1992; Couch & Sharples 1987; MacLaren, Ellis & Couch 1988; Newberry, Boroson & Kirshner 1990; Fabricant, McClintock & Bautz 1991; Abraham et al 1996).…”

Section: Introductionmentioning

confidence: 99%

Abundance diagnosis of E+A (post-starburst) galaxies

Goto

2007

Monthly Notices of the Royal Astronomical Society

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E+A galaxies are characterized as a galaxy with strong Balmer absorption lines but without any [OII] or H$\alpha$ emission lines. The existence of strong Balmer absorption lines means that E+A galaxies have experienced a starburst within the last $<$1-1.5 gigayear. However, the lack of [OII] or H$\alpha$ emission lines indicates that E+A galaxies do not have any on-going star formation. Therefore, E+A galaxies are interpreted as a post-starburst galaxy. Morphologically, E+A galaxies appear as early-type galaxies, implying E+A galaxies may be one of the progenitors of present-day elliptical galaxies. However, there remained other possibilities such as the dusty starburst scenario, where E+A galaxies have on-going star formation, but optical emission lines are invisible due to the heavy obscuration by dust. Therefore, an additional evidence of the post-starburst phenomena has been eagerly awaited. Using one of the largest samples of 451 E+A galaxies carefully selected from the Sloan Digital Sky Survey Data Release 4, here we show the abundance diagnosis of E+A galaxies using Mg and Fe lines. Our findings are as follows :(i) E+A galaxies has enhanced $\alpha$-element abundance ratio compared to the star-forming galaxies with similar Balmer absorption strength. Since the truncation of strong starburst is required to enhance the alpha element ratio, this is an additional evidence that E+A galaxies are in the post-starburst phase; (ii) the metallicity and $\alpha$-element abundance of E+A galaxies are consistent with those of elliptical galaxies, suggesting that E+A galaxies could be one of the progenitors of present-day elliptical galaxies in terms of chemical abundances.Comment: Accepted for publication in MNRA

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Spectral energy distributions of galaxies in high-redshift clusters - III. Abell 370 at z = 0.37

Cited by 29 publications

References 0 publications

Spatially resolved medium resolution spectroscopy of an interacting E+A (post-starburst) system with the Subaru Telescope^★

Abundance diagnosis of E+A (post-starburst) galaxies

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Spectral energy distributions of galaxies in high-redshift clusters - III. Abell 370 at z = 0.37

Cited by 29 publications

References 0 publications

Spatially resolved medium resolution spectroscopy of an interacting E+A (post-starburst) system with the Subaru Telescope★

Abundance diagnosis of E+A (post-starburst) galaxies

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Product

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Spatially resolved medium resolution spectroscopy of an interacting E+A (post-starburst) system with the Subaru Telescope^★