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, Michael L.; Morris, Simon L.; Yee, H. K. C.; Carlberg, R. G.; Ellingson, E.

doi:10.1086/308056

Cited by 868 publications

(623 citation statements)

References 97 publications

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“…[23] (hereafter D4000 n ), where narrower bands (3850-3950Å and 4000-4100Å) have been used in order to be less sensitive to dust reddening. The amplitude of this feature, due to metal absorption lines, depends on the age and metallicity of the stellar population, as well as on the star formation history.…”

Section: The Method: From Spectra To Agesmentioning

confidence: 99%

“…This break is a discontinuity of the spectral continuum around λ rest = 4000Å due to metal absorption lines whose amplitude correlates linearly with the age and metal abundance (metallicity, Z) of the stellar population (in some age and metallicity ranges), that is weakly dependent (for old passive stellar populations) on star formation history (SF H), and basically not affected by dust reddening [7,[22][23][24] (see also Sect. 3.3, and figures therein).…”

Section: Contents 1 Introductionmentioning

confidence: 99%

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Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Moresco

Cimatti

Jiménez

et al. 2012

J. Cosmol. Astropart. Phys.

727

365

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Abstract. We present new improved constraints on the Hubble parameter H(z) in the redshift range 0.15 < z < 1.1, obtained from the differential spectroscopic evolution of early-type galaxies as a function of redshift. We extract a large sample of early-type galaxies (∼ 11000) from several spectroscopic surveys, spanning almost 8 billion years of cosmic lookback time (0.15 < z < 1.42). We select the most massive, red elliptical galaxies, passively evolving and without signature of ongoing star formation. Those galaxies can be used as standard cosmic chronometers, as firstly proposed by Jimenez & Loeb (2002), whose differential age evolution as a function of cosmic time directly probesWe analyze the 4000Å break (D4000) as a function of redshift, use stellar population synthesis models to theoretically calibrate the dependence of the differential age evolution on the differential D4000, and estimate the Hubble parameter taking into account both statistical and systematical errors.We provide 8 new measurements of H(z) (see Tab. 4), and determine its change in H(z) to a precision of 5 − 12% mapping homogeneously the redshift range up to z ∼ 1.1; for the first time, we place a constraint on H(z) at z = 0 with a precision comparable with the one achieved for the Hubble constant (about 5-6% at z ∼ 0.2), and covered a redshift range (0.5 < z < 0.8) which is crucial to distinguish many different quintessence cosmologies.These measurements have been tested to best match a ΛCDM model, clearly providing a statistically robust indication that the Universe is undergoing an accelerated expansion. This method shows the potentiality to open a new avenue in constrain a variety of alternative cosmologies, especially when future surveys (e.g. Euclid) will open the possibility to extend it up to z ∼ 2.-1 -

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Section: The Method: From Spectra To Agesmentioning

confidence: 99%

Section: Contents 1 Introductionmentioning

confidence: 99%

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Moresco

Cimatti

Jiménez

et al. 2012

J. Cosmol. Astropart. Phys.

727

365

View full text Add to dashboard Cite

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“…Then we sum over the continuum-normalized flux in the central passband to obtain the equivalent width of the line. For [O II] and Hδ, we use the standard definitions from Balogh et al (1999) and Worthey & Ottaviani (1997), respectively. For Hα and [N II], we adopt the window definitions from Yan et al (2006).…”

Section: Mean Stellar Populations Of the Lrgsmentioning

confidence: 99%

Characterizing the chemically enriched circumgalactic medium of ∼38 000 luminous red galaxies in SDSS DR12

Huang

Chen

Johnson

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We report a definitive detection of chemically-enriched cool gas around massive, quiescent galaxies at z ≈ 0.4 − 0.7. The result is based on a survey of 37621 luminous red galaxy (LRG)-QSO pairs in SDSS DR12 with projected distance d < 500 kpc. LRGs at d < 50 kpc, provides important insights into the origin of the observed chemically-enriched cool gas in LRG halos. We consider different scenarios and conclude that the observed Mg II absorbers around LRGs are best-explained by a combination of cool clouds formed in thermally unstable LRG halos and satellite accretion through filaments.

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“…The numerous studies showed that galaxy properties seem to correlate (significantly) with environment, for example, galaxies in dense environments (i.e., clusters or groups) have high proportion of early type morphologies (e.g., Oemler 1974;Dressler 1980;Whitmore, Gilmore & Jones 1993, Deng et al 2006a) and low SFRs (e.g., Balogh et al 1997Balogh et al , 1999Poggianti et al 1999). Many authors have investigated correlations between environment and galaxy properties, such as ones between environment and morphology (e.g., Postman & Geller 1984;Dressler et al 1997;Hashimoto & Oemler 1999;Fasano et al 2000;Tran et al 2001;Goto et al 2003;Helsdon & Ponman 2003;Treu et al 2003), ones between environment and star formation rate (e.g., Hashimoto et al 1998;Lewis et al 2002;G´omez et al 2003;Balogh et al 2004a;Tanaka et al 2004;Kelm, Focardi & Sorrentino 2005), and ones between environment and colour (e.g., Tanaka et al 2004;Balogh et al 2004b;Hogg et al 2004).…”

Section: Introductionmentioning

confidence: 99%

Local Environmental Dependence of Galaxy Properties in a Volume-Limited Sample of Main Galaxies

Deng

Zhang

et al. 2007

Chin. J. Astron. Astrophys.

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Using a volume-limited sample of Main Galaxies from the SDSS Data Release 5, we investigate the dependence of galaxy properties on local environment. For each galaxy, the local three-dimensional density is calculated. We find that galaxy morphologies strongly depend on local environment: galaxies in dense environments have predominantly early type morphologies, but other galaxy properties do not present significant dependence on local environment. Clearly, this puts a important constraint on proposed physical mechanisms.

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Cited by 868 publications

References 97 publications

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Characterizing the chemically enriched circumgalactic medium of ∼38 000 luminous red galaxies in SDSS DR12

Local Environmental Dependence of Galaxy Properties in a Volume-Limited Sample of Main Galaxies

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