Narrow-band photometry and the evolution of galaxies. III - The intermediate-redshift sample

Rakos, K. D.; Schombert, James M.; Kreidl, T. J.

doi:10.1086/170368

Cited by 16 publications

(15 citation statements)

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“…We present new photometry for 8 clusters from z = 0.6 to z = 1 (the limit of ground based, optical photometry). When combined with our previous results from our zero, low (z = 0.2) and intermediate (z = 0.4) redshift samples (Fiala, Rakos and Stockton 1986, Rakos, Fiala and Schombert 1988, Rakos, Schombert and Kreidl 1991, we can use the results to address four galaxy evolution questions: 1) the change in the fraction of red to blue galaxies with redshift (Butcher-Oemler effect), 2) the nature of blue cluster galaxies, 3) the mean colors of ellipticals as a function of redshift (color evolution) and 4) the redshift of galaxy formation.…”

Section: Introductionsupporting

confidence: 55%

Color evolution from Z = 0 to Z = 1

Rakos¹,

Schombert²

1995

ApJ

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149

184

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Rest frame Strömgren photometry (3500Å, 4100Å, 4750Å and 5500Å) is presented for 509 galaxies in 17 rich clusters between z = 0 and z = 1 as a test of color evolution. Our observations confirm a strong, rest frame, Butcher-Oemler effect where the fraction of blue galaxies increases from 20% at z = 0.4 to 80% at z = 0.9. We also find that a majority of these blue cluster galaxies are composed of normal disk or post-starbursts systems based on color criteria. When comparing our colors to the morphological results from HST imaging, we propose that the blue cluster galaxies are a population of latetype, LSB objects who fade and are then destroyed by the cluster tidal field. After isolating the red objects from Butcher-Oemler objects, we have compared the mean color of these old, non-star forming objects with SED models in the literature as a test for passive galaxy evolution in ellipticals. We find good agreement with single burst models which predict a mean epoch of galaxy formation at z = 5. Tracing the red envelope for ellipticals places the earliest epoch of galaxy formation at z = 10.

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Section: Introductionsupporting

confidence: 55%

Color evolution from Z = 0 to Z = 1

Rakos¹,

Schombert²

1995

ApJ

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149

184

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“…Up to date, many authors have employed the D 4000 to study the stellar composition and star formation history of early-type galaxies (e.g. McClure & van den Bergh 1968;Spinrad 1980Spinrad , 1986Bruzual 1983;Laurikainen & Jaakkola 1985;Hamilton 1985;Dressler 1987;Dressler & Shectman 1987;Johnstone et al 1987;Kimble et al 1989;Dressler & Gunn 1990;Rakos et al 1991;Charlot et al 1993;Charlot & Silk 1994;Davidge & Clark 1994;Songaila et al 1994;Belloni et al 1995;Davidge & Grinder 1995;Cardiel et al 1995Cardiel et al , 1998Abraham et al 1996;Hammer et al 1997;Longhetti et al 1998;Ponder et al 1998). The reliable analysis of the break measurements rests on the comparison of the data with the predictions of stellar population models (e.g.…”

Section: −00988 E(b−v )mentioning

confidence: 99%

Empirical calibration of the λ4000 Å break

Gorgas

Cardiel

Pedraz

et al. 1999

Astron. Astrophys. Suppl. Ser.

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Abstract. Empirical fitting functions, describing the behaviour of the λ4000Å break, D 4000 , in terms of effective temperature, metallicity and surface gravity, are presented. For this purpose, the break has been measured in 392 stars from the Lick/IDS Library. We have followed a very detailed error treatment in the reduction and fitting procedures, allowing for a reliable estimation of the break uncertainties. This calibration can be easily incorporated into stellar population models to provide accurate predictions of the break amplitude for, relatively old, composite systems.

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“…Since [c1] and [m1] 5 are reddening independent (Strömgren 1966), and they also have promising Zsp values, we take a close look at these two indices. Rakos et al (1991) suggested m1 is a metal-line idex, while c1 is a Balmer discontinuity index. Figure 3 Schombert et al (1993), shown as filled Triangles in Figure 3; (2) Nearby Es and globular clusters (GCs) from Rakos et al (1990).…”

Section: • Strömgren Systemmentioning

confidence: 99%

On distinguishing age from metallicity with photometric data

Tang

Worthey

2013

Monthly Notices of the Royal Astronomical Society

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In the study of galaxy integrated light, if photometric indicators could extract age and metallicity information of high enough quality, photometry might be vastly more efficient than spectroscopy for the same astrophysical goals. Toward this end, we search three photometric systems: David Dunlap Observatory (DDO), Beijing-Arizona-Taiwan-Connecticut (BATC), and Strömgren systems for their ability to disentangle age and abundance effects. Only the Strömgren [c 1 ] vs. [m 1 ] plot shows moderate age-metallicity disentanglement. We also add to the discussion of optical to near-infrared Johnson-Cousins broad band colours, finding a great decrease in age sensitivity when updated isochrones are used.

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Narrow-band photometry and the evolution of galaxies. III - The intermediate-redshift sample

Cited by 16 publications

References 0 publications

Color evolution from Z = 0 to Z = 1

Color evolution from Z = 0 to Z = 1

Empirical calibration of the λ4000 Å break

On distinguishing age from metallicity with photometric data

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