The CNOC2 Field Galaxy Luminosity Function. I. A Description of Luminosity Function Evolution

Lin, Huan; Yee, H. K. C.; Carlberg, R. G.; Morris, Simon L.; Sawicki, Marcin; Patton, David R.; Wirth, G.; Shepherd, C. W.

doi:10.1086/307297

Cited by 220 publications

(389 citation statements)

References 54 publications

(93 reference statements)

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“…A similar formalism was used in the analysis of CNOC2 data by Lin et al (1999). The linear form of equation (20) approximates the passively evolving stellar populations of the BC96 models.…”

Section: Methodsmentioning

confidence: 99%

“…The parameters M Ã and Ã in equation (12) In estimating the parameters of this LF [Q; m; M Ã ð0Þ; , and Ã ð0Þ], we follow the procedure described in Lin et al (1999). First, we use the STY method with p i defined in the same way as equation (14) to estimate M Ã ð0Þ, Q, and .…”

Section: Methodsmentioning

confidence: 99%

“…Mpc 3 (Lin et al 1999). Note that this rough estimate, based upon equation (18), is accurate only when the depth of the survey volume in each dimension is much greater than the correlation scale (i.e., x4r 0 ; y4r 0 , and z4r 0 ).…”

Section: Normalization For the Sty-estimated Lfmentioning

confidence: 96%

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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

133

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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: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

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

133

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show abstract

“…This noevolution assumption is usually justified by appealing to results from galaxy number counts ( Im et al 2002;Schade et al 1999) and the redshift distribution of lens galaxies (Ofek et al 2003), which are consistent with the hypothesis that the early-type population evolves only through passive luminosity evolution. However, the observational status of early-type evolution has been controversial (Lin et al 1999;Kauffmann et al 1996;Totani & Yoshii 1998;Fried et al 2001), and the observational uncertainties are large enough that dynamical number or mass evolution in the early-type galaxy population cannot be ruled out.…”

Section: A Model For Redshift Evv Olution Of the Lens Populationmentioning

confidence: 99%

Improved Cosmological Constraints from Gravitational Lens Statistics

Mitchell¹,

Keeton²,

Frieman³

et al. 2005

ApJ

131

238

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We combine the Cosmic Lens All-Sky Survey (CLASS) with new Sloan Digital Sky Survey (SDSS) data on the local velocity dispersion distribution function of E /S0 galaxies, ( ), to derive lens statistics constraints on Ã and m . Previous studies of this kind relied on a combination of the E /S0 galaxy luminosity function and the FaberJackson relation to characterize the lens galaxy population. However, ignoring dispersion in the Faber-Jackson relation leads to a biased estimate of ( ) and therefore biased and overconfident constraints on the cosmological parameters. The measured velocity dispersion function from a large sample of E/S0 galaxies provides a more reliable method for probing cosmology with strong lens statistics. Our new constraints are in good agreement with recent results from the redshift-magnitude relation of Type Ia supernovae. Adopting the traditional assumption that the E/S0 velocity function is constant in comoving units, we find a maximum likelihood estimate of Ã ¼ 0:74 0:78 for a spatially flat universe (where the range reflects uncertainty in the number of E/S0 lenses in the CLASS sample) and a 95% confidence upper bound of Ã < 0:86. If ( ) instead evolves in accord with the extended PressSchechter theory, then the maximum likelihood estimate for Ã becomes 0.72-0.78, with the 95% confidence upper bound Ã < 0:89. Even without assuming flatness, lensing provides independent confirmation of the evidence from Type Ia supernovae for a nonzero dark energy component in the universe.

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“…We use the results from Faber et al (2007) for the evolution of B-band magnitudes from the DEEP2 and COMBO-17 surveys, which is ∆M * B ∼ −1.23 mag per unit redshift (with the sign indicating that galaxies were intrinsically brighter in the past), for a combined sample of blue and red galaxies. Typically, estimates of evolution in the redder bands are less than the estimates of evolution in bluer bands (Lin et al 1999;Blanton et al 2003). Assuming that the evolution is a smooth function of the wavelength, the evolution in I-band should be in between B and K band.…”

Section: Volume-limitingmentioning

confidence: 99%

The impact of cosmic variance on simulating weak lensing surveys

Kannawadi¹,

Mandelbaum²,

Lackner³

2015

Monthly Notices of the Royal Astronomical Society

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Upcoming weak lensing surveys will survey large cosmological volumes to measure the growth of cosmological structure with time and thereby constrain dark energy. One major systematic uncertainty in this process is the calibration of the weak lensing shape distortions, or shears. Most upcoming surveys plan to test several aspects of their shear estimation algorithms using sophisticated image simulations that include realistic galaxy populations based on high-resolution data from the Hubble Space Telescope (HST). However, existing datasets from the HST cover very small cosmological volumes, so cosmic variance could cause the galaxy populations in them to be atypical. A narrow redshift slice from such surveys could be dominated by a single large overdensity or underdensity. In that case, the morphology-density relation could alter the local galaxy populations and yield an incorrect calibration of shear estimates as a function of redshift. We directly test this scenario using the COSMOS survey, the largest-area HST survey to date, and show how the statistical distributions of galaxy shapes and morphological parameters (e.g., Sérsic n) are influenced by redshift-dependent cosmic variance. The typical variation in RMS ellipticity due to environmental effects is 5 per cent (absolute, not relative) for redshift bins of width ∆z = 0.05, which could result in uncertain shear calibration at the 1 per cent level. We conclude that the cosmic variance effects are large enough to exceed the systematic error budget of future surveys, but can be mitigated with careful choice of training dataset and sufficiently large redshift binning.

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The CNOC2 Field Galaxy Luminosity Function. I. A Description of Luminosity Function Evolution

Cited by 220 publications

References 54 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

Improved Cosmological Constraints from Gravitational Lens Statistics

The impact of cosmic variance on simulating weak lensing surveys

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