The Sloan Digital Sky Survey Photometric System

Fukugita, M.; Ichikawa, Takashi; Gunn, James E.; Doi, Mamoru; Shimasaku, K.; Schneider, D.

doi:10.1086/117915

Cited by 2,856 publications

(3,030 citation statements)

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“…The imaging is carried out by driftscanning the sky in photometric conditions [31], in five bands (ugriz) [32,33] using a specially designed widefield camera [34]. Using these data, objects are targeted for spectroscopy [35] and are observed with a 640-fiber spectrograph on the same telescope.…”

Section: B Sdss Luminous Red Galaxiesmentioning

confidence: 99%

Correlating the CMB with luminous red galaxies: The integrated Sachs-Wolfe effect

et al. 2005

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We present a 2.5σ detection of the Integrated Sachs-Wolfe (ISW) effect and discuss the constraints it places on cosmological parameters. We cross-correlate microwave temperature maps from the WMAP satellite with a 4000 deg 2 luminous red galaxy (LRG) overdensity map measured by the Sloan Digital Sky Survey. These galaxies have accurate photometric redshifts (∆z ∼ 0.03) and an approximately volume limited redshift distribution from z ∼ 0.2 to z ∼ 0.6 well suited to detecting the ISW effect. Accurate photometric redshifts allow us to perform a reliable auto-correlation analysis of the LRGs, eliminating the uncertainty in the galaxy bias, and combined with cross correlation signal, constrains cosmological parameters -in particular, the matter density. We use a minimum variance power spectrum estimator that optimally weights the data according to expected theoretical templates. We find a 2.5σ signal in the Ka, Q, V, and W WMAP bands, after combining the information from multipoles 2 ≤ l < 400. This is consistent with the expected amplitude of the ISW effect, but requires a lower matter density than is usually assumed: the amplitude, parametrized by the galaxy bias assuming ΩM = 0.3, ΩΛ = 0.7 and σ8 = 0.9, is bg = 4.05 ± 1.54 for V band, with similar results for the other bands. This should be compared to bg = 1.82 ± 0.02 from the auto-correlation analysis. These data provide only a weak confirmation (2.5σ) of dark energy, but provide a significant upper limit: ΩΛ = 0.80 +0.03 −0.06 (1σ) +0.05 −0.19 (2σ), assuming a cosmology with ΩM + ΩΛ = 1, Ω b = 0.05, and σ8 = 0.9, and w = −1. The weak cross-correlation signal rules out low matter density/high dark energy density universes and, in combination with other data, strongly constrains models with w < −1.3. We provide a simple prescription to incorporate these constraints into cosmological parameter estimation methods for (ΩM , σ8, w). We find no evidence for a systematic contamination of ISW signal, either from Galactic or extragalactic sources, but we do detect some large statistical fluctuations on smaller scales that could affect analyses without the template weighting.

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Section: B Sdss Luminous Red Galaxiesmentioning

confidence: 99%

Correlating the CMB with luminous red galaxies: The integrated Sachs-Wolfe effect

et al. 2005

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“…The SDSS observes galaxies in five photometric bands (u, g, r, i, z) centered at (3540, 4770, 6230, 7630, 9130 Å). The imaging camera was described by Gunn et al (1998), while the photometric system and the photometric calibration of the SDSS imaging data were roughly described by Fukugita et al (1996), Hogg et al (2001) and Smith et al (2002) respectively. Pier et al (2003) described the methods and algorithms involved in the astrometric calibration of the survey, and present a detailed analysis of the accuracy achieved.…”

Section: Datamentioning

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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“…This object is one of the ∼10 5 quasar candidates for which the survey is obtaining redshifts, in addition to the ∼10 6 galaxies which comprise the bulk of the spectroscopic targets (Blanton et al 2003), selected from astrometrically calibrated drift-scanned imaging data (Gunn et al 1998;Pier et al 2003) on the SDSS ugriz AB asinh magnitude system (Fukugita et al 1996;Lupton et al 1999;Hogg et al 2001;Stoughton et al 2002;Smith et al 2002).…”

Section: Introductionmentioning

confidence: 99%

VLT + UVES spectroscopy of the low-ionization intrinsic absorber in SDSS J001130.56+005550.7

Hutsemékers

Brinkmann²

2004

A&A

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Abstract. We analyse high-resolution VLT+UVES spectra of the low-ionization intrinsic absorber observed in the BAL QSO SDSS J001130.56+005550.7. Two narrow absorption systems at velocities −600 km s −1 and −22 000 km s −1 are detected. The low-velocity system is part of the broad absorption line (BAL), while the high-velocity one is well detached. While most narrow absorption components are only detected in the high-ionization species, the lowest velocity component is detected in both highand low-ionization species, including in the excited Si  and C  lines. From the analysis of doublet lines, we find that the narrow absorption lines at the low-velocity end of the BAL trough are completely saturated but do not reach zero flux, their profiles being dominated by a velocity-dependent covering factor. The covering factor is significantly smaller for Mg  than for Si  and N , which demonstrates the intrinsic nature of absorber. From the analysis of the excited Si  and C  lines in the lowest velocity component, we find an electron density 10 3 cm −3 . Assuming photoionization equilibrium, we derive a distance 20 kpc between the low-ionization region and the quasar core. The correspondence in velocity of the high-and low-ionization features suggests that all these species must be closely associated, hence formed at the same distance of ∼20 kpc, much higher than the distance usually assumed for BAL absorbers.

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The Sloan Digital Sky Survey Photometric System

Cited by 2,856 publications

References 0 publications

Correlating the CMB with luminous red galaxies: The integrated Sachs-Wolfe effect

Correlating the CMB with luminous red galaxies: The integrated Sachs-Wolfe effect

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

VLT + UVES spectroscopy of the low-ionization intrinsic absorber in SDSS J001130.56+005550.7

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