An Improved Photometric Calibration of the Sloan Digital Sky Survey Imaging Data

Padmanabhan, Nikhil; Schlegel, David J.; Finkbeiner, Douglas P.; Barentine, John C.; Blanton, M. R.; Brewington, H.; Gunn, James E.; Harvanek, Michael; Hogg, David W.; Ivezić, Željko; Johnston, David; Kent, S.; Kleinman, S. J.; Knapp, G. R.; Krzesiński, Jurek; Long, Daniel C.; Neilsen, Eric H.; Nitta, A.; Loomis, Craig; Lupton, Robert H.; Roweis, Sam T.; Snedden, Stephanie A.; Strauss, Michael A.; Tucker, D. L.

doi:10.1086/524677

Cited by 557 publications

(576 citation statements)

References 46 publications

Supporting

Mentioning

564

Contrasting

Order By: Relevance

“…The SDSS magnitude ranges used are 14 < u < 20, 15 < g < 20, 15 < r < 20, 14 < i < 19 and 13.5 < z < 18.5. The standard SDSS calibration was used here for simplicity, rather than the uber-calibration of Padmanabhan et al (2008). As with the APASS comparison in Section 4.1, the ESO calibration clearly shows ±0.05 mag offsets on the scale of single concatenations.…”

Section: Atlas-sdss Equatorial Comparisonmentioning

confidence: 95%

The VLT Survey Telescope ATLAS

Shanks¹,

Metcalfe²,

Chehade³

et al. 2015

Mon. Not. R. Astron. Soc.

199

203

View full text Add to dashboard Cite

The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details.

show abstract

Section: Atlas-sdss Equatorial Comparisonmentioning

confidence: 95%

The VLT Survey Telescope ATLAS

Shanks¹,

Metcalfe²,

Chehade³

et al. 2015

Mon. Not. R. Astron. Soc.

199

203

View full text Add to dashboard Cite

show abstract

“…These surveys obtained wide-field CCD photometry (Gunn et al 1998(Gunn et al , 2006 in five passbands (u, g, r, i, z;Fukugita et al 1996), internally calibrated using the 'uber-calibration' process described in Padmanabhan et al (2008), amassing a total footprint of 11,663 deg 2 . From this imaging data, galaxies within a footprint of 9380 deg 2 (Abazajian et al 2009) were selected for spectroscopic follow-up as part of the main galaxy sample (MGS; Strauss et al 2002), which, to good approximation, consists of all galaxies with rpet < 17.77, where rpet is the extinction-corrected r-band Petrosian magnitude.…”

Section: Datamentioning

confidence: 99%

The clustering of the SDSS DR7 main Galaxy sample – I. A 4 per cent distance measure at z = 0.15

Ross

Samushia

Howlett

et al. 2015

Monthly Notices of the Royal Astronomical Society

1,639

1,452

View full text Add to dashboard Cite

We create a sample of spectroscopically identified galaxies with z < 0.2 from the Sloan Digital Sky Survey (SDSS) Data Release 7, covering 6813 deg 2 . Galaxies are chosen to sample the highest mass haloes, with an effective bias of 1.5, allowing us to construct 1000 mock galaxy catalogs (described in Paper II), which we use to estimate statistical errors and test our methods. We use an estimate of the gravitational potential to "reconstruct" the linear density fluctuations, enhancing the Baryon Acoustic Oscillation (BAO) signal in the measured correlation function and power spectrum. Fitting to these measurements, we determine D V (z eff = 0.15) = (664 ± 25)(r d /r d,fid ) Mpc; this is a better than 4 per cent distance measurement. This "fills the gap" in BAO distance ladder between previously measured local and higher redshift measurements, and affords significant improvement in constraining the properties of dark energy. Combining our measurement with other BAO measurements from BOSS and 6dFGS galaxy samples provides a 15 per cent improvement in the determination of the equation of state of dark energy and the value of the Hubble parameter at z = 0 (H 0 ). Our measurement is fully consistent with the Planck results and the ΛCDM concordance cosmology, but increases the tension between Planck+BAO H 0 determinations and direct H 0 measurements.

show abstract

“…In Appendix A, we compare our samples based on DR8 photometry to LRG samples based on DR7 photometry and to the original spectroscopic target catalogs. In addition to covering a larger area than DR7, the DR8 photometry uses a new sky subtraction algorithm, affecting mainly bright galaxies (r < 16) (Abazajian et al 2009), and a new calibration (Padmanabhan et al 2008). While the total numbers of LRGs selected using DR7 and DR8 photometry are the same, the actual galaxy samples differ at the ∼ 5% level.…”

Section: Luminous Red Galaxiesmentioning

confidence: 99%

Luminous red galaxies in clusters: central occupation, spatial distributions and miscentring

Hoshino

Leauthaud

Lackner

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Luminous Red Galaxies (LRG) from the Sloan Digital Sky Survey are considered among the best understood samples of galaxies, and they are employed in a broad range of cosmological studies. Because they form a relatively homogeneous population, with high stellar masses and red colors, they are expected to occupy halos in a relatively simple way. In this paper, we study how LRGs occupy massive halos via direct counts in clusters and we reveal several unexpected trends suggesting that the connection between LRGs and dark matter halos may not be straightforward. Using the redMaPPer cluster catalog, we derive the central occupation of LRGs as a function richness, N cen (λ). Assuming no correlation between cluster mass and central galaxy luminosity at fixed richness, we show that clusters contain a significantly lower fraction of central LRGs than predicted from the two-point correlation function. At halo masses of 10 14.5 M , we find N cen = 0.73, compared to N cen of 0.89 from correlation studies. Our central occupation function for LRGs converges to 0.95 at large halo masses. A strong anti-correlation between central luminosity and cluster mass at fixed richness is required to reconcile our results with those based on clustering studies. We also derive P BNC , the probability that the brightest cluster member is not the central galaxy. We find P BNC ≈ 20 − 30% which is a factor of ∼ 2 lower than the value found by Skibba et al. (2011). Finally, we study the radial offsets of bright non-central LRGs from cluster centers and show that bright noncentral LRGs follow a different radial distribution compared to red cluster members, which follow a Navarro-Frank-White profile. This work demonstrates that even the most massive clusters do not always have an LRG at the center, and that the brightest galaxy in a cluster is not always the central galaxy.

show abstract

An Improved Photometric Calibration of the Sloan Digital Sky Survey Imaging Data

Cited by 557 publications

References 46 publications

The VLT Survey Telescope ATLAS

The VLT Survey Telescope ATLAS

The clustering of the SDSS DR7 main Galaxy sample – I. A 4 per cent distance measure at z = 0.15

Luminous red galaxies in clusters: central occupation, spatial distributions and miscentring

Contact Info

Product

Resources

About