Galaxy–Galaxy Weak-lensing Measurements from SDSS. I. Image Processing and Lensing Signals
[1];
[5];
[8];
[9];
- Shanghai Astronomical Observatory (China); Shanghai Jiaotong Univ. (China); Carnegie Mellon Univ., Pittsburgh, PA (United States)
- Carnegie Mellon Univ., Pittsburgh, PA (United States); Shanghai Jiaotong Univ. (China)
- Carnegie Mellon Univ., Pittsburgh, PA (United States)
- Shanghai Normal Univ. (China)
- Univ. of Massachusetts, Amherst, MA (United States); Tsinghua Univ., Beijing (China)
- Yale Univ., New Haven, CT (United States)
- Chinese Academy of Sciences (CAS), Beijing (China). Key Lab. for Computational Astrophysics
- Univ. of Chicago, IL (United States); Argonne National Lab. (ANL), Argonne, IL (United States); Univ. of Chicago, IL (United States). Kavli Inst. for Cosmological Physics (KICP)
- Peking Univ., Beijing (China)
- Univ. of Illinois at Urbana-Champaign, IL (United States). Dept. of Astronomy
- Istituto Nazionale di Astrofisica (INAF), Napoli (Italy); Istituto Nazionale di Astrofisica (INAF), Padova (Italy)
We present our image processing pipeline that corrects the systematics introduced by the point-spread function (PSF). Using this pipeline, we processed Sloan Digital Sky Survey (SDSS) DR7 imaging data in r band and generated a galaxy catalog containing the shape information. Based on our shape measurements of the galaxy images from SDSS DR7, we extract the galaxy–galaxy (GG) lensing signals around foreground spectroscopic galaxies binned in different luminosities and stellar masses. We estimated the systematics, e.g., selection bias, PSF reconstruction bias, PSF dilution bias, shear responsivity bias, and noise rectification bias, which in total is between -9.1% and 20.8% at 2σ levels. The overall GG lensing signals we measured are in good agreement with Mandelbaum et al. The reduced $χ^2$ between the two measurements in different luminosity bins are from 0.43 to 0.83. Larger reduced $χ^2$ from 0.60 to 1.87 are seen for different stellar mass bins, which is mainly caused by the different stellar mass estimator. The results in this paper with higher signal-to-noise ratio are due to the larger survey area than SDSS DR4, confirming that more luminous/massive galaxies bear stronger GG lensing signals. We divide the foreground galaxies into red/blue and star-forming/quenched subsamples and measure their GG lensing signals. We find that, at a specific stellar mass/luminosity, the red/quenched galaxies have stronger GG lensing signals than their counterparts, especially at large radii. These GG lensing signals can be used to probe the galaxy–halo mass relations and their environmental dependences in the halo occupation or conditional luminosity function framework.
- Research Organization:
- Argonne National Laboratory (ANL), Argonne, IL (United States)
- Sponsoring Organization:
- Chinese Academy of Sciences (CAS) - Strategic Priority Research Program; National Natural Science Foundation of China (NSFC)
- Grant/Contract Number:
- AC02-06CH11357
- OSTI ID:
- 1494715
- Journal Information:
- The Astrophysical Journal (Online), Journal Name: The Astrophysical Journal (Online) Journal Issue: 1 Vol. 836; ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)Copyright Statement
- Country of Publication:
- United States
- Language:
- English
Mapping the Real Space Distributions of Galaxies in SDSS DR7. II. Measuring the Growth Rate, Clustering Amplitude of Matter, and Biases of Galaxies at Redshift 0.1
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journal | July 2018 |
The First Constraint from SDSS Galaxy–Galaxy Weak Lensing Measurements on Interacting Dark Energy Models
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journal | April 2019 |
| Mapping the Real Space Distributions of Galaxies in SDSS DR7: II. Measuring the growth rate, clustering amplitude of matter and biases of galaxies at redshift $0.1$ | text | January 2017 |
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