No galaxy left behind: accurate measurements with the faintest objects in the Dark Energy Survey

Suchyta, E.; Huff, Eric; Aleksić, J.; Melchior, P.; Jouvel, S.; MacCrann, N.; Ross, Ashley J.; Crocce, M.; Gaztañaga, E.; Honscheid, K.; Leistedt, Boris; Peiris, Hiranya V.; Rykoff, E. S.; Sheldon, E.; Abbott, T. M. C.; Abdalla, F. B.; Allam, S.; Banerji, M.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Burke, D. L.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Cunha, C. E.; D’Andrea, C. B.; Costa, L. N. da; DePoy, D. L.; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Doel, P.; Eifler, T. F.; Estrada, J.; Evrard, A. E.; Flaugher, B.; Fosalba, P.; Frieman, Joshua A.; Gerdes, D. W.; Gruen, D.; Gruendl, R. A.; James, D. J.; Jarvis, Mike; Kuêhn, K.; Kuropatkin, N.; Lahav, O.; Lima, M.; Maia, M. A. G.; March, M.; Marshall, J. L.; Miller, Christopher J.; Miquel, R.; Neilsen, Eric H.; Nichol, R. C.; Nord, B.; Ogando, R. L. C.; Percival, Will J.; Reil, K.; Roodman, A.; Šako, M.; Sánchez, E.; Scarpine, V.; Sevilla-Noarbe, I.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Swanson, M. E. C.; Tarlè, G.; Thaler, J. J.; Thomas, Daniel; Vikram, V.; Walker, A. R.; Wechsler, Risa H.; Zhang, Y.

doi:10.1093/mnras/stv2953

Cited by 97 publications

(111 citation statements)

References 57 publications

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“…The high percentage of sources missed in DES is due to various problems, one of them being that the griz 10σ depths differ by 2 mag between the two data sets. This accounts for most of the undetected sources in DES: when we simulate fake faint galaxies with BALROG 3 (Suchyta et al 2016) on the DES image of RXJ2248, we find that the completeness in riz bands (which are those used to run the detection) drops below 20 per cent between magnitude 24 and 25, justifying the incompleteness found when comparing to the even deeper CLASH survey. We also expected one of the problems to be blending, especially close to the bright cluster core.…”

Section: O M Pa R I S O N O F D E S a N D C L A S Hmentioning

confidence: 67%

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Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

Palmese

Lahav

Banerji

et al. 2016

Mon. Not. R. Astron. Soc.

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We derive the stellar mass fraction in the galaxy cluster RXC J2248.7−4431 observed with the Dark Energy Survey (DES) during the Science Verification period. We compare the stellar mass results from DES (five filters) with those from the Hubble Space Telescope Cluster Lensing And Supernova Survey (CLASH; 17 filters). When the cluster spectroscopic redshift is assumed, we show that stellar masses from DES can be estimated within 25 per cent of CLASH values. We compute the stellar mass contribution coming from red and blue galaxies, and study the relation between stellar mass and the underlying dark matter using weak lensing studies with DES and CLASH. An analysis of the radial profiles of the DES total and stellar mass yields a stellar-to-total fraction of f = (6.8 ± 1.7) × 10 −3 within a radius of r 200c 2 Mpc. Our analysis also includes a comparison of photometric redshifts and star/galaxy separation efficiency for both data sets. We conclude that space-based small field imaging can be used to calibrate the galaxy properties in DES for the much wider field of view. The technique developed to derive the stellar mass fraction in galaxy clusters can be applied to the ∼100 000 clusters that will be observed within this survey and yield important information about galaxy evolution.

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Section: O M Pa R I S O N O F D E S a N D C L A S Hmentioning

confidence: 67%

“…The median 10σ depths of SV data are g ∼ 24.45, r ∼ 24.30, i ∼ 23.50, z ∼ 22.90, Y ∼ 21.70, which reach close to the expected DES full depths. Limiting magnitudes were estimated for the 200 deg 2 SPT-E part of the wide-field SV area using BALROG (Suchyta et al 2016) and PSF magnitude errors for true point sources.…”

Section: Datamentioning

confidence: 99%

Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

Palmese

Lahav

Banerji

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The methods we have presented, both correcting for systematic dependencies and ensuring the robustness of these corrections, can be used as a guide for future analyses. Possible improvements to the work include incorporating image simulations [55] and using mode projection techniques [16].…”

Section: Discussionmentioning

confidence: 99%

Dark Energy Survey year 1 results: Galaxy clustering for combined probes

Elvin-Poole¹,

Crocce²,

Ross³

et al. 2018

Phys. Rev. D

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163

235

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We measure the clustering of DES year 1 galaxies that are intended to be combined with weak lensing samples in order to produce precise cosmological constraints from the joint analysis of large-scale structure and lensing correlations. Two-point correlation functions are measured for a sample of 6.6 × 10 5 luminous red galaxies selected using the REDMAGIC algorithm over an area of 1321 square degrees, in the redshift range 0.15 < z < 0.9, split into five tomographic redshift bins. The sample has a mean redshift uncertainty of σ z =ð1 þ zÞ ¼ 0.017. We quantify and correct spurious correlations induced by spatially variable survey properties, testing their impact on the clustering measurements and covariance. We demonstrate the sample's robustness by testing for stellar contamination, for potential biases that could arise from the systematic correction, and for the consistency between the two-point auto-and cross-correlation functions. We show that the corrections we apply have a significant impact on the resultant measurement of cosmological parameters, but that the results are robust against arbitrary choices in the correction method. We find the linear galaxy bias in each redshift bin in a fiducial cosmology to be bðσ 8 =0.81Þj z¼0.24 ¼ 1.40 AE 0.07, bðσ 8 =0.81Þj z¼0.38 ¼ 1.60 AE 0.05, bðσ 8 =0.81Þj z¼0.53 ¼ 1.60 AE 0.04 for galaxies with luminosities L=L Ã > 0.5, bðσ 8 =0.81Þj z¼0.68 ¼ 1.93 AE 0.04 for L=L Ã > 1 and bðσ 8 =0.81Þj z¼0.83 ¼ 1.98 AE 0.07 for L=L Ã > 1.5, broadly consistent with expectations for the redshift and luminosity dependence of the bias of red galaxies. We show these measurements to be consistent with the linear bias obtained from tangential shear measurements.

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“…These can be stars, galaxies described by single-or double-Sérsic models, or galaxies described by the sum of a de Vaucouleurs and an exponential profile. SynPipe is similar in spirit to the BALROG simulation package used for the DES survey as described by Suchyta et al (2016), with two main differences. The first is that SynPipe interfaces with hscPipe and can therefore be used to create synthetic objects with properties measured in the same way as HSC data.…”

Section: Synthetic Object Pipelinementioning

confidence: 99%

The first-year shear catalog of the Subaru Hyper Suprime-Cam Subaru Strategic Program Survey

Mandelbaum

Miyatake

Hamana

et al. 2017

Publications of the Astronomical Society of Japan

228

195

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We present and characterize the catalog of galaxy shape measurements that will be used for cosmological weak lensing measurements in the Wide layer of the first year of the Hyper Suprime-Cam (HSC) survey. The catalog covers an area of 136.9 deg 2 split into six fields, with a mean i-band seeing of 0.58 ′′ and 5σ point-source depth of i ∼ 26. Given conservative galaxy selection criteria for first year science, the depth and excellent image quality results in unweighted and weighted source number densities of 24.6 and 21.8 arcmin −2 , respectively. We define the requirements for cosmological weak lensing science with this catalog, then focus on characterizing potential systematics in the catalog using a series of internal null tests for problems with point-spread function (PSF) modeling, shear estimation, and other aspects of the image processing. We find that the PSF models narrowly meet requirements for weak lensing science with this catalog, with fractional PSF model size residuals of approximately 0.003 (requirement: 0.004) and the PSF model shape correlation function ρ 1 < 3 × 10 −7 (requirement:A variety of galaxy shape-related null tests are statistically consistent with zero, but star-galaxy shape correlations reveal additive systematics on on > 1• scales that are sufficiently large as to require mitigation in cosmic shear measurements. Finally, we discuss the dominant systematics and the planned algorithmic changes to reduce them in future data reductions.

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No galaxy left behind: accurate measurements with the faintest objects in the Dark Energy Survey

Cited by 97 publications

References 57 publications

Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

Dark Energy Survey year 1 results: Galaxy clustering for combined probes

The first-year shear catalog of the Subaru Hyper Suprime-Cam Subaru Strategic Program Survey

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