The First Release COSMOS Optical and Near‐IR Data and Catalog

Capak, P.; Aussel, H.; Ajiki, Masaru; McCracken, H. J.; Mobasher, Bahram; Scoville, N. Z.; Shopbell, P. L.; Taniguchi, Yoshiaki; Thompson, D. J.; Tribiano, S.; Sasaki, S.; Blain, A. W.; Brusa, M.; Carilli, C. L.; Comastri, A.; Carollo, C. M.; Cassata, P.; Colbert, James; Ellis, Richard S.; Elvis, M.; Giavalisco, Mauro; Green, W.; Guzzo, L.; Hasinger, G.; Ilbert, O.; Impey, C.; Jahnke, K.; Kartaltepe, Jeyhan S.; Kneib, Jean-Paul; Koda, Jin; Koekemoer, Anton M.; Komiyama, Yutaka; Leauthaud, A.; LeFèvre, O.; Lilly, S. J.; Liu, Charles; Massey, Richard; Miyazaki, Satoshi; Murayama, Takashi; Nagao, Tohru; Peacock, J. A.; Pickles, Andrew; Porciani, Cristiano; Renzini, A.; Rhodes, Jason; Rich, R. Michael; Salvato, M.; Sanders, D. B.; Scarlata, Claudia; Schiminovich, David; Schinnerer, E.; Scodeggio, M.; Sheth, Kartik; Shioya, Yasuhiro; Tasca, L.; Taylor, James E.; Yan, Lin; Zamorani, G.

doi:10.1086/519081

Cited by 707 publications

(442 citation statements)

References 53 publications

(46 reference statements)

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“…Details of the Subaru observations and data processing are described by Taniguchi et al (2007) and Capak et al (2007). Note that follow-up spectroscopy has been performed for 24 LAEs in the sample and that all of them showed Lyα emission at z ≈ 5.7 (P. Capak et al 2009, in preparation) verifying the effectiveness of the adopted selection method.…”

Section: Observational Data and Acs Counterparts Of Laesmentioning

confidence: 95%

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HUBBLE SPACE TELESCOPE/ADVANCED CAMERA FOR SURVEYS MORPHOLOGY OF Lyα EMITTERS AT REDSHIFT 5.7 IN THE COSMOS FIELD

Taniguchi

Murayama

Scoville

et al. 2009

ApJ

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We present detailed morphological properties of Lyα emitters (LAEs) at z ≈ 5.7 in the COSMOS field based on Hubble Space Telescope Advanced Camera for Surveys (ACS) data. The ACS imaging in the F814W filter covered 85 LAEs of the 119 LAEs identified in the full two square degree field, and 47 LAEs of them are detected in the ACS images. Nearly half of them are spatially extended with a size larger than 0.15 arcsec (∼0.88 kpc at z = 5.7) and up to 0.4 arcsec (∼2.5 kpc at z = 5.7). The others are nearly unresolved compact objects. Two LAEs show double-component structures indicating interaction or merging of building components to form more massive galaxies. By stacking the ACS images of all the detected sources, we obtain a Sersic parameter of n ∼ 0.7 with a half-light radius of 0.13 arcsec (0.76 kpc), suggesting that the majority of ACS detected LAEs have not spheroidal-like but disk-like or irregular light profiles. Comparing ACS F814W magnitudes (I 814 ) with Subaru/Suprime-Cam magnitudes in the NB816, i , and z bands, we find that the ACS imaging in the F814W band mainly probes UV continuum rather than Lyα line emission. UV continuum sizes tend to be larger for LAEs with larger Lyα emission regions as traced by the NB816 imaging. The nondetection of 38 LAEs in the ACS images is likely due to the fact that their surface brightness is too low both in the UV continuum and Lyα emission. Estimating I 814 for the ACS-undetected LAEs from the z and NB816 magnitudes, we find that 16 of these are probably LAEs with a size larger than 0.15 arcsec in UV continuum. All these results suggest that our LAE sample contains systematically larger LAEs in UV continuum size than those previously studied at z ∼ 6.

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Section: Observational Data and Acs Counterparts Of Laesmentioning

confidence: 95%

“…Note that the 3σ limiting magnitude of the F814W images is 27.3 mag in a 1 diameter aperture. All magnitudes are corrected for the Galactic extinction of A F814W = 0.035 (Capak et al 2007). In Table 4, we list the photometric properties of the LAE candidates from M07.…”

Section: Observational Data and Acs Counterparts Of Laesmentioning

confidence: 99%

HUBBLE SPACE TELESCOPE/ADVANCED CAMERA FOR SURVEYS MORPHOLOGY OF Lyα EMITTERS AT REDSHIFT 5.7 IN THE COSMOS FIELD

Taniguchi

Murayama

Scoville

et al. 2009

ApJ

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“…[50], the same catalog used to obtain the HOD parameters described in Sec. II C. Specifically, we use the Subaru i þ filter [51] to define the i-band magnitude cuts. The COSMOS data have a depth i þ ∼ 26.2 (AB magnitude, 5σ in a 3 00 aperture).…”

Section: A a Toy Model For An F Nl Galaxy Surveymentioning

confidence: 99%

Designing an inflation galaxy survey: How to measure σ(fNL)∼1 using scale-dependent galaxy bias

Putter

Doré

2017

Phys. Rev. D

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The most promising method for measuring primordial non-Gaussianity in the post-Planck era is to detect large-scale, scale-dependent galaxy bias. Considering the information in the galaxy power spectrum, we here derive the properties of a galaxy clustering survey that would optimize constraints on primordial nonGaussianity using this technique. Specifically, we ask the question of what survey design is needed to reach a precision σðf loc NL Þ ≈ 1. To answer this question, we calculate the sensitivity to f loc NL as a function of galaxy number density, redshift accuracy and sky coverage. We include the multitracer technique, which helps minimize cosmic variance noise, by considering the possibility of dividing the galaxy sample into stellar mass bins. We show that the ideal survey for f loc NL looks very different than most galaxy redshift surveys scheduled for the near future. Since those are more or less optimized for measuring the baryon acoustic oscillation scale, they typically require spectroscopic redshifts. On the contrary, to optimize the f loc NL measurement, a deep, wide, multiband imaging survey is preferred. An uncertainty σðf loc NL Þ ¼ 1 can be reached with a full-sky survey that is complete to an i-band AB magnitude i ≈ 23 and has a number density ∼8 arcmin −2 . Requirements on the multiband photometry are set by a modest photo-z accuracy σðzÞ= ð1 þ zÞ < 0.1 and the ability to measure stellar mass with a precision ∼0.2 dex or better (or another proxy for halo mass with equivalent scatter). Finally, we estimate that for the idealized case of a survey measuring all halos down to a mass 10 10 h −1 M ⊙ on the full sky out to high redshift, in principle a precision of order σðf NL Þ ∼ 0.1 can be achieved.

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“…2: High, medium, and low SNR uncorrelated Gaussian noise added to a simulated resampled and integrated spectrum also taking into consideration the spectral energy distributions and the emission-line strengths. First, we define a master catalog for the analyses, with the COSMOSSNAP simulation pipeline [12], which calibrates property distributions with real data from the COSMOS survey [13], thereby ensuring that realistic relationships between galaxy type, color, size, redshift and SED are preserved. As a result, we have constructed a master galaxy catalogue with magnitudes, colors, shapes and photometric redshifts for 538.000 galaxies on a 1.38 deg 2 region of the sky down to an i-band magnitude of ∼ 24.5.…”

Section: A Generating Euclid-like Simulated Templatesmentioning

confidence: 99%

Denoising galaxy spectra with coupled dictionary learning

Fotiadou

Tsagkatakis

Moraes

et al. 2017

2017 25th European Signal Processing Conference (EUSIPCO)

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Abstract-The Euclid satellite aims to measure accurately the global properties of the Universe, with particular emphasis on the properties of the mysterious Dark Energy that is driving the acceleration of its expansion. One of its two main observational probes relies on accurate measurements of the radial distances of galaxies through the identification of important features in their individual light spectra that are redshifted due to their receding velocity. However, several challenges for robust automated spectroscopic redshift estimation remain unsolved, one of which is the characterization of the types of spectra present in the observed galaxy population. This paper proposes a denoising technique that exploits the mathematical frameworks of Sparse Representations and Coupled Dictionary Learning, and tests it on simulated Euclid-like noisy spectroscopic templates. The reconstructed spectral profiles are able to improve the accuracy, reliability and robustness of automated redshift estimation methods. The key contribution of this work is the design of a novel model which considers coupled feature spaces, composed of high-and low-quality spectral profiles, when applied to the spectroscopic data denoising problem. The coupled dictionary learning technique is formulated within the context of the Alternating Direction Method of Multipliers, optimizing each variable via closed-form expressions. Experimental results suggest that the proposed powerful coupled dictionary learning scheme reconstructs successfully spectral profiles from their corresponding noisy versions, even with extreme noise scenarios.

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The First Release COSMOS Optical and Near‐IR Data and Catalog

Cited by 707 publications

References 53 publications

HUBBLE SPACE TELESCOPE/ADVANCED CAMERA FOR SURVEYS MORPHOLOGY OF Lyα EMITTERS AT REDSHIFT 5.7 IN THE COSMOS FIELD

HUBBLE SPACE TELESCOPE/ADVANCED CAMERA FOR SURVEYS MORPHOLOGY OF Lyα EMITTERS AT REDSHIFT 5.7 IN THE COSMOS FIELD

Designing an inflation galaxy survey: How to measure σ(fNL)∼1 using scale-dependent galaxy bias

Denoising galaxy spectra with coupled dictionary learning

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