FERENGI: Redshifting galaxies from SDSS to GEMS, STAGES and COSMOS

Abstract

We describe the creation of a set of artificially "redshifted" galaxies in the range 0.1<z<1.1 using a set of ~100 SDSS low redshift (v<7000 km/s) images as input. The intention is to generate a training set of realistic images of galaxies of diverse morphologies and a large range of redshifts for the GEMS and COSMOS galaxy evolution projects. This training set allows other studies to investigate and quantify the effects of cosmological redshift on the determination of galaxy morphologies, distortions and other galaxy properties that are potentially sensitive to resolution, surface brightness and bandpass issues. We use galaxy images from the SDSS in the u, g, r, i, z filter bands as input, and computed new galaxy images from these data, resembling the same galaxies as located at redshifts 0.1<z<1.1 and viewed with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS). In this process we take into account angular size change, cosmological surface brightness dimming, and spectral change. The latter is achieved by interpolating a spectral energy distribution that is fit to the input images on a pixel-to-pixel basis. The output images are created for the specific HST ACS point spread function and the filters used for GEMS (F606W and F850LP) and COSMOS (F814W). All images are binned onto the desired pixel grids (0.03" for GEMS and 0.05" for COSMOS) and corrected to an appropriate point spread function. Noise is added corresponding to the data quality of the two projects and the images are added onto empty sky pieces of real data images. We make these datasets available from our website, as well as the code - FERENGI: "Full and Efficient Redshifting of Ensembles of Nearby Galaxy Images" - to produce datasets for other redshifts and/or instruments.

11 pages, 10 figures, 3 tables

Cited by in corpus (23)

• Clumpy Galaxies in CANDELS. I. The Definition of UV Clumps and the Fraction of Clumpy Galaxies at 0.5<z<3
• Galaxy Zoo: Morphological Classifications for 120,000 Galaxies in HST Legacy Imaging
• Galaxy Merger Rates up to z $\sim$ 3 using a Bayesian Deep Learning Model $-$ A Major-Merger classifier using IllustrisTNG Simulation data
• MegaMorph -- multi-wavelength measurement of galaxy structure: physically meaningful bulge-disc decomposition of galaxies near and far
• Early results from GLASS-JWST XIV: A first morphological atlas of the 1 < z < 5 Universe in the rest-frame optical
• Galaxy Evolution in all Five CANDELS Fields and IllustrisTNG: Morphological, Structural, and the Major Merger Evolution to $z\sim 3$
• The Formation of Bulges, Discs and Two Component Galaxies in the CANDELS Survey at z < 3
• The structural and size evolution of star-forming galaxies over the last 11 Gyrs
• Revealing the cosmic evolution of boxy/peanut-shaped bulges from HST COSMOS and SDSS
• MegaMorph: classifying galaxy morphology using multi-wavelength Sérsic profile fits
• A comparison of the morphological properties between local and z~1 infrared luminous galaxies. Are local and high-z (U)LIRGs different?
• Quantifying Non-parametric Structure of High-redshift Galaxies with Deep Learning
• Kpc-scale Properties of Emission-line Galaxies
• The Role of Major Mergers and Nuclear Star Formation in Nearby Obscured Quasars
• Observations of the Initial Formation and Evolution of Spiral galaxies at $1<z<3$ in the CANDELS fields
• Merging Galaxies with Tidal Tails in COSMOS to z=1
• Redshifting galaxies from DESI to JWST CEERS: Correction of biases and uncertainties in quantifying morphology
• Exploring the progenitors of brightest cluster galaxies at z~2
• Bulgeless disks, dark galaxies, inverted color gradients, and other expected phenomena at higher z. The chromatic surface brightness modulation (CMOD) effect
• Systematic errors on optical-SED stellar mass estimates for galaxies across cosmic time and their impact on cosmology
• The MOSDEF Survey: An Improved Voronoi Binning Technique on Spatially Resolved Stellar Populations at z~2
• The PSF Smoothing Effect on Concentration-Related Parameters of High Redshift Galaxies in HST and JWST
• The MOSDEF Survey: Probing Resolved Stellar Populations at $z\sim 2$ Using a New Bayesian-defined Morphology Metric Called Patchiness