Reconstructing the galaxy density field with photometric redshifts

Abstract

Context. Measuring environment for large numbers of galaxies in the distant Universe is an open problem in astrophysics, as environment is important in determining many properties of galaxies during their formation and evolution. In order to measure galaxy environments, we need galaxy positions and redshifts. Photometric redshifts are more easily available for large numbers of galaxies, but at the price of larger uncertainties than spectroscopic redshifts. Aims. We study how photometric redshifts affect the measurement of galaxy environment and how the reconstruction of the density field may limit an analysis of the galaxy stellar mass function (GSMF) in different environments. Methods. Through the use of mock galaxy catalogues, we measured galaxy environment with a fixed aperture method, using each galaxy's true and photometric redshifts. We varied the parameters defining the fixed aperture volume and explored different configurations. We also used photometric redshifts with different uncertainties to simulate the case of various surveys. We then computed GSMF of the mock galaxy catalogues as a function of redshift and environment to see how the environmental estimate based on photometric redshifts affects their analysis. Results. We found that the most extreme environments can be reconstructed in a fairly accurate way only when using high-precision photometric redshifts with σ ∆z/(1+z) 0.01, with a fraction ≥60 ÷ 80% of galaxies placed in the correct density quartile and a contamination of ≤10% by opposite quartile interlopers. A length of the volume in the radial direction comparable to the ±1.5σ error of photometric redshifts and a fixed aperture radius of a size similar to the physical scale of the studied environment grant a better reconstruction than other volume configurations. When using this kind of an estimate of the density field, we found that any difference between the starting GSMF (divided accordingly to the true galaxy environment) is damped on average by ∼0.3 dex with photometric redshifts, but is still resolvable. Although derived with mock galaxy catalogues, these results may be used to interpret real data, as we obtained them by comparing results between the true redshift and photometric redshift case, therefore, in a way that does not completely depend on how well the mock catalogues reproduce the real galaxy distribution. Conclusions. This work allows us several useful considerations on how to interpret results of an analysis of the GSMF in different environments when the density field is measured with photometric redshifts and represents a preparatory study for future wide area photometric redshift surveys, such as the Euclid Survey. We plan to apply the result of this work to an environmental analysis of the GSMF in the UltraVISTA Survey in future work.

Cosmic Web of Galaxies in the COSMOS Field: Public Catalog and Different Quenching for Centrals and Satellites

“…0.01 can still fairly accurately construct the density field (e.g., Cooper et al 2005;Malavasi et al 2016), with more optimistic studies such as Lai et al (2016) showing that even larger uncertainties can still reveal the general environmentally driven trends. Therefore, reliable and accurate photometric redshift measurements are of crucial importance.…”

“…We estimate the density field for a series of overlapping redshift slices (z-slice) with variable widths to z=1.2. As suggested by Malavasi et al (2016), z-slice widths are selected to be within…”

On the fast quenching of young low-mass galaxies up to z ∼ 0.6: new spotlight on the lead role of environment

“…To measure the local density of environment surrounding galaxies in our photo-z sample, we adopted a method similar to Lani et al (2013) and Malavasi et al (2016). In brief, we counted the number of galaxies lying in a cylinder of fixed aperture centered on each galaxy for which we measured the density.…”

“…In brief, we counted the number of galaxies lying in a cylinder of fixed aperture centered on each galaxy for which we measured the density. The cylinder physical depth was set at 1 Gyr, which turned out to be a good compromise to avoid galaxy exclusion and excessive dilution in our case 5 (for a detailed analysis of the completeness and purity associated with the use of photometric redshifts for reconstructing the galaxy density field, please refer to Malavasi et al 2016).…”

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

“…Several analyses have used some of the most precise photometric redshifts available to date (Scoville et al 2013;Darvish et al 2015;Malavasi et al 2016). Despite this, spectroscopic measurements of galaxy redshifts (z spec ) are generally required in order to minimise the uncertainties in the radial position of galaxies.…”