Measuring the Redshift Evolution of Clustering: the Hubble Deep Field South

By Stéphane Arnouts, L. Moscardini, E. Vanzella, Stéphane Colombi, S. Cristiani, A. Fontana, E. Giallongo, S. Matarrese, P. Saracco. 2001

194 citations recorded by the source corpus.

ABSTRA C T We present an analysis of the evolution of galaxy clustering in the redshift interval 0 # z # 4:5 in the Hubble Deep Field South (HDF-South). The HST optical data are combined with infrared ISAAC/VLT observations, and photometric redshifts are used for all the galaxies brighter than IAB # 27:5. The clustering signal is obtained in different redshift bins using two different approaches: a standard one, which uses the best redshift estimate of each object, and a second one, which takes into account the redshift probability function of each object. This second method makes it possible to improve the information in the redshift intervals where contamination from objects with insecure redshifts is important. With both methods, we find that the clustering strength up to z . 3:5 in the HDF-South is consistent with the previous results in the HDF-North. Whereas at redshift lower than z , 1 the HDF galaxy population is un/anti-biasedOb # 1U with respect to the underlying dark matter, at high redshift the bias increases up to bOz , 3U . 2‐3, depending on the cosmological model. These results support previous claims that, at high redshift, galaxies are preferentially located in massive haloes, as predicted by the biased galaxy formation scenario. In order to quantify the impact of cosmic errors on our analyses, we have used analytical expressions from Bernstein. Once the behaviour of higher-order moments is assumed, our results show that errors in the clustering measurements in the HDF surveys are indeed dominated by pure shot-noise in most regimes, as assumed in our analysis. We also show that future observations with instruments like the Advanced Camera on HST will improve the signal-to-noise ratio by at least a factor of 2, as a consequence, more detailed analyses of the errors will be required. In fact, pure shot-noise will give a smaller contribution with respect to other sources of errors, such as finite volume effects or non-Poissonian discreteness effects.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7cea7ffc1d99af3b4c4697d7c6946ed760e35b83

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

Photometric redshifts for the SDSS Data Release 12 (2016, methodology): “…traditional maximum likelihood template-based photometric redshift estimation methods (Bolzonella, Miralles & Pelló 2000; Csabai et al. 2000; Arnouts et al. 2002; Ilbert et al. 2006) solve the following problem: c© 2016 RAS, MNRAS 000, 1–12 (zphot,i; ti;m0,i) = arg min (z;t;m0) D∑ p=1 (…”
Accurate photometric redshifts for the CFHT legacy survey calibrated using the VIMOS VLT deep survey (2006, methodology): “The redshift Probability Distribution Function for each object (see Arnouts et al. 2002) is directly derived from the χ2 distribution PDFz ∝ exp ( −χ 2(z) 2 ) .”
THE STAR FORMATION HISTORY OF MASS-SELECTED GALAXIES IN THE COSMOS FIELD (2010, methodology): “26 As described in detail by I10 all photo-z’s used in our study were obtained using a χ2 template-fitting procedure implemented in the code Le Phare (Arnouts et al. 2002; Ilbert et al. 2006) and a library of 21 templates.”
Photometric redshift analysis in the Dark Energy Survey Science Verification data (2014, methodology): “LePhare (Arnouts et al. (2002); Ilbert et al. (2006)) is a public template fitting code that uses a χ2 minimization of differences between observed and theoretical magnitudes to find the best template (galaxy type) and redshift.”
Euclid preparation (2021, methodology): “We randomised the true redshift assuming a Gaussian distribution with σ = σtrue, where σtrue is defined as the median value of the LePhare photo-z errors.”
The VIMOS-VLT deep survey - Evolution of the galaxy luminosity function up to z = 2 in first epoch data (2004, unknown): “We sum the normalized PDFz of all galaxies to estimate the expected redshift distribution (Arnouts et al. 2002).”
Mass assembly in quiescent and star-forming galaxies since z ≃ 4 from UltraVISTA (2013, methodology): “The photometric redshifts are derived usingLe Phare following a procedure similar to Ilbert et al. (2009).”
The Horizon-AGN simulation: evolution of galaxy properties over cosmic time (2016, methodology): “Photometric redshifts, rest-frame magnitudes and stellar masses are computed using SED fitting via the LePhare code (Arnouts et al. 1999, 2002; Ilbert et al. 2006), following the methodology described in Ilbert et al. (2013).”
PHAT: PHoto-z Accuracy Testing (2010, background): “Le Phare is based on a standard template fitting procedure.”
The COSMOS2015 galaxy stellar mass function . Thirteen billion years of stellar mass assembly in ten snapshots (2017, methodology): “2.2) after recomputing their stellar mass with LePhare to be consistent with our catalogue.”
The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4 (2013, methodology): “…multi-wavelength data to derive the SEDs of our PEP sources, which we interpreted and classified by performing a χ2 fit (using the Le Phare code2; Arnouts et al. 2002 and Ilbert et al. 2006) with the semi-empirical template library of Polletta et al. (2007), representative of different classes…”
STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, methodology): “Redshifts were attributed to individual galaxies via a standard χ2 fitting procedure (Arnouts et al. 2002) encoded in Le Phare24, written by S. Arnouts and O. Ilbert.”
GALAXY STELLAR MASS ASSEMBLY BETWEEN 0.2 < z < 2 FROM THE S-COSMOS SURVEY (2009, methodology): “We derived photometric redshifts using the Le Phare2 code (Arnouts et al. 2002 and Ilbert et al. 2006b) with a χ2 template-fitting method.”
Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes since z ~ 1.2 (2011, methodology): “Our photometric redshifts were measured using LePhare (Arnouts et al. 2002) following the procedures outlined in Ilbert et al. (2006) and Coupon et al. (2009).”
Photometric redshifts for the CFHTLS T0004 deep and wide fields (2008, methodology): “In particular, the “Le Phare” photometric redshift code (Arnouts et al. 1999, Arnouts et al. 2002, I06) has shown to be well adapted for joint photometric and spectroscopic surveys like the CFHTLS. I06 usedLe Phare with the CFHTLSDeep photometric catalogues and VVDS spectroscopic redshifts (Le…”
THE COSMOS2015 CATALOG: EXPLORING THE 1 < z < 6 UNIVERSE WITH HALF A MILLION GALAXIES (2016, methodology): “We derive the stellar mass using LePhare following exactly the same method as in Ilbert et al. (2015).”
The WIRCam Deep Survey I. Counts, colours, and mass-functions derived from near-infrared imaging in the CFHTLS deep fields (2011, methodology): “We use the “Le Phare”6 (Arnouts et al. 2002; Ilbert et al. 2006) package to measure photometric redshifts and galaxy properties with aχ2 templatefitting method, based on the method of Ilbert et al. (2006) and Ilbert et al. (2009).”
The Spatial Clustering of Star-forming Galaxies at Redshifts 1.4 ≲ z ≲ 3.5 (2004, result): “The survey analyzed here is several times larger than its predecessors; the surveyed area of 0.81 deg2 is roughly 700 times larger than the area analyzed by Arnouts et al. (2002) and 4 times larger than the areas analyzed by Giavalisco & Dickinson (2001) and Ouchi et al. (2001).”