2010A&A...509A.105M


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.03CET00:56:48

2010A&A...509A.105M - Astronomy and Astrophysics, volume 509, A105-105 (2010/1-1)

Looking for the first galaxies: lensing or blank fields?

MAIZY A., RICHARD J., DE LEO M.A., PELLO R. and KNEIB J.P.

Abstract (from CDS):

The identification and study of the first galaxies remains one of the most exciting topics in observational cosmology. The determination of the best possible observing strategies is a very important choice in order to build up a representative sample of spectroscopically confirmed sources at high-z (z>7), beyond the limits of present-day observations. This paper is intended to precisely adress the relative efficiency of lensing and blank fields in the identification and study of galaxies at 6≲z≲12. The detection efficiency and field-to-field variance are estimated from direct simulations of both blank and lensing fields observations. Present known luminosity functions in the UV are used to determine the expected distribution and properties of distant samples at z>6 for a variety of survey configurations. Different models for well known lensing clusters are used to simulate in details the magnification and dilution effects on the backgound distant population of galaxies. The presence of a strong-lensing cluster along the line of sight has a dramatic effect on the number of observed sources, with a positive magnification bias in typical ground-based ``shallow'' surveys (AB≲25.5). The positive magnification bias increases with the redshift of sources and decreases with both depth of the survey and the size of the surveyed area. The maximum efficiency is reached for lensing clusters at z∼0.1-0.3. Observing blank fields in shallow surveys is particularly inefficient as compared to lensing fields if the UV LF for LBGs is strongly evolving at z>7. Also in this case, the number of z≥8 sources expected at the typical depth of JWST (AB∼28-29) is much higher in lensing than in blank fields (e.g. a factor of ∼10 for AB≲28). All these results have been obtained assuming that number counts derived in clusters are not dominated by sources below the limiting surface brightness of observations, which in turn depends on the reliability of the usual scalings applied to the size of high-z sources. Blank field surveys with a large field of view are needed to prove the bright end of the LF at z>6-7, whereas lensing clusters are particularly useful for exploring the mid to faint end of the LF.

Abstract Copyright:

Journal keyword(s): gravitational lensing: strong - galaxies: high-redshift - galaxies: luminosity function, mass function - galaxies: clusters: general

Simbad objects: 4

goto Full paper

goto View the reference in ADS

Number of rows : 4

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Hubble Ultra Deep Field reg 03 32 39.0 -27 47 29           ~ 1342 0
2 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1037 0
3 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 635 1
4 ACO S 1077 ClG 22 58 52.34 -34 46 54.6           ~ 180 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2010A&A...509A.105M and select 'bookmark this link' or equivalent in the popup menu


2021.03.03-00:56:48

© Université de Strasbourg/CNRS

    • Contact