We use a model developed by Xu,Ferrara,and Chen(Mon Not Roy Astron Soc,submitted) to compute the 21 cm line absorption signatures imprinted by star-forming dwarf galaxies(DGs) and starless minihalos(MHs). The method,based on a statistical comparison of the equivalent width(W ν ) distribution and flux correlation function,allows us to derive a simple selection criteria for candidate DGs at very high(z ≤ 8) redshift. We find that ≈18% of the total number of DGs along a line of sight to a target radio source(GRB or quasar) can be identified by the condition W ν<0; these objects correspond to the high-mass tail of the DG distribution at high redshift,and are embedded in large HII regions. The criterion W ν>0.37 kHz instead selects ≈11% of MHs. Selected candidate DGs could later be re-observed in the near-IR by the JWST with high efficiency,thus providing a direct probe of the most likely reionization sources.
Taking into account the noise from intrinsic ellipticities of source galaxies,we study the efficiency and completeness of halo detections from weak lensing convergence maps.Particularly,with numerical simulations,we compare the Gaussian filter with the so called MRLens treatment based on the modification of the Maximum Entropy Method.For a pure noise field without lensing signals,a Gaussian smoothing results in a residual noise field that is approximately Gaussian in terms of statistics if a large enough number of galaxies are included in the smoothing window.On the other hand,the noise field after the MRLens treatment is significantly non-Gaussian,resulting in complications in characterizing the noise effects.Considering weak-lensing cluster detections,although the MRLens treatment effectively deletes false peaks arising from noise,it removes the real peaks heavily due to its inability to distinguish real signals with relatively low amplitudes from noise in its restoration process.The higher the noise level is,the larger the removal effects are for the real peaks.For a survey with a source density ng-30 arcmin-2,the number of peaks found in an area of 3×3 deg2 after MRLens filtering is only-50 for the detection threshold κ = 0.02,while the number of halos with M > 5 × 1013 M and with redshift z ≤ 2 in the same area is expected to be-530.For the Gaussian smoothing treatment,the number of detections is-260,much larger than that of the MRLens.The Gaussianity of the noise statistics in the Gaussian smoothing case adds further advantages for this method to circumvent the problem of the relatively low efficiency in weak-lensing cluster detections.Therefore,in studies aiming to construct large cluster samples from weak-lensing surveys,the Gaussian smoothing method performs significantly better than the MRLens treatment.
