Day 916

Wednesday.


1506.08820
Cosmic star formation history and AGN evolution near and far: from AKARI to SPICA
Goto, et al

IR luminosity is fundamental to understanding the cosmic SFH and AGN evolution, since their most intense stages are often obscured by dust.  AKARI provided unique data sets to probe these both at low and high z.  AKARI performed an all-sky survey in 6 IR bands (9,18,65,90,140, and 160um) with 3-10x better spatial resolution, AKARI can measure the total L_TIR of individual galaxies much more precisely, and thus, the total IR L density of the local universe.  In the AKARI NEP deep field, construct rest frame 8um, 12um and total IR (TIR) LFs at 0.15<z<2.2 using 4128 IR sources.  A continuous filter coverage in the MIR wavelength (2.4, 3.2, 4.1, 7,9,11,15,18 and 24 um) by the AKARI satellite allows estimation of rest frame 8 and 12 um luminosities without using a large extrapolation based on a SED fit, which was the largest uncertainty in previous work.  By combining these two results, reveal dust-hidden cosmic SFH and AGN evolution from z=0 to 2.2, all probed by the AKARI satellite.  The next generation space IR telescope, SPICA, will revolutionize the view of the IR universe with superb sensitivity of the cooled 3m space telescope.  Conclude with a survey proposal and future prospects with SPICA.


1506.08821
Evolution of mid-infrared galaxy luminosity functions from the entire AKARI NEP-deep field with new CFHT photometry
Goto, et al

Present IR galaxy LFs in the AKARI North Ecliptic Pole (NEP) deep field using the wider CFHT optical/NIR images.  ... The resulting rest frame 8um, 12um and TIR LFs at 0.15<z<2.2 are consistent with previous works, but with reduced uncertainties, especially at the high luminosity-end, thanks to the wide field coverage.  In terms of cosmic infrared luminosity density, found that it evolves as ~(1+z)^4.2±0.4.


1506.09156
The ERA method with idealizing PSF for precise weak gravitational lensing shear analysis
Okura, Futamase

Generalize ERA method of PSF correction for more realistic situations.  The method re-smears the observed galaxy image and PSF image by an appropriate function called Re-Smearing Function (RSF) to make new images with have the same ellipticity with the lensed (i.e., intrinsic) galaxy image.  It has been shown that the method avoids a systematic error arising from an approximation in the usual PSF correction in moment method such as KSB for simple PSF shape.  By adopting an idealized PSF, generalize ERA method applicable for arbitrary PSF.  This is confirmed with simulated complex PSF shapes.  Also consider the effect of pixel noise and found that the effect causes systematic overestimation.