In this paper, the authors performed a census of dust-obscured CSFH in the entire AKARI NEP field in 5 broad bands and estimated total infrared LFs at 0.35$ <$z$<$2.2.
Abstract:
Much of the star formation is obscured by dust. For the complete understanding of the cosmic star formation history (CSFH), infrared (IR) census is indispensable. AKARI carried out deep mid-infrared observations using its continuous 9-band filters in the North Ecliptic Pole (NEP) field (5.4 deg$^2$). This took significant amount of satellite's lifetime, $\sim$10\% of the entire pointed observations.
By combining archival Spitzer (5 bands) and WISE (4 bands) mid-IR photometry, we have, in total, 18 band mid-IR photometry, which is the most comprehensive photometric coverage in mid-IR for thousands of galaxies. However previously, we only had shallow optical imaging ($\sim$25.9ABmag) in a small area of 1.0 deg$^2$. As a result, there remained thousands of AKARI's infrared sources undetected in optical.
Using the new Hyper Suprime-Cam on Subaru telescope, we obtained deep enough optical images of the entire AKARI NEP field in 5 broad bands ($g\sim$27.5mag). These provided photometric redshift, and thereby IR luminosity for the previously undetected faint AKARI IR sources. Combined with the accurate mid-IR luminosity measurement, we constructed mid-IR LFs, and thereby performed a census of dust-obscured CSFH in the entire AKARI NEP field.
We have measured restframe 8$\mu$m, 12$\mu$m luminosity functions (LFs), and estimated total infrared LFs at 0.35$<$z$<$2.2. Our results are consistent with our previous work, but with much reduced statistical errors thanks to the large area coverage of the new data. We have possibly witnessed the turnover of CSFH at $z\sim$2.
TL;DR: In this article, the authors reported ALMA far-infrared (FIR) observations of six IR-bright GRB host galaxies, which are selected for the brightness in IR among them, four host galaxies are detected for the first time in the rest-frame FIR.
TL;DR: In this article , the authors presented a catalog of radio sources from Karl J. Jansky Very Large Array 3 GHz observations of the TDF, which were obtained to aid the study of dust-obscured galaxies that contribute significantly to cosmic star formation at high redshifts.
TL;DR: In this article, the authors focus on the broad patterns in the star formation properties of galaxies along the Hubble sequence and their implications for understanding galaxy evolution and the physical processes that drive the evolution.
TL;DR: The James Webb Space Telescope (JWST) as discussed by the authors is a large (6.6 m), cold (<50 K), infrared-optimized space observatory that will be launched early in the next decade into orbit around the second Earth-Sun Lagrange point.
TL;DR: In this article, the evolution of the mid-infrared local luminosity function with redshift to the spectrum of the cosmic infrared background (CIRB) at j[ 5 km and the galaxy counts from various surveys at midinfrared, far infrared, and submillimeter wavelengths was investigated.
TL;DR: In this paper, the authors examined the infrared (IR) 3-500μm spectral energy distributions (SEDs) of galaxies at 0 < z < 2.5, supplemented by a local reference sample from IRAS, ISO, Spitzer, and AKARI data.
TL;DR: In this paper, the authors analyzed a sample of ~2600 Spitzer MIPS 24 μm sources and located in the Chandra Deep Field-South to characterize the evolution of the comoving infrared (IR) energy density of the universe up to z ~ 1.
Q1. What are the contributions mentioned in the paper "Infrared luminosity functions based on 18 mid-infrared bands: revealing cosmic star formation history with akari and hyper suprime-cam*" ?
Combined with the accurate mid-IR luminosity measurement, the authors constructed mid-IR LFs, and thereby performed a census of dust-obscured CSFH in the entire AKARI NEP field.
Q2. Why do they use the L15 flux?
The L18W flux (Matsuhara et al. 2006) are used to apply the 1/Vmax method, because it is a wide, sensitive filter (but using the L15 flux limit does not change their main results).
Q3. What is the common wavelength of the AKARI NEP?
Mid-infrared (mid-IR) is one of the less explored wavelengths due to the earth’s atmosphere, and difficulties in developing sensitive detectors.
Q4. What are the uncertainties of the LF?
Uncertainties of the LF values includefluctuations in the number of sources in each luminosity bin, the photometric redshift uncertainties, the k-correction uncertainties, and the flux errors.
Q5. What is the largest FoV of a Subaru telescope?
It has the largest FoV among optical cameras on 8m-class telescopes, and can cover the AKARI NEP wide field (5.4 deg2) with only 4 FoV (Fig.1).
Q6. Why is IR from 12m LFs larger?
even with AKARI’s sensitivity, the observation might not be deep enough to reliably measure the faint-end slope of 12µm LFs, possibly because 12µm does not contain as luminous emission lines as in the case of 8µm.