Infrared luminosity functions based on 18 mid-infrared bands: revealing cosmic star formation history with AKARI and Hyper Suprime-Cam
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Citations
Dust Spectral Energy Distributions of Nearby Galaxies: an Insight from the Herschel Reference Survey
The ALPINE-ALMA [CII] survey - The nature, luminosity function, and star formation history of dusty galaxies up to z ≃ 6
UV and U-band luminosity functions from CLAUDS and HSC-SSP - I. Using four million galaxies to simultaneously constrain the very faint and bright regimes to z ∼ 3
Fast radio bursts to be detected with the Square Kilometre Array
The Variability of the Star Formation Rate in Galaxies: I. Star Formation Histories Traced by EW(H$\alpha$) and EW(H$\delta_A$)
References
Evolution of infrared luminosity functions of galaxies in the AKARI NEP-deep field - Revealing the cosmic star formation history hidden by dust
Estimating the total infrared luminosity of galaxies up to z ∼ 2 from mid- and far-infrared observations
Mapping dusty star formation in and around a cluster at z = 0.81 by wide-field imaging with AKARI
INFRARED SPECTROGRAPH SPECTROSCOPY AND MULTI-WAVELENGTH STUDY OF LUMINOUS STAR-FORMING GALAXIES AT z ≃ 1.9
The Local Galaxy 8 μm Luminosity Function
Related Papers (5)
Infrared luminosity functions based on 18 mid-infrared bands: revealing cosmic star formation history with AKARI and Hyper Suprime-Cam∗
Evolution of mid-infrared galaxy luminosity functions from the entire AKARI NEP deep field with new CFHT photometry
Frequently Asked Questions (6)
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.