Infrared luminosity functions based on 18 mid-infrared bands: revealing cosmic star formation history with AKARI and Hyper Suprime-Cam∗
Summary (3 min read)
1 Introduction
- Mid-infrared (mid-IR) is one of the less explored wavelengths due to the earth’s atmosphere, and difficulties in developing sensitive detectors.
- Using AKARI’s 9 mid-IR band photometry, mid-IR SED diagnosis can be performed for thousands of galaxies, for the first time, over the large enough area to overcome cosmic variance.
- Environmental effects on galaxy evolution can be also investigated with the large volume coverage (Koyama et al. 2008; Goto et al. 2010a).
- Previously, the authors were limited by a poor optical coverage both in area and depths.
- To overcome these problems, the authors have newly obtained deeper optical data over the entire AKARI NEP wide field, using the Hyper-Suprime Cam on the Subaru telescope.
2 Data
- To rectify the situation and to fully exploit the AKARI’s spacebased data, the authors carried out an optical survey of the AKARI NEP wide field (PI:Goto) using Subaru’s new Hyper Suprime-Cam (HSC; Miyazaki et al. 2018) in five optical bands (g,r, i,z, and y, Oi et al. 2018 submitted).
- The HSC has a field-of-view (FoV) of 1.5 deg in diameter, covered with 104 red-sensitive CCDs.
- See Oi et al. (2018, submitted) for more details of the observation and data reduction.
- Subaru telescope does not have u∗-band capability, while it is critically important to accurately estimate photometric redshifts (photo-z) of low-z galaxies.
- Therefore, the authors obtained u∗band image of the AKARI NEP wide field using the Megaprime camera of Canada France Hawaii Telescope (PI:Goto, Goto et al. 2017).
3 Analysis
- Uncertainties of the LF values include fluctuations in the number of sources in each luminosity bin, the photometric redshift uncertainties, the k-correction uncertainties, and the flux errors.
- To estimate errors, the authors used Monte Carlo simulations from 1000 simulated catalogs.
- These sources are assigned with a new redshift, to follow a Gaussian distribution centered at the photo-z with the width of ∆z/(1+ z) (∼ 0.060, Oi et al. in preparation).
- A new flux is also assigned following a Gaussian distribution with the width of flux error.
- For total infrared (TIR) LF errors, the authors re-performed the SED fit for the 1000 simulated catalogs.
4 Results
- The authors first present monochromatic 8µm LFs, because the 8µm luminosity (L8µm) has been known as a good indicator of the TIR luminosity (Babbedge et al.
- Various previous studies are shown in dash-dotted lines.
- The authors 12µm LFs show steady evolution with increasing redshift.
- 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).
- AKARI’s TIR LFs are at least consistent with one of the previous studies.
4.4.1 Total IR Luminosity Density from L8µm LFs
- First, the authors estimate Total IR Luminosity Density from L8µm LFs.
- To do so, the authors need to convert L8µm to the total infrared luminosity.
- Possible SED evolution, and the presence of AGN will induce further uncertainty.
- Murata et al. (2014) also reported that L8µm/LTIR is constant at below the main sequence, while it decreases with starburstiness at above the main sequence, concluding that starburst galaxies have deficient PAH emission compared with main-sequence galaxies.
- The authors further test this issue using their data in Section 5.
4.4.2 Total IR Luminosity Density from L12µm LFs
- Due to the same reasons as L8µm (improved statistics, and availability of 140 and 160µm), the authors use the following conversion (Goto et al. 2011b).
- The authors caution readers again here for the use of a single conversion for varieties of galaxies with different SFR at different redshifts.
- Results should be interpreted with this uncertainty in mind.
4.4.3 Integration to TIR density
- The derived total LFs are multiplied by LTIR and integrated to measure the TIR density ( ΩTIR).
- With the lowest redshift LF, the authors first fit the normalization (Φ∗) and slopes (α,β).
- At the first glance, ΩIR from 8µm and TIR LFs are consistent with each other.
- 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.
- This is an interesting implication, but it is unfortunate that their error bars are too large to draw significant conclusions.
5 Discussion
- In the previous section, in addition to LTIR measurement, the authors converted L8µm and L12µm into LTIR.
- The conversions are based on local star-forming galaxies.
- Following the results in the literature discussed in Section 4.3, in this section, the authors compare LTIR estimated from L8µm and L12µm from equations 1 and 2 in three overlapping redshift ranges in Fig.6 using their data.
- One can immediately notice that the relation deviates at logLTIR >12 (or equivalently at z > 1).
- 4 and 5 between midand far-IR measurements could be the result of the change in the SED, rather than incorrect measurements on either.
6 Summary
- Previously AKARI NEP wide field lacked deep optical photometry, and thereby, accurate photo-z, despite the presence of space-based 9-band mid-IR photometry from AKARI.
- Combined with the CFHT u-band imaging the authors have also taken, for the first time, they used all of the AKARI’s data over the 5.4 deg2.
- The authors also estimated total infrared LFs through SED fitting to the 18- band mid-IR data.
- Thanks to the large area coverage, the brightends are better-determined.
- It is interesting to note that ΩIR becomes smaller at z > 1.2, possibly suggesting the turnover of the CSFH.
Acknowledgments
- The authors thank the anonymous referee for many insightful comments, which significantly improved the paper.
- The authors are grateful for Tina Wang, and Simon Ho for careful proof-reading of the paper.
- TG acknowledges the support by the Ministry of Science and Technology of Taiwan through grant 105-2112-M-007-003-MY3.
- MI acknowledges the support from the grant No. 2017R1A3A3001362 of the National Research Foundation of Korea (NRF).
- YO acknowledges the support by the Ministry of Science and Technology of Taiwan through grant MOST 107-2119-M-001-026.
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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.