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- checking whether there are emission-line objects classified as AGN (IRAC, X-ray, radio) in the samples that are identified as CIV, CIII], ..., Hα emitters.
- evaluating the contribution of the power-law (PL) component on the SED fitting (ref. Caputi 2013, ApJ, 768, 103) for one LAE candidate with AGN evidence that was removed in step 3 since its reduced χ^2 was larger than 3 (e.g., ID 283297 which shows a PL-like SED in IRAC bands) at least.
- evaluating the contribution of the power-law (PL) component on the SED fitting (ref. Caputi 2013, ApJ, 768, 103) for several IA-band excess objects with AGN evidence that were not identified as strong emission-line in step 2 since its reduced χ^2 was larger than 3 (e.g., ID 181907 which shows a PL-like SED in IRAC bands).
- revising the method fot evaluating the contribution of the power-law (PL) component on the SED fitting. Although Caputi (2013) set b = 0.1, 0.2, ..., 1.0, we set b using the analytical formula.
- making a plot of distribution in the SFR--Mstar plane for SF-MAESTLO and AGN-MAESTLO
- AGN-MAESTLO is re-selected from the above-constructed sample
- for AGN-MAESTLO, both of the SFR and Mstar should be evaluated from the stellar component
as of 2015/06/20 †
- making the Figure and Table for AGN-MAESTLO in the same format with Fig. 1 and Tab. 1 of the MAESTLO paper
- see above Figure and Table
as of 2015/06/24 †
- evaluating the contribution of the power-law (PL) component on the SED fitting (ref. Caputi 2013, ApJ, 768, 103) for one AGN-MAESTLO (e.g., ID 608131 which shows a PL-like SED in IRAC bands) at least.
- Caputi13 evaluate the PL contribution for 174 24 μm selected galaxies w/ S_ν(24 μm) >= 80 μJy and z_spec > 1 using the following equation:
- S_ν(λ) = S_ν^stellar(λ) + b S_ν(8 μm)(λ / 8 μm)^α, where α = 1.3, 2.0, 3.0 and b = 0.0, 0.1, ..., 1.0
- the three adopted α values are representative of the IR PL indices that characterize different types of AGNs, with different hot-dust components (e.g., Alonso-Herrero+03, 06; Polletta+06; Honig+10)
- b = 0.0 (1.0) corresponds to the pure stellar (PL) type
- if b is non-zero, the best-fit value of Mstar is expected to decrease and the rest-frame V-J color of the best-fit stellar component is also expected to be bluer compared with those of b = 0
- SED fitting:
- U-V vs. V-J:
- SFR vs Mstar:
as of 2015/06/24 †
- checking whether there are emission-line objects classified as AGN (IRAC, X-ray, radio) in the sample with reduced χ^2 > 3 in steps 2 & 3.
- this AI is for constructing a well-defined sample of AGN w/ Lya emission: in the current selection, the objects having non-stellar like SED (e.g., PL dominated one) can be excluded by the criteria of reduced χ^2 <= 3 both in step 2 and step 3
- in this sense, the current sample of AGN-MAESTLO is still incomplete
- the objects to which the IRAC-color criteria cannot be applied (i.e., undetected in some of the IRAC bands) are remained to be excluded in this step; this is for constructing a secure sample of AGN w/ Lya emission
- step 3 (reduced χ^2 > 3):
- step 2 (others):
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AGN-MAESTLO2.eps
