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- executing a 2 comp. (i.e., stellar + PL) SED fitting to the following 2 LAE candidates with AGN evidence that were removed in step 3 since their reduced χ^2 were larger than 3: ID 283297 and 1199858, which show a PL-like SED in IRAC bands and are presented in p.3 of meeting150624v2.pdf:
- executing a 2 comp. (i.e., stellar + PL) SED fitting to the following 6 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: ID 157838, 181907, 287107, 306055, 307397, and 565710, which show a PL-like SED in IRAC bands and are presented in p.5 of meeting150624v2.pdf:
- revising the method to determine the parameter b which represents the fraction of the PL component to the total (stellar + PL) at λ = 8 μm
- after the revision of the method to determine the parameter b is finished, re-executing the 2 comp. SED fittings for the following samples as a test of the program: ID 608131 (AGN-MAESTLO), ID 157838, 181907, 287107, 306055, 307397, and 565710 (classified as "others" in step 2), and ID 283297 and 1199858 (rejected in step 3 via the criteria of χ_ν^2 <= 3)
- after the cross-matching analysis with new Chandra data by S. Toft is done, selecting the objects detected in Chandra among the objects classified as "others" in Step 2 or having reduced χ^2 > 3 in Step 3 and revising the tables shown below in the Fixed Action Items as of 2015/06/24
- a cross matched catalog w/ Chandra (from S. Toft on 8th July, 2015):
lya_x_2arcsec.txt
- the above catalog seems to extract the IA-excess objects detected by Chandra within |ΔR.A.| < 2 arcsec & |ΔDecl.| < 2 arcsec
- the catalogs matched with Chandra within Δr < 1, 2 arcsec are the following (made by Y. Shioya on 9th July, 2015): lya_x_1arcsec_circ.txt lya_x_2arcsec_circ.txt
- executing the 2 comp. SED fitting for all objects selected in the above processes (i.e., the objects classified as AGN via our selection criteria used in Step 4 among the objects classified as "others" in Step 2 or having reduced χ^2 > 3 in Step 3)
- 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 2015/07/02 †
- sending a list of objects in which the ID and (RA,DEC) of the IA-excess objects selected in Step 1 are written to S. Toft to ask a cross-matching with new Chandra data
as of 2015/6/29 †
- 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.
- since the SEDs of these objects are well fitted by stellar population only, we will not perform the 2 component SED fitting for them
as of 2015/6/27 †
- making a list of the IA-excess objects selected in Step 1 (i.e., 5357 objects)
- list of all IA-excess objects selected in Step 1 (5357 objects): allIAexObj_RA_DEC.txt
- list of the IA-excess objects selected in Step 1, which have not been cross-matched (4768 objects = 5357 - 589 LAEs): allIAexObj_nonRealLAE.txt
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):
- 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 2015/06/20 †
- 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
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