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[[FrontPage]] - [[Action Items Related to AGN-MAESTLO>AGN-MAESTLO#ActionItem]] - [[Manuscript>AGN-MAESTLO#Manuscript]] - [[Figures>AGN-MAESTLO#Figures]] - [[Fixed Action Items>AGN-MAESTLO#FixedAIs]] * &aname(ActionItem){Action Items Related to AGN-MAESTLO}; [#e0af5dd9] - 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: &ref(p3_meeting150624v2.jpg,,30%); - 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: &ref(p5_meeting150624v2.jpg,,30%); - 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): &ref(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): &ref(lya_x_1arcsec_circ.txt); &ref(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 * &aname(Manuscript){Manuscript}; [#pa779959] ** &aname(Figures){Figures}; [#v459d6e0] - Fig. 1: &ref(AGN-MAESTLO2.jpg,,15%); &ref(AGN-MAESTLO2.eps); - Tab. 1: &ref(AGN_MAESTLO_Table1.jpg,,30%); * &aname(FixedAIs){Fixed Action Items}; [#o13db940] ** as of 2015/10/01 [#t8f417f9] - revising a list of objects showing evidences of AGNs in the sample of no-solution (N_sol = 0) in step 2 based on Step2.dat (20150927). &ref(Nsol0_allIA_AGN_150927.txt); -- summay: &ref(Table_Nsol0_AGN_150927.jpg,,40%); ** as of 2015/09/10 [#i6c3c9a0] - revising a list of objects showing evidences of AGNs in the sample of no-solution (N_sol = 0) in step 2 based on Step.dat (20150907). &ref(Nsol0_allIA_AGN_150907.txt); -- summay: &ref(Table_Nsol0_AGN_150907.jpg,,70%); ** as of 2015/07/31 [#r957a59c] - revising a list of objects showing evidences of AGNs in the sample of no-solution (N_sol = 0) in step 2. &ref(Nsol0_allIA_AGN.txt); -- summay: &ref(Table_Nsol0_AGN.jpg,,40%); ** as of 2015/07/02 [#pfc3c006] - 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 [#dea57504] - 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 [#obb1a271] - 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): &ref(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): &ref(allIAexObj_nonRealLAE.txt); ** as of 2015/06/24 [#h75114d1] - 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): &ref(step3rcsgt3.jpg,,40%); -- step 2 (others): &ref(step2others.jpg,,40%); - evaluating the contribution of the power-law (PL) component on the SED fitting (ref. [[Caputi 2013, ApJ, 768, 103:http://ads.nao.ac.jp/abs/2013ApJ...768..103C]]) 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:http://ads.nao.ac.jp/abs/2003AJ....126...81A]], [[06:http://ads.nao.ac.jp/abs/2006ApJ...640..167A]]; [[Polletta+06:http://ads.nao.ac.jp/abs/2006ApJ...642..673P]]; [[Honig+10:http://ads.nao.ac.jp/abs/2010A%26A...515A..23H]]) --- 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: &ref(ID608131stell+PL.jpg,,20%); -- U-V vs. V-J: &ref(UVvsVJ_AGN_MAESTLOv2.jpg,,15%); -- SFR vs Mstar: &ref(SFRvsMs_AGN_SFGv2.jpg,,15%); ** as of 2015/06/20 [#g85c6606] - 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 [[FrontPage]]
タイムスタンプを変更しない
[[FrontPage]] - [[Action Items Related to AGN-MAESTLO>AGN-MAESTLO#ActionItem]] - [[Manuscript>AGN-MAESTLO#Manuscript]] - [[Figures>AGN-MAESTLO#Figures]] - [[Fixed Action Items>AGN-MAESTLO#FixedAIs]] * &aname(ActionItem){Action Items Related to AGN-MAESTLO}; [#e0af5dd9] - 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: &ref(p3_meeting150624v2.jpg,,30%); - 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: &ref(p5_meeting150624v2.jpg,,30%); - 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): &ref(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): &ref(lya_x_1arcsec_circ.txt); &ref(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 * &aname(Manuscript){Manuscript}; [#pa779959] ** &aname(Figures){Figures}; [#v459d6e0] - Fig. 1: &ref(AGN-MAESTLO2.jpg,,15%); &ref(AGN-MAESTLO2.eps); - Tab. 1: &ref(AGN_MAESTLO_Table1.jpg,,30%); * &aname(FixedAIs){Fixed Action Items}; [#o13db940] ** as of 2015/10/01 [#t8f417f9] - revising a list of objects showing evidences of AGNs in the sample of no-solution (N_sol = 0) in step 2 based on Step2.dat (20150927). &ref(Nsol0_allIA_AGN_150927.txt); -- summay: &ref(Table_Nsol0_AGN_150927.jpg,,40%); ** as of 2015/09/10 [#i6c3c9a0] - revising a list of objects showing evidences of AGNs in the sample of no-solution (N_sol = 0) in step 2 based on Step.dat (20150907). &ref(Nsol0_allIA_AGN_150907.txt); -- summay: &ref(Table_Nsol0_AGN_150907.jpg,,70%); ** as of 2015/07/31 [#r957a59c] - revising a list of objects showing evidences of AGNs in the sample of no-solution (N_sol = 0) in step 2. &ref(Nsol0_allIA_AGN.txt); -- summay: &ref(Table_Nsol0_AGN.jpg,,40%); ** as of 2015/07/02 [#pfc3c006] - 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 [#dea57504] - 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 [#obb1a271] - 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): &ref(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): &ref(allIAexObj_nonRealLAE.txt); ** as of 2015/06/24 [#h75114d1] - 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): &ref(step3rcsgt3.jpg,,40%); -- step 2 (others): &ref(step2others.jpg,,40%); - evaluating the contribution of the power-law (PL) component on the SED fitting (ref. [[Caputi 2013, ApJ, 768, 103:http://ads.nao.ac.jp/abs/2013ApJ...768..103C]]) 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:http://ads.nao.ac.jp/abs/2003AJ....126...81A]], [[06:http://ads.nao.ac.jp/abs/2006ApJ...640..167A]]; [[Polletta+06:http://ads.nao.ac.jp/abs/2006ApJ...642..673P]]; [[Honig+10:http://ads.nao.ac.jp/abs/2010A%26A...515A..23H]]) --- 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: &ref(ID608131stell+PL.jpg,,20%); -- U-V vs. V-J: &ref(UVvsVJ_AGN_MAESTLOv2.jpg,,15%); -- SFR vs Mstar: &ref(SFRvsMs_AGN_SFGv2.jpg,,15%); ** as of 2015/06/20 [#g85c6606] - 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 [[FrontPage]]
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