TransferFromMARK のバックアップ(No.5)

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• バックアップ一覧
• ソース を表示
• TransferFromMARK は削除されています。
  • 1 (2016-08-05 (金) 17:05:39)
  • 2 (2017-03-18 (土) 15:51:51)
  • 3 (2017-03-18 (土) 21:43:04)
  • 4 (2017-03-21 (火) 12:56:41)
  • 5 (2017-03-21 (火) 15:49:08)
  • 6 (2017-03-21 (火) 17:42:45)

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FrontPage

This page contains all of the codes, scripts, and data which are used to obtain the final catalog of strong line emitters.

• Step 0: Basic Data and Catalog?
• Step 1: Selection of Strong Line Emitter Candidates?
• Step 2: Determination of z_ph and Identification of Emission Line?
• Step 3: Selection of Strong Line Emitters and Calculation of Physical Quantities?
• Step 4: Classifying AGN Candidates?

All in one script †

• SelectIAexcessObjects_All.sh
  • see this script first and then one can find the codes, scripts, and data files which are required to obtain the final catalogs of strong line emitters

Step 0: Basic Data and Catalog †

• cosmos_phot_20120626bs.tbl: the latest version of i-band selected photometric catalog including the UltraVISTA DR1 data
  • it has too huge file size (~11 GB) to be uploaded here
  • it can be downloaded from the COSMOS internal page
  • [note] the file we used in the following Step 1 are slightly modified from the original photometric catalog in the following two points by using DoPhotcat20.sh:
    • removing the header and the 1st column which shows the object name
    • sorting the IDs in ascending order
• photoz_zml_vers2.0_010312-fulls.out: the latest version of photo-z catalog
  • it has also too huge file size (~1.5 GB) to be uploaded here
  • it can be downloaded from the COSMOS internal page
  • [note] the file we used in the following Step 1 are also slightly modified from the original photo-z catalog in the following one point by using photoz_vers2.0_sort.sh:
    • sort the IDs in ascending order
• NewMasking.reg: (RA,DEC) of the masked-out regions
• Chandra_MatchedCatalog.dat: ID, (RA,DEC), and X-ray fluxes of the cross-matched IA-excess candidates
  • cross-matching condition: angular distance is smaller than or equals to 1 arcsec
• XMM_MatchedCatalog.dat: ID, (RA,DEC), and X-ray fluxes of the cross-matched IA-excess candidates
  • cross-matching condition: angular distance is smaller than or equals to the positional error for the object in the XMM-Newton source catalog
• VLA_MatchedCatalog.dat: ID, (RA,DEC), and X-ray fluxes of the cross-matched IA-excess candidates
  • cross-matching condition: angular distance is smaller than or equals to 1 arcsec
• code (F90) and script to make the above 2 cross-matched catalogs (i.e., XMM and VLA): Step0_CrossMatching.f90, Step0_CrossMatching.sh
  • input files: cosmos_xmm_200811_v2.tbl, vla-cosmos_lp_sources_v2_20080615.tbl

Step 1: Selection of Strong Line Emitter Candidates †

• code (F90) and scripts to select strong line emitter candidates: Step1.f90, Step1.sh
  • sub code to separate the candidates into groups (F90): Step1_makeGroup.f90

• catalog of the 6,164 Step 1 selected line emitter candidates: Step1.dat

• table of the 6,164 Step 1 selected line emitter candidates: table_Step1.txt
  • this table is extracted from one of the output file of Step1.sh, IdonBand.dat, by using the awk script, count_Step1_IdonBand.awk

Step 2: Determination of z_ph and Identification of Emission Line †

• code (F90) and scripts to determine z_ph and identify emission line: Step2_zph.f90, Step2.sh
• catalogs of the 6,140 Step 2 selected line emitter candidates: Step2.dat
• table of the 6,140 Step 2 selected line emitter candidates: table_Step2.txt
  • this table is extracted from Step2.dat by using the awk script, count_Step2.awk

• catalog of the 1,052 LAE candidates (included in Step2.dat): Step2_LAE_all.dat
  • + Step 3 SED-fitting results: Step3_LAE_all.dat
  • this LAE candidate catalog is extracted from Step2.dat by using the script of make_LAE_catalog_Step2.sh as follows:
    • make_LAE_catalog_Step2.awk + Step2.dat --> Step2_LAE_all.dat, Step2_LAE_single.dat, Step2_LAE_double.dat, Step2_LAE_triple.dat
    • make_zph_list.awk + Step2_LAE_all.dat --> zph_list_LAE_all.txt
    • extract_ID.awk + Step2_LAE_all.dat --> list_LAE_all.txt
    • count_LAE_Step2.awk + Step2_LAE_all.dat --> table_Step2_LAE_all.txt
    • remove_LAEcand.awk + Step2.dat --> Step2_woLAE.dat

• catalog of the 4,734 low-z emitter candidates (included in Step2.dat): Step2_lowz_all.dat
  • + Step 3 SED-fitting results: Step3_lowz_all.dat
  • this low-z emitter candidate catalog is extracted from Step2_woLAE.dat by using the script of make_lowz_catalog_Step2.sh as follows:

• make_lowz_catalog_Step2.awk + Step2_woLAE.dat --> Step2_lowz_all.dat, Step2_lowz_single.dat, Step2_lowz_double.dat, Step2_lowz_triple.dat
• make_zph_list.awk + Step2_lowz_all.dat --> zph_list_lowz_all.txt

• catalog of the 354 others (included in Step2.dat): Step2_others.dat
  • + Step 3 SED-fitting results: Step3_others.dat
  • this other emitter candidate catalog is extracted from Step2_woLAE.dat by using the awk script of make_others_catalog_Step2.awk
    • make_zph_list.awk + Step2_others.dat --> zph_list_others.txt

• code (F90) and script to write the observed SED of the line emitter candidates selected in Step 2: Step2_writeSED.f90, Step2_writeSED.sh
  • the output files are the followings: obsSED_LAE.tar.gz, obsSED_lowz.tar.gz, obsSED_others.tar.gz
    • the format of these output files are found from obsSED_ID1000100.dat, which is included in obsSED_LAE.tar.gz

Step 3: Selection of Strong Line Emitters and Calculation of Physical Quantities †

• SED fitting code (F90): Step3_SEDfit.f90
  • input files: zph_list_LAE_all.txt, zph_list_lowz_all.txt, zph_list_others.txt, and the SED templates (see below)
  • scripts: Step3_SEDfit_LAE.sh, Step3_SEDfit_lowz.sh, Step3_SEDfit_others.sh

• the SED templates:
  • the SED templates have so huge file size (~ 1.5 GB at a certain redshift) that they cannot be uploaded here
  • the SED templates are uploaded on newngli:
    • /net/newngli/data/kobayashi/SEDtemplates/{LAE,lowz,others}/SEDtemp_z*p***_{young,old}.dat: time evolution of fnu for 37 broadbands
    • /net/newngli/data/kobayashi/SEDtemplates/Mstar+Lnu_{young,old}.dat: time evolution of Mstar, SFR, L1350, L1500, and L2um
  • their format is the following: format_SEDtemp.txt

• the code making the SED templates (F90): Step3_makeSEDtemplate.f90
  • [note] because making the SED templates is highly time-consuming, the SED templates were made separately by using several computers
  • input files: inputfile_makeSEDtemplate.tar.gz (e.g.) makeSEDtemplate_LAE1.in
  • scripts: scripts_Step3_makeSEDtemplate.tar.gz (e.g.) Step3_makeSEDtemplate_LAE1.sh
  • the above input files and scripts were created by the following code, script, and input files:
    • code (F90): makescripts.f90
    • script: makescripts.sh
    • input files: makeSEDtemplate_LAE, makeSEDtemplate_nonLAE, makeSEDtemplate_others

• catalogs of the Step3 selected 770 LAEs: Step3_LAE_all_final.dat
  • this catalog is extracted from the catalog of 1,052 Step2 selected LAE candidates (Step3_LAE_all.dat) by using the script of step3_LAE.sh as follows:
    1. extract_Nundet5.awk + Step3_LAE_all.dat --> Step3_LAE_all_Nundet5.dat, tab-Step3_LAE_all_Nundet5.dat
    2. extract_chinu2lteq3.awk + Step3_LAE_all_Nundet5.dat --> Step3_LAE_all_Nundet5+chinu2lteq3.dat, tab-Step3_LAE_all_Nundet5+chinu2lteq3.dat
    3. extract_step3_final.awk + Step3_LAE_all_Nundet5+chinu2lteq3.dat --> Step3_LAE_all_final.dat, tab-Step3_LAE_all_final.dat

• code (F90) and script to write the best-fit SED of the line emitters selected in Step 3: Step3_writeSED.f90, Step3_writeSED.sh
  • the output files are the followings: bestSED_LAE.tar.gz, bestSED_lowz1.tar.gz, bestSED_lowz2.tar.gz, bestSED_lowz3.tar.gz, bestSED_lowz4.tar.gz, bestSED_others.tar.gz
    • the format of these output files are found from bestSED_ID1000100.dat, which is included in bestSED_LAE.tar.gz
  • gnuplot script to plot these SEDs: &ref(): File not found: "plot-SED.gpl" at page "TransferFromMARK";
    • this gnuplot script is automatically made by running the above script of Step3_writeSED.sh

Step 4: Classifying AGN Candidates †

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