Transfer のバックアップ(No.15)

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Action Items Related to Transfer to Kajisawa-san?
Programs & Scripts?
Catalogs?
Fixed Action Items?
Documents?

Action Items Related to Transfer to Kajisawa-san †

2015/08/04: executing the procedures in Step 2, 3, and 4 for the newly added 785 IA-excess candidates: IdonBand_add_150804.dat
- these candidates are added because of the changes of (1) limiting magnitudes of 7 IA-bands (i.e., IA464, IA484, IA505, IA527, IA574, IA624, and IA827), (2) the coefficients estimating the frequency-matched continuum, and (3) the equation which judges whether each object is inside or outside of the circular-shaped masked-out regions
  - the limiting magnitudes used originally were old one which were listed in the previous data paper but now were modified by M. Kajisawa on 17th Feb. 2015 --> the limiting magnitudes modified by M. Kajisawa on 17th Feb. 2015 are now adopted; the previous limiting magnitudes were wrong because they were the background fluctuations evaluated without mask to bright objects (email from M. Kajisawa on 16:24 4th Aug. 2015)
  - the coefficients estimating the frequency-matched continuum were originally calculated in another program and then were substituted in the program for Step 1 by reading a data file in which the coefficients rounded up to the third decimal place are written --> the coefficients are now evaluating directly from the effective wavelengths in the program for Step 1
  - the equation which judges whether an object at (RA,DEC) is inside or outside of the masked-out region with a radius of r centered on (RA0,DEC0) used originally was wrong (dr = sqrt[(RA - RA0)^2 + (DEC - DEC0)^2]) --> the correct equation is now used (dr = acos[cos(DEC)cos(DEC0)cos(RA-RA0) + sin(DEC)sin(DEC0)])

showing the 1σ errors of the best-fit model SED for EWobs, Mstar, L(Lya), SFR(Lya), SFR(SED), log10[tau/Gyr], Z, and E(B-V)

showing the programs, scripts, and catalogs with their manuals to select the IA-excess objects in Step 1, 2, 3, and 4

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Programs & Scripts †

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Step 0 Related †

the program to make the catalog cosmos_phot_20120626b.tbl?, in which the header and 1st column of the original COSMOS photometric catalog cosmos_phot_20120626.tbl? are removed (written by Y. Shioya): photcat20.f
the script to make the input COSMOS photometric catalog cosmos_phot_20120626bs.tbl?, in which the objects are listed in ascending order of the ID, from the original COSMOS photometric catalog without its header and 1st column cosmos_phot_20120626b.tbl? (written by Y. Shioya): DoPhotcat20.sh
the script to make the input COSMOS photo-z catalog photoz_zml_vers2.0_010312-fulls.out?, in which the objects are listed in ascending order of the ID, from the original COSMOS photo-z catalog photoz_zml_vers2.0_010312-full.out? (written by Y. Shioya): photoz_vers2.0_sort.sh
the program to make the cross-matched catalogs between the objects in the COSMOS photometric catalog and the objects in the XMM-Newton source catalog or VLA source catalog (written by MARK): Step0_CrossMatching.f90
- input files:
  - (1) the latest version of the COSMOS i-band selected photometric catalog including the UltraVISTA DR1 data: cosmos_phot_20120626bs.tbl?
  - (2) the latest version of the COSMOS photo-z catalog: photoz_zml_vers2.0_010312-fulls.out?
  - (3) the latest version of the XMM-Newton source catalog: cosmos_xmm_200811_v2.tbl?
  - (4) the latest version of the VLA source catalog: vla-cosmos_lp_sources_v2_20080615.tbl?
  - (5) the (RA,DEC) information for the masked-out regions defined in the 12 IA-band images by Y. Shioya: NewMasking.reg
- output files:
  - (1) XMM_MatchedCatalog.dat: the cross-matched catalog between the objects listed in the COSMOS photometric catalog and the XMM-Newton source catalog. The cross-matching condition is that the angular separation between the (RA,DEC) of the COSMOS photometric catalog and the XMM-Newton source catalog is less than or equal to the positional error of the XMM-Newton, which is different for each object.
  - (2) VLA_MatchedCatalog.dat: the cross-matched catalog between the objects listed in the COSMOS photometric catalog and the VLA source catalog. The cross-matching condition is that the angular separation between the (RA,DEC) of the COSMOS photometric catalog and the VLA source catalog is less than or equal to 1 arcsec.
- usage (see script, Step0_CrossMatching.sh):
```
./Step0_CrossMatching.out AbsolutePathOfInputFiles AbsolutePathOfOutputFiles
(e.g.,) ./Step0_CrossMatching.out /home/kobayasi/work/EhimeUniv/COSMOS20/IAexcess-Lya/data/Step0/ /home/kobayasi/work/EhimeUniv/COSMOS20/IAexcess-Lya/data/Step1/
```

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Step 1 Related †

the script to execute the sample selection of Step 1: Step1.sh
the program to make the catalog for Step 1 (written by MARK): Step1.f90
- input files:
  - (1) the latest version of i-band selected photometric catalog including the UltraVISTA DR1 data: cosmos_phot_20120626bs.tbl?
  - (2) the latest version of photo-z catalog: photoz_zml_vers2.0_010312-fulls.out?
  - (3) the (RA,DEC) information for the masked-out regions defined in the 12 IA-band images by Y. Shioya: NewMasking.reg
  - (4) IDs of the Step 1 IA-excess candidates which have been already asked for cross-matching with the Chandra to S. Toft: allIAexObj_RA_DEC.txt
  - (5) IDs of the AGN candidates detected in Chandra: Chandra_AGN_all.txt
  - (6) the cross-matched catalog between the objects listed in the COSMOS photometric catalog and the XMM-Newton source catalog: XMM_MatchedCatalog.dat
  - (7) the cross-matched catalog between the objects listed in the COSMOS photometric catalog and the VLA source catalog: VLA_MatchedCatalog.dat
- output files:
  - (1) Step1.dat: all-in-one catalog of the Step 1 selected IA-excess candidates
  - (2) IdonBand.dat: a catalog of the Step 1 selected IA-excess candidates in the previous format defined by Y. Shioya
- usage:
```
./Step1.out AbsolutePathOfInputFiles AbsolutePathOfOutputFiles
(e.g.,) ./Step1.out /home/kobayasi/work/EhimeUniv/COSMOS20/IAexcess-Lya/data/Step0/ /home/kobayasi/work/EhimeUniv/COSMOS20/IAexcess-Lya/data/Step1/
```
  - all of the input files should be located in the directory represented as AbsolutePathOfInputFiles?
  - all of the output files are written in the directory represented as AbsolutePathOfOutputFiles?
the program to classify the objects according to their combination of excess IA bands (written by Y. Shioya, modified by MARK): Step1_makeGroup.f90
- input file: IdonBands.dat, in which the IA-excess candidates are listed in ascending order of an integer that represents the sum of excess IA bands
- output files:
  - (1) group_ionband.dat: a list of the existing combination of the excess IA bands
  - (2) group/****.txt (**** = 0001--9999, which represents the combination of the excess IA bands, group_150826.tar.gz): catalogs of the IA-excess candidates with the combination of the excess IA bands
- usage:
```
./Step1_makeGroup.out AbsolutePathOfInputFiles
(e.g.,) ./Step1_makeGroup.out /home/kobayasi/work/EhimeUniv/COSMOS20/IAexcess-Lya/data/Step1/
```

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Step 2 Related †

the program to make the catalog for Step 2: &ref(): File not found: "Step2_zph.f" at page "Transfer-Step2-Catalogs";
- see Transfer-Step2-Catalogs? for detailed description of this program

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Step 3 Related †

the scripts and lists to make the input files for the SED fittings of low-z emitters (transferred on 2015/07/02): Step2_lowzSEDfit_scripts.tar.gz
- the parent script: DoMkSSforSF.sh
  - this script (1) copies IA_zph_out/IAxxx_zph.out to MkSSforSF.in as the input file to the program, (2) executes the program, and (3) moves MkSSforSF.out as the output file from the program to SEDfit_150305_lowz_IAxxx.tcsh
- the input files for the parent script: IA427_zph.out IA464_zph.out IA484_zph.out IA505_zph.out IA527_zph.out IA574_zph.out IA624_zph.out IA679_zph.out IA709_zph.out IA738_zph.out IA767_zph.out IA827_zph.out
  - in each file, all of the redshifts possible for the filter are written in the following format: [1st column] 3 digits for the IA-band name [other columns] (1)z (2)3 digits for the IA-band name (3)emission line (1:Lya, 2:CIV, 3:CIII], 4:MgII, 5:[OII], 6:[OIII]+Hb, 7:Ha+[NII], 99:others)
- the source code of the program: MkSSforSF.f
  - this program generates the script file for the SED fittings of low-z emitters named "MkSSforSF.out" from the input file named "MkSSforSF.in"
- the output script files: SEDfit_150305_lowz_IA427.tcsh SEDfit_150305_lowz_IA464.tcsh SEDfit_150305_lowz_IA484.tcsh SEDfit_150305_lowz_IA505.tcsh SEDfit_150305_lowz_IA527.tcsh SEDfit_150305_lowz_IA574.tcsh SEDfit_150305_lowz_IA624.tcsh SEDfit_150305_lowz_IA679.tcsh SEDfit_150305_lowz_IA709.tcsh SEDfit_150305_lowz_IA738.tcsh SEDfit_150305_lowz_IA767.tcsh SEDfit_150305_lowz_IA827.tcsh

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Step 4 Related †

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Catalogs †

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Step 1 Related? †

catalog of 6208 IA-excess candidates selected in Step 1: Step1.dat
- format is written as headers in the above catalog and in this page?
- (2015/08/16) Note: AGN flags for Chandra, XMM, and VLA are not complete yet.

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Step 2 Related? †

list of IA-band excess candidates: Step2.txt
- format: (1)ID (2,3)RA,DEC[deg] (4)flag for detection in all 4 IRAC bands[0:no, 1:yes] (5--9)flag for AGN from IRAC color, XMM, Chandra, VLA, and one of them[0:non-AGN,1:AGN] (10)Nex^temp (11)Nsol (12--27)quantities related to the primary z_ph solution (28--43)quantities related to the secondary z_ph solution (44--55)flag for 12 IA bands[0:undetected, 1:detected] (56)N_undetectedIA
  - for primary solution : (12)P(z_ph) (13)chi_nu^2(z_ph) (14)z_ph (15--26)line ID for 12 IA bands (1:Lya, 2:CIV, 3:CIII], 4:MgII, 5:[OII], 6:[OIII]+Hb, 7:Ha+[NII], 99:others) (27)N_ex^cons
  - for secondary solution: (28)P(z_ph2)/P(z_ph) (29)chi_nu^2(z_ph2)[-99 for the objects w/o secondary solution] (30)z_ph2[-99 for the objects w/o secondary solution] (31--42)line ID for 12 IA bands (1:Lya, 2:CIV, 3:CIII], 4:MgII, 5:[OII], 6:[OIII]+Hb, 7:Ha+[NII], 99:others) (43)N_ex^cons
  - (15,31,44)IA427 (16,32,45)IA464 (17,33,46)IA484 (18,34,47)IA505 (19,35,48)IA527 (20,36,49)IA574 (21,37,50)IA624 (22,38,51)IA679 (23,39,52)IA709 (24,40,53)IA738 (25,41,54)IA767 (26,42,55)IA827

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Step 3 Related †

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Step 4 Related †

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Fixed Action Items †

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as of xxx †

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Documents †

Determination of the Masked-out Regions from the 12 IA-band images
- Cosmos20Ses130618.pdf Cosmos20Ses130626.pdf

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