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Below, you can find merged tables containing SDSS and INT photometry and all spectroscopy available for "all" galaxies in A2192 and 963.

This table is based on the catalog of SDSS-DR8 sources in the WSRT FoV, althoufh it also contains galaxies that are not in SDSS but appear in INT images for example. It list 2 ID's in coordinate format.

Although all redshifts are listed, I also include a column with "zmio", where I give a single (best quality) redshift value. Note that in these tables I don't put a trust column for 'zmio' but from the other redshift columns you can see if there is more than one z available, if it was only observed with WHT, etc. In general, give low trust to LH redshifts. Then, for the cases where there is ONLY a WHT redshift, consider bad redshifts those with WHT_trust <= -2.

I have further folded in the INT_catalogue ID's (from Sextractor) and HI ID's for the HI detections.
I also included some other useful information such as stellar masses, morphologies, etc when available.

Final HI masses, etc still need to come, but when that information comes, you'll only need to match it to the HI ID's in this table.

Also final membership flags will come soon too, when I redo all the cluster_velocity dispersions.

Tables are in ascii format. When there is no information available you'll find a: ""

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**Master table for A2192:**  {{budhies:A2192_merged_master_tables.dat.tar.gz}}

The columns are:
  - INT_ID  (coordinate format)         
  - SDSS_ID (coordinate format)              
  - dist    (when matching SDSS with INT coordinates)
  - ID_HI    
  - HI_Opt_count_reliab: **=1** if optical counterpart has a redshift and its consistent with HI_z; **=2** if there is no optical redshift but seems plausible!
  - HI_Assotiation_flag: =1 if the optical counterpart has nearby companions, also with optical redshifts close to the HI detection; =2 if the optical counterpart has nearby companions but without optical redshift available to confirm.
  - INT_catID  (from sextractor)
  - INT_ra       
  - INT_dec     
  - u        (SDSS mags, not corrected for reddening) #
  - uerr   
  -  g       
  -  gerr    
  - r        
  - rerr    
  -  i       
  -  ierr    
  -  z     
  -  zerr    
  -  INTmB    (B-band magnitude / INT)     #
  - INTmR     (R-band magnitude / INT)
  - SDSSz:    sloan redshift
  - SDSSzerr   
  - WHTz   
  - WHTztrust_re 
  - WIYINz   
  - WIYINzerr 
  - zmio:   Unique redshift    
  - spec_type (for WHT spectra only) 
  - combined_ew_oii   (either WHT or SDSS)
  - Morph  
  - Mor_Trust   
  - Ms_Zib        (stellar mass) 
  - HI_z          (HI redshift)
  - RA_HI   
  - DEC_HI


**Master table for A963:**  {{budhies:A963_merged_master_tables.dat.tar.gz}}
The columns are:

  - INT_id     (coordinate format)           
  - SDSS_id    (coordinate format)          
  - dist    (when matching SDSS with INT coordinates)
  - HI_id  
  - HI_flag1: **=1** if optical counterpart has a redshift and its consistent with HI_z; **=2** if there is no optical redshift but seems plausible! 
  - HI_flag2: =1 if the optical counterpart has nearby companions, also with optical redshifts close to the HI detection; =2 if the optical counterpart has nearby companions but without optical redshift available to confirm. 
  - INT_cat_ID  (sextractor number)
  - INT_ra       
  - INT_dec     
  - u_sdss   (NOT DERREDENED)   #
  - uerr    
  - g_sdss   
  - gerr     
  - r_sdss   
  - rerr     
  - i_sdss   
  - ierr     
  - z_sdss   
  - zerr    
  - INT_mB   (INT mags)      #
  - INT_mR   
  - SDSS_z     (redshifts available)
  - SDSS_zerr   
  - WHT_z   
  - WHT_trust_re 
  - LH_z   (Lavery & Henry's redshifts) *
  - LH_zerr 
  - OC_z   (Czoske's redshifts) *
  - OC_zerr   
  - zmio_re    (unique redshift)
  - spec_type 
  - combined_ew_oii   
  - finalfinalMor: morphology
  - finalMorTrust
  - Ms_zib         (stellar mass)
  - z_HI   : HI z (matched the HI ID)


*Note that both Czoske's and Lavery & Henry's redshifts are slightly off the WHT or HI redshifts, but the WHT and HI redshifts are very consistent. You can see that in the following plots of Delta velocity vs. WHT redshift: [[budhies:tables:plots|see plots]]

** Also note that those literature redshifts are all in the very central core of the cluster!


# __IMPORTANT NOTE ABOUT MAGNITUDES:__

SDSS mags are Petrosian magnitudes (p.u p.Err_u etc), not corrected for anything (galactic extincion).  They were retrieved from the
SDSS-DR8 using the standard search tool.
INT magnitudes (B and R) come straight from the tables produced by running SExtractor in the INT images.  No further (de-reddening) corrections
were applied, and zero-point calibration still needs doing.


Discussion on how to go about this can be found [[budhies:int|here]]. Marc an I differ slightly in our ways to tackle the problem. 

From my point of view you can do 2 things to get proper B & R magnitudes:

  - Take the INT mags and correct the zero point and then dereden them.  The -median- corrections are: (R_sdss,vega - R_int,vega = 0.058) and (B_sdss,vega - B_int,vega = 0.101). And the extinction corrections are: For A963, A_B=0.064 and A_R=0.039; and for A2192, A_B=0.046 and A_R=0.028
  - Convert the SDSS magnitudes to B and R by using Blanton & Roeis 2007 formulas, and then dereden them with the same A_B and A_R listed above.

In summary, here are the __magic formulas__ for either case respectivelly:

> R_sdss,vega,dered = r - 0.0576 - 0.3718 * [(r-i) - 0.2589] - A_R - 0.21
> B_sdss,vega,dered = g + 0.2354 + 0.3915 * [(g-r) - 0.6102] - A_B + 0.09

> R_int,vega,dered,corrected_zp = R_int,vega + 0.058 - A_R 
> B_int,vega,dered,corrected_zp = B_int,vega + 0.101 - A_B


__FINAL NOTE:__

If you ever worked with the old tables, you'll notice that some things have changed. Now we have more lit redshifts for example, and the optical counterparts of some HI-detections are now changed.

In [[budhies:tables:plots_2|this page]], you can find some plots comparing the old and new tables.


====== Cluster Memberships ======

Below you can find tables containing all galaxies with a redshift, their membership and sub-membership in the case of A2192_1.
>Memberships are 1=main cluster, 2=second cluster, etc
>There is a column for "limited membership" that only flags galaxies with secure redshifts, CMD-cuts, etc. 
>The other membership flag is for people wanting to use all galaxies (no cuts whatsoever).
>The sub-memberships in A2192_1 are: 10=1a, 11=1b , 12=1c, 13=1d

Tables are {{budhies:membership_tables.tar.gz|here}}

NOTE: cl vel. disp. (sigma) were calculated from the limited sample only and then membership flags assigned.

NOTE_2: Note that I calculated cluster velocity dispersion for A963_1 this time without the LH redshifts so sigma came a little lower and memberships are a little changed. Other changes in the memberships are due to changes in the HI tables as you know....

FINAL NUMBERS:
  * A2192_1: sigma = 645 +/- 42 ,  N_all = 124 , N_lim_sample= 103
  * A2192_2: sigma = 477 +/- 103 , N_all = 22  , N_lim= 17
  * A2192_3: sigma = 340 +/- 71 ,  N_all = 43  , N_lim= 30
  * A2192_4: sigma = 454 +/- 64 ,  N_all = 30  , N_lim= 26
  * A2192_5: sigma = 717 +/- 91 ,  N_all = 40  , N_lim= 35
  * A2192_6: sigma = 579 +/- 92 ,  N_all = 32  , N_lim= 26

  * A963_1: sigma = 993 +/- 56 ,   N_all = 246  , N_lim= 140
  * A963_2: sigma = 507 +/- 158 ,  N_all = 41   , N_lim= 21
  * A963_3: sigma = 210 +/- 51 ,   N_all = 24   , N_lim= 15
  * A963_4: sigma = 290 +/- 53 ,   N_all = 33   , N_lim= 23


 --- //[[yara.jaffe@oapd.inaf.it|Yara Jaffe]] 2012/08/21 14:20//