Conversion of standardized ReadMe file for
file /./ftp/cats/J/ApJ/781/12 into FORTRAN code for loading all data files into arrays.
Note that special values are assigned to unknown or unspecified
numbers (also called NULL numbers);
when necessary, the coordinate components making up the right ascension
and declination are converted into floating-point numbers
representing these angles in degrees.
program load_ReadMe
C=============================================================================
C F77-compliant program generated by readme2f_1.81 (2015-09-23), on 2024-Apr-18
C=============================================================================
* This code was generated from the ReadMe file documenting a catalogue
* according to the "Standard for Documentation of Astronomical Catalogues"
* currently in use by the Astronomical Data Centers (CDS, ADC, A&A)
* (see full documentation at URL http://vizier.u-strasbg.fr/doc/catstd.htx)
* Please report problems or questions to
C=============================================================================
implicit none
* Unspecified or NULL values, generally corresponding to blank columns,
* are assigned one of the following special values:
* rNULL__ for unknown or NULL floating-point values
* iNULL__ for unknown or NULL integer values
real*4 rNULL__
integer*4 iNULL__
parameter (rNULL__=--2147483648.) ! NULL real number
parameter (iNULL__=(-2147483647-1)) ! NULL int number
integer idig ! testing NULL number
C=============================================================================
Cat. J/ApJ/781/12 Morphological parameters of galaxies from Spitzer (Holwerda+, 2014)
*================================================================================
*Morphological parameters of a Spitzer survey of stellar structure in galaxies.
* Holwerda B.W., Munoz-Mateos J.-C., Comeron S., Meidt S., Sheth K.,
* Laine S., Hinz J.L., Regan M.W., Gil de Paz A., Menendez-Delmestre K.,
* Seibert M., Kim T., Mizusawa T., Laurikainen E., Salo H., Laine J.,
* Gadotti D.A., Zaritsky D., Erroz-Ferrer S., Ho L.C., Knapen J.H.,
* Athanassoula E., Bosma A., Pirzkal N.
* <Astrophys. J., 781, 12 (2014)>
* =2014ApJ...781...12H (SIMBAD/NED BibCode)
C=============================================================================
C Internal variables
integer*4 i__
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'tablea1.dat' ! The morphological parameters at 3.6{mu}m for
the 2349 S^4^G galaxies
integer*4 nr__
parameter (nr__=2345) ! Number of records
character*81 ar__ ! Full-size record
character*10 Name (nr__) ! Galaxy identifier (1)
real*4 Gini (nr__) ! [0/1] The Gini index (indicator of equality:
* 1=all the flux is in one pixel, 0=all the
* pixels in the object have equal values) (2)
real*4 e_Gini (nr__) ! [0/10]? The uncertainty in Gini
real*4 M20 (nr__) ! [-4.7/-0.06] Relative contribution of brightest
* pixels to 2nd order moment of flux (M_20_) (3)
real*4 e_M20 (nr__) ! [0/10] The uncertainty in M20
real*4 C82 (nr__) ! [0/9.2] The concentration index (C_82_) (4)
real*4 e_C82 (nr__) ! [0/1.9] The uncertainty in C82
real*4 A (nr__) ! [0.07/1] The asymmetry parameter (5)
real*4 e_A (nr__) ! [0/5]? The uncertainty in A
real*4 S (nr__) ! [0.04/1.7] The smoothness parameter (6)
real*4 e_S (nr__) ! [0/7]? The uncertainty in S
real*4 Ell (nr__) ! [0/1] The ellipticity parameter (7)
real*4 e_Ell (nr__) ! [0/0.25]? The uncertainty in Ell
real*4 GM (nr__) ! [0.2/1] The Gini index of 2nd order moment
* (G_M_) (8)
real*4 e_GM (nr__) ! [0/10]? The uncertainty in GM
*Note (1): There are only 2345 objects in the tables because the code crashed
* when calculating the parameters for 4 objects. We use the
* concentration-asymmetry-smoothness (CAS) system from Bershady et al.
* (2000AJ....119.2645B), Conselice et al. (2000ApJ...529..886C), and
* Conselice 2003 (cat. J/ApJS/147/1), the Gini and M_20_ system from Lotz et
* al. 2004 (cat. J/AJ/128/163), and a hybrid parameter G_M_, the Gini
* parameter of the second-order moment (Holwerda et al.,
* 2011MNRAS.416.2426H).
*Note (2): The Gini parameter is an economic indicator of equality (G=1 if all
* the flux is in one pixel and G=0 if all the pixels in the object have equal
* values). We use the implementation from Abraham et al. 2003 (cat.
* J/ApJ/588/218) and Lotz et al. 2004 (cat. J/AJ/128/163):
* G = [1/<I>n(n-1)]{sum}_i_(2i-n-1)|I_i_| (Eq.(4) in the paper), where
* I_i_ is the intensity of pixel i in an increasing flux-ordered list of the
* n pixels in the object and <I> is the mean pixel intensity. B. W. Holwerda
* et al. (in preparation) find a weak link between Gini and current star
* formation.
*Note (3): The relative second-order moment of the brightest 20% of the flux:
* M_20_ = log({sum}^k^_i_M_i_/M_tot_), for which {sum}^k^_i_I_i_<0.2I_tot_ is
* true (Eq.(6) in the paper), where pixel K marks the top 20% point in the
* flux-ordered pixel list. The M_20_ parameter is a parameter that is
* sensitive to bright structure away from the center of the galaxy; the flux
* is weighted in favor of the outer parts. It therefore is relatively
* sensitive to tidal structures (provided of course that these are included
* in the calculation), specifically star-forming regions formed in the outer
* spiral or tidal arms. If no such structures are in the image, the 20%
* brightest pixels will most likely be concentrated in the center of the
* galaxy, which is weighted lower. Thus, one can expect low values of M_20_
* for smooth galaxies with bright nuclei (ellipticals, S0, or Sa) but much
* higher values (less negative) for galaxies with extended arms featuring
* bright HII regions.
*Note (4): The log of the ratio of the radii including 80 over 20% of the flux.
* Concentration is defined as Kent (1985ApJS...59..115K):
* C_82_ = 5log(r_80_/r_20_) (Eq.(1) in the paper), where r_%_ is the radius
* of the circular aperture that includes that percentage of the total light
* of the object.
*Note (5): In an image with n pixels with intensities I(i,j) at pixel positions
* (i,j), in which the value of the pixel is I_180_(i,j) in the image rotated
* by 180{deg}, asymmetry is defined as (Schade et al., 1995ApJ...451L...1S;
* Conselice 2003, cat. J/ApJS/147/1):
* A = {sum}_i,j_|I(i,j)-I_180_(i,j)|/2{sum}_i,j_|I(i,j)| (Eq.(2) in the
* paper).
*Note (6): Smoothness (also called clumpiness in the original Conselice 2003,
* cat. J/ApJS/147/1) is defined as:
* S = {sum}_i,j_|I(i,j)-I_S_(i,j)|/{sum}_i,j_|I(i,j)| (Eq.(3) in the paper),
* where I_S_(i,j) is the same pixel in the image after smoothing with a
* choice of kernel.
*Note (7): Scarlata et al. (2007ApJS..172..406S) added the ellipticity of a
* galaxy's image to the mix of parameters in order to classify galaxies
* according to type in the COSMOS field. Ellipticity is defined as:
* E = 1-b/a (Eq.(8) in the paper), where a and b are the major and minor axes
* of the galaxy, respectively, computed from the spatial second-order moments
* of the light along the x- and y-axes of the image in the same manner as
* SExtractor. We include this definition for completeness.
*Note (8): Instead of the intensity of the pixel (I_i_), one can use the
* second-order moment of the pixel (M_i_=I_i_[(x_i_-x_c_)^2^+(y_i_-y_c_)^2^])
* in Eq.(4). This is the G_M_ parameter (Holwerda et al.,
* 2011MNRAS.416.2426H): G_M_ = [1/<M>n(n-1)]{sum}_i_(2i-n-1)|M_i_| (Eq.(7) in
* the paper), which is an indication of the spread of pixel values weighted
* with the projected radial distance to the galaxy center. In essence, this
* is the Gini parameter with a different weighting scheme than unity for each
* pixel. Similar to the M_20_ parameter, it emphasizes the flux from the
* outer regions of the galaxy. If there is significant flux in the outer
* parts, this will boost the value of G_M_. Contrary to M_20_, it does not
* depend on a somewhat arbitrary delineation of the brightest 20% flux for
* the denominator but relies on all pixel values. Unlike the Gini parameter,
* however, it does rely on a supplied center of the galaxy (to compute M_i_).
* For concentrated galaxies, the G_M_ and Gini values will be close together,
* but as relatively more flux is evident in the outer parts of the galaxy,
* G_M_ will be higher. Holwerda et al. 2011 (cat. J/MNRAS/416/2415) found
* G_M_ to be a good single parameter to identify active mergers (sweeping
* tidal tails, etc.) from atomic hydrogen maps (HI).
c - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -
C Declarations for 'tablea2.dat' ! The morphological parameters at 4.5{mu}m for
the 2349 S^4^G galaxies
integer*4 nr__1
parameter (nr__1=2345) ! Number of records
character*81 ar__1 ! Full-size record
character*10 Name_1 (nr__1) ! Galaxy identifier (1)
real*4 Gini_1 (nr__1) ! [0/1] The Gini index (indicator of equality:
* 1=all the flux is in one pixel, 0=all the
* pixels in the object have equal values) (2)
real*4 e_Gini_1 (nr__1) ! [0/10]? The uncertainty in Gini
real*4 M20_1 (nr__1) ! [-4.7/-0.06] Relative contribution of brightest
* pixels to 2nd order moment of flux (M_20_) (3)
real*4 e_M20_1 (nr__1) ! [0/10] The uncertainty in M20
real*4 C82_1 (nr__1) ! [0/9.2] The concentration index (C_82_) (4)
real*4 e_C82_1 (nr__1) ! [0/1.9] The uncertainty in C82
real*4 A_1 (nr__1) ! [0.07/1] The asymmetry parameter (5)
real*4 e_A_1 (nr__1) ! [0/5]? The uncertainty in A
real*4 S_1 (nr__1) ! [0.04/1.7] The smoothness parameter (6)
real*4 e_S_1 (nr__1) ! [0/7]? The uncertainty in S
real*4 Ell_1 (nr__1) ! [0/1] The ellipticity parameter (7)
real*4 e_Ell_1 (nr__1) ! [0/0.25]? The uncertainty in Ell
real*4 GM_1 (nr__1) ! [0.2/1] The Gini index of 2nd order moment
* (G_M_) (8)
real*4 e_GM_1 (nr__1) ! [0/10]? The uncertainty in GM
*Note (1): There are only 2345 objects in the tables because the code crashed
* when calculating the parameters for 4 objects. We use the
* concentration-asymmetry-smoothness (CAS) system from Bershady et al.
* (2000AJ....119.2645B), Conselice et al. (2000ApJ...529..886C), and
* Conselice 2003 (cat. J/ApJS/147/1), the Gini and M_20_ system from Lotz et
* al. 2004 (cat. J/AJ/128/163), and a hybrid parameter G_M_, the Gini
* parameter of the second-order moment (Holwerda et al.,
* 2011MNRAS.416.2426H).
*Note (2): The Gini parameter is an economic indicator of equality (G=1 if all
* the flux is in one pixel and G=0 if all the pixels in the object have equal
* values). We use the implementation from Abraham et al. 2003 (cat.
* J/ApJ/588/218) and Lotz et al. 2004 (cat. J/AJ/128/163):
* G = [1/<I>n(n-1)]{sum}_i_(2i-n-1)|I_i_| (Eq.(4) in the paper), where
* I_i_ is the intensity of pixel i in an increasing flux-ordered list of the
* n pixels in the object and <I> is the mean pixel intensity. B. W. Holwerda
* et al. (in preparation) find a weak link between Gini and current star
* formation.
*Note (3): The relative second-order moment of the brightest 20% of the flux:
* M_20_ = log({sum}^k^_i_M_i_/M_tot_), for which {sum}^k^_i_I_i_<0.2I_tot_ is
* true (Eq.(6) in the paper), where pixel K marks the top 20% point in the
* flux-ordered pixel list. The M_20_ parameter is a parameter that is
* sensitive to bright structure away from the center of the galaxy; the flux
* is weighted in favor of the outer parts. It therefore is relatively
* sensitive to tidal structures (provided of course that these are included
* in the calculation), specifically star-forming regions formed in the outer
* spiral or tidal arms. If no such structures are in the image, the 20%
* brightest pixels will most likely be concentrated in the center of the
* galaxy, which is weighted lower. Thus, one can expect low values of M_20_
* for smooth galaxies with bright nuclei (ellipticals, S0, or Sa) but much
* higher values (less negative) for galaxies with extended arms featuring
* bright HII regions.
*Note (4): The log of the ratio of the radii including 80 over 20% of the flux.
* Concentration is defined as Kent (1985ApJS...59..115K):
* C_82_ = 5log(r_80_/r_20_) (Eq.(1) in the paper), where r_%_ is the radius
* of the circular aperture that includes that percentage of the total light
* of the object.
*Note (5): In an image with n pixels with intensities I(i,j) at pixel positions
* (i,j), in which the value of the pixel is I_180_(i,j) in the image rotated
* by 180{deg}, asymmetry is defined as (Schade et al., 1995ApJ...451L...1S;
* Conselice 2003, cat. J/ApJS/147/1):
* A = {sum}_i,j_|I(i,j)-I_180_(i,j)|/2{sum}_i,j_|I(i,j)| (Eq.(2) in the
* paper).
*Note (6): Smoothness (also called clumpiness in the original Conselice 2003,
* cat. J/ApJS/147/1) is defined as:
* S = {sum}_i,j_|I(i,j)-I_S_(i,j)|/{sum}_i,j_|I(i,j)| (Eq.(3) in the paper),
* where I_S_(i,j) is the same pixel in the image after smoothing with a
* choice of kernel.
*Note (7): Scarlata et al. (2007ApJS..172..406S) added the ellipticity of a
* galaxy's image to the mix of parameters in order to classify galaxies
* according to type in the COSMOS field. Ellipticity is defined as:
* E = 1-b/a (Eq.(8) in the paper), where a and b are the major and minor axes
* of the galaxy, respectively, computed from the spatial second-order moments
* of the light along the x- and y-axes of the image in the same manner as
* SExtractor. We include this definition for completeness.
*Note (8): Instead of the intensity of the pixel (I_i_), one can use the
* second-order moment of the pixel (M_i_=I_i_[(x_i_-x_c_)^2^+(y_i_-y_c_)^2^])
* in Eq.(4). This is the G_M_ parameter (Holwerda et al.,
* 2011MNRAS.416.2426H): G_M_ = [1/<M>n(n-1)]{sum}_i_(2i-n-1)|M_i_| (Eq.(7) in
* the paper), which is an indication of the spread of pixel values weighted
* with the projected radial distance to the galaxy center. In essence, this
* is the Gini parameter with a different weighting scheme than unity for each
* pixel. Similar to the M_20_ parameter, it emphasizes the flux from the
* outer regions of the galaxy. If there is significant flux in the outer
* parts, this will boost the value of G_M_. Contrary to M_20_, it does not
* depend on a somewhat arbitrary delineation of the brightest 20% flux for
* the denominator but relies on all pixel values. Unlike the Gini parameter,
* however, it does rely on a supplied center of the galaxy (to compute M_i_).
* For concentrated galaxies, the G_M_ and Gini values will be close together,
* but as relatively more flux is evident in the outer parts of the galaxy,
* G_M_ will be higher. Holwerda et al. 2011 (cat. J/MNRAS/416/2415) found
* G_M_ to be a good single parameter to identify active mergers (sweeping
* tidal tails, etc.) from atomic hydrogen maps (HI).
C=============================================================================
C Loading file 'tablea1.dat' ! The morphological parameters at 3.6{mu}m for
* the 2349 S^4^G galaxies
C Format for file interpretation
1 format(
+ A10,1X,F4.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,
+ 1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2)
C Effective file loading
open(unit=1,status='old',file=
+'tablea1.dat')
write(6,*) '....Loading file: tablea1.dat'
do i__=1,2345
read(1,'(A81)')ar__
read(ar__,1)
+ Name(i__),Gini(i__),e_Gini(i__),M20(i__),e_M20(i__),C82(i__),
+ e_C82(i__),A(i__),e_A(i__),S(i__),e_S(i__),Ell(i__),
+ e_Ell(i__),GM(i__),e_GM(i__)
if(ar__(17:20) .EQ. '') e_Gini(i__) = rNULL__
if(ar__(48:51) .EQ. '') e_A(i__) = rNULL__
if(ar__(58:61) .EQ. '') e_S(i__) = rNULL__
if(ar__(68:71) .EQ. '') e_Ell(i__) = rNULL__
if(ar__(78:81) .EQ. '') e_GM(i__) = rNULL__
c ..............Just test output...........
write(6,1)
+ Name(i__),Gini(i__),e_Gini(i__),M20(i__),e_M20(i__),C82(i__),
+ e_C82(i__),A(i__),e_A(i__),S(i__),e_S(i__),Ell(i__),
+ e_Ell(i__),GM(i__),e_GM(i__)
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
C Loading file 'tablea2.dat' ! The morphological parameters at 4.5{mu}m for
* the 2349 S^4^G galaxies
C Format for file interpretation
2 format(
+ A10,1X,F4.2,1X,F4.2,1X,F5.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,
+ 1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2,1X,F4.2)
C Effective file loading
open(unit=1,status='old',file=
+'tablea2.dat')
write(6,*) '....Loading file: tablea2.dat'
do i__=1,2345
read(1,'(A81)')ar__1
read(ar__1,2)
+ Name_1(i__),Gini_1(i__),e_Gini_1(i__),M20_1(i__),e_M20_1(i__),
+ C82_1(i__),e_C82_1(i__),A_1(i__),e_A_1(i__),S_1(i__),
+ e_S_1(i__),Ell_1(i__),e_Ell_1(i__),GM_1(i__),e_GM_1(i__)
if(ar__1(17:20) .EQ. '') e_Gini_1(i__) = rNULL__
if(ar__1(48:51) .EQ. '') e_A_1(i__) = rNULL__
if(ar__1(58:61) .EQ. '') e_S_1(i__) = rNULL__
if(ar__1(68:71) .EQ. '') e_Ell_1(i__) = rNULL__
if(ar__1(78:81) .EQ. '') e_GM_1(i__) = rNULL__
c ..............Just test output...........
write(6,2)
+ Name_1(i__),Gini_1(i__),e_Gini_1(i__),M20_1(i__),e_M20_1(i__),
+ C82_1(i__),e_C82_1(i__),A_1(i__),e_A_1(i__),S_1(i__),
+ e_S_1(i__),Ell_1(i__),e_Ell_1(i__),GM_1(i__),e_GM_1(i__)
c .......End.of.Just test output...........
end do
close(1)
C=============================================================================
stop
end