gmtmath

Reverse Polish Notation (RPN) calculator for data tables

Synopsis

gmt math [ -At_f(t)[+e][+r][+s|w] ] [ -Ccols ] [ -Eeigen ] [ -I ] [ -Nn_col[/t_col] ] [ -Q[c|i|p|n] ] [ -S[f|l] ] [ -T[min/max/inc[+b|i|l|n]|file|list] ] [ -V[level] ] [ -bbinary ] [ -dnodata[+ccol] ] [ -eregexp ] [ -fflags ] [ -ggaps ] [ -hheaders ] [ -iflags ] [ -oflags ] [ -qflags ] [ -sflags ] [ -wflags ] [ --PAR=value ] operand [ operand ] OPERATOR [ operand ] OPERATOR= [ outfile ]

Note: No space is allowed between the option flag and the associated arguments.

Description

math will perform operations like add, subtract, multiply, and numerous other operands on one or more table data files or constants using Reverse Polish Notation (RPN) syntax. Arbitrarily complicated expressions may therefore be evaluated; the final result is written to an output file [or standard output]. Data operations are element-by-element, not matrix manipulations (except where noted). Some operators only require one operand (see below). If no data tables are used in the expression then options -T, -N can be set (and optionally -bo to indicate the data type for binary tables). If STDIN is given, the standard input will be read and placed on the stack as if a file with that content had been given on the command line. By default, all columns except the “time” column are operated on, but this can be changed (see -C). Complicated or frequently occurring expressions may be coded as a macro for future use or stored and recalled via named memory locations.

_images/RPN_fig.jpg

Hewlett-Packard made lots of calculators (left) using Reverse Polish Notation, which is a post-fix system for mathematical notion originally developed by Jan_Łukasiewicz (right). Here, operands are entered first followed by an operator, e.g., “3 5 +” instead of “3 + 5 =”.

Required Arguments

operand

If operand can be opened as a file it will be read as an ASCII (or binary, see -bi) table data file. If not a file, it is interpreted as a numerical constant or a special symbol (see below). The special argument STDIN means that standard input will be read and placed on the stack; STDIN can appear more than once if necessary.

outfile

The name of a table data file that will hold the final result. If not given then the output is sent to standard output.

Optional Arguments

-At_f(t)[+e][+r][+s|w]

Requires -N and will partially initialize a table with values from the given file t_f(t) containing t and f(t) only. The t is placed in column t_col while f(t) goes into column n_col - 1 (see -N). Append +r to only place f(t) and leave the left hand side of the matrix equation alone. If used with operators LSQFIT and SVDFIT you can optionally append the modifier +e which will instead evaluate the solution and write a data set with four columns: t, f(t), the model solution at t, and the the residuals at t, respectively [Default writes one column with model coefficients]. Append +w if t_f(t has a third column with weights, or append +s if t_f(t) has a third column with 1-sigma uncertainties. In those two cases we find the weighted solution. The weights (or sigmas) will be output as the last column when +e is in effect.

-Ccols

Select the columns that will be operated on until next occurrence of -C. List columns separated by commas; ranges like 1,3-5,7 are allowed, plus -Cx can be used for -C0 and -Cy can be used for -C1. -C (no arguments) resets the default action of using all columns except time column (see -N). -Ca selects all columns, including time column, while -Cr reverses (toggles) the current choices. When -C is in effect it also controls which columns from a file will be placed on the stack.

-Eeigen

Sets the minimum eigenvalue used by operators LSQFIT and SVDFIT [1e-7]. Smaller eigenvalues are set to zero and will not be considered in the solution.

-I

Reverses the output row sequence from ascending time to descending [ascending].

-Nn_col[/t_col]

Select the number of columns and optionally the column number that contains the “time” variable [0]. Columns are numbered starting at 0 [2/0]. If input files are specified then -N will add any missing columns.

-Q[c|i|p|n]

Quick mode for scalar calculation. Shorthand for -Ca -N1/0 -T0/0/1. In this mode, constants may have dimensional units (i.e., c, i, or p), and will be converted to internal inches before computing. If one or more constants with units are encountered then the final answer will be reported in the unit set by PROJ_LENGTH_UNIT, unless overridden by appending another unit. Alternatively, append n for a non-dimensional result, meaning no unit conversion during output. To avoid any unit conversion on input, just do not use units.

-S[f|l]

Only report the first or last row of the results [Default outputs all rows]. This is useful if you have computed a statistic (say the MODE) and only want to report a single number instead of numerous records with identical values. Append l to get the last row and f to get the first row only [Default].

-T[min/max/inc[+b|i|l|n]|file|list]

Required when no input files are given. Builds an array for the “time” column (see -N). If there is no time column (i.e., your input has only data columns), give -T with no arguments; this also implies -Ca. For details on array creation, see Generate 1-D Array.

-V[level]

Select verbosity level [w]. (See full description) (See cookbook information).

-birecord[+b|l] (more …)

Select native binary format for primary table input.

-borecord[+b|l] (more …)

Select native binary format for table output. [Default is same as input, but see -o]

-d[i|o][+ccol]nodata (more …)

Replace input columns that equal nodata with NaN and do the reverse on output.

-e[~]“pattern” | -e[~]/regexp/[i] (more …)

Only accept data records that match the given pattern.

-f[i|o]colinfo (more …)

Specify data types of input and/or output columns.

-gx|y|z|d|X|Y|Dgap[u][+a][+ccol][+n|p] (more …)

Determine data gaps and line breaks.

-h[i|o][n][+c][+d][+msegheader][+rremark][+ttitle] (more …)

Skip or produce header record(s).

-icols[+l][+ddivisor][+sscale|d|k][+ooffset][,][,t[word]] (more …)

Select input columns and transformations (0 is first column, t is trailing text, append word to read one word only).

-ocols[,…][,t[word]] (more …)

Select output columns (0 is first column; t is trailing text, append word to write one word only).

-q[i|o][~]rows|limits[+ccol][+a|t|s] (more …)

Select input or output rows or data limit(s) [all].

-s[cols][+a][+r] (more …)

Set handling of NaN records for output.

-wy|a|w|d|h|m|s|cperiod[/phase][+ccol] (more …)

Convert an input coordinate to a cyclical coordinate.

-^ or just -

Print a short message about the syntax of the command, then exit (Note: on Windows just use -).

-+ or just +

Print an extensive usage (help) message, including the explanation of any module-specific option (but not the GMT common options), then exit.

-? or no arguments

Print a complete usage (help) message, including the explanation of all options, then exit.

--PAR=value

Temporarily override a GMT default setting; repeatable. See gmt.conf for parameters.

Generate 1-D Array

We will demonstrate the use of options for creating 1-D arrays via gmtmath. Make an evenly spaced coordinate array from min to max in steps of inc, e.g.,:

gmt math -o0 -T3.1/4.2/0.1 T =
3.1
3.2
3.3
3.4
3.5
3.6
3.7

Append +b if we should take log2 of min and max, get their nearest integers, build an equidistant log2-array using inc integer increments in log2, then undo the log2 conversion. E.g., -T3/20/1+b will produce this sequence:

gmt math -o0 -T3/20/1+b T =
4
8
16

Append +l if we should take log10 of min and max and build an array where inc can be 1 (every magnitude), 2, (1, 2, 5 times magnitude) or 3 (1-9 times magnitude). E.g., -T7/135/2+l will produce this sequence:

gmt math -o0 -T7/135/2+l T =
10
20
50
100

For output values less frequently than every magnitude, use a negative integer inc:

gmt math -o0 -T1e-4/1e4/-2+l T =
0.0001
0.01
1
100
10000

Append +i if inc is a fractional number and it is cleaner to give its reciprocal value instead. To set up times for a 24-frames per second animation lasting 1 minute, run:

gmt math -o0 -T0/60/24+i T =
0
0.0416666666667
0.0833333333333
0.125
0.166666666667
...

Append +n if inc is meant to indicate the number of equidistant coordinates instead. To have exactly 5 equidistant values from 3.44 and 7.82, run:

gmt math -o0 -T3.44/7.82/5+n T =
3.44
4.535
5.63
6.725
7.82

Alternatively, let inc be a file with output coordinates in the first column, or provide a comma-separated list of specific coordinates, such as the first 6 Fibonacci numbers:

gmt math -o0 -T0,1,1,2,3,5 T =
0
1
1
2
3
5

Note: Should you need to ensure that the coordinates are unique and sorted (in case the file or list are not sorted or have duplicates) then supply the +u modifier.

If you only want a single value then you must append a comma to distinguish the list from the setting of an increment.

If the module allows you to set up an absolute time series, append a valid time unit from the list year, month, day, hour, minute, and second to the given increment; add +t to ensure time column (or use -f). Note: The internal time unit is still controlled independently by TIME_UNIT. The first 7 days of March 2020:

gmt math -o0 -T2020-03-01T/2020-03-07T/1d T =
2020-03-01T00:00:00
2020-03-02T00:00:00
2020-03-03T00:00:00
2020-03-04T00:00:00
2020-03-05T00:00:00
2020-03-06T00:00:00
2020-03-07T00:00:00

A few modules allow for +a which will paste the coordinate array to the output table.

Likewise, if the module allows you to set up a spatial distance series (with distances computed from the first two data columns), specify a new increment as inc with a geospatial distance unit from the list degree (arc), minute (arc), second (arc), meter, foot, kilometer, Miles (statute), nautical miles, or survey foot; see -j for calculation mode. To interpolate Cartesian distances instead, you must use the special unit c.

Finally, if you are only providing an increment and will obtain min and max from the data, then it is possible (max - min)/inc is not an integer, as required. If so, then inc will be adjusted to fit the range. Alternatively, append +e to keep inc exact and adjust max instead (keeping min fixed).

Operators

Choose among the following operators. Here, “args” are the number of input and output arguments.

Operator

args

Returns

Type of Function

ABS

1 1

Absolute value of A

Arithmetic

ACOS

1 1

Inverse cosine (result in radians)

Calculus

ACOSD

1 1

Inverse cosine (result in degrees)

Calculus

ACOSH

1 1

Inverse hyperbolic cosine

Calculus

ACOT

1 1

Inverse of cotangent (result in radians)

Calculus

ACOTD

1 1

Inverse of cotangent (result in degrees)

Calculus

ACSC

1 1

Inverse of cosecant (result in radians)

Calculus

ACSCD

1 1

Inverse of cosecant (result in degrees)

Calculus

ADD

2 1

A + B (addition)

Arithmetic

AND

2 1

B if A equals NaN, else A

Logic

ASEC

1 1

Inverse of secant (result in radians)

Calculus

ASECD

1 1

Inverse of secant (result in degrees)

Calculus

ASIN

1 1

Inverse of sine (result in radians)

Calculus

ASIND

1 1

Inverse of sine (result in degrees)

Calculus

ASINH

1 1

Inverse of hyperbolic sine

Calculus

ATAN

1 1

Inverse of tangent (result in radians)

Calculus

ATAN2

2 1

Inverse of tangent of A/B (result in radians)

Calculus

ATAN2D

2 1

Inverse of tangent of A/B (result in degrees)

Calculus

ATAND

1 1

Inverse of tangent (result in degrees)

Calculus

ATANH

1 1

Inverse of hyperbolic tangent

Calculus

BCDF

3 1

Binomial cumulative distribution function for p = A, n = B, and x = C

Probability

BEI

1 1

Kelvin function bei (A)

Special Functions

BER

1 1

Kelvin function ber (A)

Special Functions

BITAND

2 1

A & B (bitwise AND operator)

Logic

BITLEFT

2 1

A << B (bitwise left-shift operator)

Arithmetic

BITNOT

1 1

~A (bitwise NOT operator, i.e., return two’s complement)

Logic

BITOR

2 1

A | B (bitwise OR operator)

Logic

BITRIGHT

2 1

A >> B (bitwise right-shift operator)

Arithmetic

BITTEST

2 1

1 if bit B of A is set, else 0 (bitwise TEST operator) n

Logic

BITXOR

2 1

A ^ B (bitwise XOR operator)

Logic

BPDF

3 1

Binomial probability density function for p = A, n = B, and x = C

Probability

CEIL

1 1

ceil (A) (smallest integer >= A)

Logic

CHICDF

2 1

Chi-squared cumulative distribution function for chi2 = A and nu = B

Probability

CHICRIT

2 1

Chi-squared distribution critical value for alpha = A and nu = B

Probability

CHIPDF

2 1

Chi-squared probability density function for chi2 = A and nu = B

Probability

COL

1 1

Places column A on the stack

Special Operators

COMB

2 1

Combinations n_C_r, with n = A and r = B

Probability

CORRCOEFF

2 1

Correlation coefficient r(A, B)

Probability

COS

1 1

Cosine of A (A in radians)

Calculus

COSD

1 1

Cosine of A (A in degrees)

Calculus

COSH

1 1

Hyperbolic cosine of A

Calculus

COT

1 1

Cotangent of A (A in radians)

Calculus

COTD

1 1

Cotangent of A (A in degrees)

Calculus

CSC

1 1

Cosecant of A (A in radians)

Calculus

CSCD

1 1

Cosecant of A (A in degrees)

Calculus

D2DT2

1 1

d^2(A)/dt^2 2nd derivative

Calculus

D2R

1 1

Converts degrees to radians

Special Operators

DDT

1 1

d(A)/dt Central 1st derivative

Calculus

DEG2KM

1 1

Converts spherical degrees to kilometers

Special Operators

DENAN

2 1

Replace NaNs in A with values from B

Logic

DIFF

1 1

Forward difference between adjacent elements of A (A[1]-A[0], A[2]-A[1], …, NaN)

Arithmetic

DILOG

1 1

Dilogarithm (Spence’s) function

Special Functions

DIV

2 1

A / B (division)

Arithmetic

DUP

1 2

Places duplicate of A on the stack

Special Operators

ECDF

2 1

Exponential cumulative distribution function for x = A and lambda = B

Probability

ECRIT

2 1

Exponential distribution critical value for alpha = A and lambda = B

Probability

EPDF

2 1

Exponential probability density function for x = A and lambda = B

Probability

EQ

2 1

1 if A equals B, else 0

Logic

ERF

1 1

Error function erf (A)

Probability

ERFC

1 1

Complementary Error function erfc (A)

Probability

ERFINV

1 1

Inverse error function of A

Probability

EXCH

2 2

Exchanges A and B on the stack

Special Operators

EXP

1 1

E raised to a power.

Arithmetic

FACT

1 1

A! (A factorial)

Arithmetic

FCDF

3 1

F cumulative distribution function for F = A, nu1 = B, and nu2 = C

Probability

FCRIT

3 1

F distribution critical value for alpha = A, nu1 = B, and nu2 = C

Probability

FLIPUD

1 1

Reverse order of each column

Special Operators

FLOOR

1 1

greatest integer less than or equal to A

Logic

FMOD

2 1

A % B (remainder after truncated division)

Arithmetic

FPDF

3 1

F probability density function for F = A, nu1 = B, and nu2 = C

Probability

GE

2 1

1 if A >= (greater or equal than) B, else 0

Logic

GT

2 1

1 if A > (greater than) B, else 0

Logic

HSV2LAB

3 3

Convert h,s,v triplets to l,a,b triplets, with h = A (0-360), s = B and v = C (0-1)

Special Operators

HSV2RGB

3 3

Convert h,s,v triplets to r,g,b triplets, with h = A (0-360), s = B and v = C (0-1)

Special Operators

HSV2XYZ

3 3

Convert h,s,v triplets to x,t,z triplets, with h = A (0-360), s = B and v = C (0-1)

Special Operators

HYPOT

2 1

Hypotenuse of a right triangle of sides A and B (= sqrt (A^2 + B^2))

Calculus

I0

1 1

Modified Bessel function of A (1st kind, order 0)

Special Functions

I1

1 1

Modified Bessel function of A (1st kind, order 1)

Special Functions

IFELSE

3 1

B if A is not equal to 0, else C

Logic

IN

2 1

Modified Bessel function of A (1st kind, order B)

Special Functions

INRANGE

3 1

1 if B <= A <= C, else 0

Logic

INT

1 1

Numerically integrate A

Calculus

INV

1 1

Invert (1/A)

Arithmetic

ISFINITE

1 1

1 if A is finite, else 0

Logic

ISNAN

1 1

1 if A equals NaN, else 0

Logic

J0

1 1

Bessel function of A (1st kind, order 0)

Special Functions

J1

1 1

Bessel function of A (1st kind, order 1)

Special Functions

JN

2 1

Bessel function of A (1st kind, order B)

Special Functions

K0

1 1

Modified Kelvin function of A (2nd kind, order 0)

Special Functions

K1

1 1

Modified Bessel function of A (2nd kind, order 1)

Special Functions

KEI

1 1

Kelvin function kei (A)

Special Functions

KER

1 1

Kelvin function ker (A)

Special Functions

KM2DEG

1 1

Converts kilometers to spherical degrees

Special Operators

KN

2 1

Modified Bessel function of A (2nd kind, order B)

Special Functions

KURT

1 1

Kurtosis of A

Probability

LAB2HSV

3 3

Convert l,a,b triplets to h,s,v triplets

Special Operators

LAB2RGB

3 3

Convert l,a,b triplets to r,g,b triplets

Special Operators

LAB2XYZ

3 3

Convert l,a,b triplets to x,y,z triplets

Special Operators

LCDF

1 1

Laplace cumulative distribution function for z = A

Probability

LCRIT

1 1

Laplace distribution critical value for alpha = A

Probability

LE

2 1

1 if A <= (equal or smaller than) B, else 0

Logic

LMSSCL

1 1

LMS (Least Median of Squares) scale estimate (LMS STD) of A

Probability

LMSSCLW

2 1

Weighted LMS scale estimate (LMS STD) of A for weights in B

Probability

LOG

1 1

log (A) (natural logarithm)

Arithmetic

LOG10

1 1

log10 (A) (logarithm base 10)

Arithmetic

LOG1P

1 1

log (1+A) (natural logarithm, accurate for small A)

Arithmetic

LOG2

1 1

log2 (A) (logarithm base 2)

Arithmetic

LOWER

1 1

The lowest (minimum) value of A

Arithmetic

LPDF

1 1

Laplace probability density function for z = A

Probability

LRAND

2 1

Laplace random noise with mean A and std. deviation B

Probability

LSQFIT

1 0

Let current table be [A | b] return least squares solution x = A b

Special Operators

LT

2 1

1 if A < (smaller than) B, else 0

Logic

MAD

1 1

Median Absolute Deviation (L1 STD) of A

Probability

MADW

2 1

Weighted Median Absolute Deviation (L1 STD) of A for weights in B

Probability

MAX

2 1

Maximum of A and B

Probability

MEAN

1 1

Mean value of A

Probability

MEANW

2 1

Weighted mean value of A for weights in B

Probability

MEDIAN

1 1

Median value of A

Probability

MEDIANW

2 1

Weighted median value of A for weights in B

Probability

MIN

2 1

Minimum of A and B

Probability

MOD

2 1

A mod B (remainder after floored division)

Arithmetic

MODE

1 1

Mode value (Least Median of Squares) of A

Probability

MODEW

2 1

Weighted mode value (Least Median of Squares) of A for weights in B

Probability

MUL

2 1

A x B (multiplication)

Arithmetic

NAN

2 1

NaN if A equals B, else A

Logic

NEG

1 1

Negative (-A)

Arithmetic

NEQ

2 1

1 If A is not equal to B, else 0

Logic

NORM

1 1

Normalize (A) so min(A) = 0 and max(A) = 1

Probability

NOT

1 1

NaN ia A is equal NaN, 1 if A is equal to 0, else 0

Logic

NRAND

2 1

Normal, random values with mean A and std. deviation B

Probability

OR

2 1

NaN if B equls NaN, else A

Logic

PCDF

2 1

Poisson cumulative distribution function for x = A and lambda = B

Probability

PERM

2 1

Permutations n_P_r, with n = A and r = B

Probability

PLM

3 1

Associated Legendre polynomial P(A) degree B order C

Special Functions

PLMg

3 1

Normalized associated Legendre polynomial P(A) degree B order C (geophysical convention)

Special Functions

POP

1 0

Delete top element from the stack

Special Operators

POW

2 1

A to the power of B

Arithmetic

PPDF

2 1

Poisson distribution P(x,lambda), with x = A and lambda = B

Probability

PQUANT

2 1

The B’th quantile (0-100%) of A

Probability

PQUANTW

3 1

The C’th weighted quantile (0-100%) of A for weights in B

Probability

PSI

1 1

Psi (or Digamma) of A

Special Functions

PV

3 1

Legendre function Pv(A) of degree v = real(B) + imag(C)

Special Functions

QV

3 1

Legendre function Qv(A) of degree v = real(B) + imag(C)

Special Functions

R2

2 1

Hypotenuse squared (= A^2 + B^2)

Calculus

R2D

1 1

Convert radians to degrees

Special Operators

RAND

2 1

Uniform random values between A and B

Probability

RCDF

1 1

Rayleigh cumulative distribution function for z = A

Probability

RCRIT

1 1

Rayleigh distribution critical value for alpha = A

Probability

RGB2HSV

3 3

Convert r,g,b triplets to h,s,v triplets, with r = A, g = B, and b = C (in 0-255 range)

Special Operators

RGB2LAB

3 3

Convert r,g,b triplets to l,a,b triplets, with r = A, g = B, and b = C (in 0-255 range)

Special Operators

RGB2XYZ

3 3

Convert r,g,b triplets to x,y,x triplets, with r = A, g = B, and b = C (in 0-255 range)

Special Operators

RINT

1 1

Rint (A) (round to integral value nearest to A)

Arithmetic

RMS

1 1

Root-mean-square of A

Arithmetic

RMSW

1 1

Weighted root-mean-square of A for weights in B

Arithmetic

ROLL

2 0

Cyclically shifts the top A stack items by an amount B

Special Operators

ROOTS

2 1

Treats col A as f(t) = 0 and returns its roots

Special Operators

ROTT

2 1

Rotate A by the (constant) shift B in the t-direction

Arithmetic

RPDF

1 1

Rayleigh probability density function for z = A

Probability

SEC

1 1

Secant of A (A in radians)

Calculus

SECD

1 1

Secant of A (A in degrees)

Calculus

SIGN

1 1

Sign (+1 or -1) of A

Logic

SIN

1 1

Sine of A (A in radians)

Calculus

SINC

1 1

Normalized sinc function.

Special Functions

SIND

1 1

Sine of A (A in degrees)

Calculus

SINH

1 1

Hiperbolic sine of A

Calculus

SKEW

1 1

Skewness of A

Probability

SQR

1 1

Square (to the power of 2)

Arithmetic

SQRT

1 1

Square root

Arithmetic

STD

1 1

Standard deviation of A

Probability

STDW

2 1

Weighted standard deviation of A for weights in B

Probability

STEP

1 1

Heaviside step function H(A)

Special Functions

STEPT

1 1

Heaviside step function H(t-A)

Special Functions

SUB

2 1

A - B (subtraction)

Arithmetic

SUM

1 1

Cumulative sum of A

Arithmetic

TAN

1 1

Tangent of A (A in radians)

Calculus

TAND

1 1

Tangent of A (A in degrees)

Calculus

TANH

1 1

Hyperbolic tangent of A

Calculus

TAPER

1 1

Unit weights cosine-tapered to zero within A of end margins

Special Operators

TCDF

2 1

Student’s t cumulative distribution function for t = A, and nu = B

Probability

TCRIT

2 1

Student’s t distribution critical value for alpha = A and nu = B

Probability

TN

2 1

Chebyshev polynomial Tn(-1<A<+1) of degree B

Special Functions

TPDF

2 1

Student’s t probability density function for t = A, and nu = B

Probability

UPPER

1 1

The highest (maximum) value of A

Arithmetic

VAR

1 1

Variance of A

Probability

VARW

2 1

Weighted variance of A for weights in B

Probability

VPDF

3 1

Von Mises density distribution V(x,mu,kappa), with angles = A, mu = B, and kappa = C

Probability

WCDF

3 1

Weibull cumulative distribution function for x = A, scale = B, and shape = C

Probability

WCRIT

3 1

Weibull distribution critical value for alpha = A, scale = B, and shape = C

Probability

WPDF

3 1

Weibull density distribution P(x,scale,shape), with x = A, scale = B, and shape = C

Probability

XOR

2 1

B if A equals NaN, else A

Logic

XYZ2HSV

3 3

Convert x,y,z triplets to h,s,v triplets

Special Operators

XYZ2LAB

3 3

Convert x,y,z triplets to l,a,b triplets

Special Operators

XYZ2RGB

3 3

Convert x,y,z triplets to r,g,b triplets

Special Operators

Y0

1 1

Bessel function of A (2nd kind, order 0)

Special Functions

Y1

1 1

Bessel function of A (2nd kind, order 1)

Special Functions

YN

2 1

Bessel function of A (2nd kind, order B)

Special Functions

ZCDF

1 1

Normal cumulative distribution function for z = A

Probability

ZCRIT

1 1

Normal distribution critical value for alpha = A

Probability

ZPDF

1 1

Normal probability density function for z = A

Probability

Symbols

The following symbols have special meaning:

PI

3.1415926…

E

2.7182818…

EULER

0.5772156…

PHI

1.6180339… (golden ratio)

EPS_F

1.192092896e-07 (sgl. prec. eps)

EPS_D

2.2204460492503131e-16 (dbl. prec. eps)

TMIN

Minimum t value

TMAX

Maximum t value

TRANGE

Range of t values

TINC

t increment

N

The number of records

T

Table with t-coordinates

TNORM

Table with normalized t-coordinates

TROW

Table with row numbers 1, 2, …, N-1

ASCII Format Precision

The ASCII output formats of numerical data are controlled by parameters in your gmt.conf file. Longitude and latitude are formatted according to FORMAT_GEO_OUT, absolute time is under the control of FORMAT_DATE_OUT and FORMAT_CLOCK_OUT, whereas general floating point values are formatted according to FORMAT_FLOAT_OUT. Be aware that the format in effect can lead to loss of precision in ASCII output, which can lead to various problems downstream. If you find the output is not written with enough precision, consider switching to binary output (-bo if available) or specify more decimals using the FORMAT_FLOAT_OUT setting.

Notes On Operators

  1. The operators PLM and PLMg calculate the associated Legendre polynomial of degree L and order M in x which must satisfy \(-1 \leq x \leq +1\) and \(0 \leq M \leq L\). Here, x, L, and M are the three arguments preceding the operator. PLM is not normalized and includes the Condon-Shortley phase \((-1)^M\). PLMg is normalized in the way that is most commonly used in geophysics. The Condon-Shortley phase can be added by using -M as argument. PLM will overflow at higher degrees, whereas PLMg is stable until ultra high degrees (at least 3000).

  2. Files that have the same names as some operators, e.g., ADD, SIGN, =, etc. should be identified by prepending the current directory (i.e., ./).

  3. The stack depth limit is hard-wired to 100.

  4. All functions expecting a positive radius (e.g., LOG, KEI, etc.) are passed the absolute value of their argument.

  5. The DDT and D2DT2 functions only work on regularly spaced data.

  6. All derivatives are based on central finite differences, with natural boundary conditions.

  7. ROOTS must be the last operator on the stack, only followed by =.

STORE, RECALL and CLEAR

You may store intermediate calculations to a named variable that you may recall and place on the stack at a later time. This is useful if you need access to a computed quantity many times in your expression as it will shorten the overall expression and improve readability. To save a result you use the special operator STO@label, where label is the name you choose to give the quantity. To recall the stored result to the stack at a later time, use [RCL]@label, i.e., RCL is optional. To clear memory you may use CLR@label. Note that both STO and CLR leave the stack unchanged.

  1. The bitwise operators (BITAND, BITLEFT, BITNOT, BITOR, BITRIGHT, BITTEST, and BITXOR) convert a tables’s double precision values to unsigned 64-bit ints to perform the bitwise operations. Consequently, the largest whole integer value that can be stored in a double precision value is 2^53 or 9,007,199,254,740,992. Any higher result will be masked to fit in the lower 54 bits. Thus, bit operations are effectively limited to 54 bits. All bitwise operators return NaN if given NaN arguments or bit-settings <= 0.

  2. TAPER will interpret its argument to be a width in the same units as the time-axis, but if no time is provided (i.e., plain data tables) then the width is taken to be given in number of rows.

  3. The color-triplet conversion functions (RGB2HSV, etc.) includes not only r,g,b and h,s,v triplet conversions, but also l,a,b (CIE L a b ) and sRGB (x,y,z) conversions between all four color spaces. These functions behave differently whether -Q is used or not. With -Q we expect three input constants and we place three output results on the stack. Since only the top stack item is printed, you must use operators such as POP and ROLL to get to the item of interest. Without -Q, these operators work across the three columns and modify the three column entries, returning their result as a single three-column item on the stack.

  4. The VPDF operator expects angles in degrees.

Macros

Users may save their favorite operator combinations as macros via the file gmtmath.macros in their current or user directory. The file may contain any number of macros (one per record); comment lines starting with # are skipped. The format for the macros is name = arg1 arg2 … arg2 [ : comment] where name is how the macro will be used. When this operator appears on the command line we simply replace it with the listed argument list. No macro may call another macro. As an example, the following macro expects that the time-column contains seafloor ages in Myr and computes the predicted half-space bathymetry:

DEPTH = SQRT 350 MUL 2500 ADD NEG : usage: DEPTH to return half-space seafloor depths

Note: Because geographic or time constants may be present in a macro, it is required that the optional comment flag (:) must be followed by a space. As another example, we show a macro GPSWEEK which determines which GPS week a timestamp belongs to:

GPSWEEK = 1980-01-06T00:00:00 SUB 86400 DIV 7 DIV FLOOR : usage: GPS week without rollover

Active Column Selection

When -Ccols is set then any operation, including loading of data from files, will restrict which columns are affected. To avoid unexpected results, note that if you issue a -Ccols option before you load in the data then only those columns will be updated, hence the unspecified columns will be zero. On the other hand, if you load the file first and then issue -Ccols then the unspecified columns will have been loaded but are then ignored until you undo the effect of -C.

Absolute Time Column(s)

If input data have more than one column and the “time” column (set via -N [0]) contains absolute time, then the default output format for any other columns containing absolute time will be reset to relative time. Likewise, in scalar mode (-Q) the time column will be operated on and hence it also will be formatted as relative time. Finally, if -C is used to include “time” in the columns operated on then we likewise will reset that column’s format to relative time. The user can override this behavior with a suitable -f or -fo setting. Note: We cannot guess what your operations on the time column will do, hence this default behavior. As examples, if you are computing time differences then clearly relative time formatting is required, while if you are computing new absolute times by, say, adding an interval to absolute times then you will need to use -fo to set the output format for such columns to absolute time.

Scalar Math with Units

If you use -Q to do simple calculations, please note that the support for dimensional units is limited to converting a number ending in c, i, or p to internal inches. Thus, while you can run “gmt -Qc 1c 1c MUL =”, you may be surprised that the output area is not 1 cm squared. The reason is that gmt math cannot keep track of what unit any particular item on the stack might be so it will assume it is internally in inches and then scale the final output to cm. In this particular case, the unit is in inches squared and scaling by 2.54 once will give 0.3937 inch times cm as the unit. Thus, conversions only work for linear unit calculations, such as gmt math -Qp 1c 0.5i ADD =, which will return the result as 64.34 points.

Examples

Note: Below are some examples of valid syntax for this module. The examples that use remote files (file names starting with @) can be cut and pasted into your terminal for testing. Other commands requiring input files are just dummy examples of the types of uses that are common but cannot be run verbatim as written.

To add two plot dimensions of different units, we can run

length=$(gmt math -Q 15c 2i SUB =)

To compute the ratio of two plot dimensions of different units, we select non-dimensional output and run

ratio=$(gmt math -Qn 15c 2i DIV =)

To take the square root of the content of the second data column being piped through gmtmath by process1 and pipe it through a 3rd process, use

process1 | gmt math STDIN SQRT = | process3

To take log10 of the average of 2 data files, use

gmt math file1.txt file2.txt ADD 0.5 MUL LOG10 = file3.txt

Given the file samples.txt, which holds seafloor ages in m.y. and seafloor depth in m, use the relation depth(in m) = 2500 + 350 * sqrt (age) to print the depth anomalies:

gmt math samples.txt T SQRT 350 MUL 2500 ADD SUB = | lpr

To take the average of columns 1 and 4-6 in the three data sets sizes.1, sizes.2, and sizes.3, use

gmt math -C1,4-6 sizes.1 sizes.2 ADD sizes.3 ADD 3 DIV = ave.txt

To take the 1-column data set ages.txt and calculate the modal value and assign it to a variable, try

mode_age=$(gmt math -S -T ages.txt MODE =)

To evaluate the dilog(x) function for coordinates given in the file t.txt:

gmt math -Tt.txt T DILOG = dilog.txt

To demonstrate the use of stored variables, consider this sum of the first 3 cosine harmonics where we store and repeatedly recall the trigonometric argument (2*pi*T/360):

gmt math -T0/360/1 2 PI MUL 360 DIV T MUL STO@kT COS @kT 2 MUL COS ADD @kT 3 MUL COS ADD = harmonics.txt

To use gmtmath as a RPN Hewlett-Packard calculator on scalars (i.e., no input files) and calculate arbitrary expressions, use the -Q option. As an example, we will calculate the value of Kei (((1 + 1.75)/2.2) + cos (60)) and store the result in the shell variable z:

z=$(gmt math -Q 1 1.75 ADD 2.2 DIV 60 COSD ADD KEI =)

To convert the r,g,b value for yellow to h,s,v and save the hue, try

hue=$(gmt math -Q 255 255 0 RGB2HSV POP POP =)

To use gmtmath as a general least squares equation solver, imagine that the current table is the augmented matrix [ A | b ] and you want the least squares solution x to the matrix equation A * x = b. The operator LSQFIT does this; it is your job to populate the matrix correctly first. The -A option will facilitate this. Suppose you have a 2-column file ty.txt with t and y and you would like to fit a the model y(t) = a + b*t + c*H(t-t0), where H(t) is the Heaviside step function for a given t0 = 1.55. Then, you need a 4-column augmented table loaded with t in column 1 and your observed y in column 3. The calculation becomes

gmt math -N4/1 -Aty.txt -C0 1 ADD -C2 1.55 STEPT ADD -Ca LSQFIT = solution.txt

Note we use the -C option to select which columns we are working on, then make active all the columns we need (here all of them, with -Ca) before calling LSQFIT. The second and fourth columns (col numbers 1 and 3) are preloaded with t and y, respectively, the other columns are zero. If you already have a pre-calculated table with the augmented matrix [ A | b ] in a file (say lsqsys.txt), the least squares solution is simply

gmt math -T lsqsys.txt LSQFIT = solution.txt

Users must be aware that when -C controls which columns are to be active the control extends to placing columns from files as well. Contrast the different result obtained by these very similar commands:

echo 1 2 3 4 | gmt math STDIN -C3 1 ADD =
1    2    3    5

versus

echo 1 2 3 4 | gmt math -C3 STDIN 1 ADD =
0    0    0    5

References

Abramowitz, M., and I. A. Stegun, 1964, Handbook of Mathematical Functions, Applied Mathematics Series, vol. 55, Dover, New York.

Holmes, S. A., and W. E. Featherstone, 2002, A unified approach to the Clenshaw summation and the recursive computation of very high degree and order normalized associated Legendre functions. Journal of Geodesy, 76, 279-299.

Press, W. H., S. A. Teukolsky, W. T. Vetterling, and B. P. Flannery, 1992, Numerical Recipes, 2nd edition, Cambridge Univ., New York.

Spanier, J., and K. B. Oldman, 1987, An Atlas of Functions, Hemisphere Publishing Corp.

More on Reverse Polish Notation

Reverse Polish Notation (RPN) or postfix notation is widely used in computer science because of the simplicity of implementing a stack-based computation system. The PostScipt language we used to make GMT graphics is postfix, for instance. To learn more about RPN or postfix, watch this YouTube video explanation:

See Also

gmt, grdmath