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TypefaceMaax Micro

DesignerDamien Gautier

Release 2022

Fonts In Use

Specimen

Maax is a sans-serif typeface whose design possesses few optical corrections so as to give it a certain obviousness and authenticity. Consequently, certain counterforms are relatively small, and can even become clogged when its size is reduced, or when the medium upon which the typeface is printed makes for an imprecise result.

As its name indicates, Maax Micro is a variant of the Maax typeface, specially designed for use with small and very small sizes. Inktraps, invisible to the naked eye at sizes below 8 points result in more open counterforms. These traps are designed to function by “absorbing” the ink that would otherwise build up, clogging the counterforms.

The spirit of the original typeface remains intact. Maax Micro possesses exactly the same palette of signs as Maax, including the many alternative signs that make it so original.

However, some will appreciate these surprising, sometimes extravagant forms, caused by the addition of these ink traps, modifying the principal function of this Micro version and setting the typeface in large sizes, using it as an original titling typeface.

6 Styles

Roman

Regular
Medium
Bold

Italic

Italic
Medium Italic
Bold Italic
Telescope Galileo Galilei’s development of the telescope and his observations further challenged the idea that the heavens were made from a perfect, unchanging substance. Adopting Copernicus’s heliocentric hypothesis, Galileo believed the Earth was the same as other planets. Though the reality of the famous Tower of Pisa experiment is disputed, he did carry out quantitative experiments by rolling balls on an inclined plane; his correct theory of accelerated motion was apparently derived from the results of the xperiments. Galileo also found that a body dropped vertically hits the ground at the same time as a body projected horizontally, so an Earth rotating uniformly will still have objects falling to the ground under gravity. More significantly, it asserted that uniform motion is indistinguishable from rest, and so forms the basis of the theory of relativity. Except with respect to the acceptance of Copernican astronomy, Galileo’s direct influence on science in the 17th century outside Italy was probably not very great. Although his influence on educated laymen both in Italy and abroad was considerable, among university professors, except for a few who were his own pupils, it was negligible. Between the time of Galileo and Newton, Christiaan Huygens was the foremost mathematician and physicist in Western Europe. He formulated the conservation law for elastic collisions, produced the first theorems of centripetal force, and developed the dynamical theory of oscillating systems. He also made improvements to the telescope, discovered Saturn’s moon Titan, and invented the pendulum clock. His wave theory of light, published in Traité de la lumière, was later adopted by Fresnel in the form of the Huygens-Fresnel principle. Sir Isaac Newton was the first to unify the three laws of motion (the law of inertia, his second law mentioned above, and the law of action and reaction), and to prove that these laws govern both earthly and celestial objects. Newton and most of his contemporaries hoped that classical mechanics would be able to explain all entities, including (in the form of geometric optics) light. Newton’s own explanation of Newton’s rings avoided wave principles and supposed that the light particles were altered or excited by the glass and resonated. Newton also developed the calculus which is necessary to perform the mathematical calculations involved in classical mechanics. However it was Gottfried Leibniz who, independently of Newton, developed a calculus with the notation of the derivative and integral which are used to this day. Classical mechanics retains Newton’s dot notation for time derivatives. Leonhard Euler extended Newton’s laws of motion from particles to rigid bodies with two additional laws. Working with solid materials under forces leads to deformations that can be quantified. The idea was articulated by Euler (1727), and in 1782 Giordano Riccati began to determine elasticity of some materials, followed by Thomas Young. Simeon Poisson expanded study to the third dimension with the Poisson ratio. Gabriel Lamé drew on the study for assuring stability of structures and introduced the Lamé parameters. These coefficients established linear elasticity theory and started the field of continuum mechanics. After Newton, re-formulations progressively allowed solutions to a far greater number of problems. The first was constructed in 1788 by Joseph Louis Lagrange, an Italian-French mathematician. In Lagrangian mechanics the solution uses the path of least action and follows the calculus of variations. William Rowan Hamilton re-formulated Lagrangian mechanics in 1833. The advantage of Hamiltonian mechanics was that its framework allowed a more in-depth look at the underlying principles. Most of the framework of Hamiltonian mechanics can be seen in quantum mechanics however the exact meanings of the terms differ due to quantum effects. Although classical mechanics is largely compatible with other “classical physics” theories such as classical electrodynamics and thermodynamics, some difficulties were discovered in the late 19th century that could only be resolved by more modern physics. When combined with classical thermodynamics, classical mechanics leads to the Gibbs paradox in which entropy is not a well-defined quantity. As experiments reached the atomic level, classical mechanics failed to explain, even approximately, such basic things as the energy levels and sizes of atoms. The effort at resolving these problems led to the development of quantum mechanics. Similarly, the different behaviour of classical electromagnetism and classical mechanics under velocity transformations led to the theory of relativity.Telescope
Galileo Galilei’s development of the telescope and his observations further challenged the idea that the heavens were made from a perfect, unchanging substance. Adopting Copernicus’s heliocentric hypothesis, Galileo believed the Earth was the same as other planets. Though the reality of the famous Tower of Pisa experiment is disputed, he did carry out quantitative experiments by rolling balls on an inclined plane; his correct theory of accelerated motion was apparently derived from the results of the xperiments. Galileo also found that a body dropped vertically hits the ground at the same time as a body projected horizontally, so an Earth rotating uniformly will still have objects falling to the ground under gravity. More significantly, it asserted that uniform motion is indistinguishable from rest, and so forms the basis of the theory of relativity. Except with respect to the acceptance of Copernican astronomy, Galileo’s direct influence on science in the 17th century outside Italy was probably not very great. Although his influence on educated laymen both in Italy and abroad was considerable, among university professors, except for a few who were his own pupils, it was negligible. Between the time of Galileo and Newton, Christiaan Huygens was the foremost mathematician and physicist in Western Europe. He formulated the conservation law for elastic collisions, produced the first theorems of centripetal force, and developed the dynamical theory of oscillating systems. He also made improvements to the telescope, discovered Saturn’s moon Titan, and invented the pendulum clock. His wave theory of light, published in Traité de la lumière, was later adopted by Fresnel in the form of the Huygens-Fresnel principle. Sir Isaac Newton was the first to unify the three laws of motion (the law of inertia, his second law mentioned above, and the law of action and reaction), and to prove that these laws govern both earthly and celestial objects. Newton and most of his contemporaries hoped that classical mechanics would be able to explain all entities, including (in the form of geometric optics) light. Newton’s own explanation of Newton’s rings avoided wave principles and supposed that the light particles were altered or excited by the glass and resonated. Newton also developed the calculus which is necessary to perform the mathematical calculations involved in classical mechanics. However it was Gottfried Leibniz who, independently of Newton, developed a calculus with the notation of the derivative and integral which are used to this day. Classical mechanics retains Newton’s dot notation for time derivatives. Leonhard Euler extended Newton’s laws of motion from particles to rigid bodies with two additional laws. Working with solid materials under forces leads to deformations that can be quantified. The idea was articulated by Euler (1727), and in 1782 Giordano Riccati began to determine elasticity of some materials, followed by Thomas Young. Simeon Poisson expanded study to the third dimension with the Poisson ratio. Gabriel Lamé drew on the study for assuring stability of structures and introduced the Lamé parameters. These coefficients established linear elasticity theory and started the field of continuum mechanics. After Newton, re-formulations progressively allowed solutions to a far greater number of problems. The first was constructed in 1788 by Joseph Louis Lagrange, an Italian-French mathematician. In Lagrangian mechanics the solution uses the path of least action and follows the calculus of variations. William Rowan Hamilton re-formulated Lagrangian mechanics in 1833. The advantage of Hamiltonian mechanics was that its framework allowed a more in-depth look at the underlying principles. Most of the framework of Hamiltonian mechanics can be seen in quantum mechanics however the exact meanings of the terms differ due to quantum effects. Although classical mechanics is largely compatible with other “classical physics” theories such as classical electrodynamics and thermodynamics, some difficulties were discovered in the late 19th century that could only be resolved by more modern physics. When combined with classical thermodynamics, classical mechanics leads to the Gibbs paradox in which entropy is not a well-defined quantity. As experiments reached the atomic level, classical mechanics failed to explain, even approximately, such basic things as the energy levels and sizes of atoms. The effort at resolving these problems led to the development of quantum mechanics. Similarly, the different behaviour of classical electromagnetism and classical mechanics under velocity transformations led to the theory of relativity.Galileo Galilei’s
Atomic physics Galileo Galilei’s development of the telescope and his observations further challenged the idea that the heavens were made from a perfect, unchanging substance. Adopting Copernicus’s heliocentric hypothesis, Galileo believed the Earth was the same as other planets. Though the reality of the famous Tower of Pisa experiment is disputed, he did carry out quantitative experiments by rolling balls on an inclined plane; his correct theory of accelerated motion was apparently derived from the results of the xperiments. Galileo also found that a body dropped vertically hits the ground at the same time as a body projected horizontally, so an Earth rotating uniformly will still have objects falling to the ground under gravity. More significantly, it asserted that uniform motion is indistinguishable from rest, and so forms the basis of the theory of relativity. Except with respect to the acceptance of Copernican astronomy, Galileo’s direct influence on science in the 17th century outside Italy was probably not very great. Although his influence on educated laymen both in Italy and abroad was considerable, among university professors, except for a few who were his own pupils, it was negligible. Between the time of Galileo and Newton, Christiaan Huygens was the foremost mathematician and physicist in Western Europe. He formulated the conservation law for elastic collisions, produced the first theorems of centripetal force, and developed the dynamical theory of oscillating systems. He also made improvements to the telescope, discovered Saturn’s moon Titan, and invented the pendulum clock. His wave theory of light, published in Traité de la lumière, was later adopted by Fresnel in the form of the Huygens-Fresnel principle. Sir Isaac Newton was the first to unify the three laws of motion (the law of inertia, his second law mentioned above, and the law of action and reaction), and to prove that these laws govern both earthly and celestial objects. Newton and most of his contemporaries hoped that classical mechanics would be able to explain all entities, including (in the form of geometric optics) light. Newton’s own explanation of Newton’s rings avoided wave principles and supposed that the light particles were altered or excited by the glass and resonated. Newton also developed the calculus which is necessary to perform the mathematical calculations involved in classical mechanics. However it was Gottfried Leibniz who, independently of Newton, developed a calculus with the notation of the derivative and integral which are used to this day. Classical mechanics retains Newton’s dot notation for time derivatives. Leonhard Euler extended Newton’s laws of motion from particles to rigid bodies with two additional laws. Working with solid materials under forces leads to deformations that can be quantified. The idea was articulated by Euler (1727), and in 1782 Giordano Riccati began to determine elasticity of some materials, followed by Thomas Young. Simeon Poisson expanded study to the third dimension with the Poisson ratio. Gabriel Lamé drew on the study for assuring stability of structures and introduced the Lamé parameters. These coefficients established linear elasticity theory and started the field of continuum mechanics. After Newton, re-formulations progressively allowed solutions to a far greater number of problems. The first was constructed in 1788 by Joseph Louis Lagrange, an Italian-French mathematician. In Lagrangian mechanics the solution uses the path of least action and follows the calculus of variations. William Rowan Hamilton re-formulated Lagrangian mechanics in 1833. The advantage of Hamiltonian mechanics was that its framework allowed a more in-depth look at the underlying principles. Most of the framework of Hamiltonian mechanics can be seen in quantum mechanics however the exact meanings of the terms differ due to quantum effects. Although classical mechanics is largely compatible with other “classical physics” theories such as classical electrodynamics and thermodynamics, some difficulties were discovered in the late 19th century that could only be resolved by more modern physics. When combined with classical thermodynamics, classical mechanics leads to the Gibbs paradox in which entropy is not a well-defined quantity. As experiments reached the atomic level, classical mechanics failed to explain, even approximately, such basic things as the energy levels and sizes of atoms. The effort at resolving these problems led to the development of quantum mechanics. Similarly, the different behaviour of classical electromagnetism and classical mechanics under velocity transformations led to the theory of relativity.Atomic physics
Galileo Galilei’s development of the telescope and his observations further challenged the idea that the heavens were made from a perfect, unchanging substance. Adopting Copernicus’s heliocentric hypothesis, Galileo believed the Earth was the same as other planets. Though the reality of the famous Tower of Pisa experiment is disputed, he did carry out quantitative experiments by rolling balls on an inclined plane; his correct theory of accelerated motion was apparently derived from the results of the xperiments. Galileo also found that a body dropped vertically hits the ground at the same time as a body projected horizontally, so an Earth rotating uniformly will still have objects falling to the ground under gravity. More significantly, it asserted that uniform motion is indistinguishable from rest, and so forms the basis of the theory of relativity. Except with respect to the acceptance of Copernican astronomy, Galileo’s direct influence on science in the 17th century outside Italy was probably not very great. Although his influence on educated laymen both in Italy and abroad was considerable, among university professors, except for a few who were his own pupils, it was negligible. Between the time of Galileo and Newton, Christiaan Huygens was the foremost mathematician and physicist in Western Europe. He formulated the conservation law for elastic collisions, produced the first theorems of centripetal force, and developed the dynamical theory of oscillating systems. He also made improvements to the telescope, discovered Saturn’s moon Titan, and invented the pendulum clock. His wave theory of light, published in Traité de la lumière, was later adopted by Fresnel in the form of the Huygens-Fresnel principle. Sir Isaac Newton was the first to unify the three laws of motion (the law of inertia, his second law mentioned above, and the law of action and reaction), and to prove that these laws govern both earthly and celestial objects. Newton and most of his contemporaries hoped that classical mechanics would be able to explain all entities, including (in the form of geometric optics) light. Newton’s own explanation of Newton’s rings avoided wave principles and supposed that the light particles were altered or excited by the glass and resonated. Newton also developed the calculus which is necessary to perform the mathematical calculations involved in classical mechanics. However it was Gottfried Leibniz who, independently of Newton, developed a calculus with the notation of the derivative and integral which are used to this day. Classical mechanics retains Newton’s dot notation for time derivatives. Leonhard Euler extended Newton’s laws of motion from particles to rigid bodies with two additional laws. Working with solid materials under forces leads to deformations that can be quantified. The idea was articulated by Euler (1727), and in 1782 Giordano Riccati began to determine elasticity of some materials, followed by Thomas Young. Simeon Poisson expanded study to the third dimension with the Poisson ratio. Gabriel Lamé drew on the study for assuring stability of structures and introduced the Lamé parameters. These coefficients established linear elasticity theory and started the field of continuum mechanics. After Newton, re-formulations progressively allowed solutions to a far greater number of problems. The first was constructed in 1788 by Joseph Louis Lagrange, an Italian-French mathematician. In Lagrangian mechanics the solution uses the path of least action and follows the calculus of variations. William Rowan Hamilton re-formulated Lagrangian mechanics in 1833. The advantage of Hamiltonian mechanics was that its framework allowed a more in-depth look at the underlying principles. Most of the framework of Hamiltonian mechanics can be seen in quantum mechanics however the exact meanings of the terms differ due to quantum effects. Although classical mechanics is largely compatible with other “classical physics” theories such as classical electrodynamics and thermodynamics, some difficulties were discovered in the late 19th century that could only be resolved by more modern physics. When combined with classical thermodynamics, classical mechanics leads to the Gibbs paradox in which entropy is not a well-defined quantity. As experiments reached the atomic level, classical mechanics failed to explain, even approximately, such basic things as the energy levels and sizes of atoms. The effort at resolving these problems led to the development of quantum mechanics. Similarly, the different behaviour of classical electromagnetism and classical mechanics under velocity transformations led to the theory of relativity. Galileo Galilei’s development of the telescope and his observations further challenged the idea that the heavens were made from a perfect, unchanging substance. Adopting Copernicus’s heliocentric hypothesis, Galileo believed the Earth was the same as other planets. Though the reality of the famous Tower of Pisa experiment is disputed, he did carry out quantitative experiments by rolling balls on an inclined plane; his correct theory of accelerated motion was apparently derived from the results of the xperiments. Galileo also found that a body dropped vertically hits the ground at the same time as a body projected horizontally, so an Earth rotating uniformly will still have objects falling to the ground under gravity. More significantly, it asserted that uniform motion is indistinguishable from rest, and so forms the basis of the theory of relativity. Except with respect to the acceptance of Copernican astronomy, Galileo’s direct influence on science in the 17th century outside Italy was probably not very great. Although his influence on educated laymen both in Italy and abroad was considerable, among university professors, except for a few who were his own pupils, it was negligible. Between the time of Galileo and Newton, Christiaan Huygens was the foremost mathematician and physicist in Western Europe. He formulated the conservation law for elastic collisions, produced the first theorems of centripetal force, and developed the dynamical theory of oscillating systems. He also made improvements to the telescope, discovered Saturn’s moon Titan, and invented the pendulum clock. His wave theory of light, published in Traité de la lumière, was later adopted by Fresnel in the form of the Huygens-Fresnel principle. Sir Isaac Newton was the first to unify the three laws of motion (the law of inertia, his second law mentioned above, and the law of action and reaction), and to prove that these laws govern both earthly and celestial objects. Newton and most of his contemporaries hoped that classical mechanics would be able to explain all entities, including (in the form of geometric optics) light. Newton’s own explanation of Newton’s rings avoided wave principles and supposed that the light particles were altered or excited by the glass and resonated. Newton also developed the calculus which is necessary to perform the mathematical calculations involved in classical mechanics. However it was Gottfried Leibniz who, independently of Newton, developed a calculus with the notation of the derivative and integral which are used to this day. Classical mechanics retains Newton’s dot notation for time derivatives. Leonhard Euler extended Newton’s laws of motion from particles to rigid bodies with two additional laws. Working with solid materials under forces leads to deformations that can be quantified. The idea was articulated by Euler (1727), and in 1782 Giordano Riccati began to determine elasticity of some materials, followed by Thomas Young. Simeon Poisson expanded study to the third dimension with the Poisson ratio. Gabriel Lamé drew on the study for assuring stability of structures and introduced the Lamé parameters. These coefficients established linear elasticity theory and started the field of continuum mechanics. After Newton, re-formulations progressively allowed solutions to a far greater number of problems. The first was constructed in 1788 by Joseph Louis Lagrange, an Italian-French mathematician. In Lagrangian mechanics the solution uses the path of least action and follows the calculus of variations. William Rowan Hamilton re-formulated Lagrangian mechanics in 1833. The advantage of Hamiltonian mechanics was that its framework allowed a more in-depth look at the underlying principles. Most of the framework of Hamiltonian mechanics can be seen in quantum mechanics however the exact meanings of the terms differ due to quantum effects. Although classical mechanics is largely compatible with other “classical physics” theories such as classical electrodynamics and thermodynamics, some difficulties were discovered in the late 19th century that could only be resolved by more modern physics. When combined with classical thermodynamics, classical mechanics leads to the Gibbs paradox in which entropy is not a well-defined quantity. As experiments reached the atomic level, classical mechanics failed to explain, even approximately, such basic things as the energy levels and sizes of atoms. The effort at resolving these problems led to the development of quantum mechanics. Similarly, the different behaviour of classical electromagnetism and classical mechanics under velocity transformations led to the theory of relativity. Galileo Galilei’s development of the telescope and his observations further challenged the idea that the heavens were made from a perfect, unchanging substance. Adopting Copernicus’s heliocentric hypothesis, Galileo believed the Earth was the same as other planets. Though the reality of the famous Tower of Pisa experiment is disputed, he did carry out quantitative experiments by rolling balls on an inclined plane; his correct theory of accelerated motion was apparently derived from the results of the xperiments. Galileo also found that a body dropped vertically hits the ground at the same time as a body projected horizontally, so an Earth rotating uniformly will still have objects falling to the ground under gravity. More significantly, it asserted that uniform motion is indistinguishable from rest, and so forms the basis of the theory of relativity. Except with respect to the acceptance of Copernican astronomy, Galileo’s direct influence on science in the 17th century outside Italy was probably not very great. Although his influence on educated laymen both in Italy and abroad was considerable, among university professors, except for a few who were his own pupils, it was negligible. Between the time of Galileo and Newton, Christiaan Huygens was the foremost mathematician and physicist in Western Europe. He formulated the conservation law for elastic collisions, produced the first theorems of centripetal force, and developed the dynamical theory of oscillating systems. He also made improvements to the telescope, discovered Saturn’s moon Titan, and invented the pendulum clock. His wave theory of light, published in Traité de la lumière, was later adopted by Fresnel in the form of the Huygens-Fresnel principle. Sir Isaac Newton was the first to unify the three laws of motion (the law of inertia, his second law mentioned above, and the law of action and reaction), and to prove that these laws govern both earthly and celestial objects. Newton and most of his contemporaries hoped that classical mechanics would be able to explain all entities, including (in the form of geometric optics) light. Newton’s own explanation of Newton’s rings avoided wave principles and supposed that the light particles were altered or excited by the glass and resonated. Newton also developed the calculus which is necessary to perform the mathematical calculations involved in classical mechanics. However it was Gottfried Leibniz who, independently of Newton, developed a calculus with the notation of the derivative and integral which are used to this day. Classical mechanics retains Newton’s dot notation for time derivatives. Leonhard Euler extended Newton’s laws of motion from particles to rigid bodies with two additional laws. Working with solid materials under forces leads to deformations that can be quantified. The idea was articulated by Euler (1727), and in 1782 Giordano Riccati began to determine elasticity of some materials, followed by Thomas Young. Simeon Poisson expanded study to the third dimension with the Poisson ratio. Gabriel Lamé drew on the study for assuring stability of structures and introduced the Lamé parameters. These coefficients established linear elasticity theory and started the field of continuum mechanics.Galileo Galilei’s

OpenType Features

On Contextual Alternates
CALT
08x32mm 10x65mm
On Case-Sensitive Forms
CASE
H¡¿·/\-–—(){}[]«»‹›
On Discretionary Ligatures
DLIG
tf tt
On Denominators
DNOM
H0123456789
On Diagonal Fractions
FRAC
1/2 1/4 3/4
On Standard Ligatures
LIGA
fb ff ffb ffh ffi ffj ffk ffl fft fh fjfk ft fi fl
On Numerators
NUMR
H0123456789
On Oldstyle Figures
ONUM
0123456789
On Ordinals
ORDN
No no Nos nos
On Scientific Inferiors
SINF
H2O Fe3O4
On Arrows
SS01
--W --E --S --N --NW --NE --SE --SW
On Geometric
SS02
AGIJKMQVWX aefghjklmnrstuy &$.,:;...!¡?¿·‚„“”‘’ 0123456789
On Modern
SS03
AKMNQRSVWZ akvwz &$? 0123456789
On Grotesk
SS04
ACDGJMOQR aijy .,:;...!¡?¿·‚„“”‘’ 0123456789
On Subscript
SUBS
H0123456789
On Superscript
SUPS
Mme Mr
On Tabular Numbers
TNUM
0123456789
On Slashed Zero
ZERO
102 304 506 809

Character Map

Cap Height700
X Height490
Baseline0
Ascender950
Descender-250

2

Basic Latin
!
"
#
$
%
&
'
(
)
*
+
,
-
.
/
0
1
2
3
4
5
6
7
8
9
:
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<
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[
\
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^
_
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a
b
c
d
e
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g
h
i
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k
l
m
n
o
p
q
r
s
t
u
v
w
x
y
z
{
|
}
~
Latin-1 Supplement
 
¡
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¥
¦
§
¨
©
ª
«
¬
­
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¯
°
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²
³
´
µ
·
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¹
º
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¼
½
¾
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ß
à
á
â
ã
ä
å
æ
ç
è
é
ê
ë
ì
í
î
ï
ð
ñ
ò
ó
ô
õ
ö
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ø
ù
ú
û
ü
ý
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ÿ
Latin Extended-A
Ā
ā
Ă
ă
Ą
ą
Ć
ć
Ĉ
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č
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ď
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đ
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ē
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ĕ
Ė
ė
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ę
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ě
Ĝ
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ğ
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ġ
Ģ
ģ
Ĥ
ĥ
Ħ
ħ
Ĩ
ĩ
Ī
ī
Ĭ
ĭ
Į
į
İ
ı
IJ
ij
Ĵ
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ķ
ĸ
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ł
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ń
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ņ
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ś
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š
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ū
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ű
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ų
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ż
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ž
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Latin Extended-B
Ə
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Dž
dž
Ǎ
ǎ
Ǐ
ǐ
Ǒ
ǒ
Ǔ
ǔ
Ǖ
ǖ
Ǘ
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Ǚ
ǚ
Ǜ
ǜ
DZ
Dz
dz
Ǻ
ǻ
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ǽ
Ǿ
ǿ
Ș
ș
Ț
ț
ȷ
IPA Extensions
ə
Spacing Modifier Letters
ˆ
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ˉ
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˚
˛
˜
˝
Combining Diacritical Marks
̀
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̂
̃
̄
̆
̇
̈
̊
̋
̌
̒
̦
̧
̨
̵
̶
̷
̸
Greek and Coptic
Δ
Ω
μ
π
Latin Extended Additional
Ḡ
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ỹ
General Punctuation
 
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“
”
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Currency Symbols
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Letterlike Symbols
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Number Forms
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Arrows
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→
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Mathematical Operators
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≤
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◊
●
Dingbats
❤
Alphabetic Presentation Forms
fi
fl

Supported Languages

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Maax Micro in Use