The apparent magnitude (m) of a celestial object is a number that is a measure of its brightness as seen by an observer on Earth. The brighter an object appears, the lower its magnitude value (i.e. inverse relation). The Sun, at apparent magnitude of −27, is the brightest object in the sky. It is adjusted to the value it would have in the absence of the atmosphere. Furthermore, the magnitude scale is logarithmic; a difference of one in magnitude corresponds to a change in brightness by a factor of 5√, or about 2.512.
Generally, the visible spectrum (mv) is used as a basis for the apparent magnitude. However, other spectra are also used (e.g. the near-infrared J band). In the visible spectrum, Sirius is the brightest star after the Sun. In the near-infrared J-band, Betelgeuse is the brightest. The apparent magnitude of stars is measured with a bolometer.
|Number of stars
in the night sky
The scale used to indicate magnitude originates in the Hellenistic practice of dividing stars visible to the naked eye into six magnitudes. The brightest stars in the night sky were said to be of first magnitude (m = 1), whereas the faintest were of sixth magnitude (m = 6), which is the limit of human visual perception (without the aid of a telescope). Each grade of magnitude was considered twice the brightness of the following grade (a logarithmic scale), although that ratio was subjective as no photodetectors existed. This rather crude scale for the brightness of stars was popularized by Ptolemy in his Almagest, and is generally believed to have originated with Hipparchus.
In 1856, Norman Robert Pogson formalized the system by defining a first magnitude star as a star that is 100 times as bright as a sixth-magnitude star, thereby establishing the logarithmic scale still in use today. This implies that a star of magnitude m is 2.512 times as bright as a star of magnitude m + 1. This figure, the fifth root of 100, became known as Pogson's Ratio. The zero point of Pogson's scale was originally defined by assigning Polaris a magnitude of exactly 2. Astronomers later discovered that Polaris is slightly variable, so they switched to Vega as the standard reference star, assigning the brightness of Vega as the definition of zero magnitude at any specified wavelength.
Apart from small corrections, the brightness of Vega still serves as the definition of zero magnitude for visible and near infrared wavelengths, where its spectral energy distribution (SED) closely approximates that of a black body for a temperature of 000 K. However, with the advent of 11infrared astronomy it was revealed that Vega's radiation includes an Infrared excess presumably due to a circumstellar disk consisting of dust at warm temperatures (but much cooler than the star's surface). At shorter (e.g. visible) wavelengths, there is negligible emission from dust at these temperatures. However, in order to properly extend the magnitude scale further into the infrared, this peculiarity of Vega should not affect the definition of the magnitude scale. Therefore, the magnitude scale was extrapolated to all wavelengths on the basis of the black body radiation curve for an ideal stellar surface at 000 K uncontaminated by circumstellar radiation. On this basis the 11spectral irradiance (usually expressed in janskys) for the zero magnitude point, as a function of wavelength can be computed. Small deviations are specified between systems using measurement apparatuses developed independently so that data obtained by different astronomers can be properly compared; of greater practical importance is the definition of magnitude not at a single wavelength but applying to the response of standard spectral filters used in photometry over various wavelength bands.
With the modern magnitude systems, brightness over a very wide range is specified according to the logarithmic definition detailed below, using this zero reference. In practice such apparent magnitudes do not exceed 30 (for detectable measurements). The brightness of Vega is exceeded by four stars in the night sky at visible wavelengths (and more at infrared wavelengths) as well as bright planets such as Venus, Mars, and Jupiter, and these must be described by negative magnitudes. For example, Sirius, the brightest star of the celestial sphere, has an apparent magnitude of −1.4 in the visible; negative magnitudes for other very bright astronomical objects can be found in the table below.
As the amount of light actually received by a telescope is reduced by transmission through the Earth's atmosphere, any measurement of apparent magnitude is corrected for what it would have been as seen from above the atmosphere. The dimmer an object appears, the higher the numerical value given to its apparent magnitude, with a difference of 5 magnitudes corresponding to a brightness factor of exactly 100. Therefore, the apparent magnitude m, in the spectral band x, would be given by:
which is more commonly expressed in terms of common (base 10) logarithms as:
where Fx is the observed flux using spectral filter x, and Fx,0 is the reference flux (zero-point) for that photometric filter. Since an increase of 5 magnitudes corresponds to a decrease in brightness by a factor of exactly 100, each magnitude increase implies a decrease in brightness by the factor 5√ ≈ 2.512 (Pogson's Ratio). Inverting the above formula, a magnitude difference m1 − m2 = Δm implies a brightness factor of
Example: Sun and Moon
The apparent magnitude of the Sun is −26.74 (brighter), and the mean apparent magnitude of the full moon is −12.74 (dimmer).
Difference in magnitude:
The Sun appears about 000 times brighter than the full moon. 400
Sometimes one might wish to add brightnesses. For example, photometry on closely separated double stars may only be able to produce a measurement of their combined light output. How would we reckon the combined magnitude of that double star knowing only the magnitudes of the individual components? This can be done by adding the brightnesses (in linear units) corresponding to each magnitude.
Solving for yields
where mf is the resulting magnitude after adding the brightnesses referred to by m1 and m2.
Since flux decreases with distance according to the inverse-square law, a particular apparent magnitude could equally well refer to a star at one distance, or a star four times brighter at twice that distance, and so on. When one is not interested in the brightness as viewed from Earth, but the intrinsic brightness of an astronomical object, then one refers not to the apparent magnitude but the absolute magnitude. The absolute magnitude M, of a star or astronomical object is defined as the apparent magnitude it would have as seen from a distance of 10 parsecs (about 32.6 light years). The absolute magnitude of the Sun is 4.83 in the V band (yellow) and 5.48 in the B band (blue). In the case of a planet or asteroid, the absolute magnitude H rather means the apparent magnitude it would have if it were 1 astronomical unit from both the observer and the Sun.
Standard reference values
|Band||λ (μm)||Δλ/ (FWHM)||Flux at m = 0, Fx,0 (Jy)||Flux at m = 0, Fx,0 (10−20 erg/s/cm2/Hz)|
It is important to note that the scale is logarithmic: the relative brightness of two objects is determined by the difference of their magnitudes. For example, a difference of 3.2 means that one object is about 19 times as bright as the other, because Pogson's Ratio raised to the power 3.2 is approximately 19.05.
A common misconception is that the logarithmic nature of the scale is because the human eye itself has a logarithmic response. In Pogson's time this was thought to be true (see Weber–Fechner law), but it is now believed that the response is a power law (see Stevens' power law).
Magnitude is complicated by the fact that light is not monochromatic. The sensitivity of a light detector varies according to the wavelength of the light, and the way it varies depends on the type of light detector. For this reason, it is necessary to specify how the magnitude is measured for the value to be meaningful. For this purpose the UBV system is widely used, in which the magnitude is measured in three different wavelength bands: U (centred at about 350 nm, in the near ultraviolet), B (about 435 nm, in the blue region) and V (about 555 nm, in the middle of the human visual range in daylight). The V band was chosen for spectral purposes and gives magnitudes closely corresponding to those seen by the light-adapted human eye, and when an apparent magnitude is given without any further qualification, it is usually the V magnitude that is meant, more or less the same as visual magnitude.
Because cooler stars, such as red giants and red dwarfs, emit little energy in the blue and UV regions of the spectrum their power is often under-represented by the UBV scale. Indeed, some L and T class stars have an estimated magnitude of well over 100, because they emit extremely little visible light, but are strongest in infrared.
Measures of magnitude need cautious treatment and it is extremely important to measure like with like. On early 20th century and older orthochromatic (blue-sensitive) photographic film, the relative brightnesses of the blue supergiant Rigel and the red supergiant Betelgeuse irregular variable star (at maximum) are reversed compared to what human eyes perceive, because this archaic film is more sensitive to blue light than it is to red light. Magnitudes obtained from this method are known as photographic magnitudes, and are now considered obsolete.
For objects within the Milky Way with a given absolute magnitude, 5 is added to the apparent magnitude for every tenfold increase in the distance to the object. This relationship does not apply for objects at very great distances (far beyond the Milky Way), because a correction for general relativity must then be taken into account due to the non-Euclidean nature of space.
For planets and other Solar System bodies the apparent magnitude is derived from its phase curve and the distances to the Sun and observer.
Table of notable celestial objects
|App. mag. (V)||Celestial object|
|−40.98||Rho Cassiopeiae as seen from 1 astronomical unit (AU).|
|−38.00||Rigel as seen from 1 AU. It would be seen as a large very bright bluish scorching ball of 35° apparent diameter.|
|−30.30||Sirius as seen from 1 astronomical unit|
|−29.30||Sun as seen from Mercury at perihelion|
|−27.40||Sun as seen from Venus at perihelion|
|−26.74||Sun as seen from Earth (about 400,000 times brighter than mean full moon)|
|−25.60||Sun as seen from Mars at aphelion|
|−25.00||Minimum brightness that causes the typical eye slight pain to look at|
|−23.00||Sun as seen from Jupiter at aphelion|
|−21.70||Sun as seen from Saturn at aphelion|
|−20.20||Sun as seen from Uranus at aphelion|
|−19.30||Sun as seen from Neptune|
|−18.20||Sun as seen from Pluto at aphelion|
|−16.70||Sun as seen from Eris at aphelion|
|−14.2||An illumination level of one lux |
|−12.90||Maximum brightness of perigee+perihelion full moon (mean distance value is −12.74, though both values are about 0.18 magnitude brighter when including the opposition effect)|
|−11.20||Sun as seen from Sedna at aphelion|
|−10||Comet Ikeya–Seki (1965), which was the brightest Kreutz Sungrazer of modern times|
|−9.50||Maximum brightness of an Iridium (satellite) flare|
|−7.50||The supernova of 1006, the brightest stellar event in recorded history (7200 light years away)|
|−6.50||The total integrated magnitude of the night sky as seen from Earth|
|−6.00||The Crab Supernova of 1054 (6500 light years away)|
|−5.9||International Space Station (when the ISS is at its perigee and fully lit by the Sun)|
|−4.89||Maximum brightness of Venus when illuminated as a crescent|
|−4.00||Faintest objects observable during the day with naked eye when Sun is high|
|−3.99||Maximum brightness of Epsilon Canis Majoris 4.7 million years ago, the historical brightest star of the last and next five million years|
|−3.82||Minimum brightness of Venus when it is on the far side of the Sun|
|−2.94||Maximum brightness of Jupiter|
|−2.91||Maximum brightness of Mars|
|−2.50||Faintest objects visible during the day with naked eye when Sun is less than 10° above the horizon|
|−2.50||Minimum brightness of new moon|
|−2.45||Maximum brightness of Mercury at superior conjunction (unlike Venus, Mercury is at its brightest when on the far side of the Sun, the reason being their different phase curves)|
|−1.61||Minimum brightness of Jupiter|
|−1.47||Brightest star (except for the Sun) at visible wavelengths: Sirius|
|−0.83||Eta Carinae apparent brightness as a supernova impostor in April 1843|
|−0.72||Second-brightest star: Canopus|
|−0.49||Maximum brightness of Saturn at opposition and perihelion when the rings are full open (2003)|
|−0.27||The total magnitude for the Alpha Centauri AB star system. (Third-brightest star to the naked eye)|
|−0.04||Fourth-brightest star to the naked eye Arcturus|
|−0.01||Fourth-brightest individual star visible telescopically in the sky Alpha Centauri A|
|+0.03||Vega, which was originally chosen as a definition of the zero point|
|+0.50||Sun as seen from Alpha Centauri|
|1.47||Minimum brightness of Saturn|
|1.84||Minimum brightness of Mars|
|3.03||The SN 1987A supernova in the Large Magellanic Cloud 160,000 light-years away.|
|3 to 4||Faintest stars visible in an urban neighborhood with naked eye|
|3.44||The well known Andromeda Galaxy (M31)|
|4.38||Maximum brightness of Ganymede (moon of Jupiter and the largest moon in the Solar System)|
|4.50||M41, an open cluster that may have been seen by Aristotle|
|5.20||Maximum brightness of asteroid Vesta|
|5.32||Maximum brightness of Uranus|
|5.72||The spiral galaxy M33, which is used as a test for naked eye seeing under dark skies|
|5.73||Minimum brightness of Mercury|
|5.8||Peak visual magnitude of gamma-ray burst GRB 080319B (the "Clarke Event") seen on Earth on March 19, 2008 from a distance of 7.5 billion light-years.|
|5.95||Minimum brightness of Uranus|
|6.49||Maximum brightness of asteroid Pallas|
|6.50||Approximate limit of stars observed by a mean naked eye observer under very good conditions. There are about 9,500 stars visible to mag 6.5.|
|6.64||Maximum brightness of dwarf planet Ceres in the asteroid belt|
|6.75||Maximum brightness of asteroid Iris|
|6.90||The spiral galaxy M81 is an extreme naked-eye target that pushes human eyesight and the Bortle scale to the limit|
|7.0–8.0||Extreme naked-eye limit, Class 1 on Bortle scale, the darkest skies available on Earth|
|7.78||Maximum brightness of Neptune|
|8.02||Minimum brightness of Neptune|
|8.10||Maximum brightness of Titan (largest moon of Saturn), mean opposition magnitude 8.4|
|8.94||Maximum brightness of asteroid 10 Hygiea|
|9.50||Faintest objects visible using common 7×50 binoculars under typical conditions|
|10.20||Maximum brightness of Iapetus (brightest when west of Saturn and takes 40 days to switch sides)|
|12.91||Brightest quasar 3C 273 (luminosity distance of 2.4 billion light years)|
|13.42||Maximum brightness of Triton|
|13.65||Maximum brightness of Pluto (725 times fainter than magnitude 6.5 naked eye skies)|
|15.40||Maximum brightness of centaur Chiron|
|15.55||Maximum brightness of Charon (the large moon of Pluto)|
|16.80||Current opposition brightness of Makemake|
|17.27||Current opposition brightness of Haumea|
|18.70||Current opposition brightness of Eris|
|20.70||Callirrhoe (small ~8 km satellite of Jupiter)|
|22.00||Approximate limiting magnitude of a 24-inch (600 mm) Ritchey-Chrétien telescope with 30 minutes of stacked images (6 subframes at 300 seconds each) using a CCD detector|
|22.91||Maximum brightness of Pluto's moon Hydra|
|23.38||Maximum brightness of Pluto's moon Nix|
|24.80||Amateur picture with greatest magnitude: quasar CFHQS J1641 +3755 and limit of a 30-second exposure with Large Synoptic Survey Telescope (LSST).|
|25.00||Fenrir (small ~4 km satellite of Saturn)|
|27.70||Faintest objects observable in a 10-hour image with an 8-meter class ground-based telescope such as the Subaru Telescope|
|28.00||Jupiter if it were located 5000 AU from the Sun|
|28.20||Halley's Comet in 2003 when it was 28 AU from the Sun|
|31.50||Faintest objects observable in visible light with Hubble Space Telescope|
|35.00||LBV 1806-20, a luminous blue variable star, expected magnitude at visible wavelengths due to interstellar extinction|
|36.00||Faintest objects observable in visible light with E-ELT|
See also: List of brightest stars
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