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Alioth
Location of Alioth (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Ursa Major
Right ascension 12h 54m 01.74959s[1]
Declination +55° 57′ 35.3627″[1]
Apparent magnitude (V) 1.77[2]
Characteristics
Spectral type A1III-IVp kB9
U−B color index +0.02[2]
B−V color index −0.02[2]
Variable type α2 CVn
Astrometry
Radial velocity (Rv)−9.3[3] km/s
Proper motion (μ) RA: +111.91 mas/yr[1]
Dec.: −8.24 mas/yr[1]
Parallax (π)39.51±0.20 mas[1]
Distance82.6 ± 0.4 ly
(25.3 ± 0.1 pc)
Absolute magnitude (MV)−0.2[4]
Details
Mass2.91[5] M☉
Radius4.29+0.19
−0.21[6] R☉
Luminosity104.4±9.3[6] L☉
Surface gravity (log g)3.59[6] cgs
Temperature8,908±24[6] K
Metallicity [Fe/H]+0.00[4] dex
Rotation5.088631(18)[7] days
Rotational velocity (v sin i)33[8] km/s
Age300[9] Myr
Other designations
Alioth, Allioth, Aliath, ε UMa, 77 Ursae Majoris, BD+56°1627, FK5 483, GC 17518, HD 112185, HIP 62956, HR 4905, SAO 28553, PPM 33769
Database references
SIMBADdata

Alioth /ˈæliɒθ/ ⓘ, also called Epsilon Ursae Majoris, is a star in the northern constellation of Ursa Major. The designation is Latinised from ε Ursae Majoris and abbreviated Epsilon UMa or ε UMa.[10][11] Despite being designated "ε" (epsilon), it is the brightest star in the constellation and at magnitude 1.77 is the thirty-third brightest star in the sky.

It is the star in the tail of the bear closest to its body, and thus the star in the handle of the Big Dipper (or Plough) closest to the bowl. It is also a member of the large and diffuse Ursa Major moving group. Historically, the star was frequently used in celestial navigation in the maritime trade, because it is listed as one of the 57 navigational stars.[1]

Physical characteristics

[edit]
Book plate by Sidney Hall depicting Ursa Major's stars
A light curve for Epsilon Ursae Majoris, plotted from TESS data[12]

According to Hipparcos, Epsilon Ursae Majoris is 81 light-years (25 parsecs) from the Sun. Its spectral type is A1p; the "p" stands for peculiar, as its spectrum is characteristic of an α2 Canum Venaticorum variable. Epsilon Ursae Majoris, as a representative of this type, may harbor two interacting processes: first, the star's strong magnetic field separating different elements in its hydrogen 'fuel'; second, a rotation axis at an angle to the magnetic axis may be spinning different bands of magnetically sorted elements into the line of sight between Epsilon Ursae Majoris and the Earth. The intervening elements react differently at different frequencies of light as they whip in and out of view, causing Epsilon Ursae Majoris to have very strange spectral lines that fluctuate over a period of 5.1 days. The kB9 suffix to the spectral type indicates that the calcium K line is present and representative of a B9 spectral type even though the rest of the spectrum indicates A1.

Epsilon Ursae Majoris's rotational and magnetic poles are at almost 90 degrees to one another. Darker (denser) regions of chromium form a band at right angles to the equator.

It has long been suspected that Epsilon Ursae Majoris is a spectroscopic binary, possibly with more than one companion.[13] A 2008 study suggested Alioth's 5.1-day variation may be due to a substellar object of about 14.7 Jupiter masses in an eccentric orbit (e=0.5) with an average separation of 0.055 astronomical units.[14] It is now thought that the 5.1-day period is the rotation period of the star,[7] and no companions have been detected using the most modern equipment.[15] Observations of Alioth with the Navy Precision Optical Interferometer also did not detected a companion.[6]

Epsilon Ursae Majoris has a relatively weak magnetic field for a variable of this type, 15 times weaker than α Canum Venaticorum, but it is still 100 times stronger than that of the Earth.[16]

Name and etymology

[edit]

ε Ursae Majoris (Latinised to Epsilon Ursae Majoris) is the star's Bayer designation.

The traditional name Alioth comes from the Arabic alyat al-hamal ("the sheep's fat tail"). In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[17] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[18] included a table of the first two batches of names approved by the WGSN; which included Alioth for this star.

This star was known to the Hindus as Añgiras, one of the Seven Rishis.[19]

In Chinese, 北斗 (Běi Dǒu), meaning Northern Dipper, refers to an asterism equivalent to the Big Dipper. Consequently, the Chinese name for Epsilon Ursae Majoris itself is 北斗五 (Běi Dǒu wu, English: the Fifth Star of Northern Dipper) and 玉衡 (Yù Héng, English: Star of Jade Sighting-Tube).[20]

Namesakes

[edit]

The United States Navy's Crater class cargo ship USS Allioth (AK-109) was named after the star.

See also

[edit]

References

[edit]
Revisions and contributorsEdit on WikipediaRead on Wikipedia

Alioth

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from Grokipedia
Alioth, designated Epsilon Ursae Majoris (ε UMa), is the brightest star in the northern constellation and ranks as the 33rd brightest star in the night sky with an apparent visual magnitude of 1.77. It is a chemically peculiar A-type star of spectral class A1III-IVpkB9, characterized by strong and variable chemical abundances on its surface, earning it as an Ap (peculiar) star. Located approximately 82.6 light-years (25.3 parsecs) from Earth, Alioth lies along the curved handle of the famous asterism, where it marks the star closest to the bowl. The star's traditional name, Alioth, originates from the Arabic ʾalyāt al-ḥamal, meaning "the fat tail of the sheep," a reference likely tied to its position in the bear's tail within mythology. With a mass of about 2.91 times that of the Sun, a radius roughly 4.08 times solar, and a surface temperature around 9,200 K, Alioth shines with a approximately 107 times greater than the Sun's, appearing as a brilliant of light to the . It has an estimated age of around 300 million years. Its equatorial coordinates are 12h 54m 01.7s and +55° 57' 35", with a of +111.91 mas/year in and -8.24 mas/year in . Alioth exhibits subtle photometric variability due to its and magnetic activity, with a projected rotational velocity of 33 km/s and a weak but detectable dipolar estimated at up to +128 G and -64 G at its poles. As a rapidly rotating Ap star, it displays surface abundance patches of elements like calcium, , iron, magnesium, and , which have been mapped through Doppler imaging techniques. No known exoplanets orbit Alioth, and it remains a single star system, though its peculiar chemistry continues to make it a subject of study in stellar astrophysics.

Stellar characteristics

Physical properties

Alioth is a massive A-type with a of 2.91 M⊙, significantly greater than the Sun's, which places it among the more evolved members of its spectral class. Its radius measures 4.29 R⊙, making it substantially larger than the Sun and contributing to its high of 104.4 ± 9.3 L⊙. The of the star's is 9,200 ± 200 K, indicative of its hot, white appearance, while the surface gravity is log g = 3.6 (cgs), reflecting its expanded envelope consistent with post-main-sequence evolution.
PropertyValueUnit
Mass2.91M⊙
Radius4.29R⊙
Luminosity104.4 ± 9.3L⊙
Effective temperatureK
Surface gravity(cgs)
These parameters position Alioth on the Hertzsprung-Russell diagram near the transition from the to the branch, where stars of its mass begin to exhaust core and expand. With an estimated age of approximately 300 million years, derived from its membership in the moving group, Alioth represents a relatively young but evolving stellar system, having spent much of its life fusing in its core before entering this transitional phase.

Spectral classification and variability

Alioth is classified as an A0p Cr star, a chemically peculiar A-type star of luminosity class III-IV exhibiting spectral features indicative of an α² Canum Venaticorum (α² CVn) variable. This classification reflects its evolved luminosity class (III-IV) and peculiarities in line strengths, including enhanced and lines, with the "p" denoting chemical anomalies driven by atomic diffusion in its stably stratified atmosphere. The star's spectrum shows a white-blue hue, consistent with its B-V of -0.02. As the brightest member of , Alioth has an apparent visual magnitude of 1.77, making it a prominent naked-eye object, while its is approximately -0.2. It displays photometric variability typical of α² CVn stars, with small-amplitude brightness changes of about 0.02 magnitudes in the , resulting in a double-wave modulated by . These variations arise from surface abundance inhomogeneities that alter opacity across different wavelengths, with larger amplitudes in the (up to 0.12 mag) decreasing toward the . The star's chemical peculiarities include overabundances of elements such as (mean log ε(Cr) ≈ -5.7), iron (log ε(Fe) ≈ -4.65), , (log ε(Mn) ≈ -5.6), and , contrasted by depletions in (log ε(Ti) ≈ -7.6). abundances also vary across the surface, contributing to the peculiar profile. These anomalies stem from radiative processes, which segregate elements based on their and migration velocities in the absence of significant . Observations reveal periodic variations in spectral lines of these elements, tied to the star's , with enhancements concentrated at magnetic poles and depletions at the equator for heavy metals like Cr, Fe, and Sr.

Magnetic field and rotation

Alioth exhibits a relatively weak compared to other chemically peculiar Ap stars, with a polar of approximately 400 G. This is roughly 600–1600 times the average surface magnetic field of (0.25–0.65 G) but about 10 times weaker than the field in prototypical Ap stars such as α Canum Venaticorum, which has longitudinal field extrema exceeding 4000 G. The field is predominantly dipolar in geometry, as inferred from its sinusoidal variation over the rotation cycle. The longitudinal component of the magnetic field, measured via the in circularly polarized spectra, varies smoothly from +128 G to -64 G across the 5.0887-day rotation period. Earlier measurements suggested larger variations up to +1100 G and -300 G, but high-precision observations confirm the weaker values, resolving prior discrepancies. The obliquity of the magnetic axis relative to the rotation axis is estimated at 46°–90°, with detailed modeling of surface distributions favoring values around 62°–64°. This rapid , with an equatorial of v sin i ≈ 25 km s⁻¹, induces stellar oblateness and Doppler shifts in spectral lines, broadening them and contributing to the observed line profile variations. The misaligned magnetic and axes cause the field to modulate the distribution of chemical elements on the surface, forming spots enriched in metals like Cr, Fe, and Mn at the magnetic poles. As these spots rotate into and out of view, they produce periodic changes in brightness (up to 0.02 mag) and spectral features, consistent with the oblique rotator model. No stellar companions have been confirmed to influence the or variability, with changes attributed solely to the rotational modulation of surface inhomogeneities.

Kinematics and group membership

Distance and proper motion

Alioth occupies the position in the sky at equatorial coordinates RA 12h 54m 01.8s, Dec +55° 57′ 35″ (J2000.0). The most precise measurement of its distance comes from the Gaia DR3 parallax of 39.51 ± 0.16 mas, yielding a distance of 82.6 ± 0.3 light-years (25.3 ± 0.1 pc). This places Alioth within the local volume of the galaxy, allowing for detailed kinematic analysis. Alioth exhibits proper motion components of +111.91 ± 0.16 mas/yr in and -8.24 ± 0.14 mas/yr in , as measured by DR3. These values indicate the star's transverse motion across the relative to the solar system. The corresponding tangential velocity is 14.3 km/s. Combined with its of -12.3 km/s, the full three-dimensional space motion of Alioth is characterized by velocity components U = 14 km/s (toward the ), V = 2 km/s (in the direction of galactic rotation), and W = -9 km/s (toward the north galactic pole).
Velocity ComponentValue (km/s)
-12.3
Tangential velocity14.3
U (galactocentric)14
V (galactic rotation)2
W (north galactic pole)-9
These kinematic parameters confirm Alioth's membership in the moving group, where it shares similar space with other members.

Ursa Major moving group

The moving group is a nearby consisting of approximately 60 stars that share similar space and ages of 300–500 million years, making it the closest such group to the . This association is characterized by a mean space of (U, V, W) ≈ (14, 2, -9) km/s relative to the and a low velocity dispersion of about 3 km/s in the core members, indicating a coherent kinematic structure. The group's formation is thought to represent the remnants of one or more dissolved open clusters, with the stars now dispersed but retaining their common origin through shared motion and evolutionary history. Alioth (ε UMa, HD 112185) is a confirmed nucleus member of the moving group, based on its convergent and aligning closely with the group's mean kinematics. Membership was initially established through astrometric data, which provided precise parallaxes and proper motions to identify the coherent velocity pattern among candidate stars. Subsequent analysis using data has refined and confirmed this association, incorporating higher-precision measurements to validate Alioth's position within the group's spatial and velocity distribution. The group's age of 300–500 million years is consistent with Alioth's estimated evolutionary stage, placing it among intermediate-mass A-type stars on the . Members of the moving group, including Alioth, exhibit shared chemical compositions with roughly solar metallicity ([Fe/H] ≈ 0.03 ± 0.07 dex) and homogeneous abundances in elements like carbon, oxygen, and , supporting a common birthplace in a now-dissolved cluster environment. This kinematic and chemical coherence provides key insights into the dynamical evolution of nearby stellar populations.

Nomenclature and etymology

Traditional names

The primary traditional name for ε Ursae Majoris is Alioth, derived from the Arabic phrase ʿalyat al-ḥamal, meaning "fat tail of the sheep," a reference to the star's position at the base of the tail in the constellation. This etymology traces back to medieval astronomical texts and was documented in classical references such as those compiled by Richard Hinckley Allen. In Hindu astronomical tradition, the star is known as Añgiras, named after a Vedic sage who was one of the Saptarishi (seven great sages) associated with the stars of the asterism. This identification appears in historical accounts by the Persian scholar , linking the star to figures in ancient Indian cosmology. The Chinese name for Alioth is Yù Héng (玉衡), meaning " sighting tube" or " balance," denoting its role as the fifth star in the Běi Dǒu (Northern Dipper) asterism, a key element in traditional Chinese and cosmology. Historically, it was also referred to as Běi Dǒu wǔ (北斗五), the "Fifth Star of the Northern Dipper," and designated as Mu 5 within Chinese stellar catalogs. The name Alioth was officially approved by the (IAU) Working Group on Star Names on June 30, 2016, as part of efforts to standardize proper names reflecting diverse cultural heritages.

Astronomical designations

Alioth holds the ε Ursae Majoris ( Ursae Majoris), assigned by in his 1603 Uranometria atlas based on the star's position in the constellation rather than its brightness; despite being the brightest star in , it received the fifth Greek letter because Bayer cataloged the stars from west to east across the figure. The Flamsteed designation for Alioth is 77 Ursae Majoris, as numbered by in his 1725 Historia Coelestis Britannica, where stars in each constellation are ordered by increasing . In modern catalogs, Alioth is listed as HD 112185 in the Henry Draper Catalogue, which classifies stars by spectral type. It appears as HIP 62956 in the Hipparcos Catalogue, providing precise astrometric data from the 1990s satellite mission. The mission's Data Release 3 assigns it the identifier Gaia DR3 1576683529448755328, offering high-precision and measurements. Alioth lacks an official variable star designation from the International Variable Star Index (VSX), but it is classified as an α² Canum Venaticorum (α² CVn) variable due to its periodic photometric and spectroscopic variations driven by rotation and magnetic activity, with a small photometric of about 0.02 magnitudes over its 5.1-day rotation period. Within the constellation , Alioth occupies a prominent position as the brightest member and forms the first star in the handle of the asterism, following and preceding and .

Observational history

Early records

Alioth, the brightest star in the constellation Ursa Major, is a prominent circumpolar object visible year-round from latitudes in the northern hemisphere above approximately 40°N, where it can reach altitudes of up to about 70° depending on the observer's location. In ancient Greek astronomy, Alioth was catalogued as part of Ursa Major in Ptolemy's Almagest during the 2nd century CE, where it was classified as a third-magnitude star within the bear's hindquarters. Chinese astronomers documented Alioth around the 4th century BCE in Shi Shen's , identifying it as the fifth star (Yùhéng, or " Transverse") in the asterism Běi Dǒu (Northern ), a key component of the larger constellation. In Islamic astronomy, al-Sufi described Alioth in his (completed around 964 CE) as a second-magnitude star in , noting its position near the tail and its brightness relative to neighboring stars like . During the medieval period in , Alioth featured in navigational asterisms derived from Ptolemaic traditions, as outlined in Johannes de Sacrobosco's (c. 1230), which emphasized the utility of Ursa Major's stars for determining direction and at sea. Early observers across these traditions did not note any variability in Alioth's brightness, consistent with its small amplitude of less than 0.1 magnitude, which remained undetected until modern instrumental analysis.

Modern studies

The variability of Alioth (ε UMa) was first recognized in the early through observations of its peculiar spectral lines, which showed periodic changes attributed to surface chemical inhomogeneities. Photometric variations were subsequently confirmed, leading to its classification as an α² CVn variable in the , a category for chemically peculiar A stars exhibiting rotational modulation due to strong and uneven element distributions. The of Alioth was first definitively measured in the late using Zeeman splitting in high-resolution spectra, revealing a relatively weak but oblique dipolar configuration with extrema of approximately +128 G and -64 G. Earlier attempts in the by Babcock failed to detect the field due to its low strength, but subsequent studies in the 1980s and 1990s confirmed its presence through observations. In the 2000s, observations with the Navy Precision Optical Interferometer (NPOI) helped confirm the absence of close companions. More recent high-resolution spectropolarimetry has refined the topology, showing a predominantly poloidal field with local surface strengths of several hundred Gauss. Gaia Data Release 2 (2018) delivered precise for Alioth, yielding a of 39.94 ± 0.27 mas (corresponding to a distance of about 25 parsecs) and proper motions of μ_α cos δ = 110.3 ± 0.3 mas/yr and μ_δ = -9.5 ± 0.3 mas/yr, significantly improving prior measurements. DR3 (2022) further enhanced these values to a of 39.51 ± 0.20 mas, proper motions of μ_α cos δ = 111.91 ± 0.23 mas/yr and μ_δ = -8.24 ± 0.19 mas/yr, and confirmed the absence of close stellar or substellar companions through non-detection of astrometric perturbations or orbital signatures, dispelling earlier suspicions of a spectroscopic binary based on wobbles; wide common companions are cataloged but likely unbound. High-resolution in the 2010s, including least-squares techniques, confirmed Alioth's rotational period of 5.095 days and revealed an obliquity of about 70° between the magnetic and rotational axes, driving the observed spectral and photometric variations. These studies highlighted enhancements of elements like and at magnetic poles, with Doppler maps showing ring-like distributions around the . Despite historical suggestions of companions from apparent variations and a 2008 model proposing a 14.7 Jupiter-mass substellar object in an eccentric orbit, data indicate no such close bodies exist, attributing variations to rotational effects and surface spots. Unresolved questions persist regarding long-term evolution and potential distant companions. Future observations with TESS for refined variability monitoring and JWST for could probe these, but as of November 2025, no major updates beyond DR3 have emerged, with ongoing ground-based campaigns tracking cycle modulations.

Cultural significance

Mythology and navigation

In , Alioth forms part of the constellation , which depicts the Callisto, a follower of who was seduced by and subsequently transformed into a bear by the jealous ; to prevent her from descending into the , placed her among the stars as the Great Bear, with Alioth positioned in the tail closest to the body. This tale underscores themes of divine intervention and eternal vigilance, as further influenced the ocean deities and Tethys to keep the bear circling the northern sky without setting. In , Alioth is identified as Añgiras, one of the revered Saptarishi—the seven great sages—who are personified by the prominent stars of the asterism, symbolizing wisdom, cosmic order, and the transmission of Vedic knowledge across generations. These sages, including Añgiras as a mediator between humans and gods, are said to have composed sacred hymns and guided spiritual enlightenment, with the asterism serving as a celestial reminder of their enduring legacy in the night sky. Within Chinese mythology and imperial astronomy, Alioth is known as Yù Héng, the fifth star in the Běi Dǒu (Northern Dipper) asterism, representing the "jade sighting tube"—an instrument symbolizing imperial measurement and cosmic harmony—and was integral to determining seasonal calendars, solstices, and auspicious timings for rituals. The Northern Dipper's rotation around the pole was observed to track time and predict events, with its stars embodying deities that governed fate, lifespan, and destiny in Daoist cosmology, reflecting a belief in celestial influence over human affairs. Alioth's position as the first star in the 's handle makes it a key identifier for the asterism, facilitating circumpolar orientation and serving as a to locate by extending a line from the bowl's outer stars, and Merak. Historically, this configuration supported Viking navigators in charting northern routes at night by aligning with for , while Polynesian voyagers incorporated the into their star path knowledge for across the Pacific, particularly in northern latitudes where the asterism's reliability aided long-distance voyages. Across these traditions, Alioth carries symbolic associations with direction and guidance through its navigational utility, balance via its role in Chinese imperial measurements and fate determination, and seasonal cycles as part of the ever-visible bear in myths that align with annual hunts or cosmic rhythms.

Namesakes and modern references

The USS Alioth (AK-109) was a commissioned by the on November 19, 1943, during , explicitly named after the star Alioth in the constellation to honor its prominence as one of the brightest stars visible in the northern sky. The vessel served primarily in supply operations across the Pacific Theater until its decommissioning in 1946, exemplifying the Navy's of naming ships after notable celestial bodies to evoke navigational reliability. In scientific contexts, the name Alioth has been retained and formally approved by the in as the proper name for ε Ursae Majoris, facilitating its use in catalogs and observations without additional designations. While the IAU's contests have assigned names to numerous exoplanets and host stars since 2015, no exoplanetary systems have yet been named after Alioth, though the process allows for such thematic namings based on prominent stars. Modern references to Alioth often highlight its role as a key navigational aid in the Big Dipper asterism, emphasizing its brightness (magnitude 1.77) and position for stargazing simulations. In video games, the Alioth star system features prominently in Star Trek: Bridge Commander (2002), where players engage in missions involving the destruction of a star in the system, drawing on the real star's coordinates for authenticity. Similarly, the Alioth system appears in the Elite series, including Frontier: Elite II (1993), as a habitable planetary system modeled after the star's location in Ursa Major. In popular media, Alioth serves as the name of a trans-temporal entity in the , first appearing as a void guardian in the series (2021) and returning in (2024), where its cloud-like form consumes multiversal variants, though this usage diverges from astronomical lore to focus on cosmic peril. Astronomy software and planetariums frequently feature Alioth as a highlighted object for demonstrating Ursa Major's rotation and pointer function toward , as seen in tools like Stellarium, which renders its real-time position for educational simulations. No major new namings or entities after Alioth have emerged since 2023, with modern invocations continuing to underscore its utility in orientation rather than symbolic mythology.

References

  1. https://simbad.cds.unistra.fr/simbad/sim-basic?Ident=eps+uma
  2. https://www.constellationsofwords.com/alioth/
  3. https://www.aanda.org/articles/aa/full_html/2019/01/aa34279-18/aa34279-18.html
  4. https://ui.adsabs.harvard.edu/abs/1990ApJ...358L..25B
  5. https://academic.oup.com/mnras/article/443/2/1629/1069807
  6. https://ui.adsabs.harvard.edu/abs/2003AJ....125.1980K/abstract
  7. http://www.star.ucl.ac.uk/~pac/spectral_classification.html
  8. https://arxiv.org/pdf/astro-ph/9805244.pdf
  9. https://arxiv.org/abs/1009.1297
  10. https://adsabs.harvard.edu/pdf/1990ApJ...358L..25B
  11. https://ui.adsabs.harvard.edu/abs/1952ApJ...116....8B
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  13. https://ui.adsabs.harvard.edu/abs/2023A&A...674A...1G/abstract
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  15. https://iopscience.iop.org/article/10.3847/1538-3881/153/3/95
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  17. https://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf
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  19. https://encyclopedia.pub/entry/history/show/67728
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  21. https://simbad.cds.unistra.fr/simbad/sim-id?Ident=Alioth
  22. https://www.skyatnightmagazine.com/advice/alioth.html
  23. https://www.constellation-guide.com/constellation-list/ursa-major-constellation/
  24. https://www.cambridge.org/core/journals/bulletin-of-the-school-of-oriental-and-african-studies/article/case-study-on-the-evolution-of-chinese-religious-symbols-from-talismanic-paraphernalia-to-taoist-liturgy/8F22DC531CEB02821CBE23BA0E265F6D
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  29. https://www.cosmos.esa.int/web/gaia/dr3
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  33. https://thenewkorea.wordpress.com/2015/09/17/the-seven-stars-of-the-north-5/
  34. https://shrouding-the-heavens.fandom.com/wiki/Northern_Big_Dipper
  35. https://www.constellation-guide.com/big-dipper/
  36. https://ecuip.lib.uchicago.edu/diglib/science/cultural_astronomy/cultures_vikings-2.html
  37. https://home.ifa.hawaii.edu/users/rehbock/outreach/edinfo/hawn_stars_main.html
  38. https://www.space.com/ursa-major-constellation-great-bear
  39. https://www.history.navy.mil/our-collections/photography/numerical-list-of-images/nhhc-series/nh-series/NH-84000/NH-84636.html
  40. https://www.ibiblio.org/hyperwar/USN/ships/AVS/AVS-4_Allioth.html
  41. https://www.eurekalert.org/news-releases/646047
  42. https://nameexoworlds.iau.org/
  43. https://gamefaqs.gamespot.com/pc/913867-star-trek-bridge-commander/faqs/19010
  44. https://wiki.alioth.net/index.php/Chronicles_of_the_Milky_Way
  45. https://www.slashfilm.com/1629574/deadpool-and-wolverine-loki-cloud-monster-alioth-explained/
  46. https://stellarium.org/
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