Microscopium

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Microscopium
Constellation
Microscopium IAU.svg
List of stars in Microscopium
AbbreviationMic
Genitive Microscopii
Pronunciation /ˌmaɪkrəˈskɒpiəm/ , genitive /ˌmaɪkrəˈskɒpiaɪ/
Symbolismthe Microscope
Right ascension 21h
Declination −36°
QuadrantSQ4
Area 210 sq. deg. (66th)
Main stars 5
Bayer/Flamsteed
stars		13
Stars with planets 2
Stars brighter than 3.00m0
Stars within 10.00 pc (32.62 ly)2
Brightest star γ Mic  (4.67 m )
Messier objects 0
Meteor showers Microscopids
Bordering
constellations
Visible at latitudes between +45° and −90°.
Best visible at 21:00 (9 p.m.) during the month of September.

Microscopium ("the Microscope") is a minor constellation in the southern celestial hemisphere, one of twelve created in the 18th century by French astronomer Nicolas-Louis de Lacaille and one of several depicting scientific instruments. The name is a Latinised form of the Greek word for microscope. Its stars are faint and hardly visible from most of the non-tropical Northern Hemisphere.

Contents

The constellation's brightest star is Gamma Microscopii of apparent magnitude 4.68, a yellow giant 2.5 times the Sun's mass located 223 ± 8 light-years distant. It passed within 1.14 and 3.45 light-years of the Sun some 3.9 million years ago, possibly disturbing the outer Solar System. Three star systems—WASP-7, AU Microscopii and HD 205739—have been determined to have planets, while other star —the Sun-like star HD 202628— has a debris disk. AU Microscopii and the binary red dwarf system AT Microscopii are probably a wide triple system and members of the Beta Pictoris moving group. Nicknamed "Speedy Mic", BO Microscopii is a star with an extremely fast rotation period of 9 hours, 7 minutes.

Characteristics

Microscopium is a small constellation bordered by Capricornus to the north, Piscis Austrinus and Grus to the east, Sagittarius to the west, and Indus to the south, touching on Telescopium to the southwest. The recommended three-letter abbreviation for the constellation, as adopted by the International Astronomical Union in 1922, is "Mic". [1] The official constellation boundaries, as set by Belgian astronomer Eugène Delporte in 1930, are defined by a polygon of four segments (illustrated in infobox). In the equatorial coordinate system, the right ascension coordinates of these borders lie between 20h 27.3m and 21h 28.4m, while the declination coordinates are between −27.45° and −45.09°. [2] The whole constellation is visible to observers south of latitude 45°N. [3] [lower-alpha 1] Given that its brightest stars are of fifth magnitude, the constellation is invisible to the naked eye in areas with light polluted skies. [4] [lower-alpha 2]

Features

The constellation Microscopium as it can be seen by the naked eye. Constellation Microscopium.jpg
The constellation Microscopium as it can be seen by the naked eye.

Stars

French astronomer Nicolas-Louis de Lacaille charted and designated ten stars with the Bayer designations Alpha through to Iota in 1756. A star in neighbouring Indus that Lacaille had labelled Nu Indi turned out to be in Microscopium, so Gould renamed it Nu Microscopii. Francis Baily considered Gamma and Epsilon Microscopii to belong to the neighbouring constellation Piscis Austrinus, but subsequent cartographers did not follow this. [6] In his 1725 Catalogus Britannicus, John Flamsteed labelled the stars 1, 2, 3 and 4 Piscis Austrini, which became Gamma Microscopii, HR 8076, HR 8110 and Epsilon Microscopii respectively. [7] Within the constellation's borders, there are 43 stars brighter than or equal to apparent magnitude  6.5. [lower-alpha 3] [3]

Depicting the eyepiece of the microscope is Gamma Microscopii, [8] which—at magnitude of 4.68—is the brightest star in the constellation. Having spent much of its 620-million-year lifespan as a blue-white main sequence star, it has swollen and cooled to become a yellow giant of spectral type G6III, with a diameter ten times that of the Sun. [9] Measurement of its parallax yields a distance of 223 ± 8 light years from Earth. [10] It likely passed within 1.14 and 3.45 light-years of the Sun some 3.9 million years ago, at around 2.5 times the mass of the Sun, it is possibly massive enough and close enough to disturb the Oort cloud. [11] Alpha Microscopii is also an ageing yellow giant star of spectral type G7III with an apparent magnitude of 4.90. [12] Located 400 ± 30 light-years away from Earth, [13] it has swollen to 17.5 times the diameter of the Sun. [14] Alpha has a 10th magnitude companion, visible in 7.5 cm telescopes, [15] [16] though this is a coincidental closeness rather than a true binary system. [14] Epsilon Microscopii lies 166 ± 5 light-years away, [17] and is a white star of apparent magnitude 4.7, [16] and spectral type A1V. [18] Theta1 and Theta2 Microscopii make up a wide double whose components are splittable to the naked eye. Both are white A-class magnetic spectrum variable stars with strong metallic lines, similar to Cor Caroli. They mark the constellation's specimen slide. [8]

Many notable objects are too faint to be seen with the naked eye. AX Microscopii, better known as Lacaille 8760, is a red dwarf which lies only 12.9 light-years from the Solar System. At magnitude 6.68, it is the brightest red dwarf in the sky. [19] BO Microscopii is a rapidly rotating star that has 80% the diameter of the Sun. Nicknamed "Speedy Mic", it has a rotation period of 9 hours 7 minutes. [20] An active star, it has prominent stellar flares that average 100 times stronger than those of the Sun, and are emitting energy mainly in the X-ray and ultraviolet bands of the spectrum. [21] It lies 218 ± 4 light-years away from the Sun. [22] AT Microscopii is a binary star system, both members of which are flare star red dwarfs. The system lies close to and may form a very wide triple system with AU Microscopii, [23] a young star which has a planetary system in the making with a debris disk. The three stars are candidate members of the Beta Pictoris moving group, one of the nearest associations of stars that share a common motion through space. [24]

The Astronomical Society of Southern Africa in 2003 reported that observations of four of the Mira variables in Microscopium were very urgently needed as data on their light curves was incomplete. [25] Two of them—R and S Microscopii—are challenging stars for novice amateur astronomers, [26] and the other two, U and RY Microscopii, are more difficult still. [25] Another red giant, T Microscopii, is a semiregular variable that ranges between magnitudes 7.7 and 9.6 over 344 days. [27] Of apparent magnitude 11, DD Microscopii is a symbiotic star system composed of an orange giant of spectral type K2III and white dwarf in close orbit, with the smaller star ionizing the stellar wind of the larger star. The system has a low metallicity. Combined with its high galactic latitude, this indicates that the star system has its origin in the galactic halo of the Milky Way. [28]

HD 205739 is a yellow-white main sequence star of spectral type F7V that is around 1.22 times as massive and 2.3 times as luminous as the Sun. It has a Jupiter-sized planet with an orbital period of 280 days that was discovered by the radial velocity method. [29] WASP-7 is a star of spectral type F5V with an apparent magnitude of 9.54, about 1.28 times as massive as the Sun. Its hot Jupiter planet—WASP-7b—was discovered by transit method and found to orbit the star every 4.95 days. [30] HD 202628 is a sunlike star of spectral type G2V with a debris disk that ranges from 158 to 220 AU distant. Its inner edge is sharply defined, indicating a probable planet orbiting between 86 and 158 AU from the star. [31]

Deep sky objects

Arp-Madore 2026-424 taken by Hubble. Arp-Madore 2026-424.tif
Arp-Madore 2026-424 taken by Hubble.

Describing Microscopium as "totally unremarkable", astronomer Patrick Moore concluded there was nothing of interest for amateur observers. [33] NGC 6925 is a barred spiral galaxy of apparent magnitude 11.3 which is lens-shaped, as it lies almost edge-on to observers on Earth, 3.7 degrees west-northwest of Alpha Microscopii. [34] SN 2011ei, a Type II Supernova in NGC 6925, was discovered by Stu Parker in New Zealand in July 2011. [35] NGC 6923 lies nearby and is a magnitude fainter still. [36] The Microscopium Void is a roughly rectangular region of relatively empty space, bounded by incomplete sheets of galaxies from other voids. [37] The Microscopium Supercluster is an overdensity of galaxy clusters that was first noticed in the early 1990s. The component Abell clusters 3695 and 3696 are likely to be gravitationally bound, while the relations of Abell clusters 3693 and 3705 in the same field are unclear. [38]

Meteor showers

Seen in the 1824 star chart set Urania's Mirror (in the lower left) Sidney Hall - Urania's Mirror - Sagittarius and Corona Australis, Microscopium, and Telescopium.png
Seen in the 1824 star chart set Urania's Mirror (in the lower left)

The Microscopids are a minor meteor shower that appear from June to mid-July. [39]

History

Microscopium lies in a region where Ptolemy had listed six 'unformed' stars behind the tail of Piscis Austrinus. [40] Al-Sufi did not include these stars in his revision of the Almagest, presumably because he could not identify them. [41] Microscopium was introduced in 1751–52 by Lacaille with the French name le Microscope, [42] [43] after he had observed and catalogued 10,000 southern stars during a two-year stay at the Cape of Good Hope. He devised fourteen new constellations in uncharted regions of the Southern Celestial Hemisphere not visible from Europe. All but one honoured instruments that symbolised the Age of Enlightenment. [44] Commemorating the compound microscope, [40] the Microscope's name had been Latinised by Lacaille to Microscopium by 1763. [42]

See also

Notes

  1. ↑ While parts of the constellation technically rise above the horizon to observers between 45°N and 62°N, stars within a few degrees of the horizon are to all intents and purposes unobservable. [3]
  2. ↑ Objects of magnitude 5.0 are barely visible to the unaided eye in the night skies of city-suburban transition areas. [5]
  3. ↑ Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban-rural transition night skies. [5]

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<span class="mw-page-title-main">Sculptor (constellation)</span> Constellation in the southern celestial hemisphere

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<span class="mw-page-title-main">Lacaille 9352</span> Star in the constellation Piscis Austrinus

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<span class="mw-page-title-main">Lacaille 8760</span> Star in the constellation Microscopium

Lacaille 8760 is a red dwarf star in the constellation Microscopium. It is one of the nearest stars to the Sun at about 12.9 light-years' distance, and the brightest M-class main-sequence star in Earth's night sky, although it is generally too faint to be seen without a telescope. At an apparent magnitude of +6.7, it may only be visible to the unaided eye under exceptionally good viewing conditions, under dark skies.

<span class="mw-page-title-main">Alpha Microscopii</span> Star in the constellation Microscopium

Alpha Microscopii (α Microscopii) is a star in the southern constellation of Microscopium. It is visible to the naked eye with an apparent visual magnitude of 4.89. Based upon an annual parallax shift of 8.2508 mas as seen from the Earth, it is located 395 light years from the Sun, give or take 7 light years. The star is moving nearer to the Sun with a heliocentric radial velocity of −15 km/s

<span class="mw-page-title-main">Gamma Microscopii</span> Star in the constellation Microscopium

Gamma Microscopii is the brightest star in the faint southern constellation of Microscopium. It has an apparent visual magnitude of 4.68, which is too dim to be viewed from city skies. The distance to this star has been determined using parallax measurements made with the Gaia telescope, which place it at 223 ± 8 light-years.

<span class="mw-page-title-main">BO Microscopii</span> Star in the constellation Microscopium

BO Microscopii is a star in the constellation Microscopium located about 170 light-years from the Sun. It has been dubbed "Speedy Mic" because of its very rapid rotation. The projected rotational velocity at the equator of this star is about 135 km/s (84 mi/s), which, with an estimated inclination of 70° to the line of sight from the Earth, means it completes a rotation every 0.380 ± 0.004 days. The photosphere of this star shows a high level of magnetic activity, with multiple star spots and prominences observed at the same time. As many as 25 prominences have been observed simultaneously, extending outward as far as 3.6 times the radius of the star. BO Mic is a flare star that undergoes sudden increases in X-ray and ultraviolet emissions. These events can emit a hundred times more energy than large solar flares. Speedy Mic is one of the most active stars in the vicinity of the Sun.

<span class="mw-page-title-main">Epsilon Microscopii</span> Star in the constellation Microscopium

Epsilon Microscopii, Latinized from ε Microscopii, is a single, white-hued star in the southern constellationof Microscopium. It is faintly visible to the naked eye with an apparent visual magnitude of 4.71. The annual parallax shift of the star is 19.7054 mas as measured from Earth, which yields a distance estimate of around 166 light years. It is moving further from the Sun with a radial velocity of +7 km/s.

<span class="mw-page-title-main">Iota Microscopii</span> Star in the constellation Microscopium

ι Microscopii, Latinized as Iota Microscopii, is a suspected astrometric binary star system in the southern constellation of Microscopium, near the southern constellation border with Indus. It is visible to the naked eye as a dim, yellow-white hued point of light with an apparent visual magnitude of 5.11. This object is 121 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −14 km/s.

ν Microscopii, Latinized as Nu Microscopii, is a star in the constellation Microscopium. It is an orange hued star that is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.76. It was first catalogued as Nu Indi by the French explorer and astronomer Nicolas Louis de Lacaille in 1756, before being reclassified in Microscopium and given its current Bayer designation of Nu Microscopii by Gould. The object is located at a distance of around 252 light-years from the Sun, based on parallax, and is drifting further away with a radial velocity of about +9 km/s.

Eta Microscopii, Latinised as η Microscopii, is a solitary star in the constellation Microscopium. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.53. The star is located around 910 light-years distant from the Sun based on parallax, and is drifting further away with a radial velocity of +22 km/s.

δ Microscopii, Latinised as Delta Microscopii, is a faint, orange hued binary star system in the constellation Microscopium, marking the eyepiece end of the "microscope". It is just visible to the naked eye with an apparent visual magnitude of +5.68. Based upon an annual parallax shift of 10.82 mas as seen from the Earth, it is roughly 300 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.142 due to interstellar dust.

<span class="mw-page-title-main">AV Microscopii</span> Star in the constellation Microscopium

AV Microscopii is a variable star in the southern constellation of Microscopium. It is a dim, red-hued star near the lower limit of visibility to the naked eye with a baseline apparent visual magnitude of 6.28. The star is located approximately 740 light years away from the Sun, based on parallax, but is moving closer with a radial velocity of −23 km/s. It is a member of the Milky Way's old disk population.

<span class="mw-page-title-main">R Microscopii</span> Variable star in the constellation Microscopium

R Microscopii is a star in the constellation Microscopium. It is a red giant star of spectral type M4e that is also a Mira variable, with an apparent magnitude ranging between 8.3 and 13.8 over 138 days. Located around 1000 light-years distant, it shines with a luminosity 444 times that of the Sun and has a surface temperature of 3141 K. The Astronomical Society of Southern Africa in 2003 reported that observations of R Microscopii were urgently needed as data on its light curve was incomplete.

<span class="mw-page-title-main">S Microscopii</span> Variable star in the constellation Microscopium

S Microscopii is a star in the constellation Microscopium. It is a red giant star of spectral type M3e-M5.5 that is also a Mira variable, with an apparent magnitude ranging between 7.4 and 14.8 over 210 days. The Astronomical Society of Southern Africa in 2003 reported that observations of S Microscopii were very urgently needed as data on its light curve was incomplete.

<span class="mw-page-title-main">T Microscopii</span> Variable star in the constellation Microscopium

T Microscopii is a semiregular variable star in the constellation Microscopium. It ranges from magnitude 6.74 to 8.11 over a period of 352 days. Located around 700 light-years distant, it shines with a bolometric luminosity 7,509 times that of the Sun and has a surface temperature of 2,750 K.

<span class="mw-page-title-main">Beta Microscopii</span> Constellation Microscopium star

Beta Microscopii, Latinized from β Microscopii, is a solitary star in the constellation Microscopium. It is close to the lower limit of stars that are visible to the naked eye having an apparent visual magnitude of 6.05 Based upon an annual parallax shift of 6.5022 mas as seen from Earth, this star is located 502 light years away from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.19 due to interstellar dust.

<span class="mw-page-title-main">DD Microscopii</span> Star in the constellation Microscopium

DD Microscopii, also known as CD−43°14304, is a binary star system in the constellation Microscopium. The system has a combined average apparent magnitude around 11, making it readily visible in telescopes but not to the naked eye. It is thought to be at a distance of one or two thousand parsecs, although parallax measurements place the system at a distance of around 30,000 light years.

References

Citations

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  10. ↑ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR .
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  21. ↑ Wolter, U.; Robrade, J.; Schmitt, J.H.M.M.; Ness, J.U. (2008). "Doppler imaging an X-ray flare on the ultrafast rotator BO Mic. A contemporaneous multiwavelength study using XMM-Newton and VLT". Astronomy and Astrophysics. 478 (1): L11–L14. arXiv: 0712.0899 . Bibcode:2008A&A...478L..11W. doi:10.1051/0004-6361:20078838. S2CID   62827486.
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  36. ↑ Moore, Patrick; Tirion, Wil (1997). Cambridge Guide to Stars and Planets . Cambridge: Cambridge University Press. p.  210. ISBN   978-0-521-58582-8.
  37. ↑ Maurellis, A.; Fairall, A.P.; Matravers, D.R.; Ellis, G.F.R. (1990). "A two-dimensional sheet of galaxies between two southern voids". Astronomy and Astrophysics. 229 (1): 75–79. Bibcode:1990A&A...229...75M. ISSN   0004-6361.
  38. ↑ Pearson, David W.; Batuski, David J. (2013). "Locating bound structure in an accelerating universe". Monthly Notices of the Royal Astronomical Society . 436 (1): 796–806. arXiv: 1308.5154 . Bibcode:2013MNRAS.436..796P. doi: 10.1093/mnras/stt1614 . S2CID   119271703.
  39. ↑ Molau, Sirko; Kac, Javor; Berko, Erno; Crivello, Stefano; Stomeo, Enrico; Igaz, Antal; Barentsen, Geert (July 2012). "Results of the IMO Video Meteor Network". WGN, Journal of the International Meteor Organization. 40 (5): 181–186. Bibcode:2012JIMO...40..181M.
  40. 1 2 Ridpath, Ian. "Microscopium the Microscope". Star Tales. Online edition. Retrieved 22 July 2023.
  41. ↑ Hafez, Ihsan (October 2010). Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of re-discovery. James Cook University (phd). p. 251.
  42. 1 2 Ridpath, Ian. "Lacaille's Southern Planisphere of 1756". Star Tales. Online edition. Retrieved 19 March 2015.
  43. ↑ Lacaille, Nicolas Louis (1756). "Relation abrégée du Voyage fait par ordre du Roi au cap de Bonne-espérance". Mémoires de l'Académie Royale des Sciences (in French): 519–592 [589].
  44. ↑ Wagman 2003, pp. 6–7.

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