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Microscopium
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<h2 id="characteristics">Characteristics</h2> <p>Microscopium is a small constellation bordered by <a href="/facts/Capricornus/YzjQKasz">Capricornus</a> to the north, <a href="/facts/Piscis_Austrinus/MndRqMEW">Piscis Austrinus</a> and <a href="/facts/Grus_(constellation)/xoyGI4qw">Grus</a> to the east, <a href="/facts/Sagittarius_(constellation)/ljtU4DQ2">Sagittarius</a> to the west, and <a href="/facts/Indus_(constellation)/PD27WuED">Indus</a> to the south, touching on <a href="/facts/Telescopium/HMTHvEYo">Telescopium</a> to the southwest. The recommended three-letter abbreviation for the constellation, as adopted by the <a href="/facts/International_Astronomical_Union/GMFPImXo">International Astronomical Union</a> in 1922, is "Mic".<a class="footnote-ref" id="fnref:1" href="#fn:1"><sup>1</sup></a> The official constellation boundaries, as set by Belgian astronomer <a href="/facts/Eug%25C3%25A8ne_Joseph_Delporte/IBCIUGgl">Eugène Delporte</a> in 1930, are defined by a polygon of four segments (<i>illustrated in infobox</i>). In the <a href="/facts/Equatorial_coordinate_system/dn5W4Eoo">equatorial coordinate system</a>, the <a href="/facts/Right_ascension/z4CEsTFu">right ascension</a> coordinates of these borders lie between 20h 27.3m and 21h 28.4m , while the <a href="/facts/Declination/5X4S4k9u">declination</a> coordinates are between −27.45° and −45.09°.<a class="footnote-ref" id="fnref:2" href="#fn:2"><sup>2</sup></a> The whole constellation is visible to observers south of latitude <a href="/facts/45th_parallel_north/rVorAsXN">45°N</a>.<a class="footnote-ref" id="fnref:3" href="#fn:3"><sup>3</sup></a><a class="footnote-ref" id="fnref:4" href="#fn:4"><sup>4</sup></a> Given that its brightest stars are of fifth magnitude, the constellation is invisible to the naked eye in areas with light polluted skies.<a class="footnote-ref" id="fnref:5" href="#fn:5"><sup>5</sup></a><a class="footnote-ref" id="fnref:6" href="#fn:6"><sup>6</sup></a> </p> <h2 id="features">Features</h2> <h3>Stars</h3> <p class="note">See also: <a href="/facts/List_of_stars_in_Microscopium/f4pnocHL">List of stars in Microscopium</a></p> <p>French astronomer <a href="/facts/Nicolas-Louis_de_Lacaille/zsd0KHzw">Nicolas-Louis de Lacaille</a> charted and designated ten stars with the <a href="/facts/Bayer_designation/KU2DVT47">Bayer designations</a> <a href="/facts/Alpha_Microscopii/uuUDx4d5">Alpha</a> through to <a href="/facts/Iota_Microscopii/pAD8v7Uh">Iota</a> in 1756. A star in neighbouring Indus that Lacaille had labelled Nu Indi turned out to be in Microscopium, so Gould renamed it <a href="/facts/Nu_Microscopii/4fWJqQkM">Nu Microscopii</a>. <a href="/facts/Francis_Baily/xNIlLAzn">Francis Baily</a> considered Gamma and Epsilon Microscopii to belong to the neighbouring constellation Piscis Austrinus, but subsequent cartographers did not follow this.<a class="footnote-ref" id="fnref:7" href="#fn:7"><sup>7</sup></a> In his 1725 <i>Catalogus Britannicus</i>, John Flamsteed labelled the stars 1, 2, 3 and 4 Piscis Austrini, which became Gamma Microscopii, <a href="/facts/2_Piscis_Austrini/p21nXuWH">HR 8076</a>, <a href="/facts/3_Piscis_Austrini/c0eykmm5">HR 8110</a> and Epsilon Microscopii respectively.<a class="footnote-ref" id="fnref:8" href="#fn:8"><sup>8</sup></a> Within the constellation's borders, there are 43 stars brighter than or equal to <a href="/facts/Apparent_magnitude/7pCTF1Me">apparent magnitude</a> 6.5.<a class="footnote-ref" id="fnref:9" href="#fn:9"><sup>9</sup></a><a class="footnote-ref" id="fnref:10" href="#fn:10"><sup>10</sup></a> </p><p>Depicting the eyepiece of the microscope is <a href="/facts/Gamma_Microscopii/jQrt26o0">Gamma Microscopii</a>,<a class="footnote-ref" id="fnref:11" href="#fn:11"><sup>11</sup></a> 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 <a href="/facts/Main_sequence/DJ3Wq8kd">main sequence</a> star, it has swollen and cooled to become a yellow <a href="/facts/Giant_star/kMseY7qf">giant</a> of <a href="/facts/Stellar_classification/dYrIuK9H">spectral type</a> G6III, with a diameter ten times that of the Sun.<a class="footnote-ref" id="fnref:12" href="#fn:12"><sup>12</sup></a> Measurement of its parallax yields a distance of 223 ± 8 light years from Earth.<a class="footnote-ref" id="fnref:13" href="#fn:13"><sup>13</sup></a> 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 <a href="/facts/Oort_cloud/wdP3VNxd">Oort cloud</a>.<a class="footnote-ref" id="fnref:14" href="#fn:14"><sup>14</sup></a> <a href="/facts/Alpha_Microscopii/uuUDx4d5">Alpha Microscopii</a> is also an ageing yellow giant star of spectral type G7III with an apparent magnitude of 4.90.<a class="footnote-ref" id="fnref:15" href="#fn:15"><sup>15</sup></a> Located 400 ± 30 light-years away from Earth,<a class="footnote-ref" id="fnref:16" href="#fn:16"><sup>16</sup></a> it has swollen to 17.5 times the diameter of the Sun.<a class="footnote-ref" id="fnref:17" href="#fn:17"><sup>17</sup></a> Alpha has a 10th magnitude companion, visible in 7.5 cm telescopes,<a class="footnote-ref" id="fnref:18" href="#fn:18"><sup>18</sup></a><a class="footnote-ref" id="fnref:19" href="#fn:19"><sup>19</sup></a> though this is a coincidental closeness rather than a true binary system.<a class="footnote-ref" id="fnref:20" href="#fn:20"><sup>20</sup></a> <a href="/facts/Epsilon_Microscopii/HSj04E1J">Epsilon Microscopii</a> lies 166 ± 5 light-years away,<a class="footnote-ref" id="fnref:21" href="#fn:21"><sup>21</sup></a> and is a white star of apparent magnitude 4.7,<a class="footnote-ref" id="fnref:22" href="#fn:22"><sup>22</sup></a> and spectral type A1V.<a class="footnote-ref" id="fnref:23" href="#fn:23"><sup>23</sup></a> <a href="/facts/Theta1_Microscopii/7qM4Tj5W">Theta1</a> and <a href="/facts/Theta2_Microscopii/MSQJsuD4">Theta2 Microscopii</a> make up a wide double whose components are splittable to the naked eye. Both are white A-class <a href="/facts/Alpha%25C2%25B2_Canum_Venaticorum_variable/VpU8der6">magnetic spectrum variable stars</a> with strong metallic lines, similar to <a href="/facts/Cor_Caroli/pI4X6akf">Cor Caroli</a>. They mark the constellation's specimen slide.<a class="footnote-ref" id="fnref:24" href="#fn:24"><sup>24</sup></a> </p><p>Many notable objects are too faint to be seen with the naked eye. AX Microscopii, better known as <a href="/facts/Lacaille_8760/bNmut60C">Lacaille 8760</a>, is a <a href="/facts/Red_dwarf/56CMQcF0">red dwarf</a> which lies only 12.9 light-years from the <a href="/facts/Solar_System/QIcLSazQ">Solar System</a>. At magnitude 6.68, it is the brightest red dwarf in the sky.<a class="footnote-ref" id="fnref:25" href="#fn:25"><sup>25</sup></a> <a href="/facts/BO_Microscopii/XCsehBkB">BO Microscopii</a> 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.<a class="footnote-ref" id="fnref:26" href="#fn:26"><sup>26</sup></a> An active star, it has prominent <a href="/facts/Solar_flare/6kCvPKxD">stellar flares</a> 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.<a class="footnote-ref" id="fnref:27" href="#fn:27"><sup>27</sup></a> It lies 218 ± 4 light-years away from the Sun.<a class="footnote-ref" id="fnref:28" href="#fn:28"><sup>28</sup></a> <a href="/facts/AT_Microscopii/BG8zNEyF">AT Microscopii</a> 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 <a href="/facts/AU_Microscopii/IPkKMJgs">AU Microscopii</a>,<a class="footnote-ref" id="fnref:29" href="#fn:29"><sup>29</sup></a> a young star which has a <a href="/facts/Planetary_system/6mcVtrTC">planetary system</a> in the making with a <a href="/facts/Debris_disk/ClIxTnge">debris disk</a>. The three stars are candidate members of the <a href="/facts/Beta_Pictoris_moving_group/DnWKFPl5">Beta Pictoris moving group</a>, one of the nearest <a href="/facts/Stellar_kinematics/6q1SRvDa">associations of stars</a> that share a common motion through space.<a class="footnote-ref" id="fnref:30" href="#fn:30"><sup>30</sup></a> </p><p>The <a href="/facts/Astronomical_Society_of_Southern_Africa/oT7D1lwN">Astronomical Society of Southern Africa</a> in 2003 reported that observations of four of the <a href="/facts/Mira_variable/MnudJxL9">Mira variables</a> in Microscopium were very urgently needed as data on their light curves was incomplete.<a class="footnote-ref" id="fnref:31" href="#fn:31"><sup>31</sup></a> Two of them—<a href="/facts/R_Microscopii/pxt4mStA">R</a> and <a href="/facts/S_Microscopii/SBCxVwBu">S Microscopii</a>—are challenging stars for novice amateur astronomers,<a class="footnote-ref" id="fnref:32" href="#fn:32"><sup>32</sup></a> and the other two, <a href="/facts/U_Microscopii/ymvUSH8S">U</a> and RY Microscopii, are more difficult still.<a class="footnote-ref" id="fnref:33" href="#fn:33"><sup>33</sup></a> Another red giant, <a href="/facts/T_Microscopii/Xf2SnAHV">T Microscopii</a>, is a <a href="/facts/Semiregular_variable_star/RcJ9Qw9E">semiregular variable</a> that ranges between magnitudes 7.7 and 9.6 over 344 days.<a class="footnote-ref" id="fnref:34" href="#fn:34"><sup>34</sup></a> Of apparent magnitude 11, <a href="/facts/DD_Microscopii/IUJQ2zRv">DD Microscopii</a> is a <a href="/facts/Symbiotic_star/9a33IvV2">symbiotic star</a> system composed of an orange giant of spectral type K2III and <a href="/facts/White_dwarf/gIYlTtrC">white dwarf</a> in close orbit, with the smaller star ionizing the stellar wind of the larger star. The system has a low <a href="/facts/Metallicity/nhhPqbYF">metallicity</a>. Combined with its high galactic latitude, this indicates that the star system has its origin in the <a href="/facts/Galactic_halo/A6jsautY">galactic halo</a> of the <a href="/facts/Milky_Way/ulF6lccN">Milky Way</a>.<a class="footnote-ref" id="fnref:35" href="#fn:35"><sup>35</sup></a> </p><p><a href="/facts/HD_205739/CVyqNBqq">HD 205739</a> 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 <a href="/facts/Methods_of_detecting_extrasolar_planets/vFIblQe9">radial velocity</a> method.<a class="footnote-ref" id="fnref:36" href="#fn:36"><sup>36</sup></a> <a href="/facts/WASP-7/6seDIvk7">WASP-7</a> is a star of spectral type F5V with an apparent magnitude of 9.54, about 1.28 times as massive as the Sun. Its <a href="/facts/Hot_Jupiter/9wSFCuxk">hot Jupiter</a> planet—<a href="/facts/WASP-7b/xVQB5gT0">WASP-7b</a>—was discovered by <a href="/facts/Methods_of_detecting_extrasolar_planets/vFIblQe9">transit method</a> and found to orbit the star every 4.95 days.<a class="footnote-ref" id="fnref:37" href="#fn:37"><sup>37</sup></a> <a href="/facts/HD_202628/Pg3Io6dv">HD 202628</a> 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.<a class="footnote-ref" id="fnref:38" href="#fn:38"><sup>38</sup></a> </p> <h3>Deep sky objects</h3> <p>Describing Microscopium as "totally unremarkable", astronomer <a href="/facts/Patrick_Moore/pwSzBtUg">Patrick Moore</a> concluded there was nothing of interest for amateur observers.<a class="footnote-ref" id="fnref:39" href="#fn:39"><sup>39</sup></a> <a href="/facts/NGC_6925/xG6S8IVH">NGC 6925</a> is a <a href="/facts/Barred_spiral_galaxy/cntSCFX4">barred spiral galaxy</a> 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.<a class="footnote-ref" id="fnref:40" href="#fn:40"><sup>40</sup></a> <a href="/facts/SN_2011ei/xG6S8IVH">SN 2011ei</a>, a <a href="/facts/Supernova/Pfo2J23l">Type II Supernova</a> in NGC 6925, was discovered by Stu Parker in New Zealand in July 2011.<a class="footnote-ref" id="fnref:41" href="#fn:41"><sup>41</sup></a> NGC 6923 lies nearby and is a magnitude fainter still.<a class="footnote-ref" id="fnref:42" href="#fn:42"><sup>42</sup></a> The <a href="/facts/Microscopium_Void/z39CIMJW">Microscopium Void</a> is a roughly rectangular region of relatively empty space, bounded by incomplete sheets of galaxies from other voids.<a class="footnote-ref" id="fnref:43" href="#fn:43"><sup>43</sup></a> The <a href="/facts/Microscopium_Supercluster/lYDbtmgK">Microscopium Supercluster</a> 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.<a class="footnote-ref" id="fnref:44" href="#fn:44"><sup>44</sup></a> </p> <h3>Meteor showers</h3> <p>The Microscopids are a minor <a href="/facts/Meteor_shower/ff47hYJA">meteor shower</a> that appear from June to mid-July.<a class="footnote-ref" id="fnref:45" href="#fn:45"><sup>45</sup></a> </p> <h2 id="history">History</h2> <p>Microscopium lies in a region where Ptolemy had listed six 'unformed' stars behind the tail of Piscis Austrinus.<a class="footnote-ref" id="fnref:46" href="#fn:46"><sup>46</sup></a> <a href="/facts/Al-Sufi/qzc2hHfl">Al-Sufi</a> did not include these stars in his revision of the <i>Almagest</i>, presumably because he could not identify them.<a class="footnote-ref" id="fnref:47" href="#fn:47"><sup>47</sup></a> Microscopium was introduced in 1751–52 by Lacaille with the French name <i>le Microscope</i>,<a class="footnote-ref" id="fnref:48" href="#fn:48"><sup>48</sup></a><a class="footnote-ref" id="fnref:49" href="#fn:49"><sup>49</sup></a> after he had observed and catalogued 10,000 southern stars during a two-year stay at the <a href="/facts/Cape_of_Good_Hope/2gvK5uwP">Cape of Good Hope</a>. He devised fourteen new constellations in uncharted regions of the <a href="/facts/Southern_Celestial_Hemisphere/PP2aeueF">Southern Celestial Hemisphere</a> not visible from Europe. All but one honoured instruments that symbolised the <a href="/facts/Age_of_Enlightenment/Uj2Fa8Mk">Age of Enlightenment</a>.<a class="footnote-ref" id="fnref:50" href="#fn:50"><sup>50</sup></a> Commemorating the <a href="/facts/Optical_microscope/5700vcna">compound microscope</a>,<a class="footnote-ref" id="fnref:51" href="#fn:51"><sup>51</sup></a> the Microscope's name had been Latinised by Lacaille to <i>Microscopium</i> by 1763.<a class="footnote-ref" id="fnref:52" href="#fn:52"><sup>52</sup></a> </p> <h2 id="see-also">See also</h2> <ul><li><a href="/facts/Microscopium_(Chinese_astronomy)/9uvWq8jW">Microscopium (Chinese astronomy)</a></li></ul> <h2 id="notes">Notes</h2> <h3>Citations</h3> <h3>Cited texts</h3> <ul><li>Wagman, Morton (2003). <i>Lost Stars: Lost, Missing and Troublesome Stars from the Catalogues of Johannes Bayer, Nicholas Louis de Lacaille, John Flamsteed, and Sundry Others</i>. Blacksburg, Virginia: The McDonald & Woodward Publishing Company. <a href="/facts/ISBN_(identifier)/15AdSPa9">ISBN</a> 978-0-939923-78-6.</li></ul> <h2 id="external-links">External links</h2> Wikimedia Commons has media related to Microscopium. <ul><li><a href="http://www.allthesky.com/constellations/indus/constell.html">The Deep Photographic Guide to the Constellations: Microscopium</a></li> <li><a href="http://astrojan.nhely.hu/microsc.htm">The clickable Microscopium</a></li></ul> <h2 id="references">References</h2> <ol> <li id="fn:1"><p>Russell, Henry Norris (1922). "The new international symbols for the constellations". Popular Astronomy. Vol. 30. p. 469. Bibcode:1922PA.....30..469R. <a href="/wiki/Henry_Norris_Russell" target="_blank">/wiki/Henry_Norris_Russell</a> <a href="#fnref:1" class="footnote-back-ref">↩</a></p></li> <li id="fn:2"><p>"Microscopium, constellation boundary". The Constellations. Retrieved 13 July 2012. <a href="https://www.iau.org/public/themes/constellations/#mic" target="_blank">https://www.iau.org/public/themes/constellations/#mic</a> <a href="#fnref:2" class="footnote-back-ref">↩</a></p></li> <li id="fn:3"><p>Ian Ridpath. "Constellations: Lacerta–Vulpecula". Star Tales. Self-published. Retrieved 29 November 2014. <a href="/wiki/Ian_Ridpath" target="_blank">/wiki/Ian_Ridpath</a> <a href="#fnref:3" class="footnote-back-ref">↩</a></p></li> <li id="fn:4"><p>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] <a href="/wiki/62nd_parallel_north" target="_blank">/wiki/62nd_parallel_north</a> <a href="#fnref:4" class="footnote-back-ref">↩</a></p></li> <li id="fn:5"><p>Kambič, Bojan (2009). Viewing the Constellations with Binoculars. Springer. p. 341. ISBN 978-0-387-85354-3. <a href="978-0-387-85354-3" target="_blank">978-0-387-85354-3</a> <a href="#fnref:5" class="footnote-back-ref">↩</a></p></li> <li id="fn:6"><p>Objects of magnitude 5.0 are barely visible to the unaided eye in the night skies of city-suburban transition areas.[5] <a href="#fnref:6" class="footnote-back-ref">↩</a></p></li> <li id="fn:7"><p>Wagman 2003, pp. 181, 210. - Wagman, Morton (2003). Lost Stars: Lost, Missing and Troublesome Stars from the Catalogues of Johannes Bayer, Nicholas Louis de Lacaille, John Flamsteed, and Sundry Others. Blacksburg, Virginia: The McDonald & Woodward Publishing Company. ISBN 978-0-939923-78-6. <a href="#fnref:7" class="footnote-back-ref">↩</a></p></li> <li id="fn:8"><p>Wagman 2003, p. 458. - Wagman, Morton (2003). Lost Stars: Lost, Missing and Troublesome Stars from the Catalogues of Johannes Bayer, Nicholas Louis de Lacaille, John Flamsteed, and Sundry Others. Blacksburg, Virginia: The McDonald & Woodward Publishing Company. ISBN 978-0-939923-78-6. <a href="#fnref:8" class="footnote-back-ref">↩</a></p></li> <li id="fn:9"><p>Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban-rural transition night skies.[5] <a href="#fnref:9" class="footnote-back-ref">↩</a></p></li> <li id="fn:10"><p>Ian Ridpath. "Constellations: Lacerta–Vulpecula". Star Tales. Self-published. Retrieved 29 November 2014. <a href="/wiki/Ian_Ridpath" target="_blank">/wiki/Ian_Ridpath</a> <a href="#fnref:10" class="footnote-back-ref">↩</a></p></li> <li id="fn:11"><p>Motz, Lloyd; Nathanson, Carol (1991). The Constellations: An Enthusiast's Guide to the Night Sky. London: Aurum Press. pp. 369–370. ISBN 978-1-85410-088-7. <a href="978-1-85410-088-7" target="_blank">978-1-85410-088-7</a> <a href="#fnref:11" class="footnote-back-ref">↩</a></p></li> <li id="fn:12"><p>Kaler, James B. "Gamma Mic". Stars. Retrieved 13 July 2012. <a href="http://stars.astro.illinois.edu/sow/gammamic.html" target="_blank">http://stars.astro.illinois.edu/sow/gammamic.html</a> <a href="#fnref:12" class="footnote-back-ref">↩</a></p></li> <li id="fn:13"><p>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. <a href="/wiki/Anthony_Brown_(scientist)" target="_blank">/wiki/Anthony_Brown_(scientist)</a> <a href="#fnref:13" class="footnote-back-ref">↩</a></p></li> <li id="fn:14"><p>Bailer-Jones, C.A.L. (2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. arXiv:1412.3648. Bibcode:2015A&A...575A..35B. doi:10.1051/0004-6361/201425221. S2CID 59039482. A35. <a href="/wiki/ArXiv_(identifier)" target="_blank">/wiki/ArXiv_(identifier)</a> <a href="#fnref:14" class="footnote-back-ref">↩</a></p></li> <li id="fn:15"><p>"Alpha MicroscopiI". SIMBAD. Retrieved 15 July 2012. <a href="http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Alpha+Microscopii&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id" target="_blank">http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Alpha+Microscopii&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id</a> <a href="#fnref:15" class="footnote-back-ref">↩</a></p></li> <li id="fn:16"><p>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. <a href="/wiki/Anthony_Brown_(scientist)" target="_blank">/wiki/Anthony_Brown_(scientist)</a> <a href="#fnref:16" class="footnote-back-ref">↩</a></p></li> <li id="fn:17"><p>Kaler, James B. "Alpha Mic". Stars. Retrieved 19 March 2015. <a href="http://stars.astro.illinois.edu/sow/alphamic.html" target="_blank">http://stars.astro.illinois.edu/sow/alphamic.html</a> <a href="#fnref:17" class="footnote-back-ref">↩</a></p></li> <li id="fn:18"><p>Malin, David; Frew, David J. (1995). Hartung's Astronomical Objects for Southern Telescopes, with an Addendum for Northern Observatories: A Handbook for Amateur Observers. Cambridge: Cambridge University Press. p. 287. ISBN 978-0-521-55491-6. <a href="978-0-521-55491-6" target="_blank">978-0-521-55491-6</a> <a href="#fnref:18" class="footnote-back-ref">↩</a></p></li> <li id="fn:19"><p>Ridpath, Ian; Tirion, Wil (2007). Stars and Planets Guide. Princeton, New Jersey: Princeton University Press. pp. 184–185. ISBN 978-0-691-13556-4. <a href="978-0-691-13556-4" target="_blank">978-0-691-13556-4</a> <a href="#fnref:19" class="footnote-back-ref">↩</a></p></li> <li id="fn:20"><p>Kaler, James B. "Alpha Mic". Stars. Retrieved 19 March 2015. <a href="http://stars.astro.illinois.edu/sow/alphamic.html" target="_blank">http://stars.astro.illinois.edu/sow/alphamic.html</a> <a href="#fnref:20" class="footnote-back-ref">↩</a></p></li> <li id="fn:21"><p>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. <a href="/wiki/Anthony_Brown_(scientist)" target="_blank">/wiki/Anthony_Brown_(scientist)</a> <a href="#fnref:21" class="footnote-back-ref">↩</a></p></li> <li id="fn:22"><p>Ridpath, Ian; Tirion, Wil (2007). Stars and Planets Guide. 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