Holoea - Revision history

http://210.45.112.182:8088/index.php?action=history&feed=atom&title=Holoea Holoea - Revision history 2026-07-12T20:35:53Z Revision history for this page on the wiki MediaWiki 1.45.1 http://210.45.112.182:8088/index.php?title=Holoea&diff=43186&oldid=prev YoulaAzkarrula at 02:16, 24 May 2026 2026-05-24T02:16:24Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 02:16, 24 May 2026</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l28">Line 28:</td> <td colspan="2" class="diff-lineno">Line 28:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Star Name‏‎]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Star Name‏‎]]</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:IAU-Star Name‏‎]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:IAU-Star Name‏‎]]</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Oceania]] [[Category:<del style="font-weight: bold; text-decoration: none;">Polynesia</del>]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Oceania]] [[Category:<ins style="font-weight: bold; text-decoration: none;">Polynesian</ins>]]</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Hawaiian]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Hawaiian]]</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Aur‏‎]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Aur‏‎]]</div></td></tr> </table>

YoulaAzkarrula http://210.45.112.182:8088/index.php?title=Holoea&diff=43185&oldid=prev YoulaAzkarrula at 02:15, 24 May 2026 2026-05-24T02:15:28Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 02:15, 24 May 2026</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l25">Line 25:</td> <td colspan="2" class="diff-lineno">Line 25:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Ian Ridpath's website ([http://ianridpath.com/startales Star Tales] )</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>* Ian Ridpath's website ([http://ianridpath.com/startales Star Tales] )</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div> </div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">[[Category:Asterism]]</ins></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Star Name‏‎]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Star Name‏‎]]</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:IAU-Star Name‏‎]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:IAU-Star Name‏‎]]</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Oceania]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Oceania<ins style="font-weight: bold; text-decoration: none;">]] [[Category:Polynesia</ins>]]</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Hawaiian]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Hawaiian]]</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Aur‏‎]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[Category:Aur‏‎]]</div></td></tr> </table>

YoulaAzkarrula http://210.45.112.182:8088/index.php?title=Holoea&diff=41247&oldid=prev Sushoff at 19:04, 20 April 2026 2026-04-20T19:04:36Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 19:04, 20 April 2026</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l5">Line 5:</td> <td colspan="2" class="diff-lineno">Line 5:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Concordance, Etymology, History==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Concordance, Etymology, History==</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Young Stellar Object, the name is Hawaiian for "flowing gas", discovered by Magnier et al. (1996)<ref name=":0">Magnier, E. A., Waters, L. B. F. M., Kuan, Y.-J., et al. (1996), A bipolar-outflow object in the field of M 36, A&A, 305, 936 [https://ui.adsabs.harvard.edu/abs/1996A%26A...305..936M/abstract ADSABS], and A&A</ref> with the James Clerk Maxwell Telescope at Mauna Kea, Hawaii. They refer to it in HST proposal 6459:<ref>Eugene Magnier (1996) of the University of Hawaii: THE DISK AND JET STRUCTURE OF HOLOEA, HST Proposal 6459 [https://archive.stsci.edu/proposal_search.php?id=6459&mission=hst online in MAST]</ref> <blockquote>"We have discovered an object in the field of the Galactic opencluster M36 which exhibits a nebulous tail-like structure, <del style="font-weight: bold; text-decoration: none;">abipolar </del>molecular outflow, a high-velocity ionized wind, and <del style="font-weight: bold; text-decoration: none;">abright </del>central star with spectral type ~ K0 III (Magnier et al.<del style="font-weight: bold; text-decoration: none;">,</del>1995)<ref name=":0" />. This source, which we have nick-named ``Holoea<nowiki>''</nowiki>, <del style="font-weight: bold; text-decoration: none;">mostlikely </del>represents a very early stage in the evolution <del style="font-weight: bold; text-decoration: none;">fromembedded </del>to naked T Tauri star. " </blockquote>Despite appearing close to the open star cluster M36 it is probably not a part of it. It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Young Stellar Object, the name is Hawaiian for "flowing gas", discovered by Magnier et al. (1996)<ref name=":0">Magnier, E. A., Waters, L. B. F. M., Kuan, Y.-J., et al. (1996), A bipolar-outflow object in the field of M 36, A&A, 305, 936 [https://ui.adsabs.harvard.edu/abs/1996A%26A...305..936M/abstract ADSABS], and A&A</ref> with the James Clerk Maxwell Telescope at Mauna Kea, Hawaii. They refer to it in HST proposal 6459:<ref>Eugene Magnier (1996) of the University of Hawaii: THE DISK AND JET STRUCTURE OF HOLOEA, HST Proposal 6459 [https://archive.stsci.edu/proposal_search.php?id=6459&mission=hst online in MAST]</ref> <blockquote>"We have discovered an object in the field of the Galactic opencluster M36 which exhibits a nebulous tail-like structure, <ins style="font-weight: bold; text-decoration: none;">a bipolar </ins>molecular outflow, a high-velocity ionized wind, and <ins style="font-weight: bold; text-decoration: none;">a bright </ins>central star with spectral type ~ K0 III (Magnier et al. 1995)<ref name=":0" />. This source, which we have nick-named ``Holoea<nowiki>''</nowiki>, <ins style="font-weight: bold; text-decoration: none;">most likely </ins>represents a very early stage in the evolution <ins style="font-weight: bold; text-decoration: none;">from embedded </ins>to naked T Tauri star. " </blockquote>Despite appearing close to the open star cluster M36 it is probably not a part of it. It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Morata et al. (2013)<ref>Morata et al. (2013). Millimetric and Submillimetric Observations of IRAS 05327+3404 "Holoea" in M36, The Astronomical Journal, Volume 146, Issue 3, article id. 49, 17 pp. (2013). [https://iopscience.iop.org/article/10.1088/0004-6256/146/3/49 DOI] </ref>: <blockquote>The distance to the object is then somewhat uncertain, ranging from the 1.2 kpc adopted by Hron (1987)for M36 to the 1.6 kpc for S235 (Blitz et al. 1982). We adopt a distance of 1.2 kpc. IRAS 05327+3404 drives a powerful ionized outflow, seen in both CO (2–1) and optical spectra, with unusually high velocity (∼650 km s−1) for a low-mass star. The structure of IRAS 05327+3404 is not yet clear (see Magnier et al. 1999b). It could be a binary system with a central star of optical spectral type K2 III, which is probably an FU Orionis star similar to L1551 IRS 5 (Magnier et al. 1999b), and a still embedded young star powering the outflow. The young star was classified (Magnier et al. 1999a, 1999b) as a transitional YSO between Class I and Class II, because of its rising spectral energy distribution (SED) and molecular bipolar outflow as well as its visible central star and ionized outflow. The SED also shows the presence of large amounts of circumstellar material, which, according to optical and nearIR observations of the reflection nebula, seems to be arranged in a disk with a relatively wide central hole of ∼33◦ opening angle. The ionized flow, the CO outflow, and the hole are all roughly aligned and tilted by ∼45◦ to our line of sight (Magnier et al. 1996). Additionally, the brightness of the central star has increased >1.5 mag since the 1954 POSS plates. Magnier et al. (1999b) suggest that the source might be in the process of becoming exposed and hypothesized that the unusually wide SEDcouldbeduetotherelativeisolation of IRAS05327+3404, which allowed the formation of a large circumstellar disk with high angular momentum without being disrupted by external sources. Thus, this object seems to be a good candidate to study the transition from the Class I to the Class II phase in the evolution of YSOs. Subsequent 3.6 cm Very Large Array (VLA) observations by Anglada & Rodr´ıguez (2002) detected a source, named VLA 2, inside the error ellipsoid of IRAS 05327+3404, which coincides within ∼1arcsecof the optical position of Magnier et al. (1996). H2O maser emission surveys by Wouterloot et al. (1993), Codella et al. (1995), and Sunada et al. (2007) did not detect any maser emission near IRAS 05327+3404.</blockquote></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Morata et al. (2013)<ref>Morata et al. (2013). Millimetric and Submillimetric Observations of IRAS 05327+3404 "Holoea" in M36, The Astronomical Journal, Volume 146, Issue 3, article id. 49, 17 pp. (2013). [https://iopscience.iop.org/article/10.1088/0004-6256/146/3/49 DOI] </ref>: <blockquote>The distance to the object is then somewhat uncertain, ranging from the 1.2 kpc adopted by Hron (1987)for M36 to the 1.6 kpc for S235 (Blitz et al. 1982). We adopt a distance of 1.2 kpc. IRAS 05327+3404 drives a powerful ionized outflow, seen in both CO (2–1) and optical spectra, with unusually high velocity (∼650 km s−1) for a low-mass star. The structure of IRAS 05327+3404 is not yet clear (see Magnier et al. 1999b). It could be a binary system with a central star of optical spectral type K2 III, which is probably an FU Orionis star similar to L1551 IRS 5 (Magnier et al. 1999b), and a still embedded young star powering the outflow. The young star was classified (Magnier et al. 1999a, 1999b) as a transitional YSO between Class I and Class II, because of its rising spectral energy distribution (SED) and molecular bipolar outflow as well as its visible central star and ionized outflow. The SED also shows the presence of large amounts of circumstellar material, which, according to optical and nearIR observations of the reflection nebula, seems to be arranged in a disk with a relatively wide central hole of ∼33◦ opening angle. The ionized flow, the CO outflow, and the hole are all roughly aligned and tilted by ∼45◦ to our line of sight (Magnier et al. 1996). Additionally, the brightness of the central star has increased >1.5 mag since the 1954 POSS plates. Magnier et al. (1999b) suggest that the source might be in the process of becoming exposed and hypothesized that the unusually wide SEDcouldbeduetotherelativeisolation of IRAS05327+3404, which allowed the formation of a large circumstellar disk with high angular momentum without being disrupted by external sources. Thus, this object seems to be a good candidate to study the transition from the Class I to the Class II phase in the evolution of YSOs. Subsequent 3.6 cm Very Large Array (VLA) observations by Anglada & Rodr´ıguez (2002) detected a source, named VLA 2, inside the error ellipsoid of IRAS 05327+3404, which coincides within ∼1arcsecof the optical position of Magnier et al. (1996). H2O maser emission surveys by Wouterloot et al. (1993), Codella et al. (1995), and Sunada et al. (2007) did not detect any maser emission near IRAS 05327+3404.</blockquote></div></td></tr> </table>

Sushoff http://210.45.112.182:8088/index.php?title=Holoea&diff=41246&oldid=prev Sushoff at 19:03, 20 April 2026 2026-04-20T19:03:33Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 19:03, 20 April 2026</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l5">Line 5:</td> <td colspan="2" class="diff-lineno">Line 5:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Concordance, Etymology, History==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Concordance, Etymology, History==</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Young Stellar Object, the name is Hawaiian for "flowing gas", discovered by Magnier et al. (1996)<ref name=":0">Magnier, E. A., Waters, L. B. F. M., Kuan, Y.-J., et al. (1996), A bipolar-outflow object in the field of M 36, A&A, 305, 936 [https://ui.adsabs.harvard.edu/abs/1996A%26A...305..936M/abstract ADSABS], and A&A</ref> with the James Clerk Maxwell Telescope at Mauna Kea, Hawaii. They refer to it in HST proposal 6459:<ref>Eugene Magnier (1996) of the University of Hawaii: THE DISK AND JET STRUCTURE OF HOLOEA, HST Proposal 6459 [https://archive.stsci.edu/proposal_search.php?id=6459&mission=hst online in MAST]</ref> <blockquote>"We have discovered an object in the field of the Galactic opencluster M36 which exhibits a nebulous tail-like structure, abipolar molecular outflow, a high-velocity ionized wind, and abright central star with spectral type ~ K0 III (Magnier et al.,1995). This source, which we have nick-named ``Holoea<nowiki>''</nowiki>, mostlikely represents a very early stage in the evolution fromembedded to naked T Tauri star. " </blockquote>Despite appearing close to the open star cluster M36 it is probably not a part of it. It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Young Stellar Object, the name is Hawaiian for "flowing gas", discovered by Magnier et al. (1996)<ref name=":0">Magnier, E. A., Waters, L. B. F. M., Kuan, Y.-J., et al. (1996), A bipolar-outflow object in the field of M 36, A&A, 305, 936 [https://ui.adsabs.harvard.edu/abs/1996A%26A...305..936M/abstract ADSABS], and A&A</ref> with the James Clerk Maxwell Telescope at Mauna Kea, Hawaii. They refer to it in HST proposal 6459:<ref>Eugene Magnier (1996) of the University of Hawaii: THE DISK AND JET STRUCTURE OF HOLOEA, HST Proposal 6459 [https://archive.stsci.edu/proposal_search.php?id=6459&mission=hst online in MAST]</ref> <blockquote>"We have discovered an object in the field of the Galactic opencluster M36 which exhibits a nebulous tail-like structure, abipolar molecular outflow, a high-velocity ionized wind, and abright central star with spectral type ~ K0 III (Magnier et al.,1995)<ins style="font-weight: bold; text-decoration: none;"><ref name=":0" /></ins>. This source, which we have nick-named ``Holoea<nowiki>''</nowiki>, mostlikely represents a very early stage in the evolution fromembedded to naked T Tauri star. " </blockquote>Despite appearing close to the open star cluster M36 it is probably not a part of it. It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Morata et al. (2013)<ref>Morata et al. (2013). Millimetric and Submillimetric Observations of IRAS 05327+3404 "Holoea" in M36, The Astronomical Journal, Volume 146, Issue 3, article id. 49, 17 pp. (2013). [https://iopscience.iop.org/article/10.1088/0004-6256/146/3/49 DOI] </ref>: <blockquote>The distance to the object is then somewhat uncertain, ranging from the 1.2 kpc adopted by Hron (1987)for M36 to the 1.6 kpc for S235 (Blitz et al. 1982). We adopt a distance of 1.2 kpc. IRAS 05327+3404 drives a powerful ionized outflow, seen in both CO (2–1) and optical spectra, with unusually high velocity (∼650 km s−1) for a low-mass star. The structure of IRAS 05327+3404 is not yet clear (see Magnier et al. 1999b). It could be a binary system with a central star of optical spectral type K2 III, which is probably an FU Orionis star similar to L1551 IRS 5 (Magnier et al. 1999b), and a still embedded young star powering the outflow. The young star was classified (Magnier et al. 1999a, 1999b) as a transitional YSO between Class I and Class II, because of its rising spectral energy distribution (SED) and molecular bipolar outflow as well as its visible central star and ionized outflow. The SED also shows the presence of large amounts of circumstellar material, which, according to optical and nearIR observations of the reflection nebula, seems to be arranged in a disk with a relatively wide central hole of ∼33◦ opening angle. The ionized flow, the CO outflow, and the hole are all roughly aligned and tilted by ∼45◦ to our line of sight (Magnier et al. 1996). Additionally, the brightness of the central star has increased >1.5 mag since the 1954 POSS plates. Magnier et al. (1999b) suggest that the source might be in the process of becoming exposed and hypothesized that the unusually wide SEDcouldbeduetotherelativeisolation of IRAS05327+3404, which allowed the formation of a large circumstellar disk with high angular momentum without being disrupted by external sources. Thus, this object seems to be a good candidate to study the transition from the Class I to the Class II phase in the evolution of YSOs. Subsequent 3.6 cm Very Large Array (VLA) observations by Anglada & Rodr´ıguez (2002) detected a source, named VLA 2, inside the error ellipsoid of IRAS 05327+3404, which coincides within ∼1arcsecof the optical position of Magnier et al. (1996). H2O maser emission surveys by Wouterloot et al. (1993), Codella et al. (1995), and Sunada et al. (2007) did not detect any maser emission near IRAS 05327+3404.</blockquote></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Morata et al. (2013)<ref>Morata et al. (2013). Millimetric and Submillimetric Observations of IRAS 05327+3404 "Holoea" in M36, The Astronomical Journal, Volume 146, Issue 3, article id. 49, 17 pp. (2013). [https://iopscience.iop.org/article/10.1088/0004-6256/146/3/49 DOI] </ref>: <blockquote>The distance to the object is then somewhat uncertain, ranging from the 1.2 kpc adopted by Hron (1987)for M36 to the 1.6 kpc for S235 (Blitz et al. 1982). We adopt a distance of 1.2 kpc. IRAS 05327+3404 drives a powerful ionized outflow, seen in both CO (2–1) and optical spectra, with unusually high velocity (∼650 km s−1) for a low-mass star. The structure of IRAS 05327+3404 is not yet clear (see Magnier et al. 1999b). It could be a binary system with a central star of optical spectral type K2 III, which is probably an FU Orionis star similar to L1551 IRS 5 (Magnier et al. 1999b), and a still embedded young star powering the outflow. The young star was classified (Magnier et al. 1999a, 1999b) as a transitional YSO between Class I and Class II, because of its rising spectral energy distribution (SED) and molecular bipolar outflow as well as its visible central star and ionized outflow. The SED also shows the presence of large amounts of circumstellar material, which, according to optical and nearIR observations of the reflection nebula, seems to be arranged in a disk with a relatively wide central hole of ∼33◦ opening angle. The ionized flow, the CO outflow, and the hole are all roughly aligned and tilted by ∼45◦ to our line of sight (Magnier et al. 1996). Additionally, the brightness of the central star has increased >1.5 mag since the 1954 POSS plates. Magnier et al. (1999b) suggest that the source might be in the process of becoming exposed and hypothesized that the unusually wide SEDcouldbeduetotherelativeisolation of IRAS05327+3404, which allowed the formation of a large circumstellar disk with high angular momentum without being disrupted by external sources. Thus, this object seems to be a good candidate to study the transition from the Class I to the Class II phase in the evolution of YSOs. Subsequent 3.6 cm Very Large Array (VLA) observations by Anglada & Rodr´ıguez (2002) detected a source, named VLA 2, inside the error ellipsoid of IRAS 05327+3404, which coincides within ∼1arcsecof the optical position of Magnier et al. (1996). H2O maser emission surveys by Wouterloot et al. (1993), Codella et al. (1995), and Sunada et al. (2007) did not detect any maser emission near IRAS 05327+3404.</blockquote></div></td></tr> </table>

Sushoff http://210.45.112.182:8088/index.php?title=Holoea&diff=41245&oldid=prev Sushoff at 19:02, 20 April 2026 2026-04-20T19:02:41Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 19:02, 20 April 2026</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l5">Line 5:</td> <td colspan="2" class="diff-lineno">Line 5:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Concordance, Etymology, History==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Concordance, Etymology, History==</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Young Stellar Object, the name is Hawaiian for "flowing gas", discovered by Magnier et al. (1996)<ref name=":0">Magnier, E. A., Waters, L. B. F. M., Kuan, Y.-J., et al. (1996), A bipolar-outflow object in the field of M 36, A&A, 305, 936 [https://ui.adsabs.harvard.edu/abs/1996A%26A...305..936M/abstract ADSABS], and A&A</ref> with the James Clerk Maxwell Telescope at Mauna Kea, Hawaii. </div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Young Stellar Object, the name is Hawaiian for "flowing gas", discovered by Magnier et al. (1996)<ref name=":0">Magnier, E. A., Waters, L. B. F. M., Kuan, Y.-J., et al. (1996), A bipolar-outflow object in the field of M 36, A&A, 305, 936 [https://ui.adsabs.harvard.edu/abs/1996A%26A...305..936M/abstract ADSABS], and A&A</ref> with the James Clerk Maxwell Telescope at Mauna Kea, Hawaii. <ins style="font-weight: bold; text-decoration: none;">They refer to it in HST proposal 6459:<ref>Eugene Magnier (1996) of the University of Hawaii: THE DISK AND JET STRUCTURE OF HOLOEA, HST Proposal 6459 [https://archive.stsci.edu/proposal_search.php?id=6459&mission=hst online in MAST]</ref> <blockquote>"We have discovered an object in the field of the Galactic opencluster M36 which exhibits a nebulous tail-like structure, abipolar molecular outflow, a high-velocity ionized wind, and abright central star with spectral type ~ K0 III (Magnier et al.,1995). This source, which we have nick-named ``Holoea<nowiki>''</nowiki>, mostlikely represents a very early stage in the evolution fromembedded to naked T Tauri star. " </blockquote></ins>Despite appearing close to the open star cluster M36 it is probably not a part of it. It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div> </div></td><td colspan="2" class="diff-side-added"></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Despite appearing close to the open star cluster M36 it is probably not a part of it. It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.</div></td><td colspan="2" class="diff-side-added"></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Morata et al. (2013)<ref>Morata et al. (2013). Millimetric and Submillimetric Observations of IRAS 05327+3404 "Holoea" in M36, The Astronomical Journal, Volume 146, Issue 3, article id. 49, 17 pp. (2013). [https://iopscience.iop.org/article/10.1088/0004-6256/146/3/49 DOI] </ref>: <blockquote>The distance to the object is then somewhat uncertain, ranging from the 1.2 kpc adopted by Hron (1987)for M36 to the 1.6 kpc for S235 (Blitz et al. 1982). We adopt a distance of 1.2 kpc. IRAS 05327+3404 drives a powerful ionized outflow, seen in both CO (2–1) and optical spectra, with unusually high velocity (∼650 km s−1) for a low-mass star. The structure of IRAS 05327+3404 is not yet clear (see Magnier et al. 1999b). It could be a binary system with a central star of optical spectral type K2 III, which is probably an FU Orionis star similar to L1551 IRS 5 (Magnier et al. 1999b), and a still embedded young star powering the outflow. The young star was classified (Magnier et al. 1999a, 1999b) as a transitional YSO between Class I and Class II, because of its rising spectral energy distribution (SED) and molecular bipolar outflow as well as its visible central star and ionized outflow. The SED also shows the presence of large amounts of circumstellar material, which, according to optical and nearIR observations of the reflection nebula, seems to be arranged in a disk with a relatively wide central hole of ∼33◦ opening angle. The ionized flow, the CO outflow, and the hole are all roughly aligned and tilted by ∼45◦ to our line of sight (Magnier et al. 1996). Additionally, the brightness of the central star has increased >1.5 mag since the 1954 POSS plates. Magnier et al. (1999b) suggest that the source might be in the process of becoming exposed and hypothesized that the unusually wide SEDcouldbeduetotherelativeisolation of IRAS05327+3404, which allowed the formation of a large circumstellar disk with high angular momentum without being disrupted by external sources. Thus, this object seems to be a good candidate to study the transition from the Class I to the Class II phase in the evolution of YSOs. Subsequent 3.6 cm Very Large Array (VLA) observations by Anglada & Rodr´ıguez (2002) detected a source, named VLA 2, inside the error ellipsoid of IRAS 05327+3404, which coincides within ∼1arcsecof the optical position of Magnier et al. (1996). H2O maser emission surveys by Wouterloot et al. (1993), Codella et al. (1995), and Sunada et al. (2007) did not detect any maser emission near IRAS 05327+3404.</blockquote></div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Morata et al. (2013)<ref>Morata et al. (2013). Millimetric and Submillimetric Observations of IRAS 05327+3404 "Holoea" in M36, The Astronomical Journal, Volume 146, Issue 3, article id. 49, 17 pp. (2013). [https://iopscience.iop.org/article/10.1088/0004-6256/146/3/49 DOI] </ref>: <blockquote>The distance to the object is then somewhat uncertain, ranging from the 1.2 kpc adopted by Hron (1987)for M36 to the 1.6 kpc for S235 (Blitz et al. 1982). We adopt a distance of 1.2 kpc. IRAS 05327+3404 drives a powerful ionized outflow, seen in both CO (2–1) and optical spectra, with unusually high velocity (∼650 km s−1) for a low-mass star. The structure of IRAS 05327+3404 is not yet clear (see Magnier et al. 1999b). It could be a binary system with a central star of optical spectral type K2 III, which is probably an FU Orionis star similar to L1551 IRS 5 (Magnier et al. 1999b), and a still embedded young star powering the outflow. The young star was classified (Magnier et al. 1999a, 1999b) as a transitional YSO between Class I and Class II, because of its rising spectral energy distribution (SED) and molecular bipolar outflow as well as its visible central star and ionized outflow. The SED also shows the presence of large amounts of circumstellar material, which, according to optical and nearIR observations of the reflection nebula, seems to be arranged in a disk with a relatively wide central hole of ∼33◦ opening angle. The ionized flow, the CO outflow, and the hole are all roughly aligned and tilted by ∼45◦ to our line of sight (Magnier et al. 1996). Additionally, the brightness of the central star has increased >1.5 mag since the 1954 POSS plates. Magnier et al. (1999b) suggest that the source might be in the process of becoming exposed and hypothesized that the unusually wide SEDcouldbeduetotherelativeisolation of IRAS05327+3404, which allowed the formation of a large circumstellar disk with high angular momentum without being disrupted by external sources. Thus, this object seems to be a good candidate to study the transition from the Class I to the Class II phase in the evolution of YSOs. Subsequent 3.6 cm Very Large Array (VLA) observations by Anglada & Rodr´ıguez (2002) detected a source, named VLA 2, inside the error ellipsoid of IRAS 05327+3404, which coincides within ∼1arcsecof the optical position of Magnier et al. (1996). H2O maser emission surveys by Wouterloot et al. (1993), Codella et al. (1995), and Sunada et al. (2007) did not detect any maser emission near IRAS 05327+3404.</blockquote></div></td></tr> </table>

Sushoff http://210.45.112.182:8088/index.php?title=Holoea&diff=41244&oldid=prev Sushoff at 18:55, 20 April 2026 2026-04-20T18:55:27Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 18:55, 20 April 2026</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l1">Line 1:</td> <td colspan="2" class="diff-lineno">Line 1:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Authors: {{PAGEAUTHORS}}</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Authors: {{PAGEAUTHORS}}</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>----</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>----</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>[[File:Fig1_M36%2BHoloea_1996A%26A...305..936M.jpg|thumb|Fig.1 in Magnier et al. (1996) which presents the young stellar object in the field of view close to the star cluster M36.]]</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>[[File:Fig1_M36%2BHoloea_1996A%26A...305..936M.jpg|thumb|Fig.1 in Magnier et al. (1996)<ins style="font-weight: bold; text-decoration: none;"><ref name=":0" /> </ins>which presents the young stellar object in the field of view close to the star cluster M36.]]</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Holoea is a modern star name adopted by the International Astronomical Union in the IAU-Catalog of Star Names (IAU-CSN). Its origin is Hawaiian. It is the name of the star IRAS 05327+3404 (Vmag = 18.62) in constellation [[Auriga]].</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Holoea is a modern star name adopted by the International Astronomical Union in the IAU-Catalog of Star Names (IAU-CSN). Its origin is Hawaiian. It is the name of the star IRAS 05327+3404 (Vmag = 18.62) in constellation [[Auriga]].</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Concordance, Etymology, History==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Concordance, Etymology, History==</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Young Stellar Object, the name is Hawaiian for "flowing gas", discovered by Magnier et al. (1996)<ref>Magnier, E. A., Waters, L. B. F. M., Kuan, Y.-J., et al. (1996), A bipolar-outflow object in the field of M 36, A&A, 305, 936 [https://ui.adsabs.harvard.edu/abs/1996A%26A...305..936M/abstract ADSABS], and A&A</ref> with the James Clerk Maxwell Telescope at Mauna Kea, Hawaii. </div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Young Stellar Object, the name is Hawaiian for "flowing gas", discovered by Magnier et al. (1996)<ref <ins style="font-weight: bold; text-decoration: none;">name=":0"</ins>>Magnier, E. A., Waters, L. B. F. M., Kuan, Y.-J., et al. (1996), A bipolar-outflow object in the field of M 36, A&A, 305, 936 [https://ui.adsabs.harvard.edu/abs/1996A%26A...305..936M/abstract ADSABS], and A&A</ref> with the James Clerk Maxwell Telescope at Mauna Kea, Hawaii. </div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Despite appearing close to the open star cluster M36 it is probably not a part of it. It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Despite appearing close to the open star cluster M36 it is probably not a part of it. It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.</div></td></tr> </table>

Sushoff http://210.45.112.182:8088/index.php?title=Holoea&diff=41243&oldid=prev Sushoff at 18:54, 20 April 2026 2026-04-20T18:54:56Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 18:54, 20 April 2026</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l1">Line 1:</td> <td colspan="2" class="diff-lineno">Line 1:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Authors: {{PAGEAUTHORS}}</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Authors: {{PAGEAUTHORS}}</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>----</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>----</div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">[[File:Fig1_M36%2BHoloea_1996A%26A...305..936M.jpg|thumb|Fig.1 in Magnier et al. (1996) which presents the young stellar object in the field of view close to the star cluster M36.]]</ins></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Holoea is a modern star name adopted by the International Astronomical Union in the IAU-Catalog of Star Names (IAU-CSN). Its origin is Hawaiian. It is the name of the star IRAS 05327+3404 (Vmag = 18.62) in constellation [[Auriga]].</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Holoea is a modern star name adopted by the International Astronomical Union in the IAU-Catalog of Star Names (IAU-CSN). Its origin is Hawaiian. It is the name of the star IRAS 05327+3404 (Vmag = 18.62) in constellation [[Auriga]].</div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> </table>

Sushoff http://210.45.112.182:8088/index.php?title=Holoea&diff=41237&oldid=prev Sushoff: /* IAU Working Group on Star Names */ 2026-04-20T06:16:56Z

<p><span class="autocomment">IAU Working Group on Star Names</span></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 06:16, 20 April 2026</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l14">Line 14:</td> <td colspan="2" class="diff-lineno">Line 14:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==IAU Working Group on Star Names==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==IAU Working Group on Star Names==</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>The name was <del style="font-weight: bold; text-decoration: none;">discussed and </del>approved by the IAU WGSN in 2026, following a suggestion by the SIMBAD team. </div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>The name was approved by the IAU WGSN in 2026, following a suggestion by the SIMBAD team. </div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> </table>

Sushoff http://210.45.112.182:8088/index.php?title=Holoea&diff=41170&oldid=prev Sushoff at 11:32, 18 April 2026 2026-04-18T11:32:32Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 11:32, 18 April 2026</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l11">Line 11:</td> <td colspan="2" class="diff-lineno">Line 11:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Mythology==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Mythology==</div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">no mythology</ins></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==IAU Working Group on Star Names==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==IAU Working Group on Star Names==</div></td></tr> </table>

Sushoff http://210.45.112.182:8088/index.php?title=Holoea&diff=41169&oldid=prev Sushoff at 11:25, 18 April 2026 2026-04-18T11:25:24Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="en"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">← Older revision</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">Revision as of 11:25, 18 April 2026</td> </tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l4">Line 4:</td> <td colspan="2" class="diff-lineno">Line 4:</td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Concordance, Etymology, History==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Concordance, Etymology, History==</div></td></tr> <tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Young Stellar Object, the name is Hawaiian for "flowing gas".</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Young Stellar Object, the name is Hawaiian for "flowing gas"<ins style="font-weight: bold; text-decoration: none;">, discovered by Magnier et al</ins>. <ins style="font-weight: bold; text-decoration: none;">(1996)<ref>Magnier, E. A., Waters, L. B. F. M., Kuan, Y.-J., et al. (1996), A bipolar-outflow object in the field of M 36, A&A, 305, 936 [https://ui.adsabs.harvard.edu/abs/1996A%26A...305..936M/abstract ADSABS], and A&A</ref> with the James Clerk Maxwell Telescope at Mauna Kea, Hawaii. </ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div> </div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">Despite appearing close to the open star cluster M36 it is probably not a part of it. It may be a member of the more distant S235 region. The young star driving the outflow was classified as transitional between class I and class II and appears to be surrounded by large amounts of circumstellar material.</ins></div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div> </div></td></tr> <tr><td colspan="2" class="diff-side-deleted"></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">Morata et al. (2013)<ref>Morata et al. (2013). Millimetric and Submillimetric Observations of IRAS 05327+3404 "Holoea" in M36, The Astronomical Journal, Volume 146, Issue 3, article id. 49, 17 pp. (2013). [https://iopscience.iop.org/article/10.1088/0004-6256/146/3/49 DOI] </ref>: <blockquote>The distance to the object is then somewhat uncertain, ranging from the 1.2 kpc adopted by Hron (1987)for M36 to the 1.6 kpc for S235 (Blitz et al. 1982). We adopt a distance of 1.2 kpc. IRAS 05327+3404 drives a powerful ionized outflow, seen in both CO (2–1) and optical spectra, with unusually high velocity (∼650 km s−1) for a low-mass star. The structure of IRAS 05327+3404 is not yet clear (see Magnier et al. 1999b). It could be a binary system with a central star of optical spectral type K2 III, which is probably an FU Orionis star similar to L1551 IRS 5 (Magnier et al. 1999b), and a still embedded young star powering the outflow. The young star was classified (Magnier et al. 1999a, 1999b) as a transitional YSO between Class I and Class II, because of its rising spectral energy distribution (SED) and molecular bipolar outflow as well as its visible central star and ionized outflow. The SED also shows the presence of large amounts of circumstellar material, which, according to optical and nearIR observations of the reflection nebula, seems to be arranged in a disk with a relatively wide central hole of ∼33◦ opening angle. The ionized flow, the CO outflow, and the hole are all roughly aligned and tilted by ∼45◦ to our line of sight (Magnier et al. 1996). Additionally, the brightness of the central star has increased >1.5 mag since the 1954 POSS plates. Magnier et al. (1999b) suggest that the source might be in the process of becoming exposed and hypothesized that the unusually wide SEDcouldbeduetotherelativeisolation of IRAS05327+3404, which allowed the formation of a large circumstellar disk with high angular momentum without being disrupted by external sources. Thus, this object seems to be a good candidate to study the transition from the Class I to the Class II phase in the evolution of YSOs. Subsequent 3.6 cm Very Large Array (VLA) observations by Anglada & Rodr´ıguez (2002) detected a source, named VLA 2, inside the error ellipsoid of IRAS 05327+3404, which coincides within ∼1arcsecof the optical position of Magnier et al. (1996). H2O maser emission surveys by Wouterloot et al. (1993), Codella et al. (1995), and Sunada et al. (2007) did not detect any maser emission near IRAS 05327+3404.</blockquote></ins></div></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br></td></tr> <tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Mythology==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==Mythology==</div></td></tr> </table>

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