Langbahn Team – Weltmeisterschaft

Chamaeleon complex

IRAS image of Chamaeleon I, II and III. The Dark Doodad Nebula is the red filament at the top.

The Chamaeleon complex is a large star forming region (SFR) at the surface of the Local Bubble that includes the Chamaeleon I, Chamaeleon II, and Chamaeleon III dark clouds. It occupies nearly all of the constellation Chamaeleon and overlaps into Apus, Musca, Carina and Octans. The mean density of X-ray sources is about one source per square degree.[1]

Chamaeleon I dark cloud

Chamaeleon I with Herschel, showing protoplanetary disks imaged with SPHERE.

The Chamaeleon I (Cha I) cloud is one of the nearest active star formation regions at ~160 pc.[2] It is relatively isolated from other star-forming clouds, so it is unlikely that older pre-main sequence (PMS) stars have drifted into the field.[2] The total stellar population is 200–300.[2] The Cha I cloud is further divided into the North cloud or region and South cloud or main cloud. Star-formation began 3-4 Myrs in the southern region and 5-6 Myr ago in the northern region. The stars have a median age of about 2 Myrs.[3] The age was later revised to 1-2 Myr.[4]

HD 97300 emits X-rays, illuminates the reflection nebula IC 2631 and is one of the highest mass members of the Cha I cloud, spectral type B9V, a Herbig Ae/Be star without emission lines.[2]

Cha Helpha 1 is an object of spectral type M8 in the Chamaeleon I dark cloud that was determined in 1998 to be an X-ray source and as such is the first X-ray emitting brown dwarf found.

There are some seventy to ninety X-ray sources in the Chamaeleon I star forming region.[5] The Uhuru X-ray source (4U 1119–77) is within the Chamaeleon I cloud. This source region within the Chamaeleon I dark cloud was observed by ROSAT on February 9 at 22:14:47 UTC to February 18, 1991, 17:59:12 UTC, and on March 6, 1991, from 09:12:19 to 13:05:13 UTC.[5] This cloud contains both "weak" T Tauri (WTT) stars and "classical" T Tauri (CTT) stars.[5] Chamaeleon I X-ray ROSAT source 66 is at RA 11h 17m 36.4-37.9s Dec -77° 04' 27-50", is a CTT, Chamaeleon I No. T56, aka CTT star HM 32.[5]

The Chamaeleon I dark cloud was observed with the Imaging Proportional Counter (IPC) on board the Einstein Observatory for 2.5 h on January 23–24, 1981, identifying some 22 X-ray sources.[6] None of these sources was closer than 8' to 4U 1119–77.

A survey of stars in Chamaeleon I with VLT/SPHERE showed that 13 out of 20 systems showed a protoplanetary disk in polarized scattered light. Systems such as HD 97048, SZ Chamaeleontis, and the WW Chamaeleontis showed morphological structures.[7] HD 97048 also shows a kink in its carbon monoxide gas disk structure, which was interpreted with the presence of a protoplanet inside around the star and inside the disk.[8] Another notable member of Chamaeleon I is OTS 44, which is a planetary-mass object surrounded by a disk.[9][10][11] Another notable object is Cha J11110675-7636030, which has a mass of 3-6 MJ and might be surrounded by a protoplanetary disk.[12]

Chamaeleon II dark cloud

Chamaeleon II and III with Herschel

Chamaeleon II contains the Uhuru source 4U 1302–77. It is close to RXJ 1303.1-7706 at RA 13h 03m 04.70s Dec -77° 06' 55.0", a K7-M0 new WTT.[1] The Chamaeleon II dark cloud contains some 40 X-ray sources.[13] Observation in Chamaeleon II was carried out from September 10 to 17, 1993.[13] Source RXJ 1301.9-7706, a new WTTS candidate of spectral type K1, is closest to 4U 1302–77.[13] Stars in Chamaeleon II have a mean age of 2-6 Myr.[14] This age was later revised to 1-2 Myr. Cha II stars have a larger disk fraction than Cha I in this study.[4] A study with ALMA detected 22 disks around stars in Cha II in continuum.[15] There are also candidate planetary-mass objects in Cha II that are surrounded by disks.[16]

Chamaeleon III dark cloud

"Chamaeleon III appears to be devoid of current star-formation activity."[17] There are two particularly prominent nebulae associated with this area. The smaller is commonly known as the Thumbprint Nebula[7] and the larger The Talon Nebula.[8]

Extended definition

The cloud is sometimes extended with an eastern part,[18] and together with the distinctively long Dark Doodad Nebula (or Musca nebula) to the north the complex is called the Musca-Chamaeleonis Molecular Cloud.[19]

Two foreground associations are found near the Chamaeleon dark clouds. These are named after ε Chamaeleontis (3-5 Myr, distance 110 parsec)[20] and η Chamaeleontis (4-8 Myr, distance 97 parsec).[21][20] The proper motion of these associations are distinct from Chamaeleon I and II, but it is unclear whether the associations are physically connected to the dark clouds.[22] One notable member of the ε Chamaeleontis association is WISEA J120037.79-784508.3, which is one of the closest brown dwarfs that is surrounded by a disk.[23]

  • Infrared view (VIRCam) of the north of Cha I (reflection nebula IC 2631)
    Infrared view (VIRCam) of the north of Cha I (reflection nebula IC 2631)
  • Infrared view (VIRCam) of the middle of Cha I, with Ass Cha T 2-21 (top) and Ced 110 IRS 4 (middle)
    Infrared view (VIRCam) of the middle of Cha I, with Ass Cha T 2-21 (top) and Ced 110 IRS 4 (middle)
  • Infrared view (VIRCam) of the south of Cha I, including HD 97048, DI Chamaeleontis (both at the upper left) and Cha IRN (bright nebula at the lower right)
    Infrared view (VIRCam) of the south of Cha I, including HD 97048, DI Chamaeleontis (both at the upper left) and Cha IRN (bright nebula at the lower right)
  • Another view of the south of Cha I, this time with Hubble
    Another view of the south of Cha I, this time with Hubble
  • Detailed view of the two disks of Ced 110 IRS4 (center) and the surrounding nebula with JWST
    Detailed view of the two disks of Ced 110 IRS4 (center) and the surrounding nebula with JWST
  • DI Chamaeleontis nebula in detail with Hubble
    DI Chamaeleontis nebula in detail with Hubble
  • Detail of the young star Cha IRN with HH909A, with Hubble
    Detail of the young star Cha IRN with HH909A, with Hubble
  • The distinctively thin Doodad nebula can be seen south of the large Coalsack nebula at the top.
    The distinctively thin Doodad nebula can be seen south of the large Coalsack nebula at the top.
  • This is a ROSAT false-color image in X-rays between 500 eV and 1.1 keV of the Chamaeleon I dark cloud. The contours are 100 μm emission from dust measured by the IRAS satellite.
    This is a ROSAT false-color image in X-rays between 500 eV and 1.1 keV of the Chamaeleon I dark cloud. The contours are 100 μm emission from dust measured by the IRAS satellite.

See also

References

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  2. ^ a b c d Feigelson ED, Lawson WA (Oct 2004). "An X-ray census of young stars in the Chamaeleon I North Cloud". Astrophys. J. 614 (10): 267–83. arXiv:astro-ph/0406529. Bibcode:2004ApJ...614..267F. doi:10.1086/423613.
  3. ^ Luhman, K. L. (2007-11-01). "The Stellar Population of the Chamaeleon I Star-forming Region*". The Astrophysical Journal Supplement Series. 173 (1): 104–136. arXiv:0710.3037. Bibcode:2007ApJS..173..104L. doi:10.1086/520114. ISSN 0067-0049.
  4. ^ a b Galli, P. A. B.; Bouy, H.; Olivares, J.; Miret-Roig, N.; Sarro, L. M.; Barrado, D.; Berihuete, A.; Bertin, E.; Cuillandre, J. -C. (2021-02-01). "Chamaeleon DANCe. Revisiting the stellar populations of Chamaeleon I and Chamaeleon II with Gaia-DR2 data". Astronomy and Astrophysics. 646: A46. arXiv:2012.00329. Bibcode:2021A&A...646A..46G. doi:10.1051/0004-6361/202039395. ISSN 0004-6361.
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  6. ^ Feigelson ED, Kriss GA (Mar 1989). "Soft X-ray observations of pre-main-sequence stars in the Chamaeleon dark cloud". Astrophys. J. 338 (3): 262–76. Bibcode:1989ApJ...338..262F. doi:10.1086/167196. hdl:2060/19880002197. S2CID 121939381.
  7. ^ a b Lehtinen K, Mattila K, Schnur G, Prusti T (1995). "The Thumbprint nebula: The distribution of molecular gas and dust in a regular BOK globule". Astronomy and Astrophysics. 295: 487–503. Bibcode:1995A&A...295..487L.
  8. ^ a b Chadwick, Stephen; Cooper, Ian (11 December 2012). Imaging the Southern Sky. Springer. p. 272. ISBN 978-1461447498.
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  11. ^ Joergens, V.; Bonnefoy, M.; Liu, Y.; Bayo, A.; Wolf, S.; Chauvin, G.; Rojo, P. (2013). "OTS 44: Disk and accretion at the planetary border". Astronomy & Astrophysics. 558 (7): L7. arXiv:1310.1936. Bibcode:2013A&A...558L...7J. doi:10.1051/0004-6361/201322432. S2CID 118456052.
  12. ^ Esplin, T. L.; Luhman, K. L.; Faherty, J. K.; Mamajek, E. E.; Bochanski, J. J. (2017-08-01). "A Survey for Planetary-mass Brown Dwarfs in the Chamaeleon I Star-forming Region". The Astronomical Journal. 154 (2): 46. arXiv:1706.00058. Bibcode:2017AJ....154...46E. doi:10.3847/1538-3881/aa74e2. ISSN 0004-6256.
  13. ^ a b c Alcalá JM, Covino E, Sterzik MF, Schmitt JH, Krautter J, Neuhäuser R (Mar 2000). "A ROSAT pointed observation of the Chamaeleon II dark cloud". Astron. Astrophys. 355 (3): 629–38. Bibcode:2000A&A...355..629A.
  14. ^ Spezzi, Loredana; Alcalá, Juan M.; Covino, Elvira; Frasca, Antonio; Gandolfi, Davide; Oliveira, Isa; Chapman, Nicholas; Evans, Neal J., II; Huard, Tracy L.; Jørgensen, Jes K.; Merín, Bruno; Stapelfeldt, Karl R. (2008-06-01). "The Young Population of the Chamaeleon II Dark Cloud". The Astrophysical Journal. 680 (2): 1295–1318. arXiv:0802.4351. Bibcode:2008ApJ...680.1295S. doi:10.1086/587931. ISSN 0004-637X.{{cite journal}}: CS1 maint: multiple names: authors list (link)
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  16. ^ Allers, K. N.; Kessler-Silacci, J. E.; Cieza, L. A.; Jaffe, D. T. (2006-06-01). "Young, Low-Mass Brown Dwarfs with Mid-Infrared Excesses". The Astrophysical Journal. 644 (1): 364–377. arXiv:astro-ph/0602249. Bibcode:2006ApJ...644..364A. doi:10.1086/503355. ISSN 0004-637X.
  17. ^ Yamauchi S, Hamaguchi K, Koyama K, Murakami H (Oct 1998). "ASCA Observations of the Chamaeleon II Dark Cloud". Publ. Astron. Soc. Jpn. 50 (10): 465–74. Bibcode:1998PASJ...50..465Y. doi:10.1093/pasj/50.5.465.
  18. ^ Bonne, L.; Bontemps, S.; Schneider, N.; Clarke, S. D.; Arzoumanian, D.; Fukui, Y.; Tachihara, K.; Csengeri, T.; Guesten, R.; Ohama, A.; Okamoto, R.; Simon, R.; Yahia, H.; Yamamoto, H. (2020-11-26). "Formation of the Musca filament: evidence for asymmetries in the accretion flow due to a cloud–cloud collision". Astronomy & Astrophysics. 644. EDP Sciences: A27. arXiv:2010.12479. Bibcode:2020A&A...644A..27B. doi:10.1051/0004-6361/202038281. ISSN 0004-6361.
  19. ^ Hacar, A.; Kainulainen, J.; Tafalla, M.; Beuther, H.; Alves, J. (2016-02-24). "The Musca cloud: A 6 pc-long velocity-coherent, sonic filament". Astronomy & Astrophysics. 587. EDP Sciences: A97. arXiv:1511.06370. Bibcode:2016A&A...587A..97H. doi:10.1051/0004-6361/201526015. ISSN 0004-6361.
  20. ^ a b Murphy, Simon J.; Lawson, Warrick A.; Bessell, Michael S. (2013-10-01). "Re-examining the membership and origin of the ɛ Cha association". Monthly Notices of the Royal Astronomical Society. 435 (2): 1325–1349. arXiv:1305.4177. Bibcode:2013MNRAS.435.1325M. doi:10.1093/mnras/stt1375. ISSN 0035-8711.
  21. ^ Mamajek, Eric E.; Lawson, Warrick A.; Feigelson, Eric D. (1999-05-01). "The η Chamaeleontis Cluster: A Remarkable New Nearby Young Open Cluster". The Astrophysical Journal. 516 (2): L77–L80. Bibcode:1999ApJ...516L..77M. doi:10.1086/312005. ISSN 0004-637X.
  22. ^ Lopez Martí, B.; Jimenez Esteban, F.; Bayo, A.; Barrado, D.; Solano, E.; Rodrigo, C. (2013-03-01). "Proper motions of young stars in Chamaeleon. I. A Virtual Observatory study of spectroscopically confirmed members". Astronomy and Astrophysics. 551: A46. arXiv:1302.7167. Bibcode:2013A&A...551A..46L. doi:10.1051/0004-6361/201220128. ISSN 0004-6361.
  23. ^ Schutte, Maria C.; Lawson, Kellen D.; Wisniewski, John P.; Kuchner, Marc J.; Silverberg, Steven M.; Faherty, Jacqueline K.; Gagliuffi, Daniella C. Bardalez; Kiman, Rocio; Gagné, Jonathan; Meisner, Aaron; Schneider, Adam C.; Bans, Alissa S.; Debes, John H.; Kovacevic, Natalie; Bosch, Milton K.D.; Luca, Hugo A. Durantini; Holden, Jonathan; Hyogo, Michiharu (2020-08-04). "Discovery of a Nearby Young Brown Dwarf Disk". The Astrophysical Journal. 160 (4): 156. arXiv:2007.15735v2. Bibcode:2020AJ....160..156S. doi:10.3847/1538-3881/abaccd. ISSN 1538-3881. S2CID 220920317.
Quelle: https://en.wikipedia.org/wiki/Chamaeleon_complex