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Journal articles on the topic 'Chamaeleon'

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Author: Grafiati

Published: 10 December 2022

Last updated: 28 January 2023

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1

SEABRA, SOFIA G., INÊS SATAR, and OCTÁVIO S. PAULO. "Microsatellite loci isolated from Chamaeleo chamaeleon." Journal of Genetics 94, S1 (January 4, 2015): 144–47. http://dx.doi.org/10.1007/s12041-014-0463-z.

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2

Fouda, Yosra A., Dalia A. Sabry, and Dalia F. Abou-Zaid. "Functional Anatomical, Histological and Ultrastructural Studies of three Chameleon Species: Chamaeleo Chamaeleon, Chamaeleo Africanus, and Chamaeleon Vulgaris." International Journal of Morphology 33, no. 3 (September 2015): 1045–53. http://dx.doi.org/10.4067/s0717-95022015000300038.

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3

Dimaki, Maria, Anna Hundsdörfer, and Uwe Fritz. "Eastern Mediterranean chameleons (Chamaeleo chamaeleon, Ch. africanus) are distinct." Amphibia-Reptilia 29, no. 4 (2008): 535–40. http://dx.doi.org/10.1163/156853808786230415.

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AbstractBased on mitochondrial 16S rRNA sequences, we suggest that the founder individuals of the introduced Greek population of Chamaeleo africanus originated in the Nile Delta region of Egypt. In Ch. chamaeleon, we discovered in the eastern Mediterranean new 16S rRNA haplotypes, being highly distinct from previously published western Mediterranean haplotypes. Eastern Mediterranean haplotypes were found in samples from northern Syria, Cyprus, Crete, Samos, Malta and Tunisia. The occurrence of an eastern Mediterranean haplotype in Tunisia and of distinct haplotypes in Morocco could argue for a phylogeographic break in northwestern Africa.

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4

Eshar, David, Roi Lapid, and Valerie Head. "Transilluminated Jugular Blood Sampling in the Common Chameleon (Chamaeleo chamaeleon)." Journal of Herpetological Medicine and Surgery 28, no. 1 (January 1, 2018): 19. http://dx.doi.org/10.5818/17-10-127.1.

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5

CUADRADO, MARIANO, JOSÉ MARTÍN, and PILAR LÓPEZ. "Camouflage and escape decisions in the common chameleon Chamaeleo chamaeleon." Biological Journal of the Linnean Society 72, no. 4 (April 2001): 547–54. http://dx.doi.org/10.1111/j.1095-8312.2001.tb01337.x.

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6

Sidhom, Marwa, Khaled Said, Noureddine Chatti, Fabio M. Guarino, Gaetano Odierna, Agnese Petraccioli, Orfeo Picariello, and Marcello Mezzasalma. "Karyological and bioinformatic data on the common chameleon Chamaeleo chamaeleon." Data in Brief 30 (June 2020): 105640. http://dx.doi.org/10.1016/j.dib.2020.105640.

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7

Hartigan, Patrick. "New T Tauri stars in Chamaeleon I and Chamaeleon II." Astronomical Journal 105 (April 1993): 1511. http://dx.doi.org/10.1086/116530.

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8

Baran, İbrahim, Max Kasparek, and Mehmet Öz. "On the occurrence and status of the Chameleon,Chamaeleo chamaeleon, in Turkey." Zoology in the Middle East 2, no. 1 (January 1988): 52–56. http://dx.doi.org/10.1080/09397140.1988.10637558.

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9

Cuadrado, Mariano. "Mate guarding and social mating system in male common chameleons (Chamaeleo chamaeleon)." Journal of Zoology 255, no. 4 (February 28, 2006): 425–35. http://dx.doi.org/10.1017/s0952836901001510.

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10

Díaz-Paniagua, Carmen. "Effect of cold temperature on the length of incubation of Chamaeleo chamaeleon." Amphibia-Reptilia 28, no. 3 (2007): 387–92. http://dx.doi.org/10.1163/156853807781374782.

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AbstractCommon chameleon eggs spend the first months of incubation at low temperatures. I incubated eggs of different clutches at 25°C in four treatments with respectively 0, 84, 119 and 149 days of initial cold period (at 14°C). Treatments with longer cold periods had longer total incubation but shorter periods of incubation at 25°C. Eggs which did not experience initial cold period showed low synchronization at hatching. Hatchling body mass and length were influenced by the length of the cold period. Hatchlings were largest and heaviest for cold periods of intermediate length which had similar duration than the cold period experienced by eggs in nature. These results suggest that the cold torpor period of Common chameleon embryos contributes to optimization of development and growth, and synchronizes hatching.

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11

Voirin, Jordan, Carlo F. Manara, and Timo Prusti. "A revised estimate of the distance to the clouds in the Chamaeleon complex using the Tycho–Gaia Astrometric Solution." Astronomy & Astrophysics 610 (February 2018): A64. http://dx.doi.org/10.1051/0004-6361/201731153.

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Context. The determination of the distance to dark star-forming clouds is a key parameter to derive the properties of the cloud itself and of its stellar content. This parameter is still loosely constrained even in nearby star-forming regions. Aim. We want to determine the distances to the clouds in the Chamaeleon-Musca complex and explore the connection between these clouds and the large-scale cloud structures in the Galaxy. Methods. We used the newly estimated distances obtained from the parallaxes measured by the Gaia satellite and included in the Tycho–Gaia Astrometric Solution catalog. When known members of a region are included in this catalog we used their distances to infer the distance to the cloud. Otherwise, we analyzed the dependence of the color excess on the distance of the stars and looked for a turn-on of this excess, which is a proxy of the position of the front-edge of the star-forming cloud. Results. We are able to measure the distance to the three Chamaeleon clouds. The distance to Chamaeleon I is 179-10-10+11+11pc, where the quoted uncertainties are statistical and systematic uncertainties, respectively, ~20 pc further away than previously assumed. The Chamaeleon II cloud is located at the distance of 181-5-10+6+11pc, which agrees with previous estimates. We are able to measure for the first time a distance to the Chamaeleon III cloud of 199-7-11+8+12pc. Finally, the distance of the Musca cloud is smaller than 603603-70-92+91+133 pc. These estimates do not allow us to distinguish between the possibility that the Chamaeleon clouds are part of a sheet of clouds parallel to the Galactic plane, or perpendicular to it. Conclusions. We measured a larger distance to the Chamaeleon I cloud than assumed in the past, confirmed the distance to the Chamaeleon II region, and measured for the first time the distance to the Chamaleon III cloud. These values are consistent with the scenario in which the three clouds are part of a single large-scale structure. Gaia Data Release 2 will allow us to put more stringent constraints on the distances to these clouds by giving us access to parallax measurements for a larger number of members of these regions.

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12

MIRALDO, ANDREIA, ISABEL PINTO, JOÃO PINHEIRO, INÊS ROSÁRIO, MARTA MAYMONE, and OCTÁVIO S. PAULO. "NOTE: DISTRIBUTION AND CONSERVATION OF THE COMMON CHAMAELEO CHAMAELEON, IN ALGARVE, SOUTHERN PORTUGAL." Israel Journal of Zoology 51, no. 2 (July 1, 2005): 157–64. http://dx.doi.org/10.1560/ev2y-9e2f-5dly-p00n.

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13

Cuadrado, Mariano, and Jon Loman. "The Effects of Age and Size on Reproductive Timing in Female Chamaeleo chamaeleon." Journal of Herpetology 33, no. 1 (March 1999): 6. http://dx.doi.org/10.2307/1565536.

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14

Andrews, Robin M., Carmen Díaz‐Paniagua, Adolfo Marco, and Alexandre Portheault. "Developmental Arrest during Embryonic Development of the Common Chameleon (Chamaeleo chamaeleon) in Spain." Physiological and Biochemical Zoology 81, no. 3 (May 2008): 336–44. http://dx.doi.org/10.1086/529449.

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15

Keren-Rotem, Tammy, Amos Bouskila, and Eli Geffen. "Ontogenetic habitat shift and risk of cannibalism in the common chameleon (Chamaeleo chamaeleon)." Behavioral Ecology and Sociobiology 59, no. 6 (November 24, 2005): 723–31. http://dx.doi.org/10.1007/s00265-005-0102-z.

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16

Mouhsine, Touria, Fethi Amani, and Abdeslam Mikdad. "Agama bibronii (Sauria : Agamidae) et Chamaeleo chamaeleon (Sauria : Chamaeleonidae) d’Ifri n’Ammar (Rif oriental, Maroc)." Quaternaire, no. 33/3 (September 1, 2022): 151–68. http://dx.doi.org/10.4000/quaternaire.16948.

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17

Franco, G. A. P. "The Chamaeleon Dark Clouds Complex: Preliminary Analysis of the Colour Excesses E(b-y) Towards the Selected Area 203." International Astronomical Union Colloquium 120 (1989): 133. http://dx.doi.org/10.1017/s0252921100023642.

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The Chamaeleon dark clouds form a large complex of interstellar obscuring material situated at ≈ 15° below the galactic plane. Although it is accepted as being one of the closest low-mass star formation region to the Sun, its distance has been debated issues. The proposed distance is in general dependent on the value assumed for the ratio of total-to-selective extinction, which in the Chamaeleon clouds has proved controversial, leading to distances estimates ranging from 115 to 215 pc.

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18

Henning, Th, and E. Thamm. "Cold dust around chamaeleon stars." Astrophysics and Space Science 212, no. 1-2 (February 1994): 215–20. http://dx.doi.org/10.1007/bf00984525.

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19

Liszt, H., M. Gerin, and I. Grenier. "Standing in the shadow of dark gas: ALMA observations of absorption from dark CO in the molecular dark neutral medium of Chamaeleon." Astronomy & Astrophysics 627 (July 2019): A95. http://dx.doi.org/10.1051/0004-6361/201935436.

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Context. We previously detected 89.2 GHz J = 1−0 HCO+ absorption in 12 directions lacking detected CO emission in the outskirts of the Chamaeleon cloud complex and toward one sightline with integrated CO emission WCO = 2.4 K km s−1. Eight sightlines had a much larger mean column density of dark neutral medium (DNM) – gas not represented in HI or CO emission – and were found to have much higher mean molecular column density. The five other sightlines had little or no DNM and were found to have much smaller but still detectable N(HCO+). Aims. To determine the CO column density along previously observed Chamaeleon sightlines and to determine why CO emission was not detected in directions where molecular gas is present. Methods. We took 12CO J = 1−0 absorption profiles toward five sightlines having higher DNM and HCO+ column densities and one sightline with smaller N(DNM) and N(HCO+). We converted the integrated HCO+ optical depths to N(H2) in the weak-excitation limit using N(HCO+)/N(H2) = 3 × 10−9 and converted the integrated CO optical depths ϒCO to CO column density using the relationship N(CO) = 1.861 × 1015 cm−2 ϒCO1.131 found along comparable lines of sight that were previously studied in J = 1−0 and J = 2−1 CO absorption and emission. Results. CO absorption was detected along the five sightlines in the higher-DNM group, with CO column densities 4 × 1013 cm−2≲ N(CO) ≲1015 cm−2 that are generally below the detectability limit of CO emission surveys. Conclusions. In the outskirts of the Chamaeleon complex, the presence of molecular DNM resulted primarily from small CO column densities at the onset of CO formation around the HI/H2 transition in diffuse molecular gas. CO relative abundances N(CO)/H2 ≲2 × 10−6 in the outskirts of Chamaeleon are comparable to those seen in UV absorption toward early-type stars, including in Chamaeleon.

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20

Bennis, M., C. Versaux-Botteri, J. Repérant, and J. A. Armengol. "Calbindin, Calretinin and Parvalbumin Immunoreactivity in the Retina of the Chameleon (Chamaeleo chamaeleon)." Brain, Behavior and Evolution 65, no. 3 (2005): 177–87. http://dx.doi.org/10.1159/000083683.

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21

Hassan Nabih Mhanna, Nahla Ibrahim, Aroub Al-Masri, Hassan Nabih Mhanna, Nahla Ibrahim, Aroub Al-Masri. "Modification of preparing the blood diluting solution method and studying the blood cell counts of some Syrian Reptiles and Amphibians using the modified method: تعديل طريقة تحضير المحلول المخفف للدم ودراسة تعداد الخلايا الدموية عند بعض أنواع الزواحف والبرمائيات السورية بالطريقة المعدلة." Journal of natural sciences, life and applied sciences 6, no. 1 (March 27, 2022): 25–35. http://dx.doi.org/10.26389/ajsrp.c071221.

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The study aimed to test the validity of the results of the modified blood diluted solution by Natt-Herrick method in order to study the complete blood count of different blood cells in two species of amphibians (Pseudepidalea viridis, Hyla savignyi) in addition to five species of reptiles (Testudo graeca, Chamaeleo chamaeleon recticrista, Ophisops elegans, Lacerta media, Phoenicolacerta laevis) by replacing methyl violet 2B dye included in its composition with methyl violet 10B , where our results were compared with the values of previous studies, there is no any significant differences between the modifying methods compare with the others references using the original methods as the results were within or close to normal limits, and thus this method can be approved.According to the values obtained in this paper, the highest number of red and white blood cells was in L. media, the lowest number of red blood cells was in T. graeca, and the lowest number of white blood cells was in O. elegans.

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22

Roccatagliata, V., G. G. Sacco, E. Franciosini, and S. Randich. "The double population of Chamaeleon I detected by Gaia DR2." Astronomy & Astrophysics 617 (September 2018): L4. http://dx.doi.org/10.1051/0004-6361/201833890.

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Context. Chamaeleon I represents an ideal laboratory to study the cluster formation in a low-mass environment. Recently, two sub-clusters spatially located in the northern and southern parts of Chamaeleon I were found with different ages and radial velocities. Aims. In this Letter we report new insights into the structural properties, age, and distance of Chamaeleon I based on the astrometric parameters from Gaia data release 2 (DR2). Methods. We identified 140 sources with a reliable counterpart in the Gaia DR2 archive. We determined the median distance of the cluster using Gaia parallaxes and fitted the distribution of parallaxes and proper motions assuming the presence of two clusters. We derived the probability of each single source of belonging to the northern or southern sub-clusters, and compared the HR diagram of the most probable members to pre-main sequences isochrones. Results. The median distance of Chamaeleon I is ~190 pc. This is consistent with the revised estimate using the Tycho-Gaia Astrometric Solution, but it is about 20 pc larger than the value commonly adopted in the literature. From a Kolmogorov–Smirnov test of the parallaxes and proper-motion distributions we conclude that the northern and southern clusters do not belong to the same parent population. The northern population has a distance dN = 192.7+0.4−0.4pc, while the southern one dS = 186.5+0.7−0.7pc. The two sub-clusters appear coeval, at variance with literature results, and most of the sources are younger than 3 Myr. The northern cluster is more elongated and extends towards the southern direction partially overlapping with the more compact cluster located in the south. A hint of a relative rotation between the two sub-clusters is also found.

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23

Cuadrado, Mariano, Isabel Molina-Prescott, and Luis Flores. "Comparison between tail and jugular venipuncture techniques for blood sample collection in common chameleons (Chamaeleo chamaeleon)." Veterinary Journal 166, no. 1 (July 2003): 93–97. http://dx.doi.org/10.1016/s1090-0233(02)00253-8.

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24

Blasco Ruiz, Manuel, J. L. Pérez-Botec, and J. M. Cabo. "Algunas reflexiones sobre el declive del camaleón común (Chamaeleo chamaeleon, L. 1758) en la Península Ibérica." Mediterránea. Serie de Estudios Biológicos, no. 17 (2000): 35–44. http://dx.doi.org/10.14198/mdtrra2000.17.04.

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25

Ouafa, Boudebia, Medila Ifriqya, and Toumi Ikram. "Evaluation of Biological Activities of Chamaeleo chamaeleon : A Reptile Used in Traditional Folk Medicine in Algeria." Journal of Biochemical Technology 13, no. 4 (2022): 15–19. http://dx.doi.org/10.51847/ed9gjaf2j7.

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26

Lawson, Warrick A., and Lisa A. Crause. "Rotational and Candidate-Eclipsing-Binary Light Curves for Pre-Main-Sequence Stars in the Chamaeleon I Star-Forming Cloud." Publications of the Astronomical Society of Australia 26, no. 1 (2009): 31–36. http://dx.doi.org/10.1071/as08018.

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AbstractWe present the results of a photometric survey for variability in ten X-ray-emitting low-mass stars in the Chamaeleon region. Eight of the stars we observed are bona fide pre-main-sequence members of the ∼2 Myr-old Chamaeleon I star-forming cloud. The other two stars are young with high levels of relative X-ray emission, but with discordant proper motions they are probable non-members of the cloud. In six of the stars we monitored, periodic variations on timescales of 2.5–11.5 d were detected, that we ascribe to stellar rotation and the presence of cool starspots. Two other stars, CHXR 20 and CHXR 85, show large amplitude variations at visual and near-infrared wavelengths and are candidate eclipsing binaries. Compared to the rotational properties of low-mass stars in the ≈8 Myr-old η Chamaeleontis cluster, we find that the older η Chamaeleontis stars have several times higher surface specific angular momentum than the younger Chamaeleon I stars. The apparent increase in angular momentum between ∼2 and 8 Myr might be due to changes in stellar internal structure as the stars evolve, or evidence for a different rotational history between members of the two star-forming regions.

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27

Spezzi, L., N. L. J. Cox, T. Prusti, B. Merín, Á. Ribas, C. Alves de Oliveira, E. Winston, et al. "TheHerschelGould Belt Survey in Chamaeleon II." Astronomy & Astrophysics 555 (July 2013): A71. http://dx.doi.org/10.1051/0004-6361/201321444.

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28

Chen, Wen Ping, and J. A. Graham. "Duplicity Among Young Stars in Chamaeleon." International Astronomical Union Colloquium 135 (1992): 60–62. http://dx.doi.org/10.1017/s0252921100006114.

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AbstractWe present infrared imaging results of young stars in Cha I and II clouds that show either extended structure or a nearby neighboring star. Both regions appear to show high incidence rates of pairs. After excluding possible background stars, as judged from their brightness, color, or the local stellar surface number density, a frequency of 10% is deduced for binaries in Cha I with separations 2-5″, which is comparable to that in Taurus and to that of main sequence field stars.

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29

Schmidt, T. O. B., R. Neuhäuser, N. Vogt, A. Seifahrt, T. Roell, and A. Bedalov. "Confirmation of the binary status of Chamaeleon Hα 2 – a very young low-mass binary in Chamaeleon." Astronomy & Astrophysics 484, no. 2 (March 19, 2008): 413–18. http://dx.doi.org/10.1051/0004-6361:20078381.

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30

Sato, F., J. B. Whiteoak, R. E. Otrupcek, and M. Shimizu. "Cold HI Gas in the Chamaeleon I Dark Cloud Region." Publications of the Astronomical Society of Australia 9, no. 1 (1991): 145. http://dx.doi.org/10.1017/s1323358000025315.

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31

Ribas, Á., B. Merín, H. Bouy, C. Alves de Oliveira, D. R. Ardila, E. Puga, Á. Kóspál, et al. "Identification of transitional disks in Chamaeleon withHerschel." Astronomy & Astrophysics 552 (April 2013): A115. http://dx.doi.org/10.1051/0004-6361/201220960.

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32

López Martí, Belén, Francisco Jiménez-Esteban, Amelia Bayo, David Barrado, Enrique Solano, Hervé Bouy, and Carlos Rodrigo. "Proper motions of young stars in Chamaeleon." Astronomy & Astrophysics 556 (August 2013): A144. http://dx.doi.org/10.1051/0004-6361/201321217.

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33

Hughes, Joanne, and Patrick Hartigan. "Chamaeleon II - Distance determination and HR diagram." Astronomical Journal 104 (August 1992): 680. http://dx.doi.org/10.1086/116263.

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34

Lopez Martí, B., F. Jimenez Esteban, A. Bayo, D. Barrado, E. Solano, and C. Rodrigo. "Proper motions of young stars in Chamaeleon." Astronomy & Astrophysics 551 (February 19, 2013): A46. http://dx.doi.org/10.1051/0004-6361/201220128.

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35

Gahm, G. F., K. Lehtinen, P. Carlqvist, J. Harju, M. Juvela, and K. Mattila. "The threaded molecular clumps of Chamaeleon III." Astronomy & Astrophysics 389, no. 2 (June 27, 2002): 577–88. http://dx.doi.org/10.1051/0004-6361:20020452.

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36

Gómez, M., and D. Mardones. "Near-Infrared Spectra of Chamaeleon I Stars." Astronomical Journal 125, no. 4 (April 2003): 2134–55. http://dx.doi.org/10.1086/368391.

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37

Toriseva, M., L. Bronfman, and K. Mattila. "C18O in the Chamaeleon I dark cloud." Astrophysics and Space Science 171, no. 1-2 (September 1990): 219–21. http://dx.doi.org/10.1007/bf00646851.

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38

Köhler, Rainer, and Wolfgang Brandner. "Multiplicity in T and OB Associations." Symposium - International Astronomical Union 200 (2001): 147–54. http://dx.doi.org/10.1017/s0074180900225163.

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The results of binary surveys among T Tauri stars in the T associations Taurus-Auriga and Chamaeleon, and in the OB association Scorpius-Centaurus are summarized, and implications on our understanding on the formation of binary and multiple systems are discussed.

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39

Cuadrado, Mariano. "The influence of female size on the extent and intensity of mate guarding by males in Chamaeleo chamaeleon." Journal of Zoology 246, no. 3 (November 1998): 351–58. http://dx.doi.org/10.1111/j.1469-7998.1998.tb00165.x.

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40

Lev-Ari, Tidhar, Avichai Lustig, Hadas Ketter-Katz, Yossi Baydach, and Gadi Katzir. "Avoidance of a moving threat in the common chameleon (Chamaeleo chamaeleon): rapid tracking by body motion and eye use." Journal of Comparative Physiology A 202, no. 8 (June 24, 2016): 567–76. http://dx.doi.org/10.1007/s00359-016-1106-z.

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41

McGregor, P. J., T. E. Harrison, J. H. Hough, and J. A. Bailey. "Infrared polarimetry in the Chamaeleon I dark cloud." Monthly Notices of the Royal Astronomical Society 267, no. 3 (April 1, 1994): 755–65. http://dx.doi.org/10.1093/mnras/267.3.755.

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42

Belloche, A., F. Schuller, B. Parise, Ph André, J. Hatchell, J. K. Jørgensen, S. Bontemps, A. Weiß, K. M. Menten, and D. Muders. "The end of star formation in Chamaeleon I?" Astronomy & Astrophysics 527 (February 14, 2011): A145. http://dx.doi.org/10.1051/0004-6361/201015733.

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43

Ikeda, Norio, Yoshimi Kitamura, Satoshi Takita, Munetaka Ueno, Toyoaki Suzuki, Akiko Kawamura, and Hidehiro Kaneda. "FAR-INFRARED IMAGING OBSERVATIONS OF THE CHAMAELEON REGION." Astrophysical Journal 745, no. 1 (December 28, 2011): 48. http://dx.doi.org/10.1088/0004-637x/745/1/48.

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44

Luhman, K. L., J. C. Wilson, W. Brandner, M. F. Skrutskie, M. J. Nelson, J. D. Smith, D. E. Peterson, M. C. Cushing, and E. Young. "Discovery of a Young Substellar Companion in Chamaeleon." Astrophysical Journal 649, no. 2 (October 2006): 894–99. http://dx.doi.org/10.1086/506517.

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45

Moeller, Holly V., and Matthew D. Johnson. "Preferential Plastid Retention by the Acquired PhototrophMesodinium chamaeleon." Journal of Eukaryotic Microbiology 65, no. 2 (August 7, 2017): 148–58. http://dx.doi.org/10.1111/jeu.12446.

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46

Manara, C. F., D. Fedele, G. J. Herczeg, and P. S. Teixeira. "X-Shooter study of accretion in Chamaeleon I." Astronomy & Astrophysics 585 (January 2016): A136. http://dx.doi.org/10.1051/0004-6361/201527224.

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47

Feigelson, E. D., S. Casanova, T. Montmerle, and J. Guibert. "ROSAT observations of the Chamaeleon star forming cloud." Advances in Space Research 13, no. 12 (December 1993): 311–14. http://dx.doi.org/10.1016/0273-1177(93)90128-x.

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48

Imre, Sedat, Aysel Öztunç, Turgay Çelik, and Hildebert Wagner. "Isolation of Caffeine from the Gorgonian Paramuricea chamaeleon." Journal of Natural Products 50, no. 6 (November 1987): 1187. http://dx.doi.org/10.1021/np50054a040.

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Manara, C. F., L. Testi, G. J. Herczeg, I. Pascucci, J. M. Alcalá, A. Natta, S. Antoniucci, et al. "X-shooter study of accretion in Chamaeleon I." Astronomy & Astrophysics 604 (August 2017): A127. http://dx.doi.org/10.1051/0004-6361/201630147.

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Yamauchi, Shigeo, Kenji Hamaguchi, Katsuji Koyama, and Hiroshi Murakami. "ASCA Observations of the Chamaeleon II Dark Cloud." Publications of the Astronomical Society of Japan 50, no. 5 (October 1, 1998): 465–74. http://dx.doi.org/10.1093/pasj/50.5.465.

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