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18 results for “Chamaeleon”
Far-infrared to millimeter data of protoplanetary disks: dust growth in the Taurus, Ophiuchus, and Chamaeleon I star-forming regions
<p>This repository contains the data set presented in the manuscript "Far-infrared to millimeter data of protoplanetary disks: dust growth in the Taurus, Ophiuchus, and Chamaeleon I star-forming regions" (Ribas et al. 2017), and includes a table with several sample properties (e.g. stellar properties, Herschel photometry, different spectral indices), spectral energy distributions, Spitzer/IRS and Herschel/SPIRE spectra, the median SEDs of Taurus, Ophiuchus and Chamaeleon I, and the Herschel maps used.</p> <p>ERRATUM: three Chamaeleon I sources (Hn 11, T45a, and WY Cha) were mislabeled in the original version of the manuscript, which resulted in their names, stellar parameters, extinction values, infrared slopes, and silicate feature properties being assigned to incorrect coordinates. Because the photometry and spectroscopy presented in the original article is coordinate- based, the provided SEDs and spectra were also missmatched: the data files labeled Hn 11 in the original manuscript correspond to T45a, those labeled T45a correspond to WY Cha, and those labeled WY Cha correspond to Hn 11. Additionally, due to a mislabeling issue in Manoj et al. 2011, the source formerly labeled UX Cha is actually CHSM 8284. Therefore, stellar parameters and photometry labeled UX Cha in our original manuscript correspond to CHSM 8284 The updated version of the repository fixes the issue both in the sample.csv file and in the individual SED and Spitzer/IRS spectra files. The published erratum is available here: <a href="https://iopscience.iop.org/article/10.3847/1538-4357/abb66e">https://iopscience.iop.org/article/10.3847/1538-4357/abb66e</a>.</p>
PENELLOPE - X-Shooter spectra of targets in the Chamaeleon I, eta Cha, and eps Cha regions
<p>Spectra of the targets in the Chamaeleon I, eps-Cha and eta-Cha regions observed with the VLT/X-Shooter spectrograph. These spectra are part of the PENELLOPE Large Program and are obtained close in time to the HST/ULLYSES spectra of the same targets. </p><p>Here one can find the 1D absolute flux-calibrated and telluric corrected spectra. Each object is observed simultaneously in three arms, UVB, VIS, and NIR, and the spectrum of each arm is saved in one file. The units of the spectra are: Flux [erg/s/cm2/nm]; Wavelength [nm]. In some cases, multiple observations for one target have been taken.</p><p>Data are public, we ask to ask to the authors of this release, who contributed to the observation preparation and data reduction, whether they want to be included in any publication using these data. The data reduction procedure is presented in Manara et al. (2021). Please quote this paper in any related publication. Please contact Carlo Manara for estimates of the stellar and accretion properties of these targets based on this data. </p><p>For questions or comments please contact Carlo Manara, cmanara@eso.org</p>
Figure 3 in The two-horned chamaeleons of East Africa
Figure 3. Parsimony analysis based on ND2 gene sequences. Single shortest tree. Values above branches are bootstrap value with gaps treated as missing or 5th base, below branches ML bootstrap. The partial tree on the right side shows the alternative placement of K. fischeri supported by the ML analysis.
Figure 1 in The two-horned chamaeleons of East Africa
Figure 1. Map of the Eastern Arc Range. Open triangles indicate our collection or observation stations. The distribution of each discussed two-horned species, as derived from the literature and our own observations, is indicated with a black line.
PENELLOPE - UVES spectra of targets in the Lupus and Chamaeleon regions observed in 2021
<p>Spectra of the targets in the Chamaeleon I and Lupus regions observed with the VLT/UVES spectrograph in June-July 2021. These spectra are part of the PENELLOPE Large Program and are obtained close in time to the HST/ULLYSES spectra of the same targets. </p> <p>Here one can find the 1D flux-calibrated and telluric corrected spectra. Each object is observed simultaneously in three arms, blue, redu, redl, and the spectrum of each arm is saved in one file. The units of the spectra are: Flux [10**-16 erg/s/cm2/AA]; Wavelength [AA]. Each object is typically observed 3 times, the spectra are thus labelled as ep1, ep2, ep3.</p> <p>Data are public, we ask to ask to the authors of this release, who contributed to the observation preparation and data reduction, whether they want to be included in any publication using these data. The data reduction procedure is presented in Manara et al. (2021). Please quote this paper in any related publication. Please contact Carlo Manara for estimates of the stellar and accretion properties of these targets based on the corresponding X-Shooter data, and Antonio Frasca for stellar properties based on this data. </p> <p>For questions or comments please contact Carlo Manara, cmanara@eso.org</p>
PENELLOPE - X-Shooter spectra of targets in the Lupus and Chamaeleon regions observed in 2021
<p>Spectra of the targets in the Lupus, Chamaeleon I and eta-Cha regions observed with the VLT/X-Shooter spectrograph in May-August 2021. These spectra are part of the PENELLOPE Large Program and are obtained close in time to the HST/ULLYSES spectra of the same targets. </p> <p>Here one can find the 1D absolute flux-calibrated and telluric corrected spectra. Each object is observed simultaneously in three arms, UVB, VIS, and NIR, and the spectrum of each arm is saved in one file. The units of the spectra are: Flux [erg/s/cm2/nm]; Wavelength [nm]. In some cases, multiple observations for one target have been taken.</p> <p>Data are public, we ask to ask to the authors of this release, who contributed to the observation preparation and data reduction, whether they want to be included in any publication using these data. The data reduction procedure is presented in Manara et al. (2021). Please quote this paper in any related publication. Please contact Carlo Manara for estimates of the stellar and accretion properties of these targets based on this data. </p> <p>For questions or comments please contact Carlo Manara, cmanara@eso.org</p>
PENELLOPE - ESPRESSO spectra of targets in the Lupus and Chamaeleon I regions observed in 2021
<p>Spectra of the targets in the Lupus and Chamaeleon I regions observed with the VLT/ESPRESSO spectrograph in May-August 2021. These spectra are part of the PENELLOPE Large Program and are obtained close in time to the HST/ULLYSES spectra of the same targets. </p> <p>Here one can find the 1D flux-calibrated and telluric corrected spectra. The units of the spectra are: Flux [erg/s/cm2/AA]; Wavelength [AA]. Each object is typically observed 3 times, the spectra are thus labelled as ep1, ep2, ep3. </p> <p>Data are public, we ask to ask to the authors of this release, who contributed to the observation preparation and data reduction, whether they want to be included in any publication using these data. The data reduction procedure is presented in Manara et al. (2021). Please quote this paper in any related publication. Please contact Carlo Manara for estimates of the stellar and accretion properties of these targets based on the corresponding X-Shooter data, and Antonio Frasca for stellar properties based on this data. </p> <p>For questions or comments please contact Carlo Manara, cmanara@eso.org</p>
Data from: Alternative mating tactics in male chameleons (Chamaeleo chamaeleon) are evident in both long-term body color and short-term courtship pattern
Alternative mating tactics in males of various taxa are associated with body color, body size, and social status. Chameleons are known for their ability to change body color following immediate environmental or social stimuli. In this study, we examined whether the differential appearance of male common chameleon during the breeding season is indeed an expression of alternative mating tactics. We documented body color of males and used computer vision techniques to classify images of individuals into discrete color patterns associated with seasons, individual characteristics, and social contexts. Our findings revealed no differences in body color and color patterns among males during the non-breeding season. However, during the breeding season males appeared in several color displays, which reflected body size, social status, and behavioral patterns. Furthermore, smaller and younger males resembled the appearance of small females. Consequently, we suggest that long-term color change in males during the breeding season reflects male alternative mating tactics. Upon encounter with a receptive female, males rapidly alter their appearance to that of a specific brief courtship display, which reflects their social status. The females, however, copulated indiscriminately in respect to male color patterns. Thus, we suggest that the differential color patterns displayed by males during the breeding season are largely aimed at inter-male signaling.
FIGURE 9. Haplosyllis chamaeleon. A in A taxonomic revision of the genus Haplosyllis Langerhans, 1887 (Polychaeta: Syllidae: Syllinae)
FIGURE 9. Haplosyllis chamaeleon. A—anterior chaeta; B—midbody chaetae; C—posterior chaetae. Scale bar 20 Μm.
FIGURE. Phlegmariurus chamaeleon—(Costa Rica: Herrera et al. 6392, MO). A. growth habit. A1. Apical sporangiate division. in The Lycopodiaceae of Panamá
FIGURE. Phlegmariurus chamaeleon—(Costa Rica: Herrera et al. 6392, MO). A. growth habit. A1. Apical sporangiate division.
Data from: Alternative mating tactics in male chameleons (Chamaeleo chamaeleon) are evident in both long-term body color and short-term courtship pattern
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Figure 1 from: Pinzón-Florián O (2020) First report on the gall wasp Ophelimus near migdanorum (Hymenoptera, Eulophidae) and its parasitoid Closterocerus chamaeleon (Hymenoptera, Eulophidae) in Eucalyptus globulus in Bogotá, Colombia. ZooKeys 902: 151-156. https://doi.org/10.3897/zookeys.902.39213
Figure 1 Different stages of gall development on E. globulus foliage. A Initial stage B fully developed galls C fully developed galls in the petiole. Scale bar: 1 mm.
Figure 3 from: Pinzón-Florián O (2020) First report on the gall wasp Ophelimus near migdanorum (Hymenoptera, Eulophidae) and its parasitoid Closterocerus chamaeleon (Hymenoptera, Eulophidae) in Eucalyptus globulus in Bogotá, Colombia. ZooKeys 902: 151-156. https://doi.org/10.3897/zookeys.902.39213
Figure 3 Closterocerus chamaeleon emerged from mature E. globulus leaves infested by Ophelimus sp. A Dorsal view B lateral view. Scale bars: 1 mm.
Figure 2 in The two-horned chamaeleons of East Africa
Figure 2. Parsimony analysis based on 12S/16S gene sequences. Strict consensus of three shortest trees. Values above branches are bootstrap value with gaps treated as missing or 5th base, below branches ML bootstrap.
Figures 1-2 from: Burks RA, Mottern JL, Pownall NG, Waterworth R, Paine TD (2015) First record of Closterocerus chamaeleon, parasitoid of the Eucalyptus Gall Wasp Ophelimus maskelli (Hymenoptera, Chalcidoidea, Eulophidae), in the New World. ZooKeys 504: 149-152. https://doi.org/10.3897/zookeys.504.9728
Figures 1-2 - 1 Closterocerus chamaeleon reared from Ophelimus maskelli gall collected on UCR campus; body, lateral view. UCRCENT00412686 2 Antennae and head of the same specimen, oblique anteromedial view.
Figure 2 from: Pinzón-Florián O (2020) First report on the gall wasp Ophelimus near migdanorum (Hymenoptera, Eulophidae) and its parasitoid Closterocerus chamaeleon (Hymenoptera, Eulophidae) in Eucalyptus globulus in Bogotá, Colombia. ZooKeys 902: 151-156. https://doi.org/10.3897/zookeys.902.39213
Figure 2 Ophelimus sp. Body in lateral view. Scale bar: 1 mm.
ROSAT All-Sky Survey: Chamaeleon Star Forming Region Study
This catalog contains a source list derived from observations of the ROSAT all-sky survey (RASS) in the direction of the Chamaeleon star-forming region cloud complex, as well as spectroscopic identifications for the detected X-ray sources. The main purpose of this identification program was the search for low-mass pre-main sequence stars. Sixteen previously known PMS stars were detected with high confidence by ROSAT: eight are classical T Tauri stars and eight are weak-line T Tauri stars. Seventy-seven new weak-line T Tauri stars were identified on the basis of the presence of strong Li 6707 Angstrom absorption, a spectral type later than F0, and chromospheric emission. In addition, 6 new dKe-dMe candidates were found among the RASS sources. Coordinates and count rates are given for all of the X-ray sources. This online catalog was created by the HEASARC in September 1999 based on a machine-readable table obtained from the ADC/CDS data centers (J/A+AS/114/109). This is a service provided by NASA HEASARC .
Chamaeleon I North Cloud Chandra X-Ray Point Source Catalog
This table contains the Chamaeleon (Cha) I North Cloud Chandra X-Ray point source catalog. Sensitive X-ray imaging surveys provide a new and effective tool to establish the census of pre-main-sequence (PMS) stars in nearby young stellar clusters. A deep Chandra X-Ray Observatory (CXO) observation of PMS stars in the Chamaeleon I North cloud achieved a limiting total-band X-ray luminosity of log L<sub>t</sub> ~ 10<sup>27</sup> ergs/s (0.5 - 8 keV band) in a 0.8 x 0.8 pc<sup>2</sup> region. Of the 107 X-ray sources, 37 are associated with Galactic stars, of which 27 are previously recognized cloud members. These include 3 PMS brown dwarfs: the protostellar brown dwarf ISO 192 has a particularly high level of magnetic activity. Follow-up optical photometry and spectroscopy establish that 9-10 of the Chandra sources are probably magnetically active background stars. No new X-ray-discovered stars were confidently found despite the high sensitivity of the Chandra observation. From these findings, the authors argue that the sample of 27 PMS cloud members in the Chandra field is uncontaminated and complete down to K = 12 or a stellar mass of about 0.1 solar masses. A 16'x 16' region of the Cha I North cloud was observed with the imaging array of the Advanced CCD Imaging Spectrometer (ACIS-I) detector on board the Chandra X-Ray Observatory. The observation took place on 2001 July 2.25-3.04 UT with the detector aimpoint set at 11 10 00.0, -76 35 00 (J2000.0 RA and Declination). The effective exposure was 66.3 ksec. The authors also obtained VI-band CCD images of most of the ACIS field with the 1m telescope and CCD detector at the South African Astronomical Observatory (SAAO) during 2002 February. This table was created by the HEASARC in February 2007 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/614/267">CDS catalog J/ApJ/614/267</a> files table1.dat, table2.dat and table3.dat. This is a service provided by NASA HEASARC .
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