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36 results for “Orionis”
Supplementary material 1 from: Broad GR, Stigenberg J (2021) The genus Orionis Shaw (Hymenoptera, Braconidae, Euphorinae) in the Old World. Journal of Hymenoptera Research 88: 133-145. https://doi.org/10.3897/jhr.88.76177
Bayesian analysis of Perilitini based on CO1
Figure 3 from: Broad GR, Stigenberg J (2021) The genus Orionis Shaw (Hymenoptera, Braconidae, Euphorinae) in the Old World. Journal of Hymenoptera Research 88: 133-145. https://doi.org/10.3897/jhr.88.76177
Figure 3 Details of Orionis coxator (NHMUK014425411) a head in frontal view b frons and upper head c propodeum, first metasomal segment and hind coxa in dorsolateral view.
Figure 6 from: Broad GR, Stigenberg J (2021) The genus Orionis Shaw (Hymenoptera, Braconidae, Euphorinae) in the Old World. Journal of Hymenoptera Research 88: 133-145. https://doi.org/10.3897/jhr.88.76177
Figure 6 Comparison of propodeum and first metasomal segment of aOrionis coxator and bPerilitus rutilus.
Figure 2 from: Broad GR, Stigenberg J (2021) The genus Orionis Shaw (Hymenoptera, Braconidae, Euphorinae) in the Old World. Journal of Hymenoptera Research 88: 133-145. https://doi.org/10.3897/jhr.88.76177
Figure 2 Extract from Bayesian phylogeny of Perilitini: relationships of Orionis species based on CO1 and CO1+28S analyses. Numbers on branches are posterior probabilities.
Fig. 4 in Review of the genera Orionis Shaw and Stenothremma Shaw (Braconidae) from India, with description of three new species
Fig. 4. Orionis shillongensis Gupta, van Achterberg & Pattar sp. nov., holotype, ♀ (NIM/NBAIR/Hym/ Brac/Orio/150613-H). A. Wings. B. Body in part, lateral view. C. T1, dorsal view. D. Metasoma, dorsal view, in part.
Fig. 11 in Review of the genera Orionis Shaw and Stenothremma Shaw (Braconidae) from India, with description of three new species
Fig. 11. Stenothremma flavator Gupta & van Achterberg sp. nov., holotype, ♀ (NIM/NBAIR/Hym/Brac/ Sten/181220-H). Habitus, lateral view.
Fig. 8 in Review of the genera Orionis Shaw and Stenothremma Shaw (Braconidae) from India, with description of three new species
Fig. 8. Orionis femorator Gupta, van Achterberg & Pattar sp. nov., paratype, ♀ (NIM/NBAIR/Hym/ Brac/Orio/10715-P1). Habitus, lateral view.
Fig. 14 in Review of the genera Orionis Shaw and Stenothremma Shaw (Braconidae) from India, with description of three new species
Fig. 14. Stenothremma flavator Gupta & van Achterberg sp. nov., paratype, ♂ (NIM/NBAIR/Hym/Brac/ Sten/100823-P2). Habitus, lateral view.
Fig. 13 in Review of the genera Orionis Shaw and Stenothremma Shaw (Braconidae) from India, with description of three new species
Fig. 13. Stenothremma flavator Gupta & van Achterberg sp. nov., holotype, ♀ (NIM/NBAIR/Hym/Brac/ Sten/181220-H). A. Wings. B. T1, dorsal view. C. T1, ventral view. D. T1, lateral view. E. Metasoma, lateral view.
Fig. 2 in Review of the genera Orionis Shaw and Stenothremma Shaw (Braconidae) from India, with description of three new species
Fig. 2. Orionis shillongensis Gupta, van Achterberg & Pattar sp. nov., holotype, ♀ (NIM/NBAIR/Hym/ Brac/Orio/150613-H). Habitus, in lateral view.
Figure 5 from: Broad GR, Stigenberg J (2021) The genus Orionis Shaw (Hymenoptera, Braconidae, Euphorinae) in the Old World. Journal of Hymenoptera Research 88: 133-145. https://doi.org/10.3897/jhr.88.76177
Figure 5 Unidentified Perilitus species from Cameroon (NHMUK014425412). Scale bar: 1 mm.
Figure 4 from: Broad GR, Stigenberg J (2021) The genus Orionis Shaw (Hymenoptera, Braconidae, Euphorinae) in the Old World. Journal of Hymenoptera Research 88: 133-145. https://doi.org/10.3897/jhr.88.76177
Figure 4 Perilitus mylloceri paratype female, propodeum and first metasomal segment.
Figure 1 from: Broad GR, Stigenberg J (2021) The genus Orionis Shaw (Hymenoptera, Braconidae, Euphorinae) in the Old World. Journal of Hymenoptera Research 88: 133-145. https://doi.org/10.3897/jhr.88.76177
Figure 1 Lateral habitus of Orionis coxator (NHMUK014425411). Scale bar: 2 mm.
Sigma Orionis Cluster XMM-Newton X-Ray Point Source Catalog
This table contains some of the results of an analysis of the full EPIC field in an XMM-Newton observation of the young (~2 - 4 Myr) cluster around the hot star sigma Orionis. The authors have detected 175 X-ray sources, 88 of which have been identified with cluster members, including very low-mass stars down to the substellar limit. They detected eleven new possible candidate members from the 2MASS (<a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/246">CDS Cat. <II/246></a>) catalog. The authors find that late-type stars have a median log L<sub>X</sub>/L<sub>bol</sub> ~ -3.3, i.e. very close to the saturation limit. They detected significant variability in ~ 40% of late-type members or candidates, including 10 flaring sources; rotational modulation was detected in one K-type star and possibly in another 3 or 4 stars. Spectral analysis of the brightest sources shows typical quiescent temperatures in the range T<sub>1</sub> ~ 0.3 - 0.8 keV and T<sub>2</sub> ~ 1 - 3 keV, with subsolar abundances Z ~ 0.1 - 0.3 solar, similar to what is found in other star-forming regions and associations. The authors find no significant difference in the spectral properties of classical and weak-lined T Tauri stars, although classical T Tauri stars tend to be less X-ray luminous than weak-lined T Tauri stars. XMM-Newton observations of the sigma Ori cluster, centered on the hot star sigma Ori AB, were carried out as part of the Guaranteed Time of Roberto Pallavicini using both the EPIC MOS and PN cameras and the RGS instrument. The observation (ID 0101440301) started at 21:47 UT on March 23, 2002 and ended at 9:58 UT on March 24, 2002, for a total duration of 43 ks. The EPIC cameras were operated in Full Frame mode using the thick filter. This table contains the combined list of 88 X-ray sources positionally (<= 5") associated with confirmed or candidate cluster members, and 66 X-ray sources with no such positional associations, detected above a significance threshold of 5 sigma. The two X-ray sources (source numbers 67 and 167) with 2 possible positional associations are listed twice, once for each positional association, with the X-ray information repeated. Thus, there are 156 entries in this HEASARC table. This table was created by the HEASARC in May 2007 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/446/501">CDS catalog J/A+A/446/501</a> files tablea1.dat and tableb.dat. This is a service provided by NASA HEASARC .
Kappa Orionis XMM-Newton X-Ray Point Source Catalog
X-rays are a powerful probe of activity in the early stages of star formation. They allow us to identify young stars even after they have lost the IR signatures of circumstellar disks and provide constraints on their distance. Here, the authors report on XMM-Newton observations that detected 121 young stellar objects (YSOs) in two fields between the filamentary dark cloud complex Lynds 1641S and the star Kappa Ori. These observations extend the Survey of Orion A with XMM and Spitzer (SOXS). The YSOs are contained in a ring of gas and dust apparent at millimeter wavelengths, and in far-IR and near-IR surveys. The X-ray luminosity function of the YSOs detected in the two fields indicates a distance of 250-280 pc, much closer than the Orion A cloud and similar to the distance estimates for Kappa Ori. The authors propose that the ring is a 5-8 pc diameter shell that has been swept up by Kappa Ori. This ring contains several groups of stars detected by Spitzer and WISE including one surrounding the Herbig Ae/Be star V1818 Ori. In this interpretation, the Kappa Ori ring is one of several shells swept up by massive stars within the Orion Eridanus Superbubble and is unrelated to the southern portion of Orion A/L 1641S. The XMM-Newton observations consist of two fields, north (Field N = KN) and south (Field S = KS), and were obtained in 2015 March 10 and 15 using EPIC as the primary instrument. Table 1 in the reference paper shows the details of the exposures, each one with a duration of about 50 ks and taken with the Medium filter. The authors used SAS version 14.0 to reduce the observation data files (ODFs) and to obtain calibrated lists of events for the MOS and pn instruments. They filtered the events in the 0.3-0.8 keV energy band and used only events with FLAG = 0 and PATTERN < 12 as prescribed by the SAS manual. With SAS, the authors obtained exposure maps in the 0.3-8.0 keV band and performed source detection with a code based on wavelet convolution that operated simultaneously on MOS and pn data. They used a threshold of significance of 4.5 sigma of the local background to discriminate real sources from spurious background fluctuations. However, they added few sources to the final list with significance S in 4.0 < S < 4.5 for the cases of positional match with objects in SIMBAD or PPMX catalogs. The final list was also checked for spurious sources that could appear at the border of the CCDs. In sum, the authors detected 238 X-ray sources with significance > 4 sigma of the local background; 104 sources are in KN and 134 in KS. The authors cross-correlated the positions of the X-ray sources with the coordinates of the IR catalog of Megeath et al. (2012, AJ, 144, 192). This IR catalog is the result of a survey of Orion with Spitzer that produced a classification of protostars and stars with disks. Of the 238 X-ray sources, 191 are identified within 8 arcseconds of one of 206 IR objects, 99 sources in KS, 92 sources in KN. Some X-ray sources were multiple matches within 8 arcsec of IR objects. For these cases, the authors assigned the most likely counterparts based on IR photometry and visual inspection of X-rays and IR images. However, nine X-ray sources were left associated with two or three IR objects. Among the IR matches, the authors found 15 stars with disks in KN and 35 in KS with X-ray detection. One protostar in KN and three in KS were detected in X-rays. The authors used X-ray detection of sources without IR excess as criteria to identify disk-less stars (hereafter Class III stars). They classified as Class III stars those IR objects with X-ray detections, with [4.5um]-[8.0um] colors < 0.3 mag and brighter than [4.5um] magnitude < 14. At the distance of the ONC (400 pc), the [4.5um] magnitude ~ 14 threshold at an age of 4-5 Myrs roughly identifies M3-M4 spectral types and masses around 0.3 solar masses. With this selection scheme, the authors identified 48 objects in KN and 19 in KS as Class III candidates. This table was created by the HEASARC in August 2016 based on the electronic version of Table 2 from the reference paper which was obtained from the CDS (their catalog J/ApJ/820/L28 file table2.dat). This is a service provided by NASA HEASARC .
Lambda Orionis Cluster XMM-Newton X-Ray Point Source Catalog
The authors studied the X-ray properties of the young (~1-8M yr) open cluster around the hot (O8 III) star Lambda Ori and compared them with those of the similarly-aged Sigma Ori cluster in order to investigate the possible effects of the different ambient environments. They analyzed an XMM-Newton observation of the cluster using EPIC imaging and low-resolution spectral data. They studied the variability of the detected sources, and performed a spectral analysis of the brightest sources in the field using multi-temperature models. The authors detected 167 X-ray sources above a 5-sigma detection threshold the properties of which are listed in this table, of which 58 are identified with known cluster members and candidates, from massive stars down to low-mass stars with spectral types of ~ M5.5. Another 23 sources were identified with new possible photometric candidates. Late-type stars have a median log L<sub>X</sub>/L<sub>bol</sub> ~ -3.3, close to the saturation limit. Variability was observed in ~ 35% of late-type members or candidates, including six flaring sources. The emission from the central hot star Lambda Ori is dominated by plasma at 0.2 - 0.3 keV, with a weaker component at 0.7 keV, consistent with a wind origin. The coronae of late-type stars can be described by two plasma components with temperatures T<sub>1</sub> ~ 0.3-0.8 keV and T<sub>2</sub> ~ 0.8-3 keV, and subsolar abundances Z ~ 0.1-0.3 Z<sub>sun</sub>, similar to what is found in other star-forming regions and associations. No significant difference was observed between stars with and without circumstellar discs, although the smallness of the sample of stars with discs and accretion does not definitive conclusions to be drawn. The authors concluded that the X-ray properties of Lambda Ori late-type stars are comparable to those of the coeval Sigma Ori cluster, suggesting that stellar activity in Lambda Ori has not been significantly affected by the different ambient environment. The lambda Ori cluster was observed by XMM-Newton from 20:46 UT on September 28, 2006 to 12:23 UT on September 29, 2006 (Obs. ID 0402050101), for a total duration of 56ks, using both the EPIC MOS and PN cameras and the RGS instruments. The EPIC cameras were operated in full frame mode with the thick filter. This table was created by the HEASARC in November 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/530/A150">CDS Catalog J/A+A/530/A150</a> files tablea1.dat ('X-ray sources detected in the Lambda Ori Cluster'), table1,dat ('X-ray and optical properties of sources identified with known cluster members and candidates') and table2.dat ('X-ray sources identified with possible new cluster candidates'). It does not include the objects listed in tablea2.dat ('3-sigma upper limits and optical properties of undetected cluster members and candidates'). This is a service provided by NASA HEASARC .
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