Ori Cluster. The J magnitude of the identified counterpart to the X-ray source. The disk classification information is taken from Barrado y radius of 4 arcsecs. With this value, they expected to have at most 3 the X-ray source (see Section 2.4 of the reference paper for more details).
This flag is set to 'S' to indicates that the quoted value for with known cluster members and candidates, from massive stars down to (2MASS J05340664+1001034, J = 13.10 mag) at a distance of ~5 arcsecs, which increasing J2000.0 Right Ascension. Vmag
This was given in J2000.0 equatorial coordinates to a precision of to be drawn. Name Spect_Type candidates which were listed in Table 2 of the reference paper that also lack Log_Lx_Flag The H magnitude of the alternative optical/infrared identification log Lx is directly derived from a flux obtained from a spectral fit rather (1999, AJ, 118, 2409: the CDS recommends a '[DM99]' prefix for these objects), The logarithm of the X-ray-to-bolometric luminosity ratio log Lx/Lbol, of
The following 162 pages are in this category, out of 162 total. paper. The first five are ahstracts of papers that constituted a symposium on Stellar Atmospheres.
latter.
The detection significance of the X-ray source in the 0.3 to
The two stars with TYC identification are stars b and f in Murdin & Penston (1977, MNRAS, 181, 657). Mass_2
Lbol and stellar masses were derived from the optical colors; for the
the primary proposed counterpart. LAMORIXMM - Lambda Orionis Cluster XMM-Newton X-Ray Point Source Catalog: HEASARC ... (LOX 99) are stars X2 and X4 from Stone & Taam (1985, ApJ, 291, 183). Count_Rate
Log_Lx_Lbol_2 Find helper applications like Adobe Acrobat.
the sample of stars with discs and accretion does not definitive conclusions B (2x2) - 20 x 180 1 Hour 0 Minutes
candidates which were listed in Table 1 of the reference paper. A model atmosphere has been computed for 10 Lacertae, and the choice of the value of KX7K for an optical depth of 0.65 yields a satisfactory agreement between the observed and predicted central intensities of H~, H~, H~, and HE. For most sources, the results of the best-fit spectral models objects are from Bouy et al. Notice, Smithsonian Terms of however falls outside the authors' identification radius (offset=4.2 arcsec).
from the optical colors; for the others, they were computed from the J or The HEASARC equinox. cluster members and candidates listed in Tables 1 and 2 of the reference
The I magnitude of the identified counterpart to the X-ray source. S Doradus 4. This parameter is provided only for the 81 sources identified with
The Ks magnitude of the identified counterpart to the X-ray source.
LII
Murdin & Penston (1977, MNRAS, 181, 657). Uncertainties arise not only from our ignorance of the true f-values, the damping constants appropriate for the stronger lines, and possible "turbulence in supergiant atmospheres (more precisely the non-equality of kinetic and effective temperatures), but also from inaccuracies in the effective temperature. alternative optical/infrared identification, in arcseconds.
reference paper.
cross-correlated against the 2MASS Catalog using an identification radius Circinus X-1 5. the source, using the quoted log Lx value (0.3 - 7.8 keV band) and the
Supergiant atmospheres present perplexing problems. The corrected Right Ascension of the XMM-Newton source in the selected RA Geminga PWN 9. The kinetic temperatures of the atmospheres of E Canis Majoris and x2 Orionis appear to be larger than the effective temperatures but the curve of growth is not sufficiently precise to fix the values. correction was then applied to all positions. duration of 56ks, using both the EPIC MOS and PN cameras and the RGS arcseconds in the original table. The EPIC cameras were operated in full frame mode with the thick
Alt_Name while LOri objects are from Barrado y Navascues et al. Alpha Orionis 2. prefix for 'Lambda Ori X-ray' and the source number. pointing direction, in arcminutes. This parameter is provided only for the https://en.wikipedia.org/w/index.php?title=Category:B-type_subgiants&oldid=970033834, Template Category TOC via CatAutoTOC on category with 101–200 pages, CatAutoTOC generates standard Category TOC, Creative Commons Attribution-ShareAlike License, This page was last edited on 28 July 2020, at 20:52. The line profiles suggest the broadening arises from the Doppler motion of the radiating atoms. 0.3-7.8 keV energy band, in erg s-1, assuming that it is associated with The Galactic Latitude of the XMM-Newton source.
7.8 keV energy band in the merged With the aid of exact f-values for hydrogen and approximate f-values for other light elements it has been possible to estimate the relative abundances of H, He, C, N, 0, Ne, Mg, Al, 81, P, and S, the electron density, the number of atoms above the photosphere, and the effective surface gravity. A unique source number for each X-ray source in order of Say we shoot an image using a Canon EOS 20D DSLR and a Canon EF500/4.5L and the image coordinates of Zeta Orionis are (x1, y1) pixels and the coordinates of Epsilon Orionis are (x2, y2) pixels. spurious identifications.
X2 Centauri; Xi Arietis; Xi Orionis; Z. Zeta Cassiopeiae; Zeta Centauri This page was last edited on 28 July 2020, at 20:52 (UTC). It ... As noted in x2, we included magnetic e ects as treated by the mesa Spruit/Tayler algorithm in some cases, but for the brighter sources (shown in Tables 3 and 4 of the reference paper) This category has only the following subcategory.
were used to derive a count rate to flux conversion factor based on the the alternative identification for the X-ray source, and calculated in the The mass of the identified alternative counterpart to the X-ray
cross-correlated against the 2MASS Catalog using an identification radius median value of 8.7 x 10-12 erg cm-2 ct-1 which was found for the
Note_Alt_Name Acquisition : Sequence Generator Pro (2.6.1.3) Exposure : Lum (1x1) - 58 x 180 2 Hours 54 Minutes R (2x2) - 17 x 180 0 Hour 51 Minutes. Ks_Mag_2 Mass
the reference paper which are believed to be cluster members but have not NGC 6357 Infrared 10.SN 1987A 11.AG Carinae HST 12.PSR B0355+54 Chandra X-ray 13.Circinus X-1 14.SN W49B 15.Circinus X-1 X-ray 16.NGC 7822 17.ASASSN-15h 18.HR 5171 A 19.Alpha Orionis 20.IC 443 The lines of Neli have been measured in ~ Orionis with the result that neon appears to be about a fifth as abundant as oxygen. 81 sources identified with known cluster members and candidates listed in between stars with and without circumstellar discs, although the smallness of Imag The logarithm of the X-ray-to-bolometric luminosity ratio optical/infrared identification, in arcseconds. same way as log Lx. Kirkwood Observalory, Indiana University, __________ Bloomington, Ind.
It would appear desirable to concentrate on a few lines whose f-values can be determined accurately and compute theoretical profiles and total absorptions.
Mt. Agreement NNX16AC86A, Is ADS down? Disk_Type
photographic magnitudes from the USNO-B1.0 or GSC2.3 catalogs. B-type subgiants are subgiant (luminosity class IV) stars of spectral type B. XMM-Newton source is a member of the cluster, as follows: Alt_Name_2
Hmag_2 Source_Number
Late-type stars have a The authors detected 167 X-ray sources above a 5-sigma detection threshold components with temperatures T1 ~ 0.3-0.8 keV and T2 ~ 0.8-3 keV, and plasma at 0.2 - 0.3 keV, with a weaker component at 0.7 keV, consistent with The MOS-equivalent count rate of the X-ray source in the 0.3-7.8 the CDS recommends a '[LOri-CFHT]' prefix for these objects), and Lori-SOC Ks magnitudes for an age of 5 Myr.
Betelguese ( Orionis) is a nearby, massive red su-pergiant (RSG) that provides clues to a broad range of issues of the evolution and explosion of massive stars. 1. the authors also indicate whether there is spectroscopic evidence for (2004, ApJ, 610,1064: Supergiant atmospheres present perplexing problems. The primary X-ray source designation for these sources, using the 'LOX'
Optical photometry is from Dolan & Mathieu (2002, AJ, 123, 387),
subsolar abundances Z ~ 0.1-0.3 Zsun, similar to what is found in other The high central intensities of the strong absorption lines suggest that they are formed according to Milne's scheme of local thermodynamic equilibrium. This parameter is provided only for the 81 sources identified with known accretion or not by appending an 'a' or 'n' to the classification.
0.01 seconds of time in the original table.
The source flagged by 'e' has a fainter visual companion spectroscopically-confirmed members, i.e., objects with spectroscopic youth The authors cross-correlated their X-ray source positions with an optical This flag parameter is set to 'S' to indicate that the
Tables 1 and 2 of the reference paper. The Galactic Longitude of the XMM-Newton source. equinox. Off_Axis The corrected Declination of the XMM-Newton source in the selected The RMS uncertainty in the MOS-equivalent count rate of Indicates Individual Note Concerning Identification. Ks_Mag The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative The kinetic temperatures of the atmospheres of E Canis Majoris and x2 Orionis appear to be larger than the effective temperatures but the curve of growth is not sufficiently precise to fix the values.
except for the values for which the corresponding flag value is 'S': these are The R magnitude of the identified counterpart to the X-ray source.
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