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J/A+A/439/1149      XMM spectroscopy of TWA 5                (Argiroffi+, 2005)

XMM-Newton spectroscopy of the metal depleted T Tauri star TWA 5. Argiroffi C., Maggio A., Peres G., Stelzer B., Neuhaeuser R. <Astron. Astrophys., 439, 1149-1158 (2005)> =2005A&A...439.1149A
ADC_Keywords: Stars, double and multiple ; Stars, pre-main sequence ; X-ray sources ; Spectroscopy Keywords: X-rays: stars - techniques: spectroscopic - stars: activity - stars: abundances - stars: pre-main sequence - stars: individual: TWA 5 Abstract: We present results of X-ray spectroscopy for TWA 5, a member of the young TW Hydrae association, observed with XMM-Newton. TWA 5 is a multiple system which shows Hα emission, a signature typical of classical T Tauri stars, but no infrared excess. From this analysis of the RGS and EPIC spectra, we have derived the emission measure distribution vs. temperature of the X-ray emitting plasma, its abundances, and the electron density. Description: TWA 5 was observed for ∼30ks with XMM-Newton on January 9, 2003. Objects: --------------------------------------------------- RA (2000) DE Designation(s) --------------------------------------------------- 11 31 55.3 -34 36 27 TWA 5 = TYC 7223-275-1 --------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 106 53 Strongest RGS lines of TWA 5
Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 3 A3 --- Label Label number 5- 9 F5.2 0.1nm LambdaO ?=- Observed wavelength (1) 11- 17 F7.4 0.1nm LambdaP Predicted wavelength (1) 19- 27 A9 --- Ion Ion 29- 90 A62 --- Trans Transition (upper --> lower) 93- 96 F4.2 [K] logTmax Temperature of maximum emissivity 98-102 F5.1 10-6ph/s/cm2 Flux ? Line flux (2) 104-106 F3.1 10-6ph/s/cm2 e_Flux ? rms uncertainty on Flux (2)
Note (1): Observed and predicted (APED database) wavelengths. In the cases of unresolved blends identified by the same label number, we list the main components in order of increasing predicted wavelength. Note (2): Line fluxes with uncertainties at the 68% confidence level obtained by fitting RGS1 and RGS2 spectra simultaneously. In the cases of unresolved blends identified by the same label number, we report only the total flux of the blended lines
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 27-Jul-2006
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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