Table 4: Spectral parameters obtained from fit.
Class I              
ROXN Name   kT $N_{\rm H}$ Abundance E.M. $L_{\rm X}$ $\chi^2$/d.o.f.
        (1022 cm-2)   (1052 cm-3) (1029 erg s-1)  
(1) (2) (3) (4) (5) (6) (7) (8) (9)
22 EL29   4.3(3.6-5.1) 4.9(4.4-5.3) 1.0(0.80-1.3) 16.0(13.6-18.9) 27.5 90.0/ 63.0
43 IRS43/YLW15   3.9(3.0-5.3) 3.3(2.9-3.8) [0.30] 13.1(10.2-17.3) 17.3 36.5/ 35.0
    f 3.2(2.7-3.9) 4.0(3.5-4.5) [0.30] 29.1(22.8-37.0) 34.8 56.3/ 45.0
46 IRS44/YLW16A   2.7(2.4-3.1) 5.3(4.9-5.7) 0.28(0.19-0.38) 45.6(38.3-53.9) 49.7 77.0/ 72.0
66 IRS51   2.1(1.8-2.8) 4.2(3.5-4.8) 0.62(0.27-1.18) 13.8(10.2-18.5) 16.2 51.7/ 48.0
Class II              
ROXN Name   kT $N_{\rm H}$ Abundance E.M. $L_{\rm X}$ $\chi^2$/d.o.f.
ID       (1022 cm-2)   (1052 cm-3) (1029 erg s-1)  
(1) (2) (3) (4) (5) (6) (7) (8) (9)
1 DoAr25   6.4(4.9-8.8) 1.1(0.96-1.2) 0.26(0.02-0.51) 157(141-177) 247 80.1/ 72.0
11 SR24S   2.3(2.0-2.7) 1.2(1.0-1.3) 0.24(0.07-0.43) 16.3(13.4-19.4) 15.9 107.7/ 75.0
18 WL17   2.9(2.0-4.3) 4.1(3.1-5.2) [0.30] 8.4(5.0-14.6)  9.6 27.5/ 19.0
    f 3.2(2.5-4.2) 4.5(3.8-5.4) 0.66(0.31-1.2) 18.1(13.1-25.7) 24.8 35.4/ 25.0
29 IRS34   1.8(1.1-3.7) 2.7(1.6-4.4) [0.30] 12.8(<41.5) 11.7 4.7/ 5.0
30 WL20   2.3(1.8-3.0) 2.0(1.6-2.4) [0.30] 8.1(5.9-11.4)  8.1 16.2/ 17.0
    f 3.4(2.7-4.5) 2.0(1.7-2.3) 0.34(0.04-0.75) 16.4(13.3-20.2) 20.4 34.7/ 29.0
33 GY245   2.1(1.3-5.0) 7.7(5.2-11.0) [0.30] 4.5(1.5-16.4) 4.4 10.9/ 9.0
45 VSSG25 f 2.0(1.6-2.5) 1.1(0.9-1.4) [0.30] 6.3(4.7-8.2)  5.9 29.1/ 24.0
50 IRS47 f 2.9(1.7-7.4) 2.3(1.5-3.3) [0.30] 7.5(<15.5)  8.5 1.2/ 2.0
57 GY292   2.3(2.1-2.5) 1.7(1.5-1.8) 0.23(0.14-0.36) 31.2(28.6-35.8) 30.8 159.3/153.0
61a IRS49   2.0(1.9-2.2) 1.6(1.4-1.7) 0.18(0.08-0.29) 27.1(23.9-30.7) 24.1 131.1/114.0
62 GY310 f 2.5(1.7-3.6) 0.82(0.59-1.2) [0.30] 1.8(1.4-2.4)  1.9 22.4/ 13.0
63 GY312   2.3(1.7-3.3) 7.6(6.0-8.7) [0.30] 11.4(6.4-22.5) 11.6 25.0/ 17.0
65 GY314   2.1(2.0-2.3) 1.5(1.4-1.6) 0.16(0.07-0.26) 31.6(28.4-35.0) 28.4 113.2/113.0
Class III              
ROXN Name   kT $N_{\rm H}$ Abundance E.M. $L_{\rm X}$ $\chi^2$/d.o.f.
        (1022 cm-2)   (1052 cm-3) (1029 erg s-1)  
(1) (2) (3) (4) (5) (6) (7) (8) (9)
5 GY112   0.98(0.79-1.1) 0.36(0.31-0.50) 0.10(0.06-0.16) 7.5(6.1-11.8) 4.3 40.9/ 37.0
14a GY193   1.27(1.19-1.74) 0.87(0.56-1.07) [0.30] 7.0(4.6-8.2) 6.0 29.4/ 38.0
15 GY194   1.5(1.2-1.9) 0.79(0.6-1.1) [0.30] 3.2(2.6-3.9) 2.8 20.7/ 13.0
25 WL19   2.5(1.5-4.6) 8.62(6.0-12.8) [0.30] 9.2(3.7-30.7) 9.8 8.4/ 10.0
27,28a,b ROXs20A, ROXs20B     0.13(0.06-0.18) 0.42(0.23-1.21)   4.6 59.2/ 40.0
      0.66(0.56-0.77)     1.7(0.8-2.2) 1.9  
      1.66(1.30-2.29)     2.8(1.9-3.9) 2.8  
32,34,35b,c WL5,WL4,WL3   2.5(2.2-3.0) 4.7(4.2-5.2) [0.30] 60.4(47.4-76.9) 64.2 104.6/ 74.0
36 SR12A-B     0.11(0.08-0.13) 0.12(0.08-0.17)   21.9 248.6/205.0
      0.25(0.23-0.27)     18.2(11.1-30.2) 4.4  
      0.97(0.89-1.03)     18.6(17.0-25.2) 11.1  
      3.5(2.5-6.5)     5.6(3.1-8.3) 6.5  
    f   0.06(0.03-0.10) 0.24(0.13-0.55)   24.0 74.0/ 60.0
      0.32(0.28-0.38)     7.8(4.3-17.1) 4.2  
      1.22(1.09-1.35)     15.3(5.5-22.5) 12.0  
      12.0(>3.1)     4.9(3.0-10.4) 7.7  
39 GY253   1.6(1.4-2.0) 4.5(3.9-5.2) [0.30] 24.9(17.5-34.9) 22.0 57.7/ 52.0
52 BKLT162730-244726   1.9(1.3-2.3) 1.0(0.8-1.5) [0.30] 6.6(5.3-11.2) 6.1 44.1/ 43.0
72 GY377   1.8(1.1-2.7) 1.1(0.7-1.8) [0.30] 1.7(0.9-3.6) 1.5 7.1/ 11.0
73 IRS55     1.1(1.0-1.2) 0.31(0.20-0.50)   62.3 139.3/141.0
      0.64(0.60-0.68)     46.9(28.0-67.2) 45.7  
      2.5(2.2-3.0)     15.7(12.7-19.2) 16.6  
76 GY410   1.8(1.3-2.4) 1.5(1.1-1.9) [0.30] 3.8(2.5-5.9) 3.4 8.9/ 23.0
New Class III candidates              
ROXN Name   kT $N_{\rm H}$ Abundance E.M. $L_{\rm X}$ $\chi^2$/d.o.f.
ID       (1022 cm-2)   (1052 cm-3) (1029 erg s-1)  
(1) (2) (3) (4) (5) (6) (7) (8) (9)
31 16271643-24311   4.2(2.2-15.1) 5.2(3.5-7.4) [0.30] 6.1(3.2-14.3) 8.3 25.8/ 26.0
41 GY259   3.4(>1.3) 2.2(1.1-4.5) [0.30] 1.9(0.8-6.3) 2.3 0.5/ 2.0
44 GY266   2.3(1.1-6.1) 2.8(1.6-5.0) [0.30] 2.4(1.0-8.2) 2.5 7.5/ 6.0
53 GY283   1.4(0.5-2.6) 0.47(0.2-1.5) [0.30] 0.5(0.3-3.0) 0.5 2.1/ 4.0
58 GY295   1.9(1.2-2.8) 0.34(0.2-0.6) [0.30] 0.7(0.5-0.8) 0.6 12.3/ 11.0
77 BKLT162800-244819   0.5(0.4-0.7) 0.97(0.8-1.1) [0.30] 8.7(4.4-17.2) 7.8 24.2/ 25.0
78 GY463   1.6(1.2-2.1) 2.6(2.0-3.4) [0.30] 11.0(6.8-20.2) 9.6 16.0/ 20.0
86 BKLT162823-244140   4.3(2.2-13.2) 0.87(0.5-1.3) [0.30] 4.0(2.8-6.7) 5.5 9.7/ 9.0
X-ray sources with no optical or IR counterpart          
ROXN Name   kT $N_{\rm H}$ Abundance E.M. $L_{\rm X}$ $\chi^2$/d.o.f.
ID       (1022 cm-2)   (1052 cm-3) (1029 erg s-1)  
(1) (2) (3) (4) (5) (6) (7) (8) (9)
51 .................   10.5(>3.9) 0.92(0.6-1.4) [0.30] 2.5(2.0-3.8) 4.4 40.1/ 28.0
64 .................   82.4(>20.5) 2.2(1.7-2.9) [0.30] 3.5(2.9-4.1) 5.5 64.5/ 43.0
67 .................   3.6(>1.4) 9.5(4.8-18.0) [0.30] 6.7(2.4-46.9) 8.6 25.4/ 29.0
(1) XMM-Newton source ID number, "Rho Oph X-ray sources, Newton''. (2) The source name from Col. (15) in Table 2. (3) "f'' means that the X-ray spectra are extracted during the flare phase. (4-7) The 90% confidence regions are given between parenthesis. (5) We use WABS for absorption model in XSPEC where standard solar metal abundances are used. The use of revised solar abundances (Holweger 2001; Allende Prieto et al. 2001, 2001) would increase $N_{\rm H}$ by 20 $\sim $% (Vuong et al. 2003). (6) The abundance [0.30] is fixed. (7), (8) The emission measure and X-ray luminosity are calculated from the best-fit PN parameters assuming a distance of 140 pc. Those from MOS1+MOS2 parameters are consistent within errors. The X-ray luminosity is corrected for absorption.
a These sources showed a small flare during the observation, but the X-ray counts in the flares are not sufficient to obtain their spectra.
b It is difficult to obtain an individual spectrum without contamination from neighbouring sources. We extracted the X-ray spectrum from a circular region that contains all the sources.
c Since the X-ray counts from ROXN-32 is dominant, we put the spectral parameters in the table for Class III.


Source LaTeX | All tables | In the text

Article Contents
1 Introduction
2 Observation and data analysis
3 Comparison with Chandra source detections
4 IR properties of the XMM-Newton sources
5 X-ray detection of young bona fide brown dwarfs
6 X-ray properties of Young Stellar Objects in the $\rho $ Ophiuchi cloud
7 Summary and conclusions
References
Online Material
Appendix A: Method to compute the X-ray count rate upper limit
Appendix B: Comparison between Chandra and XMM-Newton determination of $N_{\rm H}$
List of tables
List of figures