Table 2: Identification of Chandra X-ray sources with optical or infrared counterparts in the CrA star-forming region. Columns 2-4 provide information on counterparts to the X-ray sources in the optical DSS images, the 2MASS images, and the Spitzer images: "y'' means that a counterpart exists, "n'' means that no counterpart can be seen. Column 5 gives the SED class derived from the Spitzer photometry, and the last 3 columns give names, spectral types, and stellar bolometric luminosities of the stars collected from Casey et al. (1998); Olofsson et al. (1999); Walter et al. (1997); Neuhäuser et al. (2000); Wilking et al. (1992); Prato et al. (2003); Nisini et al. (2005); additional references are given in the discussion of the individual objects in Sects. 3 and 4.

Source
Counterpart SED Name SpT $L_{\rm bol}$
CXO J DSS 2MASS Spitzer class     $[L_\odot]$
190104.58-370129.6 n y y III CrA 453 M4  
190108.60-365721.3 y y y II S CrA K3 2.29
190115.86-370344.3 n n y        
190116.26-365628.4 y y y II V667 CrA M5  
190118.90-365828.4 n y y II CrA 466 M4.5  
190119.39-370142.0 n n y        
190120.86-370302.9 y y y III CrA 4111 M5  
190122.40-370055.4 n n y        
190125.61-370453.9 n y y III ISO-CrA 133    
190125.75-365919.3 n y y II ISO-CrA 134    
190127.15-365908.6 y y y III ISO-CrA 135 M 0.12
190128.72-365931.9 y y y   ISO-CrA 136    
190129.01-370148.8 y y y III ISO-CrA 137    
190132.34-365803.1 n y y II TS 2.9 = ISO-CrA 139    
190133.84-365745.0 n y y II TS 2.8 = IRS 13   0.07
190134.84-370056.7 y y y III V709 CrA K1 IV 1.55
190139.15-365329.6 y y y   HD 176386-B    
190139.34-370207.8 y y y III      
190140.40-365142.4 n y y II      
190140.81-365234.0 y y y   TY CrA  a/b/c/d B8e/K2/F-K/M  
190141.55-365831.6 n y y I IRS 2 K2 4.3
190141.62-365953.1 y y y II HBC 677    
190143.12-365020.9 n n y        
190148.02-365722.41 n y y I IRS 5 a/b K6 V/? 1.6/?
190148.46-365714.5 n n y I      
190149.35-370028.6 y y y III LS-RCrA 2 M6 (BD cand.)  
190150.45-365638.1 n y y II IRS 6A M2 0.5
190150.66-365809.9 n y y I V710 CrA = IRS 1 = HH 100 IR K5-M0 3.1
190151.11-365412.5 n y y II IRS 8    
190152.63-365700.2 n y y I IRS 9    
190153.67-365708.3 y y y   R CrA A5 IIe var  
190155.31-365722.0 n n y I IRS 7 W (= 7 A)    
190155.61-365651.1 n n y I      
190155.76-365727.7 n n y I/II      
190155.85-365204.3 n n y        
190156.39-365728.4 n n y 0/I IRS 7 E (= 7 B)    
190157.46-370311.9 n y y        
190158.32-370027.5 n n y III      
190158.79-365750.1 y y y II T CrA F0e 3.4
190200.11-370222.3 y y y III 2MASS J19020012-3702220 M4  
190201.92-370743.0 y y y III V702 CrA G5 1.55
190201.94-365400.1 n n y   B185839.6-365823 BD cand.  
190211.99-370309.4 n y y II ISO-CrA 143 BD cand. 0.01
190222.13-365541.0 y y y III HBC 679 K2 IV 0.50
190227.05-365813.2 y y y II HBC 680 M 0.72
190233.07-365821.1 y y y II ISO-CrA 159 M 0.45
1 The X-ray emission of the 0.9'' binary IRS 5a/b (Chen & Graham 1993; Nisini et al. 2005)
is marginally resolved in the Chandra image.


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