Table 2: Point sources identified in our speckle images. For details about IRS1 and the binary system IRS2a/b, we refer to the text. We identify components a to f with the stars already discovered in the image by Alvarez et al. (2004).
Name RA (J2000)a Dec (J2000)a K' Magnitudeb Comment
a 23$^{\rm h}$13$^{\rm m}$45 $.\!\!^{\rm s}$33 61$^\circ$28$^\prime $21 $.\!\!^{\prime\prime}$02 10 $.\!\!^{\rm m}$94  
b 44 $.\!\!^{\rm s}$81 10 $.\!\!^{\prime\prime}$63 11 $.\!\!^{\rm m}$29  
c 44 $.\!\!^{\rm s}$95 12 $.\!\!^{\prime\prime}$33 11 $.\!\!^{\rm m}$46  
d 45 $.\!\!^{\rm s}$11 09 $.\!\!^{\prime\prime}$69 11 $.\!\!^{\rm m}$73  
e 45 $.\!\!^{\rm s}$37 15 $.\!\!^{\prime\prime}$12 11 $.\!\!^{\rm m}$77 embedded in feature C
f 45 $.\!\!^{\rm s}$34 15 $.\!\!^{\prime\prime}$93 11 $.\!\!^{\rm m}$73 embedded in feature C
g 45 $.\!\!^{\rm s}$36 14 $.\!\!^{\prime\prime}$80 11 $.\!\!^{\rm m}$73 embedded in feature C
h 45 $.\!\!^{\rm s}$31 14 $.\!\!^{\prime\prime}$72 11 $.\!\!^{\rm m}$86  
i 45 $.\!\!^{\rm s}$29 13 $.\!\!^{\prime\prime}$74 11 $.\!\!^{\rm m}$71  
j 45 $.\!\!^{\rm s}$27 13 $.\!\!^{\prime\prime}$25 11 $.\!\!^{\rm m}$73  
k 45 $.\!\!^{\rm s}$25 13 $.\!\!^{\prime\prime}$05 11 $.\!\!^{\rm m}$81  
l 45 $.\!\!^{\rm s}$24 13 $.\!\!^{\prime\prime}$28 11 $.\!\!^{\rm m}$83  
m 45 $.\!\!^{\rm s}$22 12 $.\!\!^{\prime\prime}$71 11 $.\!\!^{\rm m}$71  
n 45 $.\!\!^{\rm s}$36 12 $.\!\!^{\prime\prime}$99 11 $.\!\!^{\rm m}$75  
o 45 $.\!\!^{\rm s}$50 10 $.\!\!^{\prime\prime}$50 11 $.\!\!^{\rm m}$60  
p 45 $.\!\!^{\rm s}$29 18 $.\!\!^{\prime\prime}$42 11 $.\!\!^{\rm m}$73  
q 45 $.\!\!^{\rm s}$16 19 $.\!\!^{\prime\prime}$69 11 $.\!\!^{\rm m}$77  
r 45 $.\!\!^{\rm s}$33 08 $.\!\!^{\prime\prime}$48 11 $.\!\!^{\rm m}$71  
a For the astrometry, the relative errors are of the order of 0 $.\!\!^{\prime\prime}$1. The absolute calibration using the reference position of IRS1 in 2MASS introduces further errors (0 $.\!\!^{\prime\prime}$2); b the photometry was done relative to IRS1 with an uncertainty of 0 $.\!\!^{\rm m}$3. For the conversion to absolute photometry, we assumed a IRS1 magnitude of 8 $.\!\!^{\rm m}$9 (Ojha et al. 2004).

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