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Table 3:

Determination of AV, R from common upper level PH lines, and R derived from stellar photometry.
    PH Emission Lines Stellar Photometry  
Object Obs.a PH Pairsb AV(mag) Rc AV(H$\alpha$-H$\beta $)d Star/Cluster R Ref.
M 8 TP 7 [6-12] 2.10 4.35   Herschel 36 4.6-5.6, 5.3 2, 3
  G-R 11 [7-20] 2.20 6.1 (5.0)e 2.1(1.4) NGC 6523 4.6 4
M 16 G-R 9 [7-18] 2.80 5.2 (3.1,4.8)f 3.2(2.3) NGC 6611 4.8 5
M 17 TP 7 [6-12] 3.50 4.1 2.35(2.0) NGC 6618 4.2 1
  G-R 9 [7-18] 3.05 4.3 (3.1) 3.4(2.7) Star 1 (Fig. 1, 5) 4.5 $\pm$ 0.25 TP
M 20 G-R 14 [7-22] 1.05 5.5 (3.1) 0.8(0.8) HD 164492 5.1 6, 7
            HD 164492 3.1 8
M 42 E 9 [7-19] 2.15 5.8 2.2(1.5) $\theta$1 Ori C 5.5 9
NGC 3603 G-R 8 [9-18] 6.9 5.4 (3.1) 7.4(5.5) NGC 3603 4.3 10
S 311 G-R 10 [7-18] 1.90 5.5 (3.1) 2.1(1.5) [NGC 2467 1.8-3.9] 11
NGC 7027 Z-R 16 [6-22] 3.9 4.4 (3.1)g 4.0 (3.1)      

Notes.  (a) Observer, TP: this paper, G-R: Garcia-Rojas et al. (2005, 2006), E: Esteban et al. (2004), Z-R: Zhang et al. (2005) and Rudy et al. (1992). (b) Number of line pairs, in brackets the range of quantum numbers considered. (c) Determined from relation (2); values in brackets used by G-R. (d) From H$\alpha$-H$\beta $ ratio and R of Col. 5; in brackets for R = 3.1. (e) For 4100 Å < $\lambda$, for shorter $\lambda$ see Garcia-Rojas et al. (2007). (f) R = 3.1 for 5500 Å < $\lambda$, R = 4.8 for $\lambda$ <5500 Å. (g) Value usually taken.

References. 1: Chini et al. (1980), Chini $\&$ Krügel (1983), Hoffmeister et al. (2008); 2: Hecht et al. (1982): 4.6-5.6; 3: Cardelli et al. (1989): 5.0; 4: McCall et al. (1990); 5: Chini et al. (1980), Chini $\&$ Wargau (1990), Chini et al. (1992); 6: Anderson (1970); 7: Lynds et al. (1985); 8: Kohoutek et al. (1999); 9: Cardelli $\&$ Clayton (1988); 10: Pandey et al. (2000); 11: Grubissich (1969), NGC 2467 may not be a physical cluster.


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