Exploring the total Galactic extinction with SDSS BHB stars

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Table 1

Seven globular clusters taken from Harris (1996, 2010 edition).

ID	Name	l	b	R_sun	[Fe/H]	E(B − V)	V_BH	g_BH^a	E(u − g)^b	E(g − r)	E(r − i)	E(i − z)


1	Pal5	0.85	45.86	23.2	–1.41	0.03	17.51	17.5	0.031	0.032	0.019	0.017
2	NGC 5904	3.86	46.8	7.5	–1.29	0.03	15.07	15.2	0.031	0.032	0.019	0.017
3	NGC 6205	59.01	40.91	7.1	–1.53	0.02	14.9	15.2	0.020	0.021	0.013	0.011
4	NGC 5466	42.15	73.59	16.0	–1.98	0.016	16.52	16.6	0.016	0.017	0.010	0.009
5	NGC 5272	42.22	78.71	10.2	–1.5	0.01	15.64	15.6	0.010	0.011	0.006	0.006
6	NGC 5024	332.96	79.76	17.9	–2.1	0.02	16.81	17.0	0.020	0.021	0.013	0.011
7	NGC 5053	335.7	78.95	17.4	–2.27	0.01	16.69	16.8	0.010	0.011	0.006	0.006

Notes.

^(a)

The g-band magnitude of BHB is estimated by averaging over the g magnitude of individual BHB stars located in the corresponding clusters.

^(b)

The reddening E(a − b) is calculated according to Eqs. (7) and (8), given R_V = 3.1. The differences of E(a − b) is within <5%0 when the R_V varies from 2.5 and 4.1. Specifically, and .

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