Table 2.

Mean monochromatic flux of Vega in the IPHAS filter system, defined as 〈fλ〉 = ∫fλ(λ)S(λ)λdλ/∫S(λ)λdλ, where S(λ) is the photon response function (which includes atmospheric transmission, filter transmission, and CCD response) and fλ(λ) is the CALSPEC SED for Vega (Bohlin 2014). For reference, we also provide the filter equivalent width EW = ∫S(λ)dλ, the mean photon wavelength λ0 = ∫S(λ)λdλ/∫S(λ)dλ, and the pivot wavelength |$\lambda _{\rm p} = \sqrt{\int\! {S(\lambda )\lambda {\rm d}\lambda } / \!\!\int {\frac{S(\lambda )}{\lambda } {\rm d}\lambda }}$|⁠. These notations follow the definitions by Bessell & Murphy (2012). After multiplying 〈fλ〉 by the EW, we find that the detected flux for Vega in Hα is 3.14 mag less than that received in r.

FilterfλEWλ0λp
(erg cm−2 s−1 Å−1)(Å)(Å)(Å)
r2.47 × 10−9785.662236211
1.81 × 10−959.665686568
i1.30 × 10−9759.976747661
FilterfλEWλ0λp
(erg cm−2 s−1 Å−1)(Å)(Å)(Å)
r2.47 × 10−9785.662236211
1.81 × 10−959.665686568
i1.30 × 10−9759.976747661
Table 2.

Mean monochromatic flux of Vega in the IPHAS filter system, defined as 〈fλ〉 = ∫fλ(λ)S(λ)λdλ/∫S(λ)λdλ, where S(λ) is the photon response function (which includes atmospheric transmission, filter transmission, and CCD response) and fλ(λ) is the CALSPEC SED for Vega (Bohlin 2014). For reference, we also provide the filter equivalent width EW = ∫S(λ)dλ, the mean photon wavelength λ0 = ∫S(λ)λdλ/∫S(λ)dλ, and the pivot wavelength |$\lambda _{\rm p} = \sqrt{\int\! {S(\lambda )\lambda {\rm d}\lambda } / \!\!\int {\frac{S(\lambda )}{\lambda } {\rm d}\lambda }}$|⁠. These notations follow the definitions by Bessell & Murphy (2012). After multiplying 〈fλ〉 by the EW, we find that the detected flux for Vega in Hα is 3.14 mag less than that received in r.

FilterfλEWλ0λp
(erg cm−2 s−1 Å−1)(Å)(Å)(Å)
r2.47 × 10−9785.662236211
1.81 × 10−959.665686568
i1.30 × 10−9759.976747661
FilterfλEWλ0λp
(erg cm−2 s−1 Å−1)(Å)(Å)(Å)
r2.47 × 10−9785.662236211
1.81 × 10−959.665686568
i1.30 × 10−9759.976747661
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