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Table 2

Coefficients p0 and p1 of FWHM(λ) = p0 + p1(λ−7000 Å) that describe the wavelength dependence of the PSF FWHM in each of the datacubes.

Pointing p0 p1 Method
No. [′′] [10-5′′/Å]

01 0.836 –4.429 fit to ID 10548, mF814W = 22.18
02 0.940 –3.182 compact galaxies, no star
03 0.944 –4.460 fit to ID 8374, mF814W = 19.39
04 0.747 –4.219 compact galaxies, no star
05 1.026 –3.003 compact galaxies, no star
06 0.835 –4.332 compact galaxies, no star
07 0.935 –3.966 compact galaxies, no star
08 0.991 –5.007 compact galaxies
09 0.833 –8.069 fit to ID 68879, mF814W = 19.73
10 0.890 –3.051 compact galaxies
11 0.989 –3.771 compact galaxies
12 1.020 –4.123 compact galaxies, no star
13 1.063 –5.285 compact galaxies
14 0.884 –4.844 compact galaxies
15 0.702 –4.441 fit to ID 5744, mF814W = 20.3
16 0.859 –3.784 fit to ID 6475, mF814W = 18.86
17 0.780 –3.534 compact galaxies
18 0.929 –3.479 compact galaxies, no star
19 0.814 –3.524 compact galaxies, no star
20 0.713 –5.196 compact galaxies, no star
21 0.836 –4.255 fit to ID 9801, mF814W = 21.92
22 0.788 –3.253 fit to ID 7813, mF814W = 20.23
23 0.777 –3.019 compact galaxies, no star
24 0.728 –4.232 compact galaxies, no star

Notes. These coefficients are used as input parameters in LSDCat for the spatial filtering. In the method column we give the ID and F814 magnitude from the Guo et al. (2013) catalogue when the polynomial coefficients were derived using this star. Otherwise we indicate with “compact galaxies”, that the minimisation utilising compact galaxies provided a p0 value closer to the AG Seeing and we therefore used p0 and p1 from this method. With “compact galaxies, no star” we indicate that no sufficiently bright star was present within the datacube, and we thus had to rely on the minimisation scheme utilising compact galaxies.

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