After the published paper was accepted, and during the preparation of the proof, an issue internal to the Publishing team occurred and a preliminary version of the manuscript was sent to the typesetters. As a result, the published paper does not correspond to the accepted version. While none of the conclusions and trends presented are affected, Figures 9, 10, 11, 13, and 18 in the published paper and the related text need to be amended. Values in the text should be updated accordingly in a few sentences as follows: In Section 3.5. The spatial distribution of the ionization parameter for P11695 is presented in Figure 1. It is generally low, ranging from 6.6 < log(q) < 7.3. This is in agreement with other galaxies in the GASP survey (Gullieuszik et al. 2017; Poggianti et al. 2017), even though in this case a clear clumpy pattern emerges, while in other galaxies a more smooth distribution is observed. Hα knots tend to have a systematically large value of q: the median value integrated across the entire galaxy is 6.8, while the median value in the Hα knots is 7. Figure 2 shows that the spatially resolved metallicity ranges between 8.3 < 12 + log(O H) < 9, with a median value of 8.6. Trends between metallicity and distance from the galaxy center are more clear in Figure 3. Along B, gradients are symmetric around the 0 position up to 5″, then the south side shows a constant decline and a sudden increase at r > 7″, while the north side of the galaxy shows some fluctuations. The minimum metallicity is log(O H) ∼ 8.4, while along A and B, for example, it is always .8.5. Finally, the E aperture catches one of the flattest gradients in the galaxy, with metallicity values >8.6 at all distances. In Section 3.6. Comparing the luminosity-weighted age and the ionization parameter (Figure 4), we find a clear anticorrelation. In Section 4.2.4. Figure 5 shows the distribution of the properties in the knots compared to those in the main body. In Section 5. P11695 has low levels of dust (AV < 1 mag), a low ionization parameter value (log(q) ∼ 6.8), and a quite young luminosity weighted age (log(LWA) ∼ 8.4). (Figure Presented).
Erratum: GASP. VII. Signs of Gas Inflow onto a Lopsided Galaxy (Astrophysical Journal (2018) 852 (94) DOI: 10.3847/1538-4357/aa992c)
Mapelli M.;
2018
Abstract
After the published paper was accepted, and during the preparation of the proof, an issue internal to the Publishing team occurred and a preliminary version of the manuscript was sent to the typesetters. As a result, the published paper does not correspond to the accepted version. While none of the conclusions and trends presented are affected, Figures 9, 10, 11, 13, and 18 in the published paper and the related text need to be amended. Values in the text should be updated accordingly in a few sentences as follows: In Section 3.5. The spatial distribution of the ionization parameter for P11695 is presented in Figure 1. It is generally low, ranging from 6.6 < log(q) < 7.3. This is in agreement with other galaxies in the GASP survey (Gullieuszik et al. 2017; Poggianti et al. 2017), even though in this case a clear clumpy pattern emerges, while in other galaxies a more smooth distribution is observed. Hα knots tend to have a systematically large value of q: the median value integrated across the entire galaxy is 6.8, while the median value in the Hα knots is 7. Figure 2 shows that the spatially resolved metallicity ranges between 8.3 < 12 + log(O H) < 9, with a median value of 8.6. Trends between metallicity and distance from the galaxy center are more clear in Figure 3. Along B, gradients are symmetric around the 0 position up to 5″, then the south side shows a constant decline and a sudden increase at r > 7″, while the north side of the galaxy shows some fluctuations. The minimum metallicity is log(O H) ∼ 8.4, while along A and B, for example, it is always .8.5. Finally, the E aperture catches one of the flattest gradients in the galaxy, with metallicity values >8.6 at all distances. In Section 3.6. Comparing the luminosity-weighted age and the ionization parameter (Figure 4), we find a clear anticorrelation. In Section 4.2.4. Figure 5 shows the distribution of the properties in the knots compared to those in the main body. In Section 5. P11695 has low levels of dust (AV < 1 mag), a low ionization parameter value (log(q) ∼ 6.8), and a quite young luminosity weighted age (log(LWA) ∼ 8.4). (Figure Presented).
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