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Erratum: "A Survey of C2H, HCN, and C18O in Protoplanetary Disks" (2019, ApJ, 876, 25)

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Published 2020 June 25 • © 2020. The American Astronomical Society. All rights reserved.
, , Citation Jennifer B. Bergner et al 2020 ApJ 896 176 DOI 10.3847/1538-4357/ab98f7

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1 Harvard University, Department of Chemistry and Chemical Biology, Cambridge, MA 02138, USA

2 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA

3 University of Michigan, Department of Astronomy, Ann Arbor, MI 48109, USA

4 National Radio Astronomical Observatory, Charlottesville, VA 22903, USA

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  1. Received 2020 May 28
  2. Accepted 2020 June 1
  3. Published

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In the published article, we calculated column densities (Equation (10)) using a column density equation adopted from Mangum & Shirley (2015). However, this equation is incompatible with the line strengths $S{\mu }^{2}$ taken from the line catalogs CDMS and JPL, due to differences in how S is defined. As a result, our column densities are underpredicted by a factor of 1/gu, where gu is the upper state degeneracy. We present updated column densities calculated according to:

Equation (1)

where $S{\mu }^{2}$ is the line intensity, $Q({T}_{\mathrm{ex}})$ is the partition function, Eu is the upper state energy, Tex is the excitation temperature, $\int {T}_{R}{dV}$ is the intensity of the main hyperfine component, and ${\tau }_{m}$ is the optical depth of the main hyperfine component.

Table 5 is revised and lists the updated disk-averaged column densities. Figures 4 and 6 are revised and show the updated radial column density profiles for C2H and HCN, respectively. Figure 12 is revised and shows the updated C2H column density profile in HD 163296. In these figures, we have also fixed an error affecting the deprojections of some sources. We note that with the fixed deprojection, the previously observed alignment between C2H column density minima and the candidate planet locations identified in HD 163296 by Teague et al. (2018) is less clear (Figure 12). Otherwise, these changes do not impact the subsequent discussion or conclusions presented in the published article.

Figure 4.

Figure 4. Deprojected and radially averaged C2H optical depth, excitation temperature, and column density profiles derived from hyperfine fitting. Lines represent the median of the down-sampled and pooled posteriors of all pixels in each radial bin, and shaded regions show 2σ confidence intervals. Purple and gray represent projections north and south of the source center along the disk major axis.

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Figure 6.

Figure 6. Deprojected and radially averaged HCN optical depth, excitation temperature, and column density profiles. For AS 209, HD 163296, V4046 Sgr, LkCa 15, and MWC 480, optical depths are derived from the H13CN isotopologue ratio. Shaded regions show uncertainties based on the standard deviations in the HCN/H13CN ratio and the HCN brightness temperature in each radial bin, as well as the uncertainty in the 12C/13C ratio. The beam major axes for HCN and H13CN are shown in the top panel for each source; arrows are used when the beam is larger than the x-axis range. For J1604-2130, profiles are derived from HCN hyperfine fitting. Lines represent the median of the down-sampled and pooled posteriors of all pixels in each radial bin, and shaded regions show 2σ confidence intervals. Blue and gray represent projections north and south of the source center along the disk major axis.

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Figure 12.

Figure 12. HD 163296 column density profile from Figure 4, overplotted with the locations of embedded planets at 83 au and 137 au identified by Teague et al. (2018).

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Table 5.  C2H and HCN Radial Extents and Disk-averaged Column Density Estimates

Source ${R}_{{{\rm{C}}}_{2}{\rm{H}}}$ (au) N(C2H) (1014 cm−2)   RHCN (au) N(HCN) (1013 cm−2)
    10 K 30 K     10 K 30 K
AS 209 115 18.0 [7.8] 9.7 [4.2]   105 37.4 [4.7] 19.5 [2.4]
CI Tau 115 11.9 [5.1] 6.4 [2.8]   ⋯ ⋯ ⋯
DM Tau 145 12.1 [5.2] 6.5 [2.8]   275 6.5 [0.8] 3.4 [0.4]
HD 163296 115 20.6 [8.9] 11.0 [4.8]   135 39.4 [4.9] 20.5 [2.6]
IM Lup 285 2.7 [1.2] 1.4 [0.6]   265 15.3 [1.9] 8.0 [1.0]
LkCa 15 185 10.8 [4.7] 5.8 [2.5]   345 6.2 [0.8] 3.2 [0.4]
MWC 480 105 26.4 [11.4] 14.1 [6.1]   245 6.4 [0.8] 3.3 [0.4]
HD 143006 115 5.6 [2.4] 3.0 [1.3]   95 47.8 [6.0] 24.9 [3.1]
J16042165 145 16.9 [7.3] 9.0 [3.9]   145 78.8 [9.8] 41.1 [5.1]
J16090075 75 11.4 [4.9] 6.1 [2.6]   65 35.9 [4.5] 18.7 [2.3]
V4046 Sgr 125 6.0 [2.6] 3.2 [1.4]   75 70.6 [8.8] 36.8 [4.6]

Note. The C2H and HCN radial extents correspond to the radius containing 80% of the line emission. The first listed numbers are corrected for an assumed optical depth of 2 for C2H and 8 for HCN; bracketed numbers are uncorrected (i.e., column density lower limits).

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10.3847/1538-4357/ab98f7