TY - JOUR
T1 - Erratum
T2 - Detecting and Characterizing Young Quasars. I. Systemic Redshifts and Proximity Zones Measurements (The Astrophysical Journal (2020) 900 (37) DOI: 10.3847/1538-4357/aba52e)
AU - Eilers, Anna Christina
AU - Hennawi, Joseph F.
AU - Decarli, Roberto
AU - Davies, Frederick B.
AU - Venemans, Bram
AU - Walter, Fabian
AU - Banados, Eduardo
AU - Fan, Xiaohui
AU - Farina, Emanuele P.
AU - Mazzucchelli, Chiara
AU - Novak, Mladen
AU - Schindler, Jan Torge
AU - Simcoe, Robert A.
AU - Wang, Feige
AU - Yang, Jinyi
N1 - Publisher Copyright:
© 2021 Institute of Physics Publishing. All rights reserved.
PY - 2021/6/10
Y1 - 2021/6/10
N2 - Due to an error in the analysis of the ALMA data, the [C II] line fluxes Fline in 6 out of the 13 analyzed quasars were underestimated, and thus also based the inferred star formation rate (SFR) on the [C II] emission. We corrected these values and show the updated measurements for the six affected quasars in the corrected Table 2. The dust continuum estimates and their derived quantities were not affected by the error. Additionally, the observed peak frequency of the [C II] emission line nobs and thus the inferred systemic redshifts of the quasars were mildly offset, causing a shift of Dnobs ? 0.02 GHz and - Dzsub mm ? 0.0005. The derived proximity zone sizes were hence affected byDRp ? 0.04 pMpc. All updated values are shown in the corrected Tables 2 and 4. These changes did not affect any of the conclusions of the paper, nor did the figures in the paper change in any noticeable way. Furthermore, since the publication of our paper the offset between the peak of the Mg II emission line and the systemic redshift derived from submillimeter emission lines estimated by Schindler et al. (2020) changed slightly in their published version compared to the preliminary value we had used. Thus we use the now published velocity offset of Dv(Mg II-[C II]) = - - 391+ km s- 455 256 1 to estimate the systemic redshifts of the three quasars in our sample, for which no submillimeter data are available and therefore the redshift estimate is based on the Mg II emission. This resulted in minor changes of Dz ? 0.001, which are updated in Table 4.
AB - Due to an error in the analysis of the ALMA data, the [C II] line fluxes Fline in 6 out of the 13 analyzed quasars were underestimated, and thus also based the inferred star formation rate (SFR) on the [C II] emission. We corrected these values and show the updated measurements for the six affected quasars in the corrected Table 2. The dust continuum estimates and their derived quantities were not affected by the error. Additionally, the observed peak frequency of the [C II] emission line nobs and thus the inferred systemic redshifts of the quasars were mildly offset, causing a shift of Dnobs ? 0.02 GHz and - Dzsub mm ? 0.0005. The derived proximity zone sizes were hence affected byDRp ? 0.04 pMpc. All updated values are shown in the corrected Tables 2 and 4. These changes did not affect any of the conclusions of the paper, nor did the figures in the paper change in any noticeable way. Furthermore, since the publication of our paper the offset between the peak of the Mg II emission line and the systemic redshift derived from submillimeter emission lines estimated by Schindler et al. (2020) changed slightly in their published version compared to the preliminary value we had used. Thus we use the now published velocity offset of Dv(Mg II-[C II]) = - - 391+ km s- 455 256 1 to estimate the systemic redshifts of the three quasars in our sample, for which no submillimeter data are available and therefore the redshift estimate is based on the Mg II emission. This resulted in minor changes of Dz ? 0.001, which are updated in Table 4.
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U2 - 10.3847/1538-4357/ac05c3
DO - 10.3847/1538-4357/ac05c3
M3 - Comment/debate
AN - SCOPUS:85109033002
SN - 0004-637X
VL - 914
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 74
ER -