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|Title:||Erratum: "Detecting and Characterizing Young Quasars. I. Systemic Redshifts and Proximity Zones Measurements" (2020, ApJ, 900, 37)||Authors:||Eilers, Anna Christina
Hennawi, Joseph F.
Davies, Frederick B.
Farina, Emanuele P.
Schindler, Jan Torge
Simcoe, Robert A.
|Issue Date:||2021||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||914||Issue:||1||First Page:||74||Abstract:||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.||URI:||http://hdl.handle.net/20.500.12386/32101||URL:||https://api.elsevier.com/content/abstract/scopus_id/85109033002
|Appears in Collections:||1.01 Articoli in rivista|
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