Correction to: MaNGA AGN dwarf galaxies (MAD) – I. A new sample of AGNs in dwarf galaxies with spatially-resolved spectroscopy
Year: 2024
Type: erratum
Abstract: We report an error in the way stellar masses (|$M_\mathrm{*}$|) and star formation rates (SFRs) were computed in the paper MaNGA AGN dwarf galaxies (MAD) – I. A new sample of AGNs in dwarf galaxies with spatially-resolved spectroscopy (Mezcua & Domínguez Sánchez 2024). The stellar masses were taken from the NASA-Sloan Atlas (NSA catalog) version v1_0_1, which is the one used by MaNGA for its targeting1, while the SFRs were taken from the MaNGA data-analysis pipeline2 (DAP). In both cases the values are given in units of |$h^2$|, where h = 1, so in Mezcua & Domínguez Sánchez (2024) we multiplied the values of |$M_\mathrm{*}$| and SFR per |$h^2$| = 0.73|$^2$| to convert them to the |$\Lambda$|-CDM cosmology with parameters |$H_{0}=73$| km s|$^{-1}$| Mpc|$^{-1}$|, |$\Omega _{\Lambda }=0.73$| and |$\Omega _{m}=0.27$| adopted in the paper. Both the |$M_\mathrm{*}$| and SFRs should however have been divided by |$h^2$| = 0.73|$^2$|. When applying this correction, the values of |$M_\mathrm{*}$| and SFRs differ from those reported in Mezcua & Domínguez Sánchez (2024). We explain here the consequent modifications to the results reported in Mezcua & Domínguez Sánchez (2024). With the corrected stellar masses, the number of dwarf galaxies selected as having |$M_\mathrm{*} \lt 3 \times 10^{9}$| M|$_{\odot }$| drops from the 3400 sources reported in Mezcua & Domínguez Sánchez (2024) to 1131 sources. To preserve the statistics reported in Mezcua & Domínguez Sánchez (2024) while ensuring a robust analysis, we adopt the widely-used dwarf stellar mass threshold of |$M_\mathrm{*} \le 10^{10}$| M|$_{\odot }$| (e.g. Manzano-King & Canalizo 2020; Siudek, Mezcua & Krywult 2023; Bichang’a et al. 2024). This results in 3306 dwarf galaxies, whose distribution of stellar masses is shown in Fig. 1. Of these, 2292 galaxies have strong signs of AGN ionisation, defined as having |$n_{\text{agn-total}} \geq$|20, where |$n_{\text{agn-total}}$|is the total number of spaxels classified as either AGN, AGN-WHAN, or SF-AGN according to the emission line diagnostic classification of Mezcua & Domínguez Sánchez (2024). Out of these 2292 dwarf galaxies, 628 AGN, 1164 SF-AGN, 114 Composite, and 165 LINERs are identified (Fig. 2). These values are very similar to those reported in Mezcua & Domínguez Sánchez (2024), so that most of the results (AGN demographics, off-nuclear AGN, obscuration) are not affected by the corrected stellar masses and SFRs when applying the less restrictive mass selection criteria of |$M_\mathrm{*} \le 10^{10}$| M|$_{\odot }$| for dwarf galaxies. However, because the values of stellar masses and SFR were included in tables 1–2 of Mezcua & Domínguez Sánchez (2024), we provide here the updated tables with the corrected values (see Tables 1–2). Distribution of the NSA Petrosian stellar masses that are consistent within 0.5 dex with the Sérsic ones for the parent sample of 3306 unique dwarf galaxies, the sample of 2292 dwarf galaxies with strong indication of AGN ionization, and the sample of 628 AGN candidates. Flow chart summarizing the selection criteria. Exemplary10 rows of the sample of 2292 dwarf galaxies with strong AGN ionization features (|$n_{\text{agn-total}} \ge$| 20). Note.Column designation: (1) MaNGA plateifu; (2) MaNGA ID; (3,4) RA, Dec. coordinates of the optical centre of the galaxy or IFU centre; (5) galaxy redshift; (6) galaxy stellar mass; (7) galaxy star formation rate within the IFU FoV as provided by the MaNGA DAP (i.e. based on the H |${\alpha }$| flux and uncorrected for extinction); (8) MaNGA BPT classification; (9) AGNs in other diagnostics [radio, X-rays, mid-infrared (MIR), or coronal lines (CL)]. The full catalogue can be found in the online version of the paper. Broad-line AGNs among the sample of 2292 dwarf galaxies. Note.Column designation: (1) MaNGA plateifu; (2,3) RA, Dec. coordinates of the optical center of the galaxy or IFU center; (4) galaxy redshift; (5) galaxy stellar mass; (6) MaNGA BPT classification; (7, 8) FWHM and luminosity of the broad H |$\alpha$| emission line component; (9) BH mass derived from the broad H |$\alpha$| component; (10) Reference for columns 7, 8, 9. The typical uncertainties of the BH masses are of 0.5 dex. aThis source has also been recently reported as a broad-line AGN by Fu et al. (2023). In Mezcua & Domínguez Sánchez (2024) the bolometric luminosity (|$L_\mathrm{bol}$|) for the sub-sample of AGN was derived from the median of the [O iii] luminosity of those spaxels classified as either AGN or Composite in the [N ii]-BPT and assuming a bolometric correction factor of 1000 (Moran et al. 2014). This yielded log |$L_\mathrm{bol} \lt 10^{42}$| erg s|$^{-1}$|, consistent with low-luminosity AGN (e.g. Mezcua & Prieto 2014) and lower than those of X-ray selected AGN dwarves (Mezcua et al. 2018), and seemed to indicate that those MaNGA AGN not identified as such when using integrated SDSS spectra were fainter that those AGN identified using both SDSS and MaNGA integral-field spectroscopy. In the case of galaxies for which all or most of the spaxels in the MaNGA IFU coverage are dominated by AGN ionization, the [O iii] luminosity integrated over the IFU field of view is one or two orders of magnitude larger than that obtained from the median of the [O iii] luminosity over all the spaxels. To avoid such an underestimation of the [O iii] luminosity and thus of the bolometric luminosity, we report here the bolometric luminosity for the sub-sample of AGN derived as the sum (rather than the median) of the [O iii] luminosities of all the AGN- or Composite-ionized spaxels. This yields log |$L_\mathrm{bol}$| = 39.3–44.3 erg s|$^{-1}$|, with most (83 per cent) of the sources still being low-luminosity AGN (see Fig. 3). The |$L_\mathrm{bol}$| ranges from log |$L_\mathrm{bol}$| = 40.3 to 44.3 erg s|$^{-1}$| for those AGN that are also SDSS AGN, while log |$L_\mathrm{bol}$| = 39.9–43.6 erg s|$^{-1}$| for those AGN missed by the SDSS. Those sources unidentified as AGN by the integrated SDSS spectra seem thus to be fainter AGN even with these newly reported |$L_\mathrm{bol}$|. Distribution of the bolometric luminosity for the AGNs (red bars), the AGNs that are also identified as AGNs by SDSS (purple bars), and the X-ray sample of AGN dwarf galaxies from Mezcua et al. (2018, blue bars).
Authors: M Mezcua, H Domínguez Sánchez
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: gold
Estimated APC paid: $3,012
OpenAlex ID: W4405228438