Context. GDS J033218.92-275302.7 (here GS-14) is a z? 5.5 galaxy with unusual UV spectral features that have been interpreted as signatures of either a double stellar population or of an active galactic nucleus (AGN). GS-14 was detected in [Câ ¯II] 158 μm as part of the ALPINE survey and was found to be the galaxy with the lowest molecular gas fraction (fmolâ =â Mmolgas/(Mmolgas+M∗)?0.1) of that sample. Aims. We exploited the multiwavelength coverage of GS-14 to investigate the properties and the origin of its emission. Methods. We fit the UV-to-near-IR spectral energy distribution (SED) with a single and double stellar population and/or AGN component. We analyzed the latest release of the VIMOS spectrum, which shows highly ionized emission lines (Oâ ¯VI1032 Ã, Nâ ¯V1240 Ã, and Nâ ¯IV] 1483,1486 Ã). The line equivalent widths and line ratios were compared with those observed in galaxies and AGN, as well as with the predictions from radiation transfer models for star-forming galaxies, AGN, and shocks. Results. The SED-fitting provides a total stellar mass of M∗â =â (4±1)Ã- 1010â Mâ , an age of the main stellar population of ? 670 Myr, and a recent (? 8 Myr) short burst of star formation (SF) of ?90â Mâ â yr1. We do not find a significant contribution from an AGN, although we do not have any coverage in the mid-IR, where the dust emission of the AGN would peak. The Nâ ¯V line has a characteristic P Cygni profile. Fitting it with stellar models suggests a ? 3 Myr old population of stars with a mass of ?5Ã - 107â Mâ, consistent with a second component of young stars, as found in the SED-fitting analysis. The Nâ ¯V profile also shows evidence for an additional component of nebular emission. The comparison of the line ratios (Nâ ¯IV]/Nâ ¯V and Oâ ¯VI/Nâ ¯V) with theoretical models allows us to associate the emission with SF or AGN, but the strong radiation field required to ionize the Oâ ¯VI is more commonly related to AGN activity. Conclusions. Studying GS-14, we found evidence for an old and already evolved stellar population at z? 5.5, and we show that the galaxy is experiencing a second short burst of SF. In addition, GS-14 carries signatures of obscured AGN activity. The AGN could be responsible for the short depletion time of this galaxy, thus making GS-14 one of the two ALPINE sources with indications of an active nucleus and an interesting target for future follow-ups to understand the connection between SF and AGN activity.
Barchiesi L., Dessauges-Zavadsky M., Vignali C., Pozzi F., Marques-Chaves R., Feltre A., et al. (2023). The ALPINE-ALMA [CII] survey: Double stellar population and active galactic nucleus activity in a galaxy at z ? 5.5. ASTRONOMY & ASTROPHYSICS, 675, A30-A30 [10.1051/0004-6361/202244838].
The ALPINE-ALMA [CII] survey: Double stellar population and active galactic nucleus activity in a galaxy at z ? 5.5
Barchiesi L.Writing – Original Draft Preparation
;Vignali C.Membro del Collaboration Group
;Pozzi F.Membro del Collaboration Group
;
2023
Abstract
Context. GDS J033218.92-275302.7 (here GS-14) is a z? 5.5 galaxy with unusual UV spectral features that have been interpreted as signatures of either a double stellar population or of an active galactic nucleus (AGN). GS-14 was detected in [Câ ¯II] 158 μm as part of the ALPINE survey and was found to be the galaxy with the lowest molecular gas fraction (fmolâ =â Mmolgas/(Mmolgas+M∗)?0.1) of that sample. Aims. We exploited the multiwavelength coverage of GS-14 to investigate the properties and the origin of its emission. Methods. We fit the UV-to-near-IR spectral energy distribution (SED) with a single and double stellar population and/or AGN component. We analyzed the latest release of the VIMOS spectrum, which shows highly ionized emission lines (Oâ ¯VI1032 Ã, Nâ ¯V1240 Ã, and Nâ ¯IV] 1483,1486 Ã). The line equivalent widths and line ratios were compared with those observed in galaxies and AGN, as well as with the predictions from radiation transfer models for star-forming galaxies, AGN, and shocks. Results. The SED-fitting provides a total stellar mass of M∗â =â (4±1)Ã- 1010â Mâ , an age of the main stellar population of ? 670 Myr, and a recent (? 8 Myr) short burst of star formation (SF) of ?90â Mâ â yr1. We do not find a significant contribution from an AGN, although we do not have any coverage in the mid-IR, where the dust emission of the AGN would peak. The Nâ ¯V line has a characteristic P Cygni profile. Fitting it with stellar models suggests a ? 3 Myr old population of stars with a mass of ?5Ã - 107â Mâ, consistent with a second component of young stars, as found in the SED-fitting analysis. The Nâ ¯V profile also shows evidence for an additional component of nebular emission. The comparison of the line ratios (Nâ ¯IV]/Nâ ¯V and Oâ ¯VI/Nâ ¯V) with theoretical models allows us to associate the emission with SF or AGN, but the strong radiation field required to ionize the Oâ ¯VI is more commonly related to AGN activity. Conclusions. Studying GS-14, we found evidence for an old and already evolved stellar population at z? 5.5, and we show that the galaxy is experiencing a second short burst of SF. In addition, GS-14 carries signatures of obscured AGN activity. The AGN could be responsible for the short depletion time of this galaxy, thus making GS-14 one of the two ALPINE sources with indications of an active nucleus and an interesting target for future follow-ups to understand the connection between SF and AGN activity.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
