SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies

Sánchez, S. F.; Barrera-Ballesteros, J. K.; Lacerda, E. A. D.; Mejía-Narváez, Alfredo; Camps-Fariña, A.; Bruzual, G.; Espinosa-Ponce, C.; Rodríguez-Puebla, Aldo; Calette, A. R.; Ibarra-Medel, H.; Ávila-Reese, V.; Hernández-Toledo, H. M.; Bershady, Matthew A.; Cano-Díaz, M.; Munguia-Cordova, A. M.

doi:10.3847/1538-4365/ac7b8f

Cited by 73 publications

(43 citation statements)

References 188 publications

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“…This log-normal distribution for the stellar masses of AGN in MaNGA was previously seen in Paper I and Sanchez et al (2022). The AGN fraction peaks around log(M/M e ) = 10.5-11.0 because of the selection biases imposed by the BPT+WHAN selection criteria (Section 4).…”

Section: Control Samplesupporting

confidence: 72%

SDSS-IV MaNGA: How Galaxy Interactions Influence Active Galactic Nuclei

Steffen

Brownstein

et al. 2023

ApJ

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We present a comparative study of active galactic nuclei (AGN) between galaxy pairs and isolated galaxies with the final data release of the MaNGA integral field spectroscopic survey. We build a sample of 391 kinematic galaxy pairs within the footprint of the survey and select AGN using the survey's spectra. We use the comoving volume densities of the AGN samples to quantify the effects that tidal interactions have on the triggering of nuclear accretion. Our hypothesis is that the pair sample contains AGN that are triggered by not only stochastic accretion but also tidally induced accretion and correlated accretion. With the level of stochastically triggered AGN fixed by the control sample, we model the strength of tidally induced accretion and correlated accretion as a function of projected separation (r p ) and compare the model expectations with the observed volume densities of dual AGN and offset AGN (single AGN in a pair). At r p ∼ 10 kpc, we find that tidal interactions induce ∼30% more AGN than stochastic fueling and cause ∼12% of the offset AGN to become dual AGN because of correlations. The strength of both these effects decreases with increasing r p . We also find that the [O iii] luminosities of the AGN in galaxy pairs are consistent with those found in isolated galaxies, likely because stochastically fed AGN dominate even among close pairs. Our results illustrate that while we can detect tidally induced effects statistically, it is challenging to separate tidally induced AGN and stochastically triggered AGN in interacting galaxies.

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Section: Control Samplesupporting

confidence: 72%

SDSS-IV MaNGA: How Galaxy Interactions Influence Active Galactic Nuclei

Steffen

Brownstein

et al. 2023

ApJ

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“…Additionally, our reconstructed SFHs are robust to multiple episodes of star formation/quenching, which played an important role in our results. The stellar masses and SFRs derived from our reconstructed SFHs are consistent with the publicly released PIPE3D stellar masses and SFRs (Sánchez et al 2016b(Sánchez et al , 2022.…”

Section: Star Formation History Reconstructionsupporting

confidence: 84%

Active Galactic Nuclei Feedback in SDSS-IV MaNGA: AGNs Have Suppressed Central Star Formation Rates

Lammers,

Iyer,

Ibarra-Medel

et al. 2023

ApJ

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Despite the importance of feedback from active galactic nuclei (AGNs) in models of galaxy evolution, observational constraints on the influence of AGN feedback on star formation remain weak. To this end, we have compared the star formation trends of 279 low-redshift AGN galaxies with 558 inactive control galaxies using integral field unit spectroscopy from the Sloan Digital Sky Survey-IV Mapping Nearby Galaxies at Apache Point Observatory survey. With a Gaussian-process-based methodology, we reconstruct nonparametric star formation histories in spatially resolved spaxels covering the face of each galaxy. Based on the galaxy-wide star formation rates (SFRs) alone, we find no obvious signatures of AGN feedback. However, the AGN galaxies have significantly suppressed central (kiloparsec-scale) SFRs, lying up to a factor of 2 below those of the control galaxies, providing direct observational evidence of AGN feedback suppressing star formation. The suppression of central SFRs in the AGN galaxies began in the central regions ∼6 Gyr ago (redshift z ∼ 0.7), taking place over a few gigayears. A small subset of the AGN galaxies were rapidly driven to quiescence shortly before being observed (in the last 500 Myr), potentially indicating instances of AGN-driven feedback. More frequently, however, star formation continues in the AGN galaxies, with suppression primarily in the central regions. This is suggestive of a picture in which integrated (gigayear-timescale) AGN feedback can significantly affect central star formation, but may be inefficient in driving galaxy-wide quenching in low-redshift galaxies, instead leaving them in the green valley.

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“…In particular, the star formation rate in each galaxy is estimated with the dust-corrected Hα luminosity using the relationship proposed by Robert C. Kennicutt (1998). This measurement should be treated as an upper limit since the PIPE3D uses the integrated Hα flux, which could include contamination of regions where the ionization source is not related to recent star formation events (see Sánchez et al 2022). We note that our classification is biased towards higher star formation rates and lower stellar masses.…”

Section: Hosts Of Emission-line Galaxiesmentioning

confidence: 99%

Classifying the full SDSS-IV MaNGA Survey using optical diagnostic diagrams: Presentation of AGN catalogs in flexible apertures

M.¹,

Wylezalek²

2023

A&A

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Accurate active galactic nucleus (AGN) identifications in large galaxy samples are crucial for the assessment of the role of AGN and AGN feedback in the co-evolution of galaxies and their central supermassive black holes. Emission-line flux-ratio diagnostics are commonly used to identify AGN in optical spectra. New large samples of integral field unit observations allow exploration of the role of aperture size in the classification process. In this paper, we present galaxy classifications for all 10 010 galaxies observed within the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey. We use Baldwin-Philips-Terlevich line fluxratio diagnostics combined with an Hα equivalent threshold in 60 apertures of varying size for the classification, and provide the corresponding catalogs. MaNGA-selected AGN primarily lie below the main sequence of star-forming galaxies, and reside in massive galaxies with stellar masses of ∼ 10 11 M ⊙ and a median Hα-derived star formation rate of ∼ 1.44M ⊙ yr −1 . We find that the number of "fake" AGN increases significantly beyond selection apertures of > 1.0 R e f f because of increased contamination from diffuse ionized gas (DIG). A comparison with previous works shows that the treatment of the underlying stellar continuum and flux measurements can significantly impact galaxy classification. Our work provides the community with AGN catalogs and galaxy classifications for the full MaNGA survey.

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SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies

Cited by 73 publications

References 188 publications

SDSS-IV MaNGA: How Galaxy Interactions Influence Active Galactic Nuclei

SDSS-IV MaNGA: How Galaxy Interactions Influence Active Galactic Nuclei

Active Galactic Nuclei Feedback in SDSS-IV MaNGA: AGNs Have Suppressed Central Star Formation Rates

Classifying the full SDSS-IV MaNGA Survey using optical diagnostic diagrams: Presentation of AGN catalogs in flexible apertures

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