The effects of diffuse ionized gas and spatial resolution on metallicity gradients: TYPHOON two-dimensional spectrophotometry of M83

Poetrodjojo, Henry; D'Agostino, Joshua; Groves, Brent; Kewley, Lisa J.; Ho, I-Ting; Rich, Jeffrey A.; Madore, Barry F.; Seibert, Mark

doi:10.1093/mnras/stz1241

Cited by 70 publications

(84 citation statements)

References 73 publications

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“…Strong line metallicity prescriptions produce well established differences in inferred metallicity and radial gradients in galaxies (Kewley & Ellison 2008;Poetrodjojo et al 2019). In Figure 20 we present best-fitting radial metallicity gradients using four different prescriptions.…”

Section: Metallicity Prescriptionsmentioning

confidence: 70%

“…DIG is detected predominantly in the Hα, Hβ, [NII] and [SII] line maps, as these lines are strongly emitted in the low density, high temperature diffuse gas (Haffner et al 2009). One major advantage of the high physical resolution of the maps employed in this work is that we can spatially distinguish HII re-gions from the surrounding diffuse emission, which when blended over larger apertures has been shown to artificially flatten metallicity gradients (Poetrodjojo et al 2019). The emission line fluxes and Hα luminosities reported here do not include any correction for the diffuse ionized gas background contributing to the integrated line flux, as seen in projection against any given HII region.…”

Section: Diffuse Ionized Gasmentioning

confidence: 99%

“…Large optical IFU projects that survey hundreds to thousands of galaxies (CALIFA -the Calar Alto Legacy Integral Field Area Survey, Sánchez et al 2012; MaNGA -Mapping Nearby Galaxies at Apache Point Observatory , Bundy et al 2015; SAMI-Sydney-AAO Multi-object Integral-field spectrograph, Bryant et al 2015) trade sample size for spatial resolution, achieving ∼kpc spatial resolution. While having the obvious advantage of large statistical samples, this can introduce undesirable systematic effects when inferring metallicity, as multiple ionization sources can contribute within a single resolution element (Ho et al 2018;Poetrodjojo et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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Mapping Metallicity Variations across Nearby Galaxy Disks

Kreckel

Blanc

et al. 2019

ApJ

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168

196

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The distribution of metals within a galaxy traces the baryon cycle and the buildup of galactic disks, but the detailed gas phase metallicity distribution remains poorly sampled. We have determined the gas phase oxygen abundances for 7,138 HII regions across the disks of eight nearby galaxies using VLT/MUSE optical integral field spectroscopy as part of the PHANGS-MUSE survey. After removing the first order radial gradients present in each galaxy, we look at the statistics of the metallicity offset (∆O/H) and explore azimuthal variations. Across each galaxy, we find low (σ=0.03-0.05 dex) scatter at any given radius, indicative of efficient mixing. We compare physical parameters for those HII regions that are 1σ outliers towards both enhanced and reduced abundances. Regions with enhanced abundances have high ionization parameter, higher Hα luminosity, lower Hα velocity dispersion, younger star clusters and associated molecular gas clouds show higher molecular gas densities. This indicates recent star formation has locally enriched the material. Regions with reduced abundances show increased Hα velocity dispersions, suggestive of mixing introducing more pristine material. We observe subtle azimuthal variations in half of the sample, but can not always cleanly associate this with the spiral pattern. Regions with enhanced and reduced abundances are found distributed throughout the disk, and in half of our galaxies we can identify subsections of spiral arms with clearly associated metallicity gradients. This suggests spiral arms play a role in organizing and mixing the ISM.

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Section: Metallicity Prescriptionsmentioning

confidence: 70%

Section: Diffuse Ionized Gasmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Mapping Metallicity Variations across Nearby Galaxy Disks

Kreckel

Blanc

et al. 2019

ApJ

Self Cite

168

196

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“…However, the selection of star forming regions through the BPT diagram as discussed above helps to largely exclude DIG regions. To further exclude spaxels that are potentially affected by DIG, we apply an additional criterion by only selecting spaxels with [SII]/Hα> 0.29 as suggested by Poetrodjojo et al (2019). With these selection criteria 1, 162 galaxies are selected.…”

Section: Sample Selectionmentioning

confidence: 99%

SDSS-IV MaNGA: environmental dependence of gas metallicity gradients in local star-forming galaxies

Lian

Thomas

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Within the standard model of hierarchical galaxy formation in a ΛCDM Universe, the environment of galaxies is expected to play a key role in driving galaxy formation and evolution. In this paper we investigate whether and how the gas metallicity and the star formation surface density (Σ SFR ) depend on galaxy environment. To this end we analyse a sample of 1162 local, star-forming galaxies from the galaxy survey Mapping Nearby Galaxies at APO (MaNGA). Generally, both parameters do not show any significant dependence on environment. However, in agreement with previous studies, we find that low-mass satellite galaxies are an exception to this rule. The gas metallicity in these objects increases while their Σ SFR decreases slightly with environmental density. The present analysis of MaNGA data allows us to extend this to spatially resolved properties. Our study reveals that the gas metallicity gradients of low-mass satellites flatten and their Σ SFR gradients steepen with increasing environmental density. By extensively exploring a chemical evolution model, we identify two scenarios that are able to explain this pattern: metal-enriched gas accretion or pristine gas inflow with varying accretion timescales. The latter scenario better matches the observed Σ SFR gradients, and is therefore our preferred solution. In this model, a shorter gas accretion timescale at larger radii is required. This suggests that 'outside-in quenching' governs the star formation processes of low-mass satellite galaxies in dense environments.

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“…Examples include ATLAS 3D , Spitzer Infrared Nearby Galaxies Survey (SINGS, Daigle et al 2006), Virgo high-resolution Hα kinematical survey (VIRGO, Chemin et al 2006), Gassendi Hα survey of SPirals (GHASP, Garrido et al 2002;Epinat et al 2008), Calar Alto Legacy Integral Field Area survey (CALIFA, Sánchez et al 2012), VIRUS-P Exploration of Nearby Galaxies (VENGA, Blanc et al 2013), Mapping Nearby Galaxies at Apache Point Observatory (MANGA, Bundy et al 2015;Yan & MaNGA Team 2016), SAMI survey (Konstantopoulos et al 2013), Las Campanas Observatory PrISM Survey (a.k.a. TYPHOON, Poetrodjojo et al 2019), and Physics at High Angular resolution in Nearby Galaxies (PHANGS, Rosolowsky et al 2019). In these surveys, star formation, chemical enrichment processes, and the gas and stellar kinematics were targeted.…”

mentioning

confidence: 99%

SIGNALS: I. Survey description

Rousseau-Nepton

Martin

Robert

et al. 2019

Monthly Notices of the Royal Astronomical Society

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SIGNALS, the Star formation, Ionized Gas, and Nebular Abundances Legacy Survey, is a large observing program designed to investigate massive star formation and H II regions in a sample of local extended galaxies. The program will use the imaging Fourier transform spectrograph SITELLE at the Canada-France-Hawaii Telescope. Over 355 hours (54.7 nights) have been allocated beginning in fall 2018 for eight consecutive semesters. Once completed, SIGNALS will provide a statistically reliable laboratory to investigate massive star formation, including over 50 000 resolved H II regions : the largest, most complete, and homogeneous database of spectroscopically and spatially resolved extragalactic H II regions ever assembled. For each field observed, three datacubes covering the spectral bands of the filters SN1 (363 -386 nm), SN2 (482 -513 nm), and SN3 (647 -685 nm) are gathered. The spectral resolution selected for each spectral band is 1000, 1000, and 5000, respectively. As defined, the project sample will facilitate the study of small-scale nebular physics and many other phenomena linked to star formation at a mean spatial resolution of ∼20 pc. This survey also has considerable legacy value for additional topics including planetary nebulae, diffuse ionized gas, and supernova remnants. The purpose of this paper is to present a general outlook of the survey, notably the observing strategy, galaxy sample, and science requirements.

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The effects of diffuse ionized gas and spatial resolution on metallicity gradients: TYPHOON two-dimensional spectrophotometry of M83

Cited by 70 publications

References 73 publications

Mapping Metallicity Variations across Nearby Galaxy Disks

Mapping Metallicity Variations across Nearby Galaxy Disks

SDSS-IV MaNGA: environmental dependence of gas metallicity gradients in local star-forming galaxies

SIGNALS: I. Survey description

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