Unique Tracks Drive the Scatter of the Spatially Resolved Star Formation Main Sequence

Hall, Christine; Courteau, Stéphane; Jarrett, T. H.; Cluver, Michelle; Meurer, G. R.; Carignan, C.; Audcent-Ross, Fiona

doi:10.3847/1538-4357/aadee1

Cited by 38 publications

(43 citation statements)

References 109 publications

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“…There are hints of a decreasing scatter with increasing stellar mass, from 0.35 to 0.23. Once again, these values fall within the typical ranges of 0.15-0.35 reported in the literature for the spatially resolved MS (Conselice et al 2016;Magdis et al 2016;Maragkoudakis et al 2017;Hall et al 2018). The importance of the scatter and the way it relates with the gas properties is explored in Morselli et al (in prep).…”

Section: Spatially Resolved Mssupporting

confidence: 77%

“…In this Section, we thus compare our panchromatic results with the spatially resolved MS relations obtained with data from CALIFA (Cano-Díaz et al 2016), MaNGA (Hsieh et al 2017;Cano-Díaz et al 2019;Bluck et al 2019), and SAMI (Medling et al 2018). For completeness, we also compare our results with the MS relations of Abdurro'uf & Akiyama (2017), that perform pixel-bypixel SED fitting to GALEX and SDSS photometry of local (0.01 < z < 0.02) massive spiral galaxies selected in the MPI-JHU (Max Planck Institute for Astrophysics-Johns Hopkins University), and of Hall et al (2018), obtained for a sample of 355 nearby galaxies, with spatially resolved observations of Hα and mid-IR emission.…”

Section: Comparison With Other Resolved Star-forming Main Sequencesmentioning

confidence: 85%

“…4.2) that usually span the range 0.7 − 1.1 despite using different SFR tracers and different redshift and stellar mass ranges for the analysis (i.e. Pérez et al 2013;Wuyts et al 2013;Hemmati et al 2014;Cano-Díaz et al 2016;González Delgado et al 2016;Abdurro'uf & Akiyama 2017;Abdurro'uf 2018;Hall et al 2018;Cano-Díaz et al 2019). It is worth noting that several of the literature works implement the orthogonal distance regression (ODR) method to find the location of the MS relation.…”

Section: Spatially Resolved Msmentioning

confidence: 99%

“…(2019). On the other hand, Hall et al (2018) reach lower Σ SFR thanks to the combination of H α and mid-IR data, but has the drawback that low Σ SFR only trace obscured SF.…”

Section: Referencementioning

confidence: 99%

“…Medling et al (2018) estimated the MS from ∼ 800 galaxies in the Sydney AAO Multi-object Integral Field Galaxy Survey (SAMI, Croom et al 2012) at z < 0.1, finding a slope of 1.0. Hall et al (2018) studied the spatially resolved MS in a sample of 93 nearby galaxies drawn from the Survey for Ionized Neutral Gas in Galaxies (SINGG, Meurer et al 2006) and the Wide-field Infrared Survey Explorer (WISE, Wright et al 2010) on scales ranging from 50pc to 10kpc. They find that the slope, scatter and normalisation of the relation do not vary when changing the spatial scale, up to 1-1.5kpc.…”

Section: Introductionmentioning

confidence: 99%

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A panchromatic spatially resolved analysis of nearby galaxies – I. Sub-kpc-scale main sequence in grand-design spirals

Enia

Rodighiero

Morselli

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We analyse the spatially resolved relation between stellar mass (M ) and star formation rate (SFR) in disk galaxies (i.e. the Main Sequence, MS). The studied sample includes eight nearby face-on grand-design spirals, e.g. the descendant of high-redshift, rotationally-supported star-forming galaxies. We exploit photometric information over 23 bands, from the UV to the far-IR, from the publicly available DustPedia database to build spatially resolved maps of stellar mass and star formation rates on sub-galactic scales of 0.5-1.5 kpc, by performing a spectral energy distribution fitting procedure that accounts for both the observed and the obscured star formation processes, over a wide range of internal galaxy environments (bulges, spiral arms, outskirts). With more than 30 thousands physical cells, we have derived a definition of the local spatially resolved MS per unit area for disks, log(Σ SF R )=0.82log(Σ * )-8.69. This is consistent with the bulk of recent results based on optical IFU, using the Hα line emission as a SFR tracer. Our work extends the analysis at lower sensitivities in both M and SFR surface densities, up to a factor ∼ 10. The self consistency of the MS relation over different spatial scales, from sub-galactic to galactic, as well as with a rescaled correlation obtained for high redshift galaxies, clearly proves its universality.

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Section: Spatially Resolved Mssupporting

confidence: 77%

Section: Comparison With Other Resolved Star-forming Main Sequencesmentioning

confidence: 85%

Section: Spatially Resolved Msmentioning

confidence: 99%

“…(2019). On the other hand, Hall et al (2018) reach lower Σ SFR thanks to the combination of H α and mid-IR data, but has the drawback that low Σ SFR only trace obscured SF.…”

Section: Referencementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A panchromatic spatially resolved analysis of nearby galaxies – I. Sub-kpc-scale main sequence in grand-design spirals

Enia

Rodighiero

Morselli

et al. 2020

Monthly Notices of the Royal Astronomical Society

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High-resolution, 3D radiative transfer modelling

Nersesian

Viaene

Baes

et al. 2020

A&A

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Context. Investigating the dust heating mechanisms in galaxies provides a deeper understanding of how the internal energy balance drives their evolution. Over the last decade radiative transfer simulations based on the Monte Carlo method have emphasised the role of the various stellar populations heating the diffuse dust. Beyond the expected heating through ongoing star formation, older stellar populations (≥8 Gyr) and even active galactic nuclei can both contribute energy to the infrared emission of diffuse dust. Aims. In this particular study we examine how the radiation of an external heating source, such as the less massive galaxy NGC 5195 in the M 51 interacting system, could affect the heating of the diffuse dust of its parent galaxy NGC 5194, and vice versa. Our goal is to quantify the exchange of energy between the two galaxies by mapping the 3D distribution of their radiation field. Methods. We used SKIRT, a state-of-the-art 3D Monte Carlo radiative transfer code, to construct the 3D model of the radiation field of M 51, following the methodology defined in the DustPedia framework. In the interest of modelling, the assumed centre-to-centre distance separation between the two galaxies is ∼10 kpc. Results. Our model is able to reproduce the global spectral energy distribution of the system, and it matches the resolved optical and infrared images fairly well. In total, 40.7% of the intrinsic stellar radiation of the combined system is absorbed by dust. Furthermore, we quantify the contribution of the various dust heating sources in the system, and find that the young stellar population of NGC 5194 is the predominant dust-heating agent, with a global heating fraction of 71.2%. Another 23% is provided by the older stellar population of the same galaxy, while the remaining 5.8% has its origin in NGC 5195. Locally, we find that the regions of NGC 5194 closer to NGC 5195 are significantly affected by the radiation field of the latter, with the absorbed energy fraction rising up to 38%. The contribution of NGC 5195 remains under the percentage level in the outskirts of the disc of NGC 5194. This is the first time that the heating of the diffuse dust by a companion galaxy is quantified in a nearby interacting system.

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Molecular gas and star formation within 12 strong galactic bars observed with IRAM-30 m

Díaz-García

Lisenfeld

Pérez

et al. 2021

A&A

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Context. While some galactic bars show recent massive star formation (SF) along them, some others do not. Whether bars with low level of SF are a consequence of low star formation efficiency, low gas inflow rate, or dynamical effects remains a matter of debate. Aims. In order to study the physical conditions that enable or prevent SF, we perform a multi-wavelength analysis of 12 strongly barred galaxies with total stellar masses log10(M⋆/M⊙)∈[10.2, 11], chosen to host different degrees of SF along the bar major axis without any prior condition on gas content. We observe the CO(1–0) and CO(2–1) emission within bars with the IRAM-30 m telescope (beam sizes of 1.7–3.9 kpc and 0.9–2.0 kpc, respectively; 7–8 pointings per galaxy on average). Methods. We estimated molecular gas masses (Mmol) from the CO(1–0) and CO(2–1) emissions. SF rates (SFRs) were calculated from GALEX near-ultraviolet (UV) and WISE 12 μm images within the beam-pointings, covering the full bar extent (SFRs were also derived from far-UV and 22 μm). Results. We detect molecular gas along the bars of all probed galaxies. Molecular gas and SFR surface densities span the ranges log10(Σmol/[M⊙ pc−2]) ∈ [0.4,2.4] and log10(ΣSFR/[M⊙ pc−1 kpc−2]]) ∈ [−3.25, −0.75], respectively. The star formation efficiency (SFE; i.e., SFR/Mmol) in bars varies between galaxies by up to an order of magnitude (SFE ∈[0.1, 1.8] Gyr−1). On average, SFEs are roughly constant along bars. SFEs are not significantly different from the mean value in spiral galaxies reported in the literature (∼0.43 Gyr−1), regardless of whether we estimate Mmol from CO(1–0) or CO(2–1). Interestingly, the higher the total stellar mass of the host galaxy, the lower the SFE within their bars. In particular, the two galaxies in our sample with the lowest SFE and ΣSFR (NGC 4548 and NGC 5850, SFE ≲ 0.25 Gyr−1, ΣSFR ≲ 10−2.25 M⊙ yr−1 kpc−2, M⋆ ≳ 1010.7 M⊙) are also those hosting massive bulges and signs of past interactions with nearby companions. Conclusions. We present a statistical analysis of the SFE in bars for a sample of 12 galaxies. The SFE in strong bars is not systematically inhibited (either in the central, middle, or end parts of the bar). Both environmental and internal quenching are likely responsible for the lowest SFEs reported in this work.

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Unique Tracks Drive the Scatter of the Spatially Resolved Star Formation Main Sequence

Cited by 38 publications

References 109 publications

A panchromatic spatially resolved analysis of nearby galaxies – I. Sub-kpc-scale main sequence in grand-design spirals

A panchromatic spatially resolved analysis of nearby galaxies – I. Sub-kpc-scale main sequence in grand-design spirals

High-resolution, 3D radiative transfer modelling

Molecular gas and star formation within 12 strong galactic bars observed with IRAM-30 m

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