Star formation is boosted (and quenched) from the inside-out: radial star formation profiles from MaNGA

Ellison, Sara L.; Sánchez, S. F.; Ibarra-Medel, H.; Antonio, Braulio; Mendel, J. Trevor; Barrera-Ballesteros, Jorge K.

doi:10.1093/mnras/stx2882

Cited by 176 publications

(225 citation statements)

References 152 publications

(248 reference statements)

Supporting

Mentioning

182

Contrasting

Order By: Relevance

“…The actual Pipe3D implementation adopts the GSD156 stellar library, that comprises 39 ages (from 1 Myr to 14 Gyr) and four metallicities (from 0.2 to 1.6 Z ), extensively described in Cid Fernandes et al (2013), and used in previous studies (e.g. Ibarra-Medel et al 2016;Ellison et al Figure 4. An example of the results of the fitting procedure to recover the best model of the stellar population and emission lines applied to a spectrum extracted from a galaxy within our compilation, NGC 1762, shifted to the rest frame.…”

Section: Discussionmentioning

confidence: 99%

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

López-Cobá¹,

Sánchez²,

Anderson

et al. 2020

View full text Add to dashboard Cite

We present here AMUSING++; the largest compilation of nearby galaxies observed with the MUSE integral field spectrograph so far. This collection consists of 635 galaxies from different MUSE projects covering the redshift interval 0.0002 < z < 0.1. The sample and its main properties are characterized and described in here. It includes galaxies of almost all morphological types, with a good coverage in the color-magnitude diagram, within the stellar mass range between 10 8 to 10 12 M , and with properties resembling those of a diameter-selected sample. The AMUSING++ sample is therefore suitable to study, with unprecendent detail, the properties of nearby galaxies at global and local scales, providing us with more than 50 million individual spectra. We use this compilation to investigate the presence of galactic outflows. We exploit the use of combined emission-line images to explore the shape of the different ionized components and the distribution along classical diagnostic diagrams to disentangle the different ionizing sources across the optical extension of each galaxy. We use the cross correlation function to estimate the level of symmetry of the emission lines as an indication of the presence of shocks and/or active galactic nuclei. We uncovered a total of 54 outflows, comprising ∼8% of the sample. A large number of the discovered outflows correspond to those driven by active galactic nuclei (∼60%), suggesting some bias in the selection of our sample. No clear evidence was found that outflow host galaxies are highly star-forming, and outflows appear to be found within all galaxies around the star formation sequence.

show abstract

Section: Discussionmentioning

confidence: 99%

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

López-Cobá¹,

Sánchez²,

Anderson

et al. 2020

View full text Add to dashboard Cite

show abstract

“…As well as looking at the role of bulges in regulating the shape of the SFMS, many studies have also studied how the position of a galaxy across the SFMS relates to the growth of their central component. Morselli et al (2017); Popesso et al (2019a) find that the average B/T of galaxies increases both above and below the SFMS and is suggested to correspond to a central enhancement of star formation activity observed in starburst galaxies (Morselli et al 2019;Belfiore et al 2018;Ellison et al 2018). These observations have pointed towards a possible scenario in which star-forming galaxies may oscillate about the SFMS due to successive compaction events followed by depletion of their cold gas reservoirs (Zolotov et al 2015;Tacchella et al 2016).…”

Section: Introductionmentioning

confidence: 87%

xGASS: the role of bulges along and across the local star-forming main sequence

Cook

Cortese

Catinella

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We use our catalogue of structural decomposition measurements for the extended GALEX Arecibo SDSS Survey (xGASS) to study the role of bulges both along and across the galaxy star-forming main sequence (SFMS). We show that the slope in the sSF R-M relation flattens by ∼0.1 dex per decade in M when re-normalising sSF R by disc stellar mass instead of total stellar mass. However, recasting the sSF R-M relation into the framework of only disc-specific quantities shows that a residual trend remains against disc stellar mass with equivalent slope and comparable scatter to that of the total galaxy relation. This suggests that the residual declining slope of the SFMS is intrinsic to the disc components of galaxies. We further investigate the distribution of bulge-to-total ratios (B/T) as a function of distance from the SFMS (∆SF R M S ). At all stellar masses, the average B/T of local galaxies decreases monotonically with increasing ∆SF R M S . Contrary to previous works, we find that the upper-envelope of the SFMS is not dominated by objects with a significant bulge component. This rules out a scenario in which, in the local Universe, objects with increased star formation activity are simultaneously experiencing a significant bulge growth. We suggest that much of the discrepancies between different works studying the role of bulges originates from differences in the methodology of structurally decomposing galaxies.

show abstract

“…Such turnover also indicates the inside-out quenching of galaxies. The quenching process is beyond the scope of the present paper, but is of major importance in the context of galaxy evolution (e.g., Li et al 2015;González Delgado et al 2016;Belfiore et al 2017;Lin et al 2017;Spindler et al 2017;Ellison et al 2018).…”

Section: Spatially Resolved Hα-m * Relation Using All Spaxels In Galamentioning

confidence: 99%

“…Using spatially resolved spectroscopy, recent studies have shown that there also exist a tight correlation between SFR and stellar mass surface density for nearby and distant star-forming galaxies (Nelson et al 2012;Wuyts et al 2013;Cano-Díaz et al 2016;Abdurro'uf & Akiyama 2017;Hsieh et al 2017;Ellison et al 2018). Recently, Hsieh et al (2017) extended the study to the quiescent population using the MaNGA survey (Mapping Nearby Galaxies at APO; Bundy et al 2015) and found that the emission line fluxes, even classified as LI(N)ER, 14 are also correlated with the underlying stellar mass surface density.…”

Section: Introductionmentioning

confidence: 99%

SDSS IV MaNGA: Dependence of Global and Spatially Resolved SFR–M_∗ Relations on Galaxy Properties

Pan

Lin

Hsieh

et al. 2018

ApJ

View full text Add to dashboard Cite

The galaxy integrated Hα star formation rate-stellar mass relation, or SFR(global)-M * (global) relation, is crucial for understanding star formation history and evolution of galaxies. However, many studies have dealt with SFR using unresolved measurements, which makes it difficult to separate out the contamination from other ionizing sources, such as active galactic nuclei and evolved stars. Using the integral field spectroscopic observations from SDSS-IV MaNGA, we spatially disentangle the contribution from different Hα powering sources for ∼1000 galaxies. We find that, when including regions dominated by all ionizing sources in galaxies, the spatially resolved relation between Hα surface density (Σ Hα (all)) and stellar mass surface density (Σ * (all)) progressively turns over at the high Σ * (all) end for increasing M * (global) and/or bulge dominance (bulge-to-total light ratio, B/T). This in turn leads to the flattening of the integrated Hα(global)-M * (global) relation in the literature. By contrast, there is no noticeable flattening in both integrated Hα(H II)-M * (H II) and spatially resolved Σ Hα (H II)-Σ * (H II) relations when only regions where star formation dominates the ionization are considered. In other words, the flattening can be attributed to the increasing regions powered by non-star-formation sources, which generally have lower ionizing ability than star formation. An analysis of the fractional contribution of non-star-formation sources to total Hα luminosity of a galaxy suggests a decreasing role of star formation as an ionizing source toward high-mass, high-B/T galaxies and bulge regions. This result indicates that the appearance of the galaxy integrated SFR-M * relation critically depends on their global properties (M * (global) and B/T) and relative abundances of various ionizing sources within the galaxies.

show abstract

Star formation is boosted (and quenched) from the inside-out: radial star formation profiles from MaNGA

Cited by 176 publications

References 152 publications

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

xGASS: the role of bulges along and across the local star-forming main sequence

SDSS IV MaNGA: Dependence of Global and Spatially Resolved SFR–M_∗ Relations on Galaxy Properties

Contact Info

Product

Resources

About

Star formation is boosted (and quenched) from the inside-out: radial star formation profiles from MaNGA

Cited by 176 publications

References 152 publications

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

xGASS: the role of bulges along and across the local star-forming main sequence

SDSS IV MaNGA: Dependence of Global and Spatially Resolved SFR–M∗ Relations on Galaxy Properties

Contact Info

Product

Resources

About

SDSS IV MaNGA: Dependence of Global and Spatially Resolved SFR–M_∗ Relations on Galaxy Properties