Time-slicing spiral galaxies with SDSS-IV MaNGA

Peterken, Thomas; Fraser-McKelvie, Amelia; Aragón-Salamanca, Alfonso; Merrifield, M. R.; Kraljic, Katarina; Knapen, Johan H.; Riffel, Rogemar A.; Brownstein, Joel R.; Drory, Niv

doi:10.1093/mnras/stz2204

Cited by 21 publications

(19 citation statements)

References 46 publications

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“…In the literature, bars have been found to be more metal-rich and less α-enhanced than their surrounding discs by Neumann et al (2020), while Carrillo et al (2020) found that the bar in NGC 2903 has similar metallicity and a higher fraction of younger stars than the outer disc, which they interpreted as evidence that gas flowing along the bar has triggered more recent star-formation activity. Further evidence for ongoing star-formation along the leading edges of bars in spiral galaxies has also been found by Peterken et al (2019) andFraser-McKelvie et al (2020). In the sample of unbarred S0s used in this work, we found that the lenses tend to have higher metallicities than discs, while the discs display more recent or longer episodes of star formation than the lenses.…”

Section: Mass-weighted Stellar Populationssupporting

confidence: 82%

Formation of S0s in extreme environments II: The star-formation histories of bulges, discs, and lenses

Johnston

Aragón-Salamanca

Fraser-McKelvie

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Different processes have been proposed to explain the formation of S0s, including mergers, disc instabilities and quenched spirals. These processes are expected to dominate in different environments, and thus leave characteristic footprints in the kinematics and stellar populations of the individual components within the galaxies. New techniques enable us to cleanly disentangle the kinematics and stellar populations of these components in IFU observations. In this paper, we use buddi to spectroscopically extract the light from the bulge, disc and lens components within a sample of 8 S0 galaxies in extreme environments observed with MUSE. While the spectra of bulges and discs in S0 galaxies have been separated before, this work is the first to isolate the spectra of lenses. Stellar populations analysis revealed that the bulges and lenses have generally similar or higher metallicities than the discs, and the α-enhancement of the bulges and discs are correlated, while those of the lenses are completely unconnected to either component. We conclude that the majority of the mass in these galaxies was built up early in the lifetime of the galaxy, with the bulges and discs forming from the same material through dissipational processes at high redshift. The lenses, on the other hand, formed over independent timescales at more random times within the lifetime of the galaxy, possibly from evolved bars. The younger stellar populations and asymmetric features seen in the field S0s may indicate that these galaxies have been affected more by minor mergers than the cluster galaxies.

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Section: Mass-weighted Stellar Populationssupporting

confidence: 82%

Formation of S0s in extreme environments II: The star-formation histories of bulges, discs, and lenses

Johnston

Aragón-Salamanca

Fraser-McKelvie

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…We use the full-spectrum stellar population fitting code STARLIGHT (Cid Fernandes et al 2005) to derive a best-fit spectrum, created from a linear combination of a set of input single stellar population (SSP) template spectra -with no assumptions or restrictions on the shape of the derived star formation histories -and an applied dust attenuation. The fitting method used is similar to that used by Peterken et al (2019), and is described fully by Peterken et al (in prep.). Here we highlight the key relevant details.…”

Section: Measuring Dust Attenuation From Stellar Population Modellingmentioning

confidence: 99%

SDSS-IV MaNGA: spatially resolved dust attenuation in spiral galaxies

Greener

Aragón-Salamanca

Merrifield

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Dust attenuation in star-forming spiral galaxies affects stars and gas in different ways due to local variations in dust geometry. We present spatially resolved measurements of dust attenuation for a sample of 232 such star-forming spiral galaxies, derived from spectra acquired by the SDSS-IV MaNGA survey. The dust attenuation affecting the stellar populations of these galaxies (obtained using full spectrum stellar population fitting methods) is compared with the dust attenuation in the gas (derived from the Balmer decrement). Both of these attenuation measures increase for local regions of galaxies with higher star formation rates; the dust attenuation affecting the stellar populations increases more so than the dust attenuation in the gas, causing the ratio of the dust attenuation affecting the stellar populations to the dust attenuation in the gas to decrease for local regions of galaxies with higher star formation rate densities. No systematic difference is discernible in any of these dust attenuation quantities between the spiral arm and interarm regions of the galaxies. While both the dust attenuation in the gas and the dust attenuation affecting the stellar populations decrease with galactocentric radius, the ratio of the two quantities does not vary with radius. This ratio does, however, decrease systematically as the stellar mass of the galaxy increases. Analysis of the radial profiles of the two dust attenuation measures suggests that there is a disproportionately high concentration of birth clouds (incorporating gas, young stars, and clumpy dust) nearer to the centres of star-forming spiral galaxies.

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“…as was done by Peterken et al (2019a) for a spiral arm]. Peterken et al (2019b) used both bar and spiral masks from GZ:3D for the galaxy MCG + 07-28-064 to demonstrate a new technique of reconstructing spatially resolved star formation histories from MaNGA data cubes. The bar (and spiral arm) masks were used as a visual indication of where these features are relative to features in stellar population metallicity as a function of age.…”

Section: Bar Regionsmentioning

confidence: 99%

Galaxy Zoo: 3D – crowdsourced bar, spiral, and foreground star masks for MaNGA target galaxies

Masters

Krawczyk

Shamsi

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The challenge of consistent identification of internal structure in galaxies – in particular disc galaxy components like spiral arms, bars, and bulges – has hindered our ability to study the physical impact of such structure across large samples. In this paper we present Galaxy Zoo: 3D (GZ: 3D) a crowdsourcing project built on the Zooniverse platform which we used to create spatial pixel (spaxel) maps that identify galaxy centres, foreground stars, galactic bars and spiral arms for 29831 galaxies which were potential targets of the MaNGA survey (Mapping Nearby Galaxies at Apache Point Observatory, part of the fourth phase of the Sloan Digital Sky Surveys or SDSS-IV), including nearly all of the 10,010 galaxies ultimately observed. Our crowd-sourced visual identification of asymmetric, internal structures provides valuable insight on the evolutionary role of non-axisymmetric processes that is otherwise lost when MaNGA data cubes are azimuthally averaged. We present the publicly available GZ:3D catalog alongside validation tests and example use cases. These data may in the future provide a useful training set for automated identification of spiral arm features. As an illustration, we use the spiral masks in a sample of 825 galaxies to measure the enhancement of star formation spatially linked to spiral arms, which we measure to be a factor of three over the background disc, and how this enhancement increases with radius.

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Time-slicing spiral galaxies with SDSS-IV MaNGA

Cited by 21 publications

References 46 publications

Formation of S0s in extreme environments II: The star-formation histories of bulges, discs, and lenses

Formation of S0s in extreme environments II: The star-formation histories of bulges, discs, and lenses

SDSS-IV MaNGA: spatially resolved dust attenuation in spiral galaxies

Galaxy Zoo: 3D – crowdsourced bar, spiral, and foreground star masks for MaNGA target galaxies

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