Orientations of sex and love

Marino, Patricia

doi:10.4324/9780429423000-9

Cited by 6 publications

(8 citation statements)

References 0 publications

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“…These templates have been extensively used within the CALIFA collaboration (e.g. Perez et al 2013, Marino et al 2013, and in other surveys (e.g. Haines et al 2015, Ibarra et al 2016.…”

Section: Manga Dr15 and Pipe3dmentioning

confidence: 99%

“…One parameter which is particularly interesting is gas-phase metallicity, or more specifically the oxygen abundance, defined as: Zg = 12 + log 10 (O/H). Here we construct the oxygen abundance from the O3N 2 index, via the Marino et al (2013) calibration for star forming regions within galaxies. Additionally, we include the level of gas extinction in V-band (AV), as inferred from the Balmer decrement, assuming a Cardelli et al 1989 attenuation curve.…”

Section: Gas-phase Analysismentioning

confidence: 99%

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Are galactic star formation and quenching governed by local, global, or environmental phenomena?

Bluck

Maiolino

Sánchez

et al. 2019

Monthly Notices of the Royal Astronomical Society

139

212

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We present an analysis of star formation and quenching in the SDSS-IV MaNGA-DR15, utilising over 5 million spaxels from ∼3500 local galaxies. We estimate star formation rate surface densities (Σ SFR ) via dust corrected Hα flux where possible, and via an empirical relationship between specific star formation rate (sSFR) and the strength of the 4000Å break (D4000) in all other cases. We train a multi-layered artificial neural network (ANN) and a random forest (RF) to classify spaxels into 'star forming' and 'quenched' categories given various individual (and groups of) parameters. We find that global parameters (pertaining to the galaxy as a whole) perform collectively the best at predicting when spaxels will be quenched, and are substantially superior to local/ spatially resolved and environmental parameters. Central velocity dispersion is the best single parameter for predicting quenching in central galaxies. We interpret this observational fact as a probable consequence of the total integrated energy from AGN feedback being traced by the mass of the black hole, which is well known to correlate strongly with central velocity dispersion. Additionally, we train both an ANN and RF to estimate Σ SFR values directly via regression in star forming regions. Local/ spatially resolved parameters are collectively the most predictive at estimating Σ SFR in these analyses, with stellar mass surface density at the spaxel location (Σ * ) being by far the best single parameter. Thus, quenching is fundamentally a global process but star formation is governed locally by processes within each spaxel.

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“…These templates have been extensively used within the CALIFA collaboration (e.g. Perez et al 2013, Marino et al 2013, and in other surveys (e.g. Haines et al 2015, Ibarra et al 2016.…”

Section: Manga Dr15 and Pipe3dmentioning

confidence: 99%

Section: Gas-phase Analysismentioning

confidence: 99%

Are galactic star formation and quenching governed by local, global, or environmental phenomena?

Bluck

Maiolino

Sánchez

et al. 2019

Monthly Notices of the Royal Astronomical Society

139

212

View full text Add to dashboard Cite

show abstract

“…Surface densities of star formation rate (Σ SFR ) are computed by using the extinction corrected Hα luminosities in equation 2 from Kennicutt (1998a), assuming a Salpeter initial mass function (to be consistent with the PIPE3D products). Metallicities are also computed by us using the extinction corrected emission line fluxes with the Marino et al (2013) O3N2 calibration. Finally, we compute inclination corrected galactocentric radii from the V-band centre of the galaxy using the b/a axial ratios from single Sersic fits provided in the NASA Sloan Atlas (NSA) catalog.…”

Section: Mangamentioning

confidence: 99%

The ALMaQUEST Survey – II. What drives central starbursts at z ∼ 0?

Ellison

Thorp

Pan

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Starburst galaxies have elevated star formation rates (SFRs) for their stellar mass. In Ellison et al. (2018) we used integral field unit (IFU) maps of star formation rate surface density (Σ SFR ) and stellar mass surface density (Σ ) to show that starburst galaxies in the local universe are driven by SFRs that are preferentially boosted in their central regions. Here, we present molecular gas maps obtained with the Atacama Large Millimeter Array (ALMA) observatory for 12 central starburst galaxies at z ∼ 0 drawn from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey. The ALMA and MaNGA data are well matched in spatial resolution, such that the ALMA maps of molecular gas surface density (Σ H 2 ) can be directly compared with MaNGA maps at kpc-scale resolution. The combination of Σ H 2 , Σ and Σ SFR at the same resolution allow us to investigate whether central starbursts are driven primarily by enhancements in star formation efficiency (SFE) or by increased gas fractions. By computing offsets from the resolved Kennicutt-Schmidt relation (Σ H 2 vs. Σ SFR ) and the molecular gas main sequence (Σ vs. Σ H 2 ), we conclude that the primary driver of the central starburst is an elevated SFE. We also show that the enhancement in Σ SFR is accompanied by a dilution in O/H, consistent with a triggering that is induced by metal poor gas inflow. These observational signatures are found in both undisturbed (9/12 galaxies in our sample) and recently merged galaxies, indicating that both interactions and secular mechanisms contribute to central starbursts.

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“…Relevant to the current work, pipe3d provides the star formation rate surface density (Σ SFR ), stellar mass surface density (Σ ), metallicity (O/H) and various emission line fluxes for each spaxel. The star formation rate is derived from the Hα flux using the Kennicutt et al (1998) relation and the gas phase metallicity is determined using the O3N2 calibration of Marino et al (2013). The pipe3d value added catalogue also provides integrated global properties including SFR and M .…”

Section: Manga Sample Selectionmentioning

confidence: 99%

Spatially resolved star formation and metallicity profiles in post-merger galaxies from MaNGA

Thorp

Ellison

Simard

et al. 2018

Monthly Notices of the Royal Astronomical Society: Letters

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Large galaxy surveys have demonstrated that galaxy-galaxy mergers can dramatically change the morphologies, star formation rates (SFRs) and metallicities of their constituents. However, most statistical studies have been limited to the measurement of global quantities, through large fibres or integrated colours. In this work, we present the first statistically significant study of spatially resolved star formation and metallicity profiles using integral field spectroscopy, using a sample of ∼20,000 spaxels in 36 visually selected post-merger galaxies from the Mapping Nearby Galaxies with Apache Point Observatory (MaNGA) survey. By measuring offsets from SFR and metallicity scaling relations on a spaxel-by-spaxel basis, we are able to quantify where in the galaxy these properties are most affected by the interaction. We find that the SFR enhancements are generally centrally peaked, by a factor of 2.5 on average, in agreement with predictions from simulations. However, there is considerable variation in the SFR behaviour in the galactic outskirts, where both enhancement and suppression are seen. The median SFR remains enhanced by 0.1 dex out to at least 1.9 Re. The metallicity is also affected out to these large radii, typically showing a suppression of ∼ −0.04 dex.

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Orientations of sex and love

Cited by 6 publications

References 0 publications

Are galactic star formation and quenching governed by local, global, or environmental phenomena?

Are galactic star formation and quenching governed by local, global, or environmental phenomena?

The ALMaQUEST Survey – II. What drives central starbursts at z ∼ 0?

Spatially resolved star formation and metallicity profiles in post-merger galaxies from MaNGA

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