The EDGE-CALIFA Survey: Interferometric Observations of 126 Galaxies with CARMA

Bolatto, Alberto D.; Wong, Tony; Utomo, Dyas; Blitz, Leo; Vogel, S. N.; Sanchez, Sebastian Francisco Sanchez; Barrera-Ballesteros, Jorge K.; Cao, Yixian; Colombo, D.; Dannerbauer, H.; García-Benito, R.; Herrera-Camus, Rodrigo; Husemann, B.; Kalinova, V.; Leroy, Adam K.; Leung, Gigi Y. C.; Levy, Rebecca C.; Mast, D.; Ostriker, Eve C.; Rosolowsky, Erik; Sandström, Karin; Teuben, Peter; Ven, Glenn van de; Walter, Fabian

doi:10.3847/1538-4357/aa86aa

Cited by 190 publications

(302 citation statements)

References 99 publications

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“…On larger scales (e.g., averaged over the entire galaxy), N is superlinear (∼1.4) for H 2 tracers, such as CO, and is close to unity for dense gas tracers, such as HCN or HCO+ (e.g., Gao & Solomon 2004). On the other hand, at smaller scales (kpc or sub-kpc), N ∼ 1 or even lower for CO-based H 2 mass (Bigiel et al 2008;Rahmani et al 2016;Bolatto et al 2017;Kreckel et al 2018). In this work, our data is well fitted by a power law with exponent N ∼ 1.05 ± 0.01 (the left panel of Figure 3), in good agreement with recent studies on kpc/sub-kpc scales (Bigiel et al 2008;Leroy et al 2013;Bolatto et al 2017;Kreckel et al 2018;Dey et al 2019).…”

Section: Sk and Extended Sk Relationsupporting

confidence: 92%

The ALMaQUEST Survey: The Molecular Gas Main Sequence and the Origin of the Star-forming Main Sequence

Lin

Pan

Ellison

et al. 2019

ApJL

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117

127

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The origin of the star forming main sequence ( i.e., the relation between star formation rate and stellar mass, globally or on kpc-scales; hereafter SFMS) remains a hotly debated topic in galaxy evolution. Using the ALMA-MaNGA QUEnching and STar formation (ALMaQUEST) survey, we show that for star forming spaxels in the main sequence galaxies, the three local quantities, star-formation rate surface density (Σ SFR ), stellar mass surface density (Σ * ), and the H 2 mass surface density (Σ H2 ), are strongly correlated with one another and form a 3D linear (in log) relation with dispersion. In addition to the two well known scaling relations, the resolved SFMS (Σ SFR vs. Σ * ) and the Schmidt-Kennicutt relation (Σ SFR vs. Σ H2 ; SK relation), there is a third scaling relation between Σ H2 and Σ * , which we refer to as the 'molecular gas main sequence' (MGMS). The latter indicates that either the local gas mass traces the gravitational potential set by the local stellar mass or both quantities follow the underlying total mass distributions. The scatter of the resolved SFMS (σ ∼ 0.25 dex) is the largest compared to those of the SK and MGMS relations (σ ∼ 0.2 dex). A Pearson correlation test also indicates that the SK and MGMS relations are more strongly correlated than the resolved SFMS. Our result suggests a scenario in which the resolved SFMS is the least physically fundamental and is the consequence of the combination of the SK and the MGMS relations.

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Section: Sk and Extended Sk Relationsupporting

confidence: 92%

The ALMaQUEST Survey: The Molecular Gas Main Sequence and the Origin of the Star-forming Main Sequence

Lin

Pan

Ellison

et al. 2019

ApJL

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117

127

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“…By 1.0 kpc resolution, the CO only (dark blue) sightlines tend to no longer trace galactic structures, but rather appear spread across the galaxy. This heavy overlap between CO and Hα emission at coarse resolution agrees with numerous previous studies showing a tight correlation between these quantities at this resolution (e.g., Bigiel et al 2008;Leroy et al 2008;Liu et al 2011;Leroy et al 2013;Bolatto et al 2017). Overall, the changes in morphology and covering fraction beyond 500 pc resolution appear less pronounced than those between 140 pc and 500 pc.…”

Section: Co Only Hα Only Co + Hαsupporting

confidence: 91%

The Gas–Star Formation Cycle in Nearby Star-forming Galaxies. I. Assessment of Multi-scale Variations

Schinnerer

Hughes

Leroy

et al. 2019

ApJ

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The processes regulating star formation in galaxies are thought to act across a hierarchy of spatial scales. To connect extragalactic star formation relations from global and kpc-scale measurements to recent cloud-scale resolution studies, we have developed a simple, robust method that quantifies the scale dependence of the relative spatial distributions of molecular gas and recent star formation. In this paper, we apply this method to eight galaxies with ∼ 1 resolution molecular gas imaging from arXiv:1910.10520v1 [astro-ph.GA] 23 Oct 2019 Schinnerer, Hughes, Leroy, Groves & PHANGS the PHANGS-ALMA and PAWS surveys that have matched resolution, high quality narrowband Hα imaging. At a common scale of 140 pc, our massive (log(M [M ]) = 9.3 − 10.7), normally starforming (SFR[M yr −1 ] = 0.3 − 5.9) galaxies exhibit a significant reservoir of quiescent molecular gas not associated with star formation as traced by Hα emission. Galactic structures act as backbones for both molecular and H II region distributions. As we degrade the spatial resolution, the quiescent molecular gas disappears, with the most rapid changes occurring for resolutions up to ∼ 0.5 kpc. As the resolution becomes poorer, the morphological features become indistinct for spatial scales larger than ∼ 1 kpc. The method is a promising tool to search for relationships between the quiescent or star-forming molecular reservoir and galaxy properties, but requires a larger sample size to identify robust correlations between the star-forming molecular gas fraction and global galaxy parameters.

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“…Important efforts have been made in order to gather direct measurements of molecular gas in galaxies present in the CALIFA sample by the EDGE-CALIFA collaboration (e.g. Bolatto et al 2017), but so far they have collected CO measurements for only 126 galaxies. We have thus estimated the molecular gas content indirectly by means of a gas-todust conversion with a correction factor that depends of the oxygen abundance as derived by S18:…”

Section: Stellar Population Synthesis and Emission-line Fittingmentioning

confidence: 99%

Galaxies hosting an active galactic nucleus: a view from the CALIFA survey

Lacerda

Sánchez

Fernandes

et al. 2020

Monthly Notices of the Royal Astronomical Society

111

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We study the presence of optically-selected Active Galactic Nuclei (AGNs) within a sample of 867 galaxies extracted from the extended Calar-Alto Legacy Integral Field spectroscopy Area (eCALIFA) spanning all morphological classes. We identify 10 Type-I and 24 Type-II AGNs, amounting to ∼ 4 per cent of our sample, similar to the fraction reported by previous explorations in the same redshift range. We compare the integrated properties of the ionized and molecular gas, and stellar population of AGN hosts and their non-active counterparts, combining them with morphological information. The AGN hosts are found in transitory parts (i.e. green-valley) in almost all analysed properties which present bimodal distributions (i.e. a region where reside star-forming galaxies and another with quiescent/retired ones). Regarding morphology, we find AGN hosts among the most massive galaxies, with enhanced central stellarmass surface density in comparison to the average population at each morphological type. Moreover, their distribution peaks at the Sab-Sb classes and none are found among very late-type galaxies (> Scd). Finally, we inspect how the AGN could act in their hosts regarding the quenching of star-formation. The main role of the AGN in the quenching process appears to be the removal (or heating) of molecular gas, rather than an additional suppression of the already observed decrease of the star-formation efficiency from late-to-early type galaxies.

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The EDGE-CALIFA Survey: Interferometric Observations of 126 Galaxies with CARMA

Cited by 190 publications

References 99 publications

The ALMaQUEST Survey: The Molecular Gas Main Sequence and the Origin of the Star-forming Main Sequence

The ALMaQUEST Survey: The Molecular Gas Main Sequence and the Origin of the Star-forming Main Sequence

The Gas–Star Formation Cycle in Nearby Star-forming Galaxies. I. Assessment of Multi-scale Variations

Galaxies hosting an active galactic nucleus: a view from the CALIFA survey

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