ALMaQUEST. IV. The ALMA-MaNGA QUEnching and STar Formation (ALMaQUEST) Survey

Lin, Lihwai; Ellison, Sara L.; Pan, Hsi-An; Thorp, Mallory; Su, Yung-Chau; Sánchez, S. F.; Belfiore, Francesco; Bothwell, M. S.; Bundy, Kevin; Chen, Yanmei; Concas, A.; Hsieh, Bau-Ching; Hsieh, Po‐Jang; Li, Cheng; Maiolino, R.; Masters, Karen L.; Newman, Jeffrey A.; Rowlands, Kate; Shi, Yong; Smethurst, Rebecca; Stark, David V.; Xiao, Ting; Yu, Po-Chieh

doi:10.3847/1538-4357/abba3a

Cited by 48 publications

(59 citation statements)

References 108 publications

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“…This case is very similar to the gas compaction and inside-out quenching episodes seen in simulations of blue nuggets (that become red nuggets) at higher redshift (Tacchella et al 2016a(Tacchella et al , 2016b. These episodes, however, need not be restricted to high-redshift, as observations with ALMA and in the MaNGA Survey (Brownson et al 2020;Lin et al 2020) have shown similar variations in central star formation efficiency sans mergers in green valley galaxies in the local universe.…”

Section: Matching Fire-cmzs With the Milky Way Cmz And External Galaxiessupporting

confidence: 74%

Fiery Cores: Bursty and Smooth Star Formation Distributions across Galaxy Centers in Cosmological Zoom-in Simulations

Orr

Hatchfield

Battersby

et al. 2021

ApJL

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We present an analysis of the R  1.5 kpc core regions of seven simulated Milky Way-mass galaxies, from the FIRE-2 (Feedback in Realistic Environments) cosmological zoom-in simulation suite, for a finely sampled period (Δt = 2.2 Myr) of 22 Myr at z ≈ 0, and compare them with star formation rate (SFR) and gas surface density observations of the Milky Way's Central Molecular Zone (CMZ). Despite not being tuned to reproduce the detailed structure of the CMZ, we find that four of these galaxies are consistent with CMZ observations at some point during this 22 Myr period. The galaxies presented here are not homogeneous in their central structures, roughly dividing into two morphological classes; (a) several of the galaxies have very asymmetric gas and SFR distributions, with intense (compact) starbursts occurring over a period of roughly 10 Myr, and structures on highly eccentric orbits through the CMZ, whereas (b) others have smoother gas and SFR distributions, with only slowly varying SFRs over the period analyzed. In class (a) centers, the orbital motion of gas and star-forming complexes across small apertures (R  150 pc, analogously |l| < 1°in the CMZ observations) contributes as much to tracers of star formation/dense gas appearing in those apertures, as the internal evolution of those structures does. These asymmetric/bursty galactic centers can simultaneously match CMZ gas and SFR observations, demonstrating that time-varying star formation can explain the CMZ's low star formation efficiency.

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Section: Matching Fire-cmzs With the Milky Way Cmz And External Galaxiessupporting

confidence: 74%

Fiery Cores: Bursty and Smooth Star Formation Distributions across Galaxy Centers in Cosmological Zoom-in Simulations

Orr

Hatchfield

Battersby

et al. 2021

ApJL

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“…In a recent work, Brownson et al (2020) found that spatially resolved H2 gas fraction (ΣH 2 /Σ * ) and SFE (ΣSF R/ΣH 2 ) are suppressed compared to typical star-forming regions, and that both contribute to reducing the resolved SSFR in seven green valley galaxies. In an interesting complementary approach, Ellison et al (2021a) compared star-forming and retired spaxels of eight galaxies from the ALMaQUEST (Lin et al 2020) survey, and concluded that the retired spaxels are typically concentrated in the inner regions of galaxies and have significantly lower molecular gas fractions than the star-forming spaxels in the same galaxy, suggesting that quenching proceeds inside-out, at least for central galaxies. Although based on small samples, such resolved studies are in qualitative agreement with the findings based on global properties.…”

Section: Longer Depletion Timescalesmentioning

confidence: 99%

The cold interstellar medium of galaxies in the Local Universe

Saintonge¹,

Catinella²

2022

Preprint

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The cold interstellar medium (ISM) plays a central role in the galaxy evolution process. It is the reservoir that fuels galaxy growth via star formation, the repository of material formed by these stars, and a sensitive tracer of internal and external processes that affect entire galaxies. Consequently, significant efforts have gone into systematic surveys of the cold ISM of the galaxies in the local Universe. This review discusses the resulting network of scaling relations connecting the atomic and molecular gas masses of galaxies with their other global properties (stellar masses, morphologies, metallicities, star formation activity...), and their implications for our understanding of galaxy evolution. Key take-home messages are as follows:• From a gas perspective, there are three main factors that determine the star formation rate of a galaxy: the total mass of its cold ISM, how much of that gas is molecular, and the rate at which any molecular gas is converted into stars. All three of these factors vary systematically across the local galaxy population.• The shape and scatter of both the star formation main sequence and the mass-metallicity relation are deeply linked to the availability of atomic and molecular gas.• Future progress will come from expanding our exploration of scaling relations into new parameter space (in particular the regime of dwarf galaxies), better connecting the cold ISM of large samples of galaxies with the environment that feeds them (the circumgalactic medium in particular), and understanding the impact of these large scales on the efficiency of the star formation process on molecular cloud scales.

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“…We use data from the ALMaQUEST 2 survey (Lin et al 2020), which is a survey performed with the Atacama Large Millimetre Array (ALMA), designed to obtain CO(1-0) 115GHz measurements from 46 local galaxies that are included in the MaNGA survey (Bundy et al 2015). The galaxies were chosen to span a broad range, in terms of specific star formation rate (sSFR), across the main sequence, including green valley and starburst galaxies.…”

Section: Almaquestmentioning

confidence: 99%

“…The angular resolution of the ALMA measurements is around 2.5", matching that of the MaNGA observations, and the sensitivity of the CO line flux ranges from about 0.02 to 0.1 Jy km s −1 beam −1 . A detailed description of the ALMaQUEST survey and of its observational parameters is given in Lin et al (2020).…”

Section: Almaquestmentioning

confidence: 99%

The ALMaQUEST survey IX: the nature of the resolved star forming main sequence

Baker

Maiolino

Bluck

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We investigate the nature of the scaling relations between the surface density of star formation rate (ΣSFR), stellar mass (Σ*), and molecular gas mass ($\Sigma _{\rm H_2}$), aiming at distinguishing between the relations that are primary, i.e. more fundamental, and those which are instead an indirect by-product of the other relations. We use the ALMaQUEST survey and analyse the data by using both partial correlations and Random Forest regression techniques. We unambiguously find that the strongest intrinsic correlation is between ΣSFR and $\Sigma _{\rm H_2}$ (i.e. the resolved Schmidt-Kennicutt relation), followed by the correlation between $\Sigma _{\rm H_2}$ and Σ* (resolved Molecular Gas Main Sequence, rMGMS). Once these two correlations are taken into account, we find that there is no evidence for any intrinsic correlation between ΣSFR and Σ*, implying that SFR is entirely driven by the amount of molecular gas, while its dependence on stellar mass (i.e. the resolved Star Forming Main Sequence, rSFMS) simply emerges as a consequence of the relationship between molecular gas and stellar mass.

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ALMaQUEST. IV. The ALMA-MaNGA QUEnching and STar Formation (ALMaQUEST) Survey

Cited by 48 publications

References 108 publications

Fiery Cores: Bursty and Smooth Star Formation Distributions across Galaxy Centers in Cosmological Zoom-in Simulations

Fiery Cores: Bursty and Smooth Star Formation Distributions across Galaxy Centers in Cosmological Zoom-in Simulations

The cold interstellar medium of galaxies in the Local Universe

The ALMaQUEST survey IX: the nature of the resolved star forming main sequence

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