The ALMaQUEST Survey – V. The non-universality of kpc-scale star formation relations and the factors that drive them. Issue 4 (12th December 2020)

• Record Type: Journal Article
• Authors: Ellison, Sara L; Lin, Lihwai; Thorp, Mallory D; Pan, Hsi-An; Scudder, Jillian M; Sánchez, Sebastian F; Bluck, Asa F L; Maiolino, Roberto
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 501:Issue 4(2021)
• Page Start: 4777
• Page End: 4797
• Publication Date: 2020-12-12
• Subjects: galaxies: evolution -- galaxies: general -- galaxies: ISM -- galaxies: star formation; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa3822
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Using a sample of ∼15 000 kpc-scale star-forming spaxels in 28 galaxies drawn from the ALMA-MaNGA QUEnching and STar formation (ALMaQUEST) survey, we investigate the galaxy-to-galaxy variation of the 'resolved' Schmidt–Kennicutt relation (rSK; $\Sigma _{\rm H_2}$ –ΣSFR ), the 'resolved' star-forming main sequence (rSFMS; Σ⋆ –ΣSFR ), and the 'resolved' molecular gas main sequence (rMGMS; Σ⋆ –$\Sigma _{\rm H_2}$ ). The rSK relation, rSFMS, and rMGMS all show significant galaxy-to-galaxy variation in both shape and normalization, indicating that none of these relations is universal between galaxies. The rSFMS shows the largest galaxy-to-galaxy variation and the rMGMS the least. By defining an 'offset' from the average relations, we compute a ΔrSK, ΔrSFMS, ΔrMGMS for each galaxy, to investigate correlations with global properties. We find the following correlations with at least 2 σ significance: The rSK is lower (i.e. lower star formation efficiency) in galaxies with higher M ⋆, larger Sersic index, and lower specific SFR (sSFR); the rSFMS is lower (i.e. lower sSFR) in galaxies with higher M ⋆ and larger Sersic index; and the rMGMS is lower (i.e. lower gas fraction) in galaxies with lower sSFR. In the ensemble of all 15 000 data points, the rSK relation and rMGMS show equally tight scatters and strong correlation coefficients, compared with a larger scatter and weaker correlation in the rSFMS. Moreover, whilst there is no correlation between ΔrSK and ΔrMGMS in the sample, the offset of a galaxy's rSFMS does correlate with both of the other two offsets. Our results therefore indicate that the rSK and rMGMS are independent relations, whereas the rSFMS is a result of their combination.