Calibrating Star Formation Rate Prescriptions at Different Scales (10 pc–1 kpc) in M31

Tomičić, Neven; Ho, I-Ting; Kreckel, Kathryn; Schinnerer, E.; Leroy, Adam K.; Groves, Brent; Sandström, Karin; Blanc, Guillermo A.; Jarrett, T. H.; Thilker, David A.; Kapala, Maria

doi:10.3847/1538-4357/ab03ce

Cited by 15 publications

(15 citation statements)

References 116 publications

(275 reference statements)

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“…We note that the degree of correlation worsens considerably for integrated SFRs instead of Σ SFR (ρ = 0.33), mostly as a result of the different sizes of the apertures used by Chen et al (2017). We remind the reader that we use the SFRs from Tomičić et al (2019), but the global conclusions do not qualitatively change if we use the SFRs from Viaene et al instead. The combined data in the right panel of Fig.…”

Section: Trends As a Function Of Velocity Dispersionmentioning

confidence: 85%

“…We overplot the results from Chen et al (2017) for the outer spiral arm segment in the north of M51 (at a resolution of 4.9 × 3.7 ∼ 150 − 200 pc). We also overplot measurements at comparable physical scales (∼100 pc) from two other normal, star-forming galaxies: NGC 3627 (Murphy et al 2015) and M31 (molecular data from Brouillet et al 2005 and SFRs from Tomičić et al 2019). We deliberately avoid lowmetallicity and starburst systems, which could introduce confusion in the trends due to chemistry.…”

Section: Trends As a Function Of Stellar Mass Surface Densitymentioning

confidence: 99%

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Dense gas is not enough: environmental variations in the star formation efficiency of dense molecular gas at 100 pc scales in M 51

Querejeta

Schinnerer

Schruba

et al. 2019

A&A

115

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It remains unclear what sets the efficiency with which molecular gas transforms into stars. Here we present a new VLA map of the spiral galaxy M51 in 33 GHz radio continuum, an extinction-free tracer of star formation, at 3 scales (∼100 pc). We combined this map with interferometric PdBI/NOEMA observations of CO(1-0) and HCN(1-0) at matched resolution for three regions in M51 (central molecular ring, northern and southern spiral arm segments). While our measurements roughly fall on the well-known correlation between total infrared and HCN luminosity, bridging the gap between Galactic and extragalactic observations, we find systematic offsets from that relation for different dynamical environments probed in M51; for example, the southern arm segment is more quiescent due to low star formation efficiency (SFE) of the dense gas, despite its high dense gas fraction. Combining our results with measurements from the literature at 100 pc scales, we find that the SFE of the dense gas and the dense gas fraction anti-correlate and correlate, respectively, with the local stellar mass surface density. This is consistent with previous kpc-scale studies. In addition, we find a significant anti-correlation between the SFE and velocity dispersion of the dense gas. Finally, we confirm that a correlation also holds between star formation rate surface density and the dense gas fraction, but it is not stronger than the correlation with dense gas surface density. Our results are hard to reconcile with models relying on a universal gas density threshold for star formation and suggest that turbulence and galactic dynamics play a major role in setting how efficiently dense gas converts into stars.

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Section: Trends As a Function Of Velocity Dispersionmentioning

confidence: 85%

Section: Trends As a Function Of Stellar Mass Surface Densitymentioning

confidence: 99%

Dense gas is not enough: environmental variations in the star formation efficiency of dense molecular gas at 100 pc scales in M 51

Querejeta

Schinnerer

Schruba

et al. 2019

A&A

115

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“…We note, in general, that we expect large parts of galaxies to more or less act as whole galaxies. However global prescriptions can fail dramatically in small regions of highly resolved, i.e., very nearby, targets (e.g., Boquien et al 2016;Tomičić et al 2019). We also emphasize that these prescriptions represent mean calibrations.…”

Section: Some Reference Conversions To Physical Quantitiesmentioning

confidence: 90%

A z = 0 Multiwavelength Galaxy Synthesis. I. A WISE and GALEX Atlas of Local Galaxies

Leroy

Sandström

Lang

et al. 2019

ApJS

Self Cite

252

460

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We present an atlas of ultraviolet and infrared images of ∼ 15, 750 local (d 50 Mpc) galaxies, as observed by NASA's WISE and GALEX missions. These maps have matched resolution (FWHM 7.5 and 15 ), matched astrometry, and a common procedure for background removal. We demonstrate that they agree well with resolved intensity measurements and integrated photometry from previous surveys. This atlas represents the first part of a program (the z = 0 Multi-wavelength Galaxy Synthesis) to create a large, uniform database of resolved measurements of gas and dust in nearby galaxies. The images and associated catalogs will be publicly available at the NASA/IPAC Infrared Science Archive. This atlas allows us estimate local and integrated star formation rates (SFRs) and stellar masses (M ) across the local galaxy population in a uniform way. In the appendix, we use the population synthesis fits of Salim et al. (2016Salim et al. ( , 2018 to calibrate integrated M and SFR estimators based on GALEX and WISE. Because they leverage an SDSS-base training set of > 100, 000 galaxies, these calibrations have high precision and allow us to rigorously compare local galaxies to Sloan Digital Sky Survey results. We provide these SFR and M estimates for all galaxies in our sample and show that our results yield a "main sequence" of star forming galaxies comparable to previous work. We also show the distribution of intensities from resolved galaxies in NUV-to-WISE1 vs. WISE1-to-WISE3 space, which captures much of the key physics accessed by these bands.

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“…As a result, there is significant galaxy-to-galaxy variation of the rSFMS and the SFE can vary by an order of magnitude or more within a given galaxy (e.g. Bemis & Wilson 2019;Tomicic et al 2019;Vulcani et al 2019a).…”

Section: Introductionmentioning

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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Calibrating Star Formation Rate Prescriptions at Different Scales (10 pc–1 kpc) in M31

Cited by 15 publications

References 116 publications

Dense gas is not enough: environmental variations in the star formation efficiency of dense molecular gas at 100 pc scales in M 51

Dense gas is not enough: environmental variations in the star formation efficiency of dense molecular gas at 100 pc scales in M 51

A z = 0 Multiwavelength Galaxy Synthesis. I. A WISE and GALEX Atlas of Local Galaxies

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

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