PHANGS CO Kinematics: Disk Orientations and Rotation Curves at 150 pc Resolution

Lang, P.; Meidt, Sharon E.; Rosolowsky, Erik; Nofech, Joseph; Schinnerer, E.; Leroy, Adam K.; Emsellem, Éric; Pessa, Ismael; Glover, Simon C. O.; Groves, Brent; Hughes, Annie; Kruijssen, J. M. Diederik; Querejeta, Miguel; Schruba, Andreas; Bigiel, Frank; Blanc, Guillermo A.; Chevance, Mélanie; Colombo, D.; Faesi, Christopher M.; Henshaw, Jonathan D.; Herrera, Cinthya N.; Liu, Daizhong; Pety, J.; Puschnig, Johannes; Saito, Toshiki; Sun, Jiayi; Usero, A.

doi:10.3847/1538-4357/ab9953

Cited by 106 publications

(140 citation statements)

References 81 publications

(117 reference statements)

Supporting

Mentioning

134

Contrasting

Order By: Relevance

“…This method provides a simple, reproducible characterization of all detected emission (e.g., Sawada et al 2012;Hughes et al 2013b;Leroy et al 2016). Complementary analyses decomposing the same CO data into individual objects (E. Rosolowsky et al 2020, in preparation; A. Hughes et al, in preparation) yield qualitatively similar conclusions.…”

Section: Data and Measurementsmentioning

confidence: 93%

See 1 more Smart Citation

Molecular Gas Properties on Cloud Scales across the Local Star-forming Galaxy Population

Sun

Leroy

Schinnerer

et al. 2020

ApJL

Self Cite

115

154

View full text Add to dashboard Cite

Using the PHANGS-ALMA CO(2-1) survey, we characterize molecular gas properties on ∼100 pc scales across 102,778 independent sightlines in 70 nearby galaxies. This yields the best synthetic view of molecular gas properties on cloud scales across the local star-forming galaxy population obtained to date. Consistent with previous studies, we observe a wide range of molecular gas surface densities (3.4 dex), velocity dispersions (1.7 dex), and turbulent pressures (6.5 dex) across the galaxies in our sample. Under simplifying assumptions about subresolution gas structure, the inferred virial parameters suggest that the kinetic energy of the molecular gas typically exceeds its self-gravitational binding energy at ∼100 pc scales by a modest factor (1.3 on average). We find that the cloud-scale surface density, velocity dispersion, and turbulent pressure (1) increase toward the inner parts of galaxies, (2) are exceptionally high in the centers of barred galaxies (where the gas also appears less gravitationally bound), and (3) are moderately higher in spiral arms than in inter-arm regions. The galaxy-wide averages of these gas properties also correlate with the integrated stellar mass, star formation rate, and offset from the star-forming main sequence of the host galaxies. These correlations persist even when we exclude regions with extraordinary gas properties in galaxy centers, which contribute significantly to the inter-galaxy variations. Our results provide key empirical constraints on the physical link between molecular cloud populations and their galactic environment.

show abstract

Section: Data and Measurementsmentioning

confidence: 93%

“…(5-6) galaxy inclination and position angle (Lang et al 2020); (7-9) galaxy global stellar mass, SFR, and the effective (half-mass) radius estimated from the measured stellar scale length (Leroy et al 2019;A. K. Leroy et al 2020a, in preparation); (10-11) CO data rms noise and channel-to-channel correlation at 150 pc resolution;…”

Section: Galaxymentioning

confidence: 99%

Molecular Gas Properties on Cloud Scales across the Local Star-forming Galaxy Population

Sun

Leroy

Schinnerer

et al. 2020

ApJL

Self Cite

115

154

View full text Add to dashboard Cite

show abstract

“…Our sample is summarized in Table 1 where we use the global parameters as reported by Leroy et al (in prep. ) based on the distance compilation of Anand et al (2021) as well as the inclinations determined by Lang et al (2020).…”

Section: Datamentioning

confidence: 99%

“…Column (7) shows the vertical offset of the galaxy from the integrated main sequence of galaxies, as defined in Leroy et al (2019). Distance measurements are presented in Anand et al (2021) and inclinations in Lang et al (2020). Uncertainties in Cols.…”

Section: Almamentioning

confidence: 99%

Star formation scaling relations at ∼100 pc from PHANGS: Impact of completeness and spatial scale

Pessa

Schinnerer

Belfiore

et al. 2021

A&A

View full text Add to dashboard Cite

Aims. The complexity of star formation at the physical scale of molecular clouds is not yet fully understood. We investigate the mechanisms regulating the formation of stars in different environments within nearby star-forming galaxies from the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) sample. Methods. Integral field spectroscopic data and radio-interferometric observations of 18 galaxies were combined to explore the existence of the resolved star formation main sequence (Σstellar versus ΣSFR), resolved Kennicutt–Schmidt relation (Σmol. gas versus ΣSFR), and resolved molecular gas main sequence (Σstellar versus Σmol. gas), and we derived their slope and scatter at spatial resolutions from 100 pc to 1 kpc (under various assumptions). Results. All three relations were recovered at the highest spatial resolution (100 pc). Furthermore, significant variations in these scaling relations were observed across different galactic environments. The exclusion of non-detections has a systematic impact on the inferred slope as a function of the spatial scale. Finally, the scatter of the Σmol. gas + stellar versus ΣSFR correlation is smaller than that of the resolved star formation main sequence, but higher than that found for the resolved Kennicutt–Schmidt relation. Conclusions. The resolved molecular gas main sequence has the tightest relation at a spatial scale of 100 pc (scatter of 0.34 dex), followed by the resolved Kennicutt–Schmidt relation (0.41 dex) and then the resolved star formation main sequence (0.51 dex). This is consistent with expectations from the timescales involved in the evolutionary cycle of molecular clouds. Surprisingly, the resolved Kennicutt–Schmidt relation shows the least variation across galaxies and environments, suggesting a tight link between molecular gas and subsequent star formation. The scatter of the three relations decreases at lower spatial resolutions, with the resolved Kennicutt–Schmidt relation being the tightest (0.27 dex) at a spatial scale of 1 kpc. Variation in the slope of the resolved star formation main sequence among galaxies is partially due to different detection fractions of ΣSFR with respect to Σstellar.

show abstract

“…Our results do not change qualitatively if we include the diffuse Hα emission within the annulus in this analysis. The orbital time within any given annulus is determined from high-resolution rotation curve fits to the molecular gas kinematics, as traced by PHANGS-ALMA observations of CO (2−1) emission (Lang et al 2020). IC 5332 is excluded from this analysis, as it contains no detected pixel above the necessary signal-to-noise (S/N) cut.…”

Section: Ancillary Datamentioning

confidence: 99%

Measuring the mixing scale of the ISM within nearby spiral galaxies

Kreckel

Blanc

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

The spatial distribution of metals reflects, and can be used to constrain, the processes of chemical enrichment and mixing. Using PHANGS-MUSE optical integral field spectroscopy, we measure the gas phase oxygen abundances (metallicities) across 7138 H ii regions in a sample of eight nearby disc galaxies. In Paper I we measure and report linear radial gradients in the metallicities of each galaxy, and qualitatively searched for azimuthal abundance variations. Here, we examine the two-dimensional variation in abundances once the radial gradient is subtracted, Δ(O/H), in order to quantify the homogeneity of the metal distribution and to measure the mixing scale over which HII region metallicities are correlated. We observe low (0.03–0.05 dex) scatter in Δ(O/H) globally in all galaxies, with significantly lower (0.02–0.03 dex) scatter on small (<600 pc) spatial scales. This is consistent with the measurement uncertainties, and implies the two-dimensional metallicity distribution is highly correlated on scales of ≲ 600” pc. We compute the two point correlation function for metals in the disc in order to quantify the scale lengths associated with the observed homogeneity. This mixing scale is observed to correlate better with the local gas velocity dispersion (of both cold and ionized gas) than with the star formation rate. Selecting only H ii regions with enhanced abundances relative to a linear radial gradient, we do not observe increased homogeneity on small scales. This suggests that the observed homogeneity is driven by the mixing introducing material from large scales rather than by pollution from recent and on-going star formation.

show abstract

PHANGS CO Kinematics: Disk Orientations and Rotation Curves at 150 pc Resolution

Cited by 106 publications

References 81 publications

Molecular Gas Properties on Cloud Scales across the Local Star-forming Galaxy Population

Molecular Gas Properties on Cloud Scales across the Local Star-forming Galaxy Population

Star formation scaling relations at ∼100 pc from PHANGS: Impact of completeness and spatial scale

Measuring the mixing scale of the ISM within nearby spiral galaxies

Contact Info

Product

Resources

About