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2021A&A...650A.134P

Query : 2021A&A...650A.134P

2021A&A...650A.134P - Astronomy and Astrophysics, volume 650A, 134-134 (2021/6-1)

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

PESSA I., SCHINNERER E., BELFIORE F., EMSELLEM E., LEROY A.K., SCHRUBA A., KRUIJSSEN J.M.D., PAN H.-A., BLANC G.A., SANCHEZ-BLAZQUEZ P., BIGIEL F., CHEVANCE M., CONGIU E., DALE D., FAESI C.M., GLOVER S.C.O., GRASHA K., GROVES B., HO I., JIMENEZ-DONAIRE M., KLESSEN R., KRECKEL K., KOCH E.W., LIU D., MEIDT S., PETY J., QUEREJETA M., ROSOLOWSKY E., SAITO T., SANTORO F., SUN J., USERO A., WATKINS E.J. and WILLIAMS T.G.

Abstract (from CDS):


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 (Σ_mol. gas_ versus ΣSFR), and resolved molecular gas main sequence (Σstellar versus Σ_mol. gas_), and we derived their slope and scatter at spatial resolutions from 100pc to 1kpc (under various assumptions).
Results. All three relations were recovered at the highest spatial resolution (100pc). 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 Σ_mol. 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 100pc (scatter of 0.34dex), 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.

Abstract Copyright: © I. Pessa et al. 2021

Journal keyword(s): galaxies: ISM - galaxies: evolution - galaxies: star formation - galaxies: general

Simbad objects: 19

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Number of rows : 19
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 M 74 AG? 01 36 41.7451236624 +15 47 01.107512304 10.52 10.00 9.46 9.16   ~ 1695 1
2 NGC 1087 H2G 02 46 25.1550134904 -00 29 55.457857644   11.5   11.4 11.5 ~ 322 0
3 NGC 1300 Sy2 03 19 41.0462219928 -19 24 40.187565432   11.16 10.42 9.90 10.7 ~ 521 0
4 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1765 2
5 NGC 1385 EmG 03 37 28.323 -24 30 04.60 11.28 11.50 10.94 10.45 11.7 ~ 264 2
6 NGC 1433 Sy2 03 42 01.4847418992 -47 13 18.929092656   10.84 9.99 9.61 10.2 ~ 372 0
7 NGC 1512 GiP 04 03 54.281 -43 20 55.86 11.30 11.43 10.54 10.37   ~ 383 1
8 NGC 1566 Sy1 04 20 00.3968473248 -54 56 16.624708764 10.29 10.19 9.73 9.21 10.1 ~ 881 2
9 NGC 1672 SyG 04 45 42.552 -59 14 50.68 10.29 10.53 9.68 9.53 10.2 ~ 390 1
10 NGC 2835 EmG 09 17 52.8523921416 -22 21 16.839119700   11.03   10.32 10.9 ~ 229 0
11 M 95 GiP 10 43 57.7313485800 +11 42 13.301191332 10.71 10.51 9.73 9.48   ~ 1092 2
12 M 66 GiP 11 20 15.0 +12 59 29 9.85 9.65 8.92     ~ 1356 4
13 M 99 H2G 12 18 49.625 +14 24 59.36 10.45 10.44 9.87     ~ 897 2
14 M 61 Sy2 12 21 54.9282582888 +04 28 25.597367184 10.07 10.18 9.65     ~ 976 2
15 M 100 AGN 12 22 54.9299993592 +15 49 20.296257960 10.04 10.05 9.35     ~ 1810 2
16 NGC 4535 H2G 12 34 20.3443516704 +08 11 51.908488116   11.1       ~ 603 0
17 NGC 5068 AG? 13 18 54.807 -21 02 20.76 11.24 10.53 10.01 9.78 10.1 ~ 282 0
18 NGC 7496 Sy2 23 09 47.2876854912 -43 25 40.279652796   11.92 13.90 10.95 11.5 ~ 284 1
19 IC 5332 GiG 23 34 27.488 -36 06 03.89 11.59 11.27 10.72 10.50 11.2 ~ 169 0

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2023.11.29-22:53:55

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