2024AJ....167...39P

Query : 2024AJ....167...39P

2024AJ....167...39P - Astron. J., 167, 39 (2024/January-0)

A Two-Component Probability Distribution Function Describes the Mid-IR Emission from the Disks of Star-forming Galaxies.

PATHAK D., LEROY A.K., THOMPSON T.A., LOPEZ L.A., BELFIORE F., BOQUIEN M., DALE D.A., GLOVER S.C.O., KLESSEN R.S., KOCH E.W., ROSOLOWSKY E., SANDSTROM K.M., SCHINNERER E., SMITH R., SUN J., SUTTER J., WILLIAMS T.G., BIGIEL F., CAO Y., CHASTENET J., CHEVANCE M., CHOWN R., EMSELLEM E., FAESI C.M., LARSON K.L., LEE J.C., MEIDT S., OSTRIKER E.C., RAMAMBASON L., SARBADHICARY S.K. and THILKER D.A.

Abstract (from CDS):

High-resolution JWST-MIRI images of nearby spiral galaxies reveal emission with complex substructures that trace dust heated both by massive young stars and the diffuse interstellar radiation field. We present high angular (0.″85) and physical resolution (20-80 pc) measurements of the probability distribution function (PDF) of mid-infrared (mid-IR) emission (7.7-21 μm) from 19 nearby star-forming galaxies from the PHANGS-JWST Cycle 1 Treasury. The PDFs of mid-IR emission from the disks of all 19 galaxies consistently show two distinct components: an approximately lognormal distribution at lower intensities and a high-intensity power law component. These two components only emerge once individual star-forming regions are resolved. Comparing with locations of H II regions identified from Very Large Telescope/MUSE Hα mapping, we infer that the power-law component arises from star-forming regions and thus primarily traces dust heated by young stars. In the continuum-dominated 21 μm band, the power law is more prominent and contains roughly half of the total flux. At 7.7-11.3 μm, the power law is suppressed by the destruction of small grains (including PAHs) close to H II regions, while the lognormal component tracing the dust column in diffuse regions appears more prominent. The width and shape of the lognormal diffuse emission PDFs in galactic disks remain consistent across our sample, implying a lognormal gas column density N(H) ≈ 1021 cm–2 shaped by supersonic turbulence with typical (isothermal) turbulent Mach numbers ≈5-15. Finally, we describe how the PDFs of galactic disks are assembled from dusty H II regions and diffuse gas and discuss how the measured PDF parameters correlate with global properties such as star formation rate and gas surface density.

Abstract Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Interstellar medium - Extragalactic astronomy - Dust physics - H II regions - Infrared astronomy - Stellar feedback

Simbad objects: 23

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Number of rows : 23
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 M 33 GiG 01 33 50.8965749232 +30 39 36.630403128 6.17 6.27 5.72     ~ 6226 1
2 M 74 G 01 36 41.7451236624 +15 47 01.107512304 10.52 10.00 9.46 9.16   ~ 1934 1
3 NGC 1087 H2G 02 46 25.1550134904 -00 29 55.457857644   11.5   11.4 11.5 ~ 379 0
4 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7988 0
5 NGC 1300 Sy2 03 19 41.0462219928 -19 24 40.187565432   11.16 10.42 9.90 10.7 ~ 616 0
6 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1987 2
7 NGC 1385 EmG 03 37 28.323 -24 30 04.60 11.28 11.50 10.94 10.45 11.7 ~ 318 2
8 NGC 1433 Sy2 03 42 01.4847418992 -47 13 18.929092656   10.84 9.99 9.61 10.2 ~ 447 0
9 NGC 1512 GiP 04 03 54.281 -43 20 55.86 11.30 11.43 10.54 10.37   ~ 457 1
10 NGC 1566 Sy1 04 20 00.3968473248 -54 56 16.624708764 10.29 10.19 9.73 9.21 10.1 ~ 1051 2
11 NGC 1672 SyG 04 45 42.552 -59 14 50.68 10.29 10.53 9.68 9.53 10.2 ~ 461 2
12 NGC 2835 EmG 09 17 52.8523921416 -22 21 16.839119700   11.03   10.32 10.9 ~ 285 0
13 M 95 GiP 10 43 57.7313485800 +11 42 13.301191332 10.71 10.51 9.73 9.48   ~ 1238 2
14 M 66 AGN 11 20 15.0 +12 59 29 9.85 9.65 8.92     ~ 1509 4
15 M 99 H2G 12 18 49.625 +14 24 59.36 10.45 10.44 9.87     ~ 1004 2
16 M 61 Sy2 12 21 54.9282582888 +04 28 25.597367184 10.07 10.18 9.65     ~ 1084 1
17 M 100 AGN 12 22 54.9299993592 +15 49 20.296257960 10.04 10.05 9.35     ~ 1963 2
18 NGC 4535 H2G 12 34 20.3443516704 +08 11 51.908488116   11.1       ~ 679 0
19 NGC 5068 AG? 13 18 54.807 -21 02 20.76 11.24 10.53 10.01 9.78 10.1 ~ 354 0
20 NGC 7469 Sy1 23 03 15.6 +08 52 26 12.60 13.00 12.34     ~ 2253 3
21 NGC 7496 Sy2 23 09 47.2876854912 -43 25 40.279652796   11.92 13.90 10.95 11.5 ~ 350 1
22 IC 5332 GiG 23 34 27.488 -36 06 03.89 11.59 11.27 10.72 10.50 11.2 ~ 216 0
23 NAME Local Group GrG ~ ~           ~ 9325 0

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