2024ApJS..271....2H

Query : 2024ApJS..271....2H

2024ApJS..271....2H - Astrophys. J., Suppl. Ser., 271, 2 (2024/March-0)

The PHANGS-AstroSat Atlas of Nearby Star-forming Galaxies.

HASSANI H., ROSOLOWSKY E., KOCH E.W., POSTMA J., NOFECH J., CORBOULD H., THILKER D., LEROY A.K., SCHINNERER E., BELFIORE F., BIGIEL F., BOQUIEN M., CHEVANCE M., DALE D.A., EGOROV O.V., EMSELLEM E., GLOVER S.C.O., GRASHA K., GROVES B., HENNY K., KIM J., KLESSEN R.S., KRECKEL K., KRUIJSSEN J.M.D., LEE J.C., LOPEZ L.A., NEUMANN J., PAN H.-A., SANDSTROM K.M., SARBADHICARY S.K., SUN J. and WILLIAMS T.G.

Abstract (from CDS):

We present the Physics at High Angular resolution in Nearby GalaxieS (PHANGS)-AstroSat atlas, which contains UV imaging of 31 nearby star-forming galaxies captured by the Ultraviolet Imaging Telescope on the AstroSat satellite. The atlas provides a homogeneous data set of far-UV and near-UV maps of galaxies within a distance of 22 Mpc and a median angular resolution of 1.″4 (corresponding to a physical scale between 25 and 160 pc). After subtracting a uniform UV background and accounting for Milky Way extinction, we compare our estimated flux densities to GALEX observations, finding good agreement. We find candidate extended UV disks around the galaxies NGC 6744 and IC 5332. We present the first statistical measurements of the clumping of the UV emission and compare it to the clumping of molecular gas traced with the Atacama Large Millimeter/submillimeter Array (ALMA). We find that bars and spiral arms exhibit the highest degree of clumping, and the molecular gas is even more clumped than the far-UV (FUV) emission in galaxies. We investigate the variation of the ratio of observed FUV to Hα in different galactic environments and kiloparsec-sized apertures. We report that ∼65% of the variation of the log10(FUV/Hα) can be described through a combination of dust attenuation with star formation history parameters. The PHANGS-AstroSat atlas enhances the multiwavelength coverage of our sample, offering a detailed perspective on star formation. When integrated with PHANGS data sets from ALMA, the Very Large Telescope-MUSE, the Hubble Space Telescope, and JWST, it develops our comprehensive understanding of attenuation curves and dust attenuation in star-forming galaxies.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Molecular gas - Interstellar medium - Ultraviolet astronomy - Stellar astronomy

Simbad objects: 37

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Number of rows : 37
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 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3588 2
2 NGC 300 GiG 00 54 53.4465638304 -37 41 03.168402396 8.83 8.69 8.13 7.46   ~ 1614 2
3 M 74 G 01 36 41.7451236624 +15 47 01.107512304 10.52 10.00 9.46 9.16   ~ 1934 1
4 NGC 1097 LIN 02 46 19.059 -30 16 29.68 10.46 9.97 9.48 8.72 9.8 ~ 1448 3
5 NGC 1300 Sy2 03 19 41.0462219928 -19 24 40.187565432   11.16 10.42 9.90 10.7 ~ 616 0
6 NGC 1317 GiP 03 22 44.2823209512 -37 06 13.180903956 12.20 11.78 11.02 10.22   ~ 240 1
7 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1987 2
8 NGC 1385 EmG 03 37 28.323 -24 30 04.60 11.28 11.50 10.94 10.45 11.7 ~ 318 2
9 NGC 1433 Sy2 03 42 01.4847418992 -47 13 18.929092656   10.84 9.99 9.61 10.2 ~ 447 0
10 HZ 4 WD* 03 55 21.9881513952 +09 47 18.135008592 13.917 14.592 14.506 14.58 14.642 DA3.4 220 0
11 NGC 1512 GiP 04 03 54.281 -43 20 55.86 11.30 11.43 10.54 10.37   ~ 457 1
12 NGC 1546 EmG 04 14 36.542 -56 03 38.92 12.15 12.31 10.92 10.84 11.2 ~ 133 1
13 NGC 1566 Sy1 04 20 00.3968473248 -54 56 16.624708764 10.29 10.19 9.73 9.21 10.1 ~ 1051 2
14 NGC 2090 GiG 05 47 01.8557074752 -34 15 01.679264784 12.17 11.70 11.20 10.43 11.0 ~ 206 1
15 NGC 2835 EmG 09 17 52.8523921416 -22 21 16.839119700   11.03   10.32 10.9 ~ 285 0
16 NGC 2903 AGN 09 32 10.111 +21 30 02.99 10.44 9.75 9.07 8.68   ~ 1204 3
17 M 95 GiP 10 43 57.7313485800 +11 42 13.301191332 10.71 10.51 9.73 9.48   ~ 1238 2
18 NGC 3621 Sy2 11 18 16.300 -32 48 45.36 10.10 9.44 9.56 8.07 10.1 ~ 661 3
19 M 66 AGN 11 20 15.0 +12 59 29 9.85 9.65 8.92     ~ 1509 4
20 M 99 H2G 12 18 49.625 +14 24 59.36 10.45 10.44 9.87     ~ 1004 2
21 NGC 4298 GiC 12 21 32.7578814360 +14 36 22.048690716   12.04 11.34     ~ 358 1
22 M 100 AGN 12 22 54.9299993592 +15 49 20.296257960 10.04 10.05 9.35     ~ 1963 2
23 NGC 4476 GiG 12 29 59.0772974472 +12 20 55.292203464 13.28 13.01 12.19     ~ 340 1
24 NGC 4535 H2G 12 34 20.3443516704 +08 11 51.908488116   11.1       ~ 679 0
25 NGC 4571 GiC 12 36 56.3722998960 +14 13 02.296534836   13.6       ~ 368 1
26 M 58 Sy2 12 37 43.59747 +11 49 05.1240 10.80 10.48 9.66     ~ 1140 2
27 NGC 4625 SyG 12 41 52.7121819576 +41 16 26.115765780 12.74 12.92 12.35     ~ 383 2
28 NGC 4654 H2G 12 43 56.638 +13 07 34.86   11.8       ~ 600 1
29 M 63 LIN 13 15 49.2741893928 +42 01 45.728076108   9.34 8.59 8.35   ~ 1292 2
30 NAME Centaurus A BLL 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4774 3
31 M 83 SBG 13 37 00.91920 -29 51 56.7400 8.85 8.11 7.52 7.21   ~ 2778 2
32 NGC 6744A G 19 08 43.9 -63 43 48   15.15   14.23   ~ 19 0
33 NGC 6744 GiG 19 09 46.1335950504 -63 51 26.897079024   9.28 8.25 8.08 9.6 ~ 303 0
34 NGC 7496 Sy2 23 09 47.2876854912 -43 25 40.279652796   11.92 13.90 10.95 11.5 ~ 350 1
35 IC 5332 GiG 23 34 27.488 -36 06 03.89 11.59 11.27 10.72 10.50 11.2 ~ 216 0
36 NGC 7793 GiG 23 57 49.7540045856 -32 35 27.701550744 10.26 9.74 9.28 9.06 9.7 ~ 1188 2
37 NAME Local Group GrG ~ ~           ~ 9325 0

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