Table 1
Hα results for the PHANGS MUSE galaxies.
| Galaxy | αMK | αpy | nHII | Fmin,Hα | Rmed | αMK,in,αpy,in | nHII,in | αMK,out, αpy,out | nHII,out | |
|---|---|---|---|---|---|---|---|---|---|---|
| IC5332 | 1.72 ± 0.033 | 1.74 ± 0.020 | 476 | 11 000 | 1.99 | 0.25 | 1.74, 1.75 | 258 | 1.70, 1.73 | 218 |
| NGC0628 | 1.66 ± 0.016 | 1.68 ± 0.017 | 1421 | 30 002 | 3.63 | 0.26 | 1.73, 1.76 | 650 | 1.61, 1.66 | 771 |
| NGC1087 | 1.56 ± 0.021 | 1.60 ± 0.013 | 588 | 50 476 | 3.60 | 0.53 | 1.48, 1.66 | 371 | 1.76, 1.71 | 217 |
| NGC1300 | 1.68 ± 0.025 | 1.71 ± 0.020 | 745 | 20 000 | 7.93 | 0.48 | 1.68, 1.60 | 398 | 1.68, 1.62 | 347 |
| NGC1365 | 1.68 ± 0.032 | 1.69 ± 0.027 | 419 | 100 000 | 13.78 | 0.40 | 1.74, 1.76 | 185 | 1.64, 1.73 | 234 |
| NGC1385 | 1.42 ± 0.020 | 1.47 ± 0.013 | 710 | 26 982 | 3.53 | 0.41 | 1.29, 1.57 | 438 | 1.74, 1.63 | 272 |
| NGC1433 | 1.86 ± 0.036 | 1.87 ± 0.035 | 588 | 30 000 | 8.76 | 0.52 | 1.88, 1.60 | 292 | 1.84, 1.66 | 296 |
| NGC1512 | 1.78 ± 0.042 | 1.82 ± 0.040 | 324 | 30 000 | 7.55 | 0.33 | 1.83, 1.61 | 163 | 1.74, 1.67 | 161 |
| NGC1566 | 1.53 ± 0.014 | 1.55 ± 0.013 | 1078 | 31 455 | 5.64 | 0.30 | 1.46, 1.59 | 665 | 1.68, 1.67 | 413 |
| NGC1672 | 1.56 ± 0.020 | 1.60 ± 0.021 | 694 | 47 592 | 8.12 | 0.47 | 1.55, 1.62 | 371 | 1.57, 1.71 | 323 |
| NGC2835 | 1.69 ± 0.030 | 1.72 ± 0.033 | 488 | 52 360 | 3.61 | 0.32 | 1.63, 1.63 | 267 | 1.78, 1.71 | 221 |
| NGC3351 | 1.67 ± 0.024 | 1.71 ± 0.020 | 670 | 19 347 | 3.99 | 0.38 | 1.66, 1.54 | 355 | 1.69, 1.61 | 315 |
| NGC3627 | 1.45 ± 0.017 | 1.50 ± 0.017 | 833 | 90 250 | 4.46 | 0.26 | 1.39, 1.64 | 433 | 1.53, 1.72 | 400 |
| NGC4254 | 1.50 ± 0.013 | 1.54 ± 0.007 | 1847 | 57 359 | 4.91 | 0.51 | 1.42, 1.58 | 1106 | 1.64, 1.68 | 741 |
| NGC4303 | 1.51 ± 0.014 | 1.55 ± 0.009 | 1613 | 48 167 | 5.51 | 0.32 | 1.45, 1.55 | 961 | 1.61, 1.66 | 652 |
| NGC4321 | 1.64 ± 0.020 | 1.67 ± 0.014 | 1005 | 61 501 | 6.39 | 0.47 | 1.59, 1.58 | 560 | 1.72, 1.69 | 445 |
| NGC4535 | 1.50 ± 0.013 | 1.53 ± 0.010 | 1260 | 9067 | 5.62 | 0.30 | 1.52, 1.37 | 629 | 1.49, 1.45 | 631 |
| NGC5068 | 1.60 ± 0.021 | 1.62 ± 0.017 | 930 | 44 785 | 2.09 | 0.37 | 1.58, 1.55 | 471 | 1.63, 1.66 | 459 |
| NGC7496 | 1.59 ± 0.032 | 1.62 ± 0.017 | 377 | 20 822 | 4.28 | 0.47 | 1.61, 1.47 | 213 | 1.58, 1.57 | 164 |
| M33 | 1.41 ± 0.026 | 1.51 ± 0.018 | 368 | 60 000 | 3.98a | 0.53 | 1.28, 1.45 | 190 | 1.52, 1.59 | 178 |
Notes. Sample of galaxies observed by Santoro et al. (2022) followed by results from fitting the Hα flux distribution with the Maschberger & Kroupa (2009) method and powerlaw.py algorithm (Alstott et al. 2014). Second column is overall slope, where the second number is determined with powerlaw.py. Third column is the number of HII regions with a flux greater than the value in Col. 4 expressed in units of 10−20 erg cm−2 sec−1. Column 4 is designed to be the true completeness limit as explained in the text. Column 5 gives the median galactocentric radius of the HII region sample for that galaxy in kpc and as a fraction of R25. The following two columns provide the inner slope with the two methods and the number of HII regions. The next two columns are the same but for the outer parts. a Corrected for a distance of 840 kpc. Due to the lower number of HII regions, the uncertainties on α are higher when the inner and outer parts are evaluated separately.
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