Table 1
Overview of the characteristics (full-width half maximum of the beam, calibration uncertainties) for the multi-wavelength dataset used in the RT analysis of M 51.
| Band | λ | FWHM | Refa | σ cal | Refa |
| [μm] | [arcsec] | ||||
|
|
|||||
| GALEX FUV | 0.15 | 4.2 | 1 | 0.05 mag | 1 |
| GALEX NUV | 0.23 | 5.3 | 1 | 0.03 mag | 1 |
| SDSS u | 0.35 | 2b | 2 | 2% | 3 |
| SDSS g | 0.48 | 2b | 2 | 2% | 3 |
| SDSS r | 0.62 | 2b | 2 | 2% | 3 |
| Hα | 0.66 | 2 | 4 | 5% | 4 |
| SDSS i | 0.76 | 2b | 2 | 2% | 3 |
| SDSS z | 0.91 | 2b | 2 | 2% | 3 |
| 2MASS J | 1.25 | 3.3c | 2 | 0.03 mag | 5 |
| 2MASS H | 1.65 | 3.1c | 2 | 0.03 mag | 5 |
| 2MASS K | 2.16 | 3.3c | 2 | 0.03 mag | 5 |
| WISE 1 | 3.4 | 6.1 | 6 | 2.4% | 7 |
| IRAC 3.6 μm | 3.6 | 1.7 | 8 | 1.8% | 9 |
| IRAC 4.5 μm | 4.5 | 1.7 | 8 | 1.9% | 9 |
| WISE 2 | 4.6 | 6.4 | 6 | 2.8% | 7 |
| IRAC 5.8 μm | 5.8 | 1.9 | 8 | 2.0% | 9 |
| IRAC 8.0 μm | 8.0 | 2.0 | 8 | 2.1% | 9 |
| WISE 3 | 12 | 6.5 | 6 | 4.5% | 7 |
| WISE 4 | 22 | 12 | 6 | 5.7% | 7 |
| MIPS 24 | 24 | 6 | 10 | 4% | 10 |
| PACS 70 | 70 | 5.8 | 11 | 5% | 12 |
| PACS 160 | 160 | 12.1 | 11 | 5% | 12 |
| SPIRE 250 | 250 | 18.2 | 13 | 4% d | 13 |
| SPIRE 350 | 350 | 24.9 | 13 | 4% d | 13 |
| SPIRE 500 | 500 | 36.3 | 13 | 4% d | 13 |
Notes.
References: (1) Morrissey et al. (2007); (2) this paper; (3) Padmanabhan et al. (2008); (4) Boselli & Gavazzi (2002); (5) Skrutskie et al. (2006); (6) Wright et al. (2010); (7) Jarrett et al. (2011); (8) Fazio et al. (2004); (9) Reach et al. (2005); (10) Engelbracht et al. (2007); (11) PACS Observers’ Manual; (12) Balog et al. (2013); (13) SPIRE Observers’ Manual.
We estimate the FWHM of the SDSS data by fitting a 2D Gaussian (IDL task starfit) to several stellar objects in the field of M 51. We apply the sum of two Gaussian kernels with FWHM of 2″ to convolve the SDSS data, which should be a good representation of the telescope’s PSF (Aniano et al. 2011).
We estimate the FWHM of the 2MASS data by fitting a 2D Gaussian (IDL task starfit) to several stellar objects in the field of M 51. We apply Gaussian kernels with FWHM of 3″ (H) and 3.5″ (J,K) to convolve the 2MASS data to the PACS 160 μm resolution (Aniano et al. 2011).
Calibration uncertainties for the Herschel SPIRE instrument are assumed to be around 4% in each band, adding in quadrature the 4% absolute calibration error from the assumed models used for Neptune (SPIRE Observers’ manual), and a random uncertainty of 1.5% accounting for the repetitive measurements of Neptune (see Bendo et al. 2013).
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