Spatially resolved interstellar dust properties in the face-on spiral galaxy M 99 as observed by NIKA2

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Volume 709 (May 2026)

A&A, 709 (2026) A1

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Table 2.

Multi-wavelength continuum maps used in this work.

Telescope/Instrument	λ_obs	$θ_{res}^{FWHM}$ $Mathematical equation: $ {\theta_{\mathrm{res}}^{\mathrm{FWHM}}} $$	Pixel size	Calibration	SED fitting	Calibrators	Ref.
	[μm]	[″]	[″]	uncertainty [%]
GALEX/FUV	0.153	4	3	4.5^a		✓	1
GALEX/NUV	0.227	5.6	3	2.7^a		✓	1
Spitzer/IRAC	3.6	1.66	0.6	10.2^a	✓	✓	1
Spitzer/IRAC	4.5	1.72	0.6	10.2^a	✓		1
Spitzer/IRAC	5.2	1.88	0.6	10.2^a	✓		1
Spitzer/IRAC	8	1.98	0.6	10.2^a	✓		1
Spitzer/MIPS	25	6	1.5	4^a	✓	✓	1
Herschel/PACS	70	9	2	5.4^a	✓		1
Herschel/PACS	100	10	3	5.4^a	✓		1
Herschel/PACS	160	13	4	5.4^a	✓		1
Herschel/SPIRE	250	18	6	5.9^a	✓		1
Herschel/SPIRE	350	25	8	5.9^a	✓		1
Herschel/SPIRE	500	36	12	5.9^a	✓		1
IRAM 30 m/NIKA2	1150	12	3	7.7^b	✓		2
Planck/HFI4	1380	300	103	1^a	✓		1
IRAM 30 m/NIKA2	2000	18	3	5.8^b	✓		2
X-VLA + Effelsberg	3 × 10⁴	15	1	5^c	✓		3
C-VLA + Effelsberg	6 × 10⁴	15	1	5^c	✓		3
L-VLA	20 × 10⁴	4.5	0.7	3^d	✓		4

Notes. From left to right, in the columns we list (increasing wavelengths) the telescope and instrument name, the central wavelength, the angular resolution (FWHM), the pixel size, and the calibration uncertainty. Finally, we indicate whether the map was used for SED fitting and/or as a calibrator.

^(a)

Galliano et al. (2021) and references therein.

^(b)

Ejlali et al. (2025, their Appendix A1) for uncertainty on the beam solid angle (i.e. 5.8% at 1.15 mm and 2.9% at 2 mm), Perotto et al. (2020) and reference therein for uncertainty on Uranus model (i.e. 5%).

^(c)

Tabatabaei et al. (2017), Chemin et al. (2016).

^(d)

Perley & Butler (2015) and the official VLA NRAO website: https://science.nrao.edu/facilities/vla/.

(1) DustPedia archive; (2) this work; (3) Chyży et al. (2007); (4) Chiang, Koch, and the PHANGS collaboration (in prep.).

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