The Tremaine-Weinberg method at high redshifts | Astronomy & Astrophysics (A&A)

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Table B.1

NIRSpec capability for measuring bar pattern speeds using the TW method

Filter	Wavelength range	FWHM_PSF	Redshift range	$l_{b}^{\min}$ $l_{\rm{b}}^{\min }$
	(μm)	(″)		(kpc)
F070LP	0.7 – 1.27	0.127	0.35 ≲ ɀ ≲ 1.45	2.90
F100LP	0.97 – 1.89	0.128	0.87 ≲ ɀ ≲ 2.65	3.26
F170LP	1.66 – 3.17	0.138	2.21 ≲ ɀ ≲ 5.13	3.01
F290LP	2.87 – 5.27	0.170	4.55 ≲ ɀ ≲ 9.19	2.77

Notes. Redshift ranges where NIRSpec filters can detect barred galaxies suitable for the TW method. These intervals are derived under the assumptions that the Mg line triplet serves as the primary absorption line used in the TW method and inclination angle is 45°. The PSF size is used to determine the minimum required bar length, $l_{b}^{\min}$ $l_{\rm{b}}^{\min }$ , for detection by the TW method. Since both the PSF size and $l_{b}^{\min}$ $l_{\rm{b}}^{\min }$ vary with redshift, we report their mean values for each filter. As mentioned in the text, we use simulated PSFs obtained from STPSF software.

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