Forward modeling of galaxy kinematics in slitless spectroscopy

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Volume 633 (January 2020)

A&A, 633 (2020) A43

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Table 1.

Main instrumental properties of past, current, and future slitless surveys.

Survey-telescope	Instrument-grism	Spectral range	Spatial scale	D	ℛ	R_kin	Galaxy number
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)
GPS ^(a)-HST	NICMOS(IR)-G141	11 000–19 000	0.20	80	200	1260–2180	33
PEARS ^(b)-HST	ACS-G800L	5500–10 500	0.05	38.5	100	1100–2100	10 000
3DHST ^(c)-HST	WFC3(IR)-G141	10 000–17 500	0.13	46.5	130	800–1400	100 000
GLASS ^(d)-HST	WFC3(IR)-G102	7500–11 500	0.13	24.5	210	640–980	2000
JWST ^(e)	NIRISS (2021)	6000–23 000	0.065	10	700	130–500	–
Euclid^(f)	NISP-R (2022)	12 500–18 500	0.30	13	380	210–310	30 000 000
WFIRST ^(g)	GRS (2028)	10 000–19 500	0.11	11	435–865	170–330	18 000 000

Notes. (1) Telescope and survey name, (2) instrument and grism, (3) wavelength coverage (in Å), (4) spatial sampling (in arcsec px⁻¹), (5) spectral sampling (= Δλ in Å px⁻¹), (6) spectroscopic resolving power ℛ ≡ λ/Δλ, (7) kinematic sampling for Hα galaxies emitters at spectral range limits (in km s⁻¹ px⁻¹), (8) approximate catalog size.

References.

^(a)

HST Grism Parallel survey Thompson et al. (1998).

^(b)

Straughn et al. (2008), Pirzkal et al. (2009).

^(c)

Brammer et al. (2012), Momcheva et al. (2016).

^(d)

Schmidt et al. (2014), Treu et al. (2015).

^(e)

Doyon et al. (2012).

^(f)

Grupp et al. (2012).

^(g)

Spergel et al. (2015).

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