3D-HST: A WIDE-FIELD GRISM SPECTROSCOPIC SURVEY WITH THE HUBBLE SPACE TELESCOPE

By G. Brammer, P. V. van Dokkum, M. Franx, M. Fumagalli, Shannon G. Patel, Hans-Walter Rix, R. Skelton, M. Kriek, E. Nelson, K. Schmidt and 20 more. 2012

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We present 3D-HST, a near-infrared spectroscopic Treasury program with the Hubble Space Telescope for studying the physical processes that shape galaxies in the distant universe. 3D-HST provides rest-frame optical spectra for a sample of ∼7000 galaxies at 1 < z < 3.5, the epoch when ∼60% of all star formation took place, the number density of quasars peaked, the first galaxies stopped forming stars, and the structural regularity that we see in galaxies today must have emerged. 3D-HST will cover three quarters (625 arcmin2) of the CANDELS Treasury survey area with two orbits of primary WFC3/G141 grism coverage and two to four orbits with the ACS/G800L grism in parallel. In the IR, these exposure times yield a continuum signal-to-noise ratio of ∼5 per resolution element at H140 ∼ 23.1 and a 5σ emission-line sensitivity of ∼5 × 10−17 erg s−1 cm−2 for typical objects, improving by a factor of ∼2 for compact sources in images with low sky background levels. The WFC3/G141 spectra provide continuous wavelength coverage from 1.1 to 1.6 μm at a spatial resolution of ∼0.″13, which, combined with their depth, makes them a unique resource for studying galaxy evolution. We present an overview of the preliminary reduction and analysis of the grism observations, including emission-line and redshift measurements from combined fits to the extracted grism spectra and photometry from ancillary multi-wavelength catalogs. The present analysis yields redshift estimates with a precision of σ(z) = 0.0034(1 + z), or σ(v) ≈ 1000 km s−1. We illustrate how the generalized nature of the survey yields near-infrared spectra of remarkable quality for many different types of objects, including a quasar at z = 4.7, quiescent galaxies at z ∼ 2, and the most distant T-type brown dwarf star known. The combination of the CANDELS and 3D-HST surveys will provide the definitive imaging and spectroscopic data set for studies of the 1 < z < 3.5 universe until the launch of the James Webb Space Telescope.

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Citations in the corpus

• UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10 (2018, background): “High-redshift constraints have improved dramatically in the past five years due to the CANDELS, 3D-HST, ULTRAVISTA, and ZFOURGE surveys (Grogin et al. 2011; Brammer et al. 2012; McCracken et al. 2012).”
• FORMING COMPACT MASSIVE GALAXIES (2015, methodology): “Catalogs and Derived Parameters We use data from the 3D-HST project (van Dokkum et al. 2011; Brammer et al. 2012b) to identify candidate compact massive galaxies.”
• THE MOSDEF SURVEY: MEASUREMENTS OF BALMER DECREMENTS AND THE DUST ATTENUATION CURVE AT REDSHIFTS z ∼ 1.4–2.6 (2015, methodology): “The targeting catalogs include photometric redshifts and, where available, HST grism redshifts (Brammer et al. 2012; Skelton et al. 2014) and external spectroscopic redshifts.”
• The illustris simulation: Public data release (2015, methodology): “(4) Stellar evolution with the associated mass loss (gas recycling) and chemical enrichment, taking into account SN Ia/II and AGB stars. (5) Galacticscale outflows with an energy-driven, kinetic wind scheme. (6) Seeding and growth of supermassive black holes. (7) Feedback from AGN in both quasar and”
• EVIDENCE FOR WIDE-SPREAD ACTIVE GALACTIC NUCLEUS-DRIVEN OUTFLOWS IN THE MOST MASSIVE z ∼ 1–2 STAR-FORMING GALAXIES (2014, background): “…versus specific SFR is shown in Figure 1, along with that of the underlying population of mass-selected galaxies from the 3D-HST Treasury survey (Brammer et al. 2012; Skelton et al. 12 KMOS3D is a multi-year survey; the current sample includes a fraction of targets for which only part of the…”
• PHIBSS: MOLECULAR GAS CONTENT AND SCALING RELATIONS IN z ∼ 1–3 MASSIVE, MAIN-SEQUENCE STAR-FORMING GALAXIES (2012, methodology): “…is also covered by the recent WFC3 J-H-band coverage in CANDELS (Grogin et al. 2011), as well as by the Hα objective prism observations in 3D-HST (Brammer et al. 2012, van Dokkum et al. 2011), including additional optical spectroscopy from the DEEP3 Galaxy Redshift Survey (Cooper et al. 2011,…”
• THE MOSDEF SURVEY: ELECTRON DENSITY AND IONIZATION PARAMETER AT z ∼ 2.3 (2015, methodology): “…Near-infrared Deep Extragalactic Legacy Survey (CANDELS; Grogin et al. 2011; Koekemoer et al. 2011) and grism spectroscopy from the 3D-HST survey (Brammer et al. 2012a), as well as observations from Chandra, Spitzer, Herschel, VLA, 6 Available at http://www.mpa-garching.mpg.de/SDSS/DR7/ The…”
• THE 3D-HST SURVEY: HUBBLE SPACE TELESCOPE WFC3/G141 GRISM SPECTRA, REDSHIFTS, AND EMISSION LINE MEASUREMENTS FOR ∼100,000 GALAXIES (2015, methodology): “The limiting magnitude of these fits is well below where we can expect to detect continuum emission at sufficient S/N (Brammer et al. 2012b).”
• Lyα EMISSION FROM A LUMINOUS z = 8.68 GALAXY: IMPLICATIONS FOR GALAXIES AS TRACERS OF COSMIC REIONIZATION (2015, methodology): “The absolute calibration for each night was derived by comparing the spectroscopic magnitude of the stars on the slitmask with photometric measures in the J-band obtained from the 3D-HST catalog (Brammer et al. 2012; Skelton et al. 2014).”
• The IllustrisTNG simulations: public data release (2018, methodology): “Surveys such as SDSS (York et al. 2000), CANDELS (Grogin et al. 2011), 3D-HST (Brammer et al. 2012), LEGA-C (van der Wel et al. 2016), SINS/zC-SINF and KMOS3D (Gen-zel et al. 2014; Wisnioski et al. 2015), KBSS (Steidel et al. 2014), and MOSDEF (Kriek et al. 2015) provide local and high redshift…”
• THE MOST LUMINOUS z ∼ 9–10 GALAXY CANDIDATES YET FOUND: THE LUMINOSITY FUNCTION, COSMIC STAR-FORMATION RATE, AND THE FIRST MASS DENSITY ESTIMATE AT 500 Myr (2013, unknown): “These spectra cover ∼1.05–1.70 μm at low resolution, reaching a 5σ emission line flux limit for compact sources of ∼2–5 × 10−17 erg s−1 cm−2 (see Brammer et al. 2012).”
• CONSTRAINING THE LOW-MASS SLOPE OF THE STAR FORMATION SEQUENCE AT 0.5 < z < 2.5 (2014, methodology): “This method is more flexible than that originally described by Brammer et al. (2012), but the redshift precision is similar with σ ∼ 0.0035(1+z).”
• UVUDF: ULTRAVIOLET THROUGH NEAR-INFRARED CATALOG AND PHOTOMETRIC REDSHIFTS OF GALAXIES IN THE HUBBLE ULTRA DEEP FIELD (2015, methodology): “Comparison with Grism Redshifts The use of the WFC3 grisms on HST to determine redshifts is increasing at a rapid pace (e.g., Brammer et al. 2012; Colbert et al. 2013; Atek et al. 2014), providing large numbers of galaxy redshifts.”
• THE KMOS3D SURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽ z ⩽ 2.7 (2014, methodology): “Survey design & sample selection We select KMOS3D targets from the 3D-HST Treasury Survey (Brammer et al. 2012; Skelton et al. 2014) in the fields accessible from the VLT (GOODS-S, COSMOS, UDS).”
• THE GRISM LENS-AMPLIFIED SURVEY FROM SPACE (GLASS). I. SURVEY OVERVIEW AND FIRST DATA RELEASE (2015, methodology): “As noted in Section 4.1, the GLASS observations are designed to comply with the 3D-HST observing strategy and were processed with an updated version of the 3D-HST reduction pipeline17 described by Brammer et al. (2012).”