Emission-line Metallicities from the Faint Infrared Grism Survey and VLT/MUSE

Pharo, John; Malhotra, Sangeeta; Rhoads, James E.; Christensen, L.; Finkelstein, Steven L.; Grogin, Norman A.; Harish, Santosh; Jiang, Tianxing; Kim, Keun-Ho; Koekemoer, Anton M.; Pirzkal, Norbert; Smith, Mark; Yang, Huan; Cimatti, A.; Ferreras, Ignacio; Hathi, N. P.; Hibon, Pascale; Meurer, G. R.; Oestlin, Goeran; Pasquali, A.; Ryan, Russell E.; Straughn, Amber N.; Windhorst, Rogier A.

doi:10.3847/1538-4357/ab08ec

“…The standard deviation of continuum-subtracted fluxes in this surrounding region is combined with the intrinsic flux error of the pixel (largely influenced by the skyline model) to get a flux error estimate, resulting in a continuum-subtracted residual spectrum and an error spectrum. This method of continuum-subtracted peak detection has demonstrated success in detecting emission lines from faint and low-mass sources in other deep surveys (e.g., Yang et al 2017;Pharo et al 2019Pharo et al , 2020. See Figure 2 for some example spectra showing the continuum subtraction.…”

Section: Redshift Fittingmentioning

confidence: 99%

The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations

Pharo

¹

,

Guo

²

,

Barro

³

et al. 2022

ApJS

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We present a catalog of spectroscopically measured redshifts over 0 < z < 2 and emission-line fluxes for 1440 galaxies. The majority (∼65%) of the galaxies come from the HALO7D survey, with the remainder from the DEEPwinds program. This catalog includes redshifts for 646 dwarf galaxies with log ( M ⋆ / M ⊙ ) < 9.5 . Eight-hundred and ten catalog galaxies did not have previously published spectroscopic redshifts, including 454 dwarf galaxies. HALO7D used the DEIMOS spectrograph on the Keck II telescope to take very deep (up to 32 hr exposure, with a median of ∼7 hr) optical spectroscopy in the COSMOS, EGS, GOODS-North, and GOODS-South CANDELS fields, and in some areas outside CANDELS. We compare our redshift results to existing spectroscopic and photometric redshifts in these fields, finding only a 1% rate of discrepancy with other spectroscopic redshifts. We measure a small increase in median photometric redshift error (from 1.0% to 1.3%) and catastrophic outlier rate (from 3.5% to 8%) with decreasing stellar mass. We obtained successful redshift fits for 75% of massive galaxies, and demonstrate a similar 70%–75% successful redshift measurement rate in 8.5 < log ( M ⋆ / M ⊙ ) < 9.5 galaxies, suggesting similar survey sensitivity in this low-mass range. We describe the redshift, mass, and color–magnitude distributions of the catalog galaxies, finding HALO7D galaxies representative of CANDELS galaxies up to i-band magnitudes of 25. The catalogs presented will enable studies of star formation, the mass–metallicity relation, star formation–morphology relations, and other properties of the z ∼ 0.7 dwarf galaxy population.

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“…In order to study the chemical enrichment of galaxies using nebular metallicity, we need to measure galaxies at different redshifts to infer a ChEH (Lu et al 2015;Cullen et al 2019;Pharo et al 2019;Urrutia et al 2019). This has the advantage of not being tied to model-dependent fits, as is the case for stellar metallicity.…”

Section: Introductionmentioning

confidence: 99%

Chemical evolution history of MaNGA galaxies

Camps-Fariña,

Sánchez,

Mejía-Narváez

et al. 2022

Preprint

1

4

0

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We show the results of a study using the spectral synthesis technique study for the full MaNGA sample showing their Chemical Enrichment History (ChEH) as well as the evolution of the stellar mass-metallicity relation (MZR) over cosmic time. We find that the more massive galaxies became enriched first and the lower mass galaxies did so later, producing a change in the MZR which becomes shallower in time. Separating the sample into morphology and star-forming status bins some particularly interesting results appear: The mass dependency of the MZR becomes less relevant for later morphological types, to the extent that it inverts for Sd/Irr galaxies, suggesting that morphology is at least as important a factor as mass in chemical evolution. The MZR for the full sample shows a flattening at the high-mass end and another at the low-mass range, but the former only appears for retired galaxies while the latter only appears for star-forming galaxies. We also find that the average metallicity gradient is currently negative for all mass bins but for low mass galaxies it was inverted at some point in the past, before which all galaxies had a positive gradient. We also compare how diverse the ChEHs are in the different bins considered as well as what primarily drives the diversity: How much galaxies become enriched or how quickly they do so.

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“…These types of observations have typically been conducted from the ground in the optical (Smith 1975;MacAlpine et al 1977;Schneider et al 1999;Salzer et al 2000Salzer et al , 2005 to avoid high nightsky background levels and contamination from telluric emission at longer wavelengths. However, investigations of optical emission lines at higher redshifts are possible from space using the near-infrared (NIR) capabilities of the Hubble Space Telescope (e.g., Atek et al 2010Atek et al , 2011Brammer et al 2012;Colbert et al 2013;Schmidt et al 2014;Momcheva et al 2016;Estrada-Carpenter et al 2019;Pharo et al 2019Pharo et al , 2020Bowman et al 2021;Simons et al 2021;Noirot et al 2022;Papovich et al 2022;Backhaus et al 2023).…”

Section: Scientific Motivationmentioning

confidence: 99%

The MUSE Ultra Deep Field (MUDF). III. Hubble Space Telescope WFC3 Grism Spectroscopy and Imaging

Revalski

¹

,

Rafelski

²

,

Fumagalli

³

et al. 2023

ApJS

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We present extremely deep Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) observations of the MUSE Ultra Deep Field. This unique region of the sky contains two quasars at z ≈ 3.22 that are separated by only ∼500 kpc, providing a stereoscopic view of gas and galaxies in emission and absorption across ∼10 billion years of cosmic time. We have obtained 90 orbits of HST WFC3 G141 near-infrared grism spectroscopy of this field in a single pointing, as well as 142 hr of optical spectroscopy with the Very Large Telescope Multi Unit Spectroscopic Explorer (MUSE). The WFC3 (F140W, F125W, and F336W) and archival WFPC2 (F702W and F450W) imaging provides five-filter photometry that we use to detect 3375 sources between z ≈ 0–6, including 1536 objects in a deep central pointing with both spectroscopic and photometric coverage. The F140W and F336W mosaics reach exceptional depths of m AB ≈ 28 and 29, respectively, providing near-infrared and rest-frame ultraviolet information for 1580 sources, and we reach 5σ continuum detections for objects as faint as m AB ≈ 27 in the grism spectra. The extensive wavelength coverage of MUSE and WFC3 allows us to measure spectroscopic redshifts for 419 sources, down to galaxy stellar masses of log(M/M ⊙) ≈7 at z ≈ 1–2. In this publication, we provide the calibrated HST data and source catalogs as High Level Science Products for use by the community, which includes photometry, morphology, and redshift measurements that enable a variety of studies aimed at advancing our models of galaxy formation and evolution in different environments.

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Emission-line Metallicities from the Faint Infrared Grism Survey and VLT/MUSE

Cited by 7 publications

References 68 publications

The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations

The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations

Chemical evolution history of MaNGA galaxies

The MUSE Ultra Deep Field (MUDF). III. Hubble Space Telescope WFC3 Grism Spectroscopy and Imaging

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