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

John Pharo, Sangeeta Malhotra, James Rhoads, Lise Christensen, Steven L. Finkelstein, Norman Grogin, Santosh Harish, Tianxing Jiang, Keunho Kim, Anton Koekemoer, Norbert Pirzkal, Mark Smith, Huan Yang, Andrea Cimatti, Ignacio Ferreras, Nimish Hathi, Pascale Hibon, Gerhardt Meurer, Goeran Oestlin, Anna Pasquali & 3 others Russell Ryan, Amber Straughn, Rogier Windhorst

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Abstract

We derive direct-measurement gas-phase metallicities of for 14 low-mass emission-line galaxies at 0.3 < z < 0.8 identified in the Faint Infrared Grism Survey. We use deep slitless G102 grism spectroscopy of the Hubble Ultra Deep Field, dispersing light from all objects in the field at wavelengths between 0.85 and 1.15 μm. We run an automatic search routine on these spectra to robustly identify 71 emission-line sources, using archival data from Very Large Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) to measure additional lines and confirm redshifts. We identify 14 objects with 0.3 < z < 0.8 with measurable [O iii]λ4363 emission lines in matching VLT/MUSE spectra. For these galaxies, we derive direct electron-temperature gas-phase metallicities with a range of . With matching stellar masses in the range of 10 7.9 M o < M < 10 10.4 M o , we construct a mass-metallicity (MZ) relation and find that the relation is offset to lower metallicities compared to metallicities derived from alternative methods (e.g., R 23 , O3N2, N2O2) and continuum selected samples. Using star formation rates derived from the Hα emission line, we calculate our galaxies' position on the Fundamental Metallicity Relation, where we also find an offset toward lower metallicities. This demonstrates that this emission-line-selected sample probes objects of low stellar masses but even lower metallicities than many comparable surveys. We detect a trend suggesting galaxies with higher Specific Star Formation (SSFR) are more likely to have lower metallicity. This could be due to cold accretion of metal-poor gas that drives star formation, or could be because outflows of metal-rich stellar winds and SNe ejecta are more common in galaxies with higher SSFR.

Original languageEnglish
Article number125
JournalAstrophysical Journal
Volume874
Issue number2
DOIs
Publication statusPublished - 1 Apr 2019

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metallicity
telescopes
galaxies
gas
star formation
metal
stellar mass
ejecta
outflow
vapor phases
spectroscopy
accretion
probe
wavelength
electron
dispersing
stellar winds
star formation rate
metals
electron energy

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Pharo, J., Malhotra, S., Rhoads, J., Christensen, L., Finkelstein, S. L., Grogin, N., ... Windhorst, R. (2019). Emission-line Metallicities from the Faint Infrared Grism Survey and VLT/MUSE. Astrophysical Journal, 874(2), [125]. https://doi.org/10.3847/1538-4357/ab08ec
Pharo, John ; Malhotra, Sangeeta ; Rhoads, James ; Christensen, Lise ; Finkelstein, Steven L. ; Grogin, Norman ; Harish, Santosh ; Jiang, Tianxing ; Kim, Keunho ; Koekemoer, Anton ; Pirzkal, Norbert ; Smith, Mark ; Yang, Huan ; Cimatti, Andrea ; Ferreras, Ignacio ; Hathi, Nimish ; Hibon, Pascale ; Meurer, Gerhardt ; Oestlin, Goeran ; Pasquali, Anna ; Ryan, Russell ; Straughn, Amber ; Windhorst, Rogier. / Emission-line Metallicities from the Faint Infrared Grism Survey and VLT/MUSE. In: Astrophysical Journal. 2019 ; Vol. 874, No. 2.
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abstract = "We derive direct-measurement gas-phase metallicities of for 14 low-mass emission-line galaxies at 0.3 < z < 0.8 identified in the Faint Infrared Grism Survey. We use deep slitless G102 grism spectroscopy of the Hubble Ultra Deep Field, dispersing light from all objects in the field at wavelengths between 0.85 and 1.15 μm. We run an automatic search routine on these spectra to robustly identify 71 emission-line sources, using archival data from Very Large Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) to measure additional lines and confirm redshifts. We identify 14 objects with 0.3 < z < 0.8 with measurable [O iii]λ4363 emission lines in matching VLT/MUSE spectra. For these galaxies, we derive direct electron-temperature gas-phase metallicities with a range of . With matching stellar masses in the range of 10 7.9 M o < M ∗ < 10 10.4 M o , we construct a mass-metallicity (MZ) relation and find that the relation is offset to lower metallicities compared to metallicities derived from alternative methods (e.g., R 23 , O3N2, N2O2) and continuum selected samples. Using star formation rates derived from the Hα emission line, we calculate our galaxies' position on the Fundamental Metallicity Relation, where we also find an offset toward lower metallicities. This demonstrates that this emission-line-selected sample probes objects of low stellar masses but even lower metallicities than many comparable surveys. We detect a trend suggesting galaxies with higher Specific Star Formation (SSFR) are more likely to have lower metallicity. This could be due to cold accretion of metal-poor gas that drives star formation, or could be because outflows of metal-rich stellar winds and SNe ejecta are more common in galaxies with higher SSFR.",
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Pharo, J, Malhotra, S, Rhoads, J, Christensen, L, Finkelstein, SL, Grogin, N, Harish, S, Jiang, T, Kim, K, Koekemoer, A, Pirzkal, N, Smith, M, Yang, H, Cimatti, A, Ferreras, I, Hathi, N, Hibon, P, Meurer, G, Oestlin, G, Pasquali, A, Ryan, R, Straughn, A & Windhorst, R 2019, 'Emission-line Metallicities from the Faint Infrared Grism Survey and VLT/MUSE' Astrophysical Journal, vol. 874, no. 2, 125. https://doi.org/10.3847/1538-4357/ab08ec

Emission-line Metallicities from the Faint Infrared Grism Survey and VLT/MUSE. / Pharo, John; Malhotra, Sangeeta; Rhoads, James; Christensen, Lise; Finkelstein, Steven L.; Grogin, Norman; Harish, Santosh; Jiang, Tianxing; Kim, Keunho; Koekemoer, Anton; Pirzkal, Norbert; Smith, Mark; Yang, Huan; Cimatti, Andrea; Ferreras, Ignacio; Hathi, Nimish; Hibon, Pascale; Meurer, Gerhardt; Oestlin, Goeran; Pasquali, Anna; Ryan, Russell; Straughn, Amber; Windhorst, Rogier.

In: Astrophysical Journal, Vol. 874, No. 2, 125, 01.04.2019.

Research output: Contribution to journalArticle

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AU - Pharo, John

AU - Malhotra, Sangeeta

AU - Rhoads, James

AU - Christensen, Lise

AU - Finkelstein, Steven L.

AU - Grogin, Norman

AU - Harish, Santosh

AU - Jiang, Tianxing

AU - Kim, Keunho

AU - Koekemoer, Anton

AU - Pirzkal, Norbert

AU - Smith, Mark

AU - Yang, Huan

AU - Cimatti, Andrea

AU - Ferreras, Ignacio

AU - Hathi, Nimish

AU - Hibon, Pascale

AU - Meurer, Gerhardt

AU - Oestlin, Goeran

AU - Pasquali, Anna

AU - Ryan, Russell

AU - Straughn, Amber

AU - Windhorst, Rogier

PY - 2019/4/1

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N2 - We derive direct-measurement gas-phase metallicities of for 14 low-mass emission-line galaxies at 0.3 < z < 0.8 identified in the Faint Infrared Grism Survey. We use deep slitless G102 grism spectroscopy of the Hubble Ultra Deep Field, dispersing light from all objects in the field at wavelengths between 0.85 and 1.15 μm. We run an automatic search routine on these spectra to robustly identify 71 emission-line sources, using archival data from Very Large Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) to measure additional lines and confirm redshifts. We identify 14 objects with 0.3 < z < 0.8 with measurable [O iii]λ4363 emission lines in matching VLT/MUSE spectra. For these galaxies, we derive direct electron-temperature gas-phase metallicities with a range of . With matching stellar masses in the range of 10 7.9 M o < M ∗ < 10 10.4 M o , we construct a mass-metallicity (MZ) relation and find that the relation is offset to lower metallicities compared to metallicities derived from alternative methods (e.g., R 23 , O3N2, N2O2) and continuum selected samples. Using star formation rates derived from the Hα emission line, we calculate our galaxies' position on the Fundamental Metallicity Relation, where we also find an offset toward lower metallicities. This demonstrates that this emission-line-selected sample probes objects of low stellar masses but even lower metallicities than many comparable surveys. We detect a trend suggesting galaxies with higher Specific Star Formation (SSFR) are more likely to have lower metallicity. This could be due to cold accretion of metal-poor gas that drives star formation, or could be because outflows of metal-rich stellar winds and SNe ejecta are more common in galaxies with higher SSFR.

AB - We derive direct-measurement gas-phase metallicities of for 14 low-mass emission-line galaxies at 0.3 < z < 0.8 identified in the Faint Infrared Grism Survey. We use deep slitless G102 grism spectroscopy of the Hubble Ultra Deep Field, dispersing light from all objects in the field at wavelengths between 0.85 and 1.15 μm. We run an automatic search routine on these spectra to robustly identify 71 emission-line sources, using archival data from Very Large Telescope (VLT)/Multi-Unit Spectroscopic Explorer (MUSE) to measure additional lines and confirm redshifts. We identify 14 objects with 0.3 < z < 0.8 with measurable [O iii]λ4363 emission lines in matching VLT/MUSE spectra. For these galaxies, we derive direct electron-temperature gas-phase metallicities with a range of . With matching stellar masses in the range of 10 7.9 M o < M ∗ < 10 10.4 M o , we construct a mass-metallicity (MZ) relation and find that the relation is offset to lower metallicities compared to metallicities derived from alternative methods (e.g., R 23 , O3N2, N2O2) and continuum selected samples. Using star formation rates derived from the Hα emission line, we calculate our galaxies' position on the Fundamental Metallicity Relation, where we also find an offset toward lower metallicities. This demonstrates that this emission-line-selected sample probes objects of low stellar masses but even lower metallicities than many comparable surveys. We detect a trend suggesting galaxies with higher Specific Star Formation (SSFR) are more likely to have lower metallicity. This could be due to cold accretion of metal-poor gas that drives star formation, or could be because outflows of metal-rich stellar winds and SNe ejecta are more common in galaxies with higher SSFR.

KW - galaxies: abundances

KW - galaxies: evolution

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Pharo J, Malhotra S, Rhoads J, Christensen L, Finkelstein SL, Grogin N et al. Emission-line Metallicities from the Faint Infrared Grism Survey and VLT/MUSE. Astrophysical Journal. 2019 Apr 1;874(2). 125. https://doi.org/10.3847/1538-4357/ab08ec