SPATIALLY RESOLVED<i>HST</i>GRISM SPECTROSCOPY OF A LENSED EMISSION LINE GALAXY AT<i>z</i>∼ 1

Frye, Brenda; Hurley, Mairéad; Bowen, David V.; Meurer, G. R.; Sharon, Keren; Straughn, Amber N.; Coe, Dan; Broadhurst, Tom; Guhathakurta, Puragra

doi:10.1088/0004-637x/754/1/17

Cited by 19 publications

(17 citation statements)

References 87 publications

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“…We show original published values for all comparison data with the caveat that they are derived using different strong-line calibrations; this has minimal effect on our conclusions since metallicity gradients are relatively insensitive to the choice of calibration (Jones et al 2013). The lensed z = 0.8 source described by Frye et al (2012) is also included with a previously unpublished gradient slope of 0.01 ± 0.03 dex kpc −1 (B. Frye, private communication). However none of the comparison data include scatter in metallicity in the formal uncertainty, hence the error bar on arc 4 is the most conservative of those shown in Figure 7.…”

Section: Metallicity Gradient Evolutionmentioning

confidence: 99%

THEGRISM LENS-AMPLIFIED SURVEY FROM SPACE(GLASS). II. GAS-PHASE METALLICITY AND RADIAL GRADIENTS IN AN INTERACTING SYSTEM ATZ≃ 2

Jones

Wang

Schmidt

et al. 2015

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We present spatially resolved gas-phase metallicity for a system of three galaxies at z = 1.85 detected in the Grism Lensed-Amplified Survey from Space (GLASS). The combination of HST's diffraction limit and strong gravitational lensing by the cluster MACS J0717+3745 results in a spatial resolution of 200 − 300 pc, enabling good spatial sampling despite the intrinsically small galaxy sizes. The galaxies in this system are separated by 50 − 200 kpc in projection and are likely in an early stage of interaction, evidenced by relatively high specific star formation rates. Their gas-phase metallicities are consistent with larger samples at similar redshift, star formation rate, and stellar mass. We obtain a precise measurement of the metallicity gradient for one galaxy and find a shallow slope compared to isolated galaxies at high redshift, consistent with a flattening of the gradient due to gravitational interaction. An alternative explanation for the shallow metallicity gradient and elevated star formation rate is rapid recycling of metal-enriched gas, but we find no evidence for enhanced gas-phase metallicities which should result from this effect. Notably, the measured stellar masses log M * /M = 7.2 − 9.1 probe to an order of magnitude below previous massmetallicity studies at this redshift. The lowest mass galaxy has properties similar to those expected for Fornax at this redshift, indicating that GLASS is able to directly study the progenitors of local group dwarf galaxies on spatially resolved scales. Larger samples from the full GLASS survey will be ideal for studying the effects of feedback, and the time evolution of metallicity gradients. These initial results demonstrate the utility of HST spectroscopy combined with gravitational lensing for characterizing resolved physical properties of galaxies at high redshift.

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Section: Metallicity Gradient Evolutionmentioning

confidence: 99%

THEGRISM LENS-AMPLIFIED SURVEY FROM SPACE(GLASS). II. GAS-PHASE METALLICITY AND RADIAL GRADIENTS IN AN INTERACTING SYSTEM ATZ≃ 2

Jones

Wang

Schmidt

et al. 2015

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“…A detailed analysis of the properties of this candidate and a discussion of its high-redshift solution are presented in Laporte et al (2014). Gravitational lensing also provides higher angular resolution allowing the study of spatially resolved star formation and the internal structure of distant galaxies (Frye et al 2012;Brammer et al 2012). The HFF observations will extend this study to the most magnified high-redshift galaxies.…”

Section: Candidate Selectionmentioning

confidence: 99%

PROBING THEz> 6 UNIVERSE WITH THE FIRST HUBBLE FRONTIER FIELDS CLUSTER A2744

Atek

Richard

Kneib

et al. 2014

ApJ

101

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“…Their Figure 3 2 ). See also Frye et al (2012) for other examples of extreme emission line galaxies with large single emission line fluxes of up to´-1.38 10 16 erg s −1 cm −2 .…”

Section: Introductionmentioning

confidence: 99%

NOT IN OUR BACKYARD: SPECTROSCOPIC SUPPORT FOR THE CLASHz= 11 CANDIDATE MACS 0647-JD

Pirzkal

Coe

Frye

et al. 2015

ApJ

Self Cite

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We report on our first set of spectroscopic Hubble Space Telescope observations of the » z 11 candidate galaxy, which is strongly lensed by the MACSJ 0647.7+7015 galaxy cluster. The three lensed images are faint and we show that these early slitless grism observations are of sufficient depth to investigate whether this high-redshift candidate, identified by its strong photometric break at » μ 1.5 m, could possibly be an emission line galaxy at a much lower redshift. While such an interloper would imply the existence of a rather peculiar object, we show here that such strong emission lines would clearly have been detected. Comparing realistic, two-dimensional simulations to these new observations, we would expect the necessary emission lines to be detected at s >5 , though we see no evidence for such lines in the dispersed data of any of the three lensed images. We therefore exclude that this object could be a low-redshift emission line interloper, which significantly increases the likelihood of this candidate being a bona fide » z 11 galaxy.

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SPATIALLY RESOLVEDHSTGRISM SPECTROSCOPY OF A LENSED EMISSION LINE GALAXY ATz∼ 1

Cited by 19 publications

References 87 publications

THEGRISM LENS-AMPLIFIED SURVEY FROM SPACE(GLASS). II. GAS-PHASE METALLICITY AND RADIAL GRADIENTS IN AN INTERACTING SYSTEM ATZ≃ 2

THEGRISM LENS-AMPLIFIED SURVEY FROM SPACE(GLASS). II. GAS-PHASE METALLICITY AND RADIAL GRADIENTS IN AN INTERACTING SYSTEM ATZ≃ 2

PROBING THEz> 6 UNIVERSE WITH THE FIRST HUBBLE FRONTIER FIELDS CLUSTER A2744

NOT IN OUR BACKYARD: SPECTROSCOPIC SUPPORT FOR THE CLASHz= 11 CANDIDATE MACS 0647-JD

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