STELLAR MASS-GAS-PHASE METALLICITY RELATION at 0.5 ≤ z ≤ 0.7

A POWER LAW with INCREASING SCATTER TOWARD the LOW-MASS REGIME

Yicheng Guo, David C. Koo, Yu Lu, John C. Forbes, Marc Rafelski, Jonathan R. Trump, Ricardo Amorín, Guillermo Barro, Romeel S Dave, S. M. Faber, Nimish P. Hathi, Hassen Yesuf, Michael C. Cooper, Avishai Dekel, Puragra Guhathakurta, Evan N. Kirby, Anton M. Koekemoer, Pablo G. Pérez-González, Lihwai Lin, Jeffery A. Newman & 4 others Joel R. Primack, David J. Rosario, Christopher N A Willmer, Renbin Yan

Research output: Contribution to journalArticle

14 Citations (Scopus)

Abstract

We present the stellar mass (M)gas-phase metallicity relation (MZR) and its scatter at intermediate redshifts (0.5 ≤ z ≤ 0.7) for 1381 field galaxies collected from deep spectroscopic surveys. The star formation rate (SFR) and color at a given M of this magnitude-limited (R ≳ 24 AB) sample are representative of normal starforming galaxies. For masses below 109 Mo, our sample of 237 galaxies is ∼10 times larger than those in previous studies beyond the local universe. This huge gain in sample size enables superior constraints on the MZR and its scatter in the low-mass regime. We find a power-law MZR at 108 Mo <M <1011 Mo: 12 + log (O/H) = (5.83 ± 0.19) +(0.30 ± 0.02) log (M/Mo). At 109 Mo <M <1010.5 Mo, our MZR shows agreement with others measured at similar redshifts in the literature. Our power-law slope is, however, shallower than the extrapolation of the MZRs of others to masses below 109 Mo. The SFR dependence of the MZR in our sample is weaker than that found for local galaxies (known as the fundamental metallicity relation). Compared to a variety of theoretical models, the slope of our MZR for low-mass galaxies agrees well with predictions incorporating supernova energy-driven winds. Being robust against currently uncertain metallicity calibrations, the scatter of the MZR serves as a powerful diagnostic of the stochastic history of gas accretion, gas recycling, and star formation of low-mass galaxies. Our major result is that the scatter of our MZR increases as Mo decreases. Our result implies that either the scatter of the baryonic accretion rate (δ? ) or the scatter of the M-Mhalo relation (δSHMR) increases as M decreases. Moreover, our measure of scatter at z = 0.7 appears consistent with that found for local galaxies. This lack of redshift evolution constrains models of galaxy evolution to have both δ and δSHMR remain unchanged from z = 0.7 to z = 0.

Original languageEnglish (US)
Article number103
JournalAstrophysical Journal
Volume822
Issue number2
DOIs
StatePublished - May 10 2016
Externally publishedYes

Fingerprint

stellar mass
metallicity
vapor phases
galaxies
gas
power law
star formation rate
accretion
slopes
recycling
gases
calibration
supernovae
star formation
extrapolation
universe
histories
history
prediction
color

Keywords

  • galaxies: abundances
  • galaxies: dwarf
  • galaxies: evolution
  • galaxies: formation
  • galaxies: fundamental parameters
  • galaxies: ISM

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

STELLAR MASS-GAS-PHASE METALLICITY RELATION at 0.5 ≤ z ≤ 0.7 : A POWER LAW with INCREASING SCATTER TOWARD the LOW-MASS REGIME. / Guo, Yicheng; Koo, David C.; Lu, Yu; Forbes, John C.; Rafelski, Marc; Trump, Jonathan R.; Amorín, Ricardo; Barro, Guillermo; Dave, Romeel S; Faber, S. M.; Hathi, Nimish P.; Yesuf, Hassen; Cooper, Michael C.; Dekel, Avishai; Guhathakurta, Puragra; Kirby, Evan N.; Koekemoer, Anton M.; Pérez-González, Pablo G.; Lin, Lihwai; Newman, Jeffery A.; Primack, Joel R.; Rosario, David J.; Willmer, Christopher N A; Yan, Renbin.

In: Astrophysical Journal, Vol. 822, No. 2, 103, 10.05.2016.

Research output: Contribution to journalArticle

Guo, Y, Koo, DC, Lu, Y, Forbes, JC, Rafelski, M, Trump, JR, Amorín, R, Barro, G, Dave, RS, Faber, SM, Hathi, NP, Yesuf, H, Cooper, MC, Dekel, A, Guhathakurta, P, Kirby, EN, Koekemoer, AM, Pérez-González, PG, Lin, L, Newman, JA, Primack, JR, Rosario, DJ, Willmer, CNA & Yan, R 2016, 'STELLAR MASS-GAS-PHASE METALLICITY RELATION at 0.5 ≤ z ≤ 0.7: A POWER LAW with INCREASING SCATTER TOWARD the LOW-MASS REGIME', Astrophysical Journal, vol. 822, no. 2, 103. https://doi.org/10.3847/0004-637X/822/2/103
Guo, Yicheng ; Koo, David C. ; Lu, Yu ; Forbes, John C. ; Rafelski, Marc ; Trump, Jonathan R. ; Amorín, Ricardo ; Barro, Guillermo ; Dave, Romeel S ; Faber, S. M. ; Hathi, Nimish P. ; Yesuf, Hassen ; Cooper, Michael C. ; Dekel, Avishai ; Guhathakurta, Puragra ; Kirby, Evan N. ; Koekemoer, Anton M. ; Pérez-González, Pablo G. ; Lin, Lihwai ; Newman, Jeffery A. ; Primack, Joel R. ; Rosario, David J. ; Willmer, Christopher N A ; Yan, Renbin. / STELLAR MASS-GAS-PHASE METALLICITY RELATION at 0.5 ≤ z ≤ 0.7 : A POWER LAW with INCREASING SCATTER TOWARD the LOW-MASS REGIME. In: Astrophysical Journal. 2016 ; Vol. 822, No. 2.
@article{e31c9bd4fb3c455983d30a8922d57514,
title = "STELLAR MASS-GAS-PHASE METALLICITY RELATION at 0.5 ≤ z ≤ 0.7: A POWER LAW with INCREASING SCATTER TOWARD the LOW-MASS REGIME",
abstract = "We present the stellar mass (M∗)gas-phase metallicity relation (MZR) and its scatter at intermediate redshifts (0.5 ≤ z ≤ 0.7) for 1381 field galaxies collected from deep spectroscopic surveys. The star formation rate (SFR) and color at a given M∗ of this magnitude-limited (R ≳ 24 AB) sample are representative of normal starforming galaxies. For masses below 109 Mo, our sample of 237 galaxies is ∼10 times larger than those in previous studies beyond the local universe. This huge gain in sample size enables superior constraints on the MZR and its scatter in the low-mass regime. We find a power-law MZR at 108 Mo <M∗ <1011 Mo: 12 + log (O/H) = (5.83 ± 0.19) +(0.30 ± 0.02) log (M∗/Mo). At 109 Mo <M∗ <1010.5 Mo, our MZR shows agreement with others measured at similar redshifts in the literature. Our power-law slope is, however, shallower than the extrapolation of the MZRs of others to masses below 109 Mo. The SFR dependence of the MZR in our sample is weaker than that found for local galaxies (known as the fundamental metallicity relation). Compared to a variety of theoretical models, the slope of our MZR for low-mass galaxies agrees well with predictions incorporating supernova energy-driven winds. Being robust against currently uncertain metallicity calibrations, the scatter of the MZR serves as a powerful diagnostic of the stochastic history of gas accretion, gas recycling, and star formation of low-mass galaxies. Our major result is that the scatter of our MZR increases as Mo decreases. Our result implies that either the scatter of the baryonic accretion rate (δṀ? ) or the scatter of the M∗-Mhalo relation (δSHMR) increases as M∗ decreases. Moreover, our measure of scatter at z = 0.7 appears consistent with that found for local galaxies. This lack of redshift evolution constrains models of galaxy evolution to have both δṀ and δSHMR remain unchanged from z = 0.7 to z = 0.",
keywords = "galaxies: abundances, galaxies: dwarf, galaxies: evolution, galaxies: formation, galaxies: fundamental parameters, galaxies: ISM",
author = "Yicheng Guo and Koo, {David C.} and Yu Lu and Forbes, {John C.} and Marc Rafelski and Trump, {Jonathan R.} and Ricardo Amor{\'i}n and Guillermo Barro and Dave, {Romeel S} and Faber, {S. M.} and Hathi, {Nimish P.} and Hassen Yesuf and Cooper, {Michael C.} and Avishai Dekel and Puragra Guhathakurta and Kirby, {Evan N.} and Koekemoer, {Anton M.} and P{\'e}rez-Gonz{\'a}lez, {Pablo G.} and Lihwai Lin and Newman, {Jeffery A.} and Primack, {Joel R.} and Rosario, {David J.} and Willmer, {Christopher N A} and Renbin Yan",
year = "2016",
month = "5",
day = "10",
doi = "10.3847/0004-637X/822/2/103",
language = "English (US)",
volume = "822",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

TY - JOUR

T1 - STELLAR MASS-GAS-PHASE METALLICITY RELATION at 0.5 ≤ z ≤ 0.7

T2 - A POWER LAW with INCREASING SCATTER TOWARD the LOW-MASS REGIME

AU - Guo, Yicheng

AU - Koo, David C.

AU - Lu, Yu

AU - Forbes, John C.

AU - Rafelski, Marc

AU - Trump, Jonathan R.

AU - Amorín, Ricardo

AU - Barro, Guillermo

AU - Dave, Romeel S

AU - Faber, S. M.

AU - Hathi, Nimish P.

AU - Yesuf, Hassen

AU - Cooper, Michael C.

AU - Dekel, Avishai

AU - Guhathakurta, Puragra

AU - Kirby, Evan N.

AU - Koekemoer, Anton M.

AU - Pérez-González, Pablo G.

AU - Lin, Lihwai

AU - Newman, Jeffery A.

AU - Primack, Joel R.

AU - Rosario, David J.

AU - Willmer, Christopher N A

AU - Yan, Renbin

PY - 2016/5/10

Y1 - 2016/5/10

N2 - We present the stellar mass (M∗)gas-phase metallicity relation (MZR) and its scatter at intermediate redshifts (0.5 ≤ z ≤ 0.7) for 1381 field galaxies collected from deep spectroscopic surveys. The star formation rate (SFR) and color at a given M∗ of this magnitude-limited (R ≳ 24 AB) sample are representative of normal starforming galaxies. For masses below 109 Mo, our sample of 237 galaxies is ∼10 times larger than those in previous studies beyond the local universe. This huge gain in sample size enables superior constraints on the MZR and its scatter in the low-mass regime. We find a power-law MZR at 108 Mo <M∗ <1011 Mo: 12 + log (O/H) = (5.83 ± 0.19) +(0.30 ± 0.02) log (M∗/Mo). At 109 Mo <M∗ <1010.5 Mo, our MZR shows agreement with others measured at similar redshifts in the literature. Our power-law slope is, however, shallower than the extrapolation of the MZRs of others to masses below 109 Mo. The SFR dependence of the MZR in our sample is weaker than that found for local galaxies (known as the fundamental metallicity relation). Compared to a variety of theoretical models, the slope of our MZR for low-mass galaxies agrees well with predictions incorporating supernova energy-driven winds. Being robust against currently uncertain metallicity calibrations, the scatter of the MZR serves as a powerful diagnostic of the stochastic history of gas accretion, gas recycling, and star formation of low-mass galaxies. Our major result is that the scatter of our MZR increases as Mo decreases. Our result implies that either the scatter of the baryonic accretion rate (δṀ? ) or the scatter of the M∗-Mhalo relation (δSHMR) increases as M∗ decreases. Moreover, our measure of scatter at z = 0.7 appears consistent with that found for local galaxies. This lack of redshift evolution constrains models of galaxy evolution to have both δṀ and δSHMR remain unchanged from z = 0.7 to z = 0.

AB - We present the stellar mass (M∗)gas-phase metallicity relation (MZR) and its scatter at intermediate redshifts (0.5 ≤ z ≤ 0.7) for 1381 field galaxies collected from deep spectroscopic surveys. The star formation rate (SFR) and color at a given M∗ of this magnitude-limited (R ≳ 24 AB) sample are representative of normal starforming galaxies. For masses below 109 Mo, our sample of 237 galaxies is ∼10 times larger than those in previous studies beyond the local universe. This huge gain in sample size enables superior constraints on the MZR and its scatter in the low-mass regime. We find a power-law MZR at 108 Mo <M∗ <1011 Mo: 12 + log (O/H) = (5.83 ± 0.19) +(0.30 ± 0.02) log (M∗/Mo). At 109 Mo <M∗ <1010.5 Mo, our MZR shows agreement with others measured at similar redshifts in the literature. Our power-law slope is, however, shallower than the extrapolation of the MZRs of others to masses below 109 Mo. The SFR dependence of the MZR in our sample is weaker than that found for local galaxies (known as the fundamental metallicity relation). Compared to a variety of theoretical models, the slope of our MZR for low-mass galaxies agrees well with predictions incorporating supernova energy-driven winds. Being robust against currently uncertain metallicity calibrations, the scatter of the MZR serves as a powerful diagnostic of the stochastic history of gas accretion, gas recycling, and star formation of low-mass galaxies. Our major result is that the scatter of our MZR increases as Mo decreases. Our result implies that either the scatter of the baryonic accretion rate (δṀ? ) or the scatter of the M∗-Mhalo relation (δSHMR) increases as M∗ decreases. Moreover, our measure of scatter at z = 0.7 appears consistent with that found for local galaxies. This lack of redshift evolution constrains models of galaxy evolution to have both δṀ and δSHMR remain unchanged from z = 0.7 to z = 0.

KW - galaxies: abundances

KW - galaxies: dwarf

KW - galaxies: evolution

KW - galaxies: formation

KW - galaxies: fundamental parameters

KW - galaxies: ISM

UR - http://www.scopus.com/inward/record.url?scp=84969504526&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84969504526&partnerID=8YFLogxK

U2 - 10.3847/0004-637X/822/2/103

DO - 10.3847/0004-637X/822/2/103

M3 - Article

VL - 822

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 103

ER -