J/ApJS/269/33 JWST z=4-10 galaxies mass-metallicity relations (Nakajima+, 2023)
JWST census for the mass-metallicity star formation relations at z=4-10 with
self-consistent flux calibration and proper metallicity calibrators.
Nakajima K., Ouchi M., Isobe Y., Harikane Y., Zhang Y., Ono Y., Umeda H.,
Oguri M.
<Astrophys. J. Suppl. Ser., 269, 33 (2023)>
=2023ApJS..269...33N 2023ApJS..269...33N
ADC_Keywords: Galaxies, IR; Spectra, infrared; Redshifts; Abundances;
Stars, masses; Magnitudes, absolute; Ultraviolet
Keywords: Chemical abundances ; Galaxy chemical evolution ; Galaxy evolution ;
James Webb Space Telescope ; High-redshift galaxies
Abstract:
We present the evolution of the mass-metallicity (MZ) relation at
z=4-10 derived with 135 galaxies identified in JWST/NIRSpec data taken
from the three major public spectroscopy programs of ERO, GLASS, and
CEERS. Because there are many discrepancies between the flux
measurements reported by the early ERO studies, we first establish our
NIRSpec data reduction procedure for reliable emission-line flux
measurements and errors, successfully explaining Balmer decrements
with no statistical tensions thorough comparisons with the early ERO
studies. Applying the reduction procedure to the 135 galaxies, we
obtain emission-line fluxes for physical property measurements. We
confirm that 10 out of the 135 galaxies with [OIII]λ4363 lines
have electron temperatures of ~(1.1-2.3)x104K, similar to lower-z
star-forming galaxies, which can be explained by heating by young
massive stars. We derive the metallicities of the 10 galaxies by a
direct method and the rest of the galaxies with strong lines using the
metallicity calibrations of Nakajima et al. applicable for these
low-mass metal-poor galaxies, anchoring the metallicities with the
direct-method measurements. We thus obtain the MZ relation and star
formation rate (SFR)-MZ relation over z=4-10. We find that there is a
small evolution of the MZ relation from z∼2-3 to z=4-10, while
interestingly the SFR-MZ relation shows no evolution up to z∼8 but a
significant decrease at z>8 beyond the errors This SFR-MZ relation
decrease at z>8 may suggest a break of the metallicity equilibrium
state via star formation, inflow, and outflow, while further
statistical and local-baseline studies are needed for a conclusion.
Description:
The JWST/NIRSpec Early Release Observations (ERO) observations were
undertaken on UT 2022 June 30, targeting the SMACS 0723 lensing
cluster field (Proposal ID: 2736). Multislit spectroscopy was taken
using the microshutter assembly (MSA), with the medium-resolution
(R∼1000) gratings/filters of G235M/F170LP and G395M/F290LP sampling
the wavelength ranges of 1.7-3.1 and 2.9-5.1um, respectively. The
total integration time was 4.86hr in G235M and G395M each.
See Section 2.1.
The Early Release Science (ERS) GLASS NIRSpec MSA observations were
carried out on UT 2022 November 10-11 for objects behind the galaxy
cluster Abell 2744 (Proposal ID: 1324). They adopted the R∼2700
high-resolution gratings/filters of G140H/F100LP, G235H/F170LP, and
G395H/F290LP, sampling the wavelength ranges of 1.0-1.9, 1.7-3.2, and
2.8-5.3um, respectively. The total integration time was 4.9hr in each
of G140H, G235H, and G395H.
See Section 2.2.
The ERS CEERS NIRSpec MSA observations were carried out on UT
2022 December 20-22 and 24 in the blank field of EGS (Proposal ID:
1345). They used both prism (R∼100) and medium-resolution (R∼1000)
gratings to cover from 1.0 to 5um in six pointings (P4, P5, P7, P8,
P9, and P10) with some overlaps of objects. Additional observations
were performed on UT 2023 February 9-10 (P11 and P12).
See Section 2.3.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 143 10 Summary of JWST objects with direct Te method
tabled1.dat 174 182 Summary of the full JWST sample
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See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
VI/109 : Population Synthesis Models at very low metallicities (Schaerer, 2003)
J/A+A/448/955 : Abundances of emission galaxies in SDSS-DR3 (Izotov+, 2006)
J/A+A/459/85 : O/H and gas densities in star-forming galaxies (Nagao+, 2006)
J/ApJ/765/140 : Stacked spectra of SDSS star forming galaxies (Andrews+, 2013)
J/ApJ/795/165 : Line ratios in z∼2-3 gal. from KBSS-MOSFIRE (Steidel+, 2014)
J/ApJ/822/42 : z∼3.3 star-forming galaxies NIR spectra (Onodera+, 2016)
J/ApJS/229/32 : CANDELS: multiwavelength catalogs in the EGS (Stefanon+, 2017)
J/ApJ/855/4 : Lyman break galaxies at z∼6-9 from HFF (Kawamata+, 2018)
J/ApJ/869/123 : Keck Lyman continuum sp. survey (KLCS) (Steidel+, 2018)
J/ApJS/259/20 : GOLDRUSH. IV. z∼3-7 galaxies (Harikane+, 2022)
J/A+A/670/A60 : Abell 2744 members (Bergamini+, 2023)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- ID Identifier (G1)
14- 15 A2 --- Flag Source flag(s) (2)
17- 17 A1 --- l_OII3727 Limit flag on OII3727
18- 21 F4.1 --- OII3727 [5/100] Flux ratio,
[OII]3727Å to Hβ (3)
23- 26 F4.1 --- e_OII3727 [2/12]? Uncertainty in OII3727
28- 28 A1 --- l_NeIII3869 Limit flag on NeIII3869
30- 33 F4.1 --- NeIII3869 [24/64]? Flux ratio,
[NeIII]3869Å to Hβ (3)
35- 37 F3.1 --- e_NeIII3869 [2/9]? Uncertainty in NeIII3869
39- 39 A1 --- l_Hdelta Limit flag on Hdelta
41- 44 F4.1 --- Hdelta [7/29] Flux ratio, Hδ to Hβ (3)
46- 48 F3.1 --- e_Hdelta [1/5]? Uncertainty in Hdelta
50- 53 F4.1 --- Hgamma [38/64] Flux ratio, Hγ to Hβ (3)
55- 58 F4.1 --- e_Hgamma [1.5/10] Uncertainty in Hgamma
60- 63 F4.1 --- OIII4363 [8/31] Flux ratio,
[OIII]4363Å to Hβ (3)
65- 67 F3.1 --- e_OIII4363 [1.4/9] Uncertainty in OIII4363
69- 73 F5.1 --- Hbeta [100] Flux ratio, Hβ to Hβ (3)
75- 78 F4.1 --- e_Hbeta [1.6/11] Uncertainty in Hbeta
80- 84 F5.1 --- OIII4959 [110/297] Flux ratio,
[OIII]4959Å to Hβ (3)
86- 89 F4.1 --- e_OIII4959 [2/16] Uncertainty in OIII4959
91- 95 F5.1 --- OIII5007 [337/829] Flux ratio,
[OIII]5007Å to Hβ (3)
97-100 F4.1 --- e_OIII5007 [3/17] Uncertainty in OIII5007
102-106 F5.3 --- zspec [4/8.5] spectroscopic redshift
108-112 F5.1 0.1nm EWHb [67/228]? Equivalent width, Hβ, in Å
114-118 F5.1 0.1nm e_EWHb [4/151]? Uncertainty in EWHb
120-123 F4.2 10+4K OIIITe [1/2.3] Electron temperature from [OIII]
125-128 F4.2 10+4K e_OIIITe [0.07/0.5] Uncertainty in OIIITe
130-133 F4.2 --- logOH [7.2/8.4] Oxygen abundance, log(O/H)+12
135-138 F4.2 --- E_logOH [0.06/0.3] Upper uncertainty in logOH
140-143 F4.2 --- e_logOH [0.05/0.2] Lower uncertainty in logOH
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Note (2): Source flags as follows:
d = The presence of high ionization line of [NeIV] is seen,
Brinchmann 2023MNRAS.525.2087B 2023MNRAS.525.2087B
dd = The presence of broad Hα is indicated, Harikane+ 2023ApJ...959...39H 2023ApJ...959...39H
Note (3): Observed flux ratios relative to Hβ*100
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Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- ID Identifier (G1)
14- 24 F11.7 deg RAdeg Right Ascension (J2000)
26- 36 F11.7 deg DEdeg Declination (J2000)
38- 42 F5.3 --- zspec [3.7/9] Spectroscopic redshift
44- 44 A1 -- l_UVMag Limit flag on MUVmag
46- 51 F6.2 mag UVMag [-22.8/-15.8]? Absolute UV magnitude
derived from the HST/WFC3 photometry
(see Section 2.3)
53- 56 F4.2 mag E_UVMag [0/7]? Upper uncertainty on UVMag
58- 61 F4.2 mag e_UVMag [0/3]? Lower uncertainty on UVMag
63- 63 A1 --- l_logMs Limit flag on logMstar
64- 68 F5.2 [Msun] logMs [6/10.2]? log of stellar mass
70- 73 F4.2 [Msun] E_logMs [0.03/2]? Upper uncertainty on logMs
75- 78 F4.2 [Msun] e_logMs [0/2]? Lower uncertainty on logMs
80- 80 A1 --- l_logSFR Limit flag on logSFR
81- 85 F5.2 [Msun/yr] logSFR [-0.04/2.5]? log of star formation rate
87- 90 F4.2 [Msun/yr] E_logSFR [0.01/0.3]? Upper uncertainty on logSFR
92- 95 F4.2 [Msun/yr] e_logSFR [0.01/0.5]? Lower uncertainty on logSFR
97- 99 I3 0.1nm EWHb [8/578]? Equivalent width, Hβ, in Å
101-103 I3 0.1nm e_EWHb [3/225]? Uncertainty in EWHb
105-105 A1 --- l_R3 Limit flag on R3
106-109 F4.1 --- R3 [1.6/11.2]? Ratio,
[OIII]5007Å/Hβ (2)
111-113 F3.1 --- e_R3 [0.1/3.2]? Uncertainty in R3
115-115 A1 --- l_R23 Limit flag on R23
117-120 F4.1 --- R23 [3.4/18]? Ratio,
[OIII]5007,4959Å+[OII]3727)/Hβ (2)
122-124 F3.1 --- e_R23 [0.2/6]? Uncertainty in R23
126-126 A1 --- l_O32 Limit flag on O32
128-131 F4.1 --- O32 [0.8/22]? Ratio,
[OIII]5007Å/[OII]3727Å (2)
133-135 F3.1 --- e_O32 [0.1/6]? Uncertainty in O32
137-140 F4.2 --- logOH [7/9]? Oxygen abundance, log(O/H)+12
142-145 F4.2 --- E_logOH [0.06/0.5]? Upper uncertainty on
147-150 F4.2 --- e_logOH [0.05/0.5]? Lower uncertainty on
152-152 I1 --- PFl [0/1]? Photometry flag (3)
154-159 A6 --- MFl Metallicity flag (4)
161-174 A14 --- Note Note (5)
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Note (2): Lower-limit values at the 3σ level. The values are
not shown (and hence the metallicities are not estimated) for
those whose measured [OIII]5007Å/4959Å line ratio is not
consistent with the theoretical value of 2.98 at the 2.5σ
level. R23 and O32 are given if the dust-reddening is properly
evaluated.
Note (3): Objects with flag=1 have the NIRCam photometry, and thus
the stellar masses are reliably determined with the SED fit and
SFRs are derived with the slit-loss corrected Hβ
luminosities. For the objects with flag=0, their masses and SFRs
are estimated with the UV luminosities of HST.
Note (4): Metallicity flag, specifying which method is adopted; the
direct Te method or the empirical indicator of R23 or R3.
Note (5): For the gravitationally lensed objects, the magnification
factor µ is noted. For the lensed objects, the values of UVMag,
mass and SFR are already corrected for the magnification. For the
CEERS objects that are multiply observed in several
pointings/gratings, the number of pointings/gratings is noted, and
their averaged values of EW(Hβ), line ratios, and metallicity are
given. The objects with spectroscopic signatures of AGNs as indicated
by (Harikane+ 2023ApJ...959...39H 2023ApJ...959...39H) are marked with Broad. These Broad
objects are not used for deriving the MZ and SFR-MZ relations due to
the unknown contribution of AGNs to the continuum level (i.e.,
uncertainty in the stellar mass estimation based on the SED fitting).
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Global notes:
Note (G1): The identifiers used in this table correspond to the spectroscopic
program the object is taken from: Early Release Observations (ERO;
see Carnall+ 2023MNRAS.518L..45C 2023MNRAS.518L..45C), GLASS (see Mascia+ 2023A&A...672A.155M 2023A&A...672A.155M),
or CEERS (see Arrabal+ 2023ApJ...951L..22A 2023ApJ...951L..22A), followed by the the
source ID in the NIRSpec microshutter assembly (MSA) configurations of
the corresponding program.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 02-Feb-2024