J/ApJ/919/143 HST-WFC3/IR grism sp. for CANDELS z∼1-2 galaxies (Henry+, 2021)
The mass-metallicity relation at z∼1-2 and its dependence on the star formation
rate.
Henry A., Rafelski M., Sunnquist B., Pirzkal N., Pacifici C., Atek H.,
Bagley M., Baronchelli I., Barro G., Bunker A.J., Colbert J., Dai Y.S.,
Elmegreen B.G., Elmegreen D.M., Finkelstein S., Kocevski D., Koekemoer A.,
Malkan M., Martin C.L., Mehta V., Pahl A., Papovich C., Rutkowski M.,
Sanchez Almeida J., Scarlata C., Snyder G., Teplitz H.
<Astrophys. J., 919, 143 (2021)>
=2021ApJ...919..143H 2021ApJ...919..143H
ADC_Keywords: Galaxies; Spectra, infrared; Photometry; Optical; Redshifts;
Abundances; Equivalent widths; Extinction
Keywords: Metallicity ; Galaxy chemical evolution
Abstract:
We present a new measurement of the gas-phase mass-metallicity
relation (MZR) and its dependence on star formation rates (SFRs) at
1.3<z<2.3. Our sample comprises 1056 galaxies with a mean redshift of
z=1.9, identified from the Hubble Space Telescope Wide Field Camera 3
(WFC3) grism spectroscopy in the Cosmic Assembly Near-infrared Deep
Extragalactic Survey and the WFC3 Infrared Spectroscopic Parallel
Survey. This sample is four times larger than previous metallicity
surveys at z∼2 and reaches an order of magnitude lower in stellar mass
(108M☉). Using stacked spectra, we find that the MZR evolves
by 0.3dex relative to z∼0.1. Additionally, we identify a subset of
49 galaxies with high signal-to-noise (S/N) spectra and redshifts
between 1.3<z<1.5, where Hα emission is observed along with
[OIII] and [OII]. With accurate measurements of SFR in these objects,
we confirm the existence of a mass-metallicity-SFR (M-Z-SFR) relation
at high redshifts. These galaxies show systematic differences from the
local M-Z-SFR relation, which vary depending on the adopted
measurement of the local relation. However, it remains difficult to
ascertain whether these differences could be due to redshift
evolution, as the local M-Z-SFR relation is poorly constrained at the
masses and SFRs of our sample. Lastly, we reproduced our sample
selection in the IllustrisTNG hydrodynamical simulation, demonstrating
that our line flux limit lowers the normalization of the simulated MZR
by 0.2dex. We show that the M-Z-SFR relation in IllustrisTNG has an
SFR dependence that is too steep by a factor of around 3.
Description:
We select galaxies from multiple WFC3 grism spectroscopic surveys that
also have multifilter HST imaging. We require spectroscopic coverage
from [OII]λλ3726,3729 to [OIII]λλ4959,5007
in order to measure metallicities. This requirement results in the
selection of galaxies at 1.3<z<2.3 for fields that have observations
in the G102 and G141 grisms, and 2.0<z<2.3 for fields with only G141
spectroscopy. In addition, we select spectroscopic surveys in the
CANDELS fields, all of which have significant photometric data
(e.g., Skelton+ 2014, J/ApJS/214/24), and fields in the WFC3 Infrared
Spectroscopic Parallel (WISP) survey that include sufficient imaging.
The CANDELS, 3D-HST, and the A Grism Hα SpecTroscopic (AGHAST)
Survey (PI Weiner, PID 11600; two-orbit depth) spectra are publicly
available from the 3D-HST collaboration on the Mikulski Archive for
Space Telescopes (MAST).
To these data, we add G102 observations in GOODS-N using the fully
reduced spectra presented in Barro+ (2019ApJS..243...22B 2019ApJS..243...22B).
Additionally, we include G102 observations data from the CANDELS
Lyα Emission at Reionization Survey (CLEAR;
Estrada-Carpenter+ 2019ApJ...870..133E 2019ApJ...870..133E and JR. Simons+ 2021, in prep).
See Section 2.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table3.dat 193 49 Measurements and derived quantities from individual
spectra with Hα SNR>10
--------------------------------------------------------------------------------
See also:
B/hst : HST Archived Exposures Catalog (STScI, 2007)
J/ApJ/617/240 : Oxygen abund. in the GOODS-North field (Kobulnicky+, 2004)
J/ApJ/723/737 : Variability selected AGNs in GOODS (Villforth+, 2010)
J/ApJS/192/6 : A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)
J/A+A/546/A122 : SDSS extremely metal-poor emission-line gal. (Izotov+, 2012)
J/ApJ/752/148 : κ-distributed electrons & OIII (Nicholls+, 2012)
J/MNRAS/424/2316 : Abundances in HII regions (Pilyugin+, 2012)
J/ApJ/765/140 : Stacked sp. of SDSS star forming galaxies (Andrews+, 2013)
J/ApJS/208/10 : κ-distribution in HII regions (Dopita+, 2013)
J/ApJS/206/10 : CANDELS multiwavelength catalog (Galametz+, 2013)
J/ApJS/207/24 : GOODS-S CANDELS multiwavelength catalog (Guo+, 2013)
J/ApJS/214/24 : 3D-HST+CANDELS catalog (Skelton+, 2014)
J/ApJ/795/165 : Line ratios in z∼2-3 gal. from KBSS-MOSFIRE (Steidel+, 2014)
J/AJ/150/31 : Phot. & redshifts of galaxies in the UDF (Rafelski+, 2015)
J/ApJ/817/10 : Star-forming galaxy metallicities (Grasshorn Gebhardt+, 2016)
J/ApJS/225/27 : 3D-HST Survey: grism spectra master catalog (Momcheva+, 2016)
J/ApJ/827/74 : [NII]/Hα ratio in galaxies with KMOS3D (Wuyts+, 2016)
J/ApJS/228/7 : Multi-wavelength data in CANDELS COSMOS field (Nayyeri+, 2017)
J/ApJS/229/32 : CANDELS: multiwavelength catalogs in the EGS (Stefanon+, 2017)
J/ApJS/236/48 : The Chandra UDS survey (X-UDS) (Kocevski+, 2018)
J/ApJ/900/183 : HST grism sp. of strong-lensing galaxy clusters (Wang+, 2020)
http://archive.stsci.edu/prepds/3d-hst/ : 3D-HST on MAST
http://archive.stsci.edu/hlsp/candels : CANDELS on MAST
http://archive.stsci.edu/prepds/wisp/ : WISP on MAST
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Field Field name
9- 13 I5 --- ID [16/48918] Object identifier
15- 26 F12.8 deg RAdeg Right Ascension (J2000)
28- 39 F12.8 deg DEdeg [-50.2/64.2] Declination (J2000)
41- 46 F6.4 --- z [1.2/1.55] Redshift from grism spectrum
48- 52 F5.2 [Msun] logM [8.17/10.4] Log stellar mass (1)
54- 57 F4.2 [Msun] e_logM [0.01/0.5] Lower 16% uncertainty in logM
59- 62 F4.2 [Msun] E_logM [0.01/0.5] Upper 84% uncertainty in logM
64- 68 F5.2 [Msun/yr] logSFR1 [-0.4/2.1] Log star formation rate (1)
70- 73 F4.2 [Msun/yr] e_logSFR1 [0.01/0.7] Lower 16% uncertainty in logSFR1
75- 78 F4.2 [Msun/yr] E_logSFR1 [0.01/0.4] Upper 84% uncertainty in logSFR1
80- 84 F5.2 10-20W/m2 FOII [0.01/48.4] The [OII] line flux (2)
86- 89 F4.2 10-20W/m2 e_FOII [0.3/4.8] Uncertainty in FOII
91- 95 F5.2 10-20W/m2 FHb [0.46/27.1] The Hβ line flux (2)
97-100 F4.2 10-20W/m2 e_FHb [0.27/6.2] Uncertainty in FHb
102-107 F6.2 10-20W/m2 FOIII [4.9/108] The [OIII] line flux (2)
109-112 F4.2 10-20W/m2 e_FOIII [0.36/5.24] Uncertainty in FOIII
114-119 F6.2 10-20W/m2 FHa+NII [3.5/157] The Hα+[NII] line flux (2)
121-124 F4.2 10-20W/m2 e_FHa+NII [0.28/3.4] Uncertainty in FHa+NII
126-130 F5.2 10-20W/m2 FSII [0/23.7]? The [SII] line flux (2)
132-135 F4.2 10-20W/m2 e_FSII [0.04/4.1]? Uncertainty in FSII
137-142 F6.1 0.1nm EWOIII [42.7/1739] Rest frame [OIII] equivalent
width (3)
144-148 F5.1 0.1nm EWHa [62/755] Rest frame Hα equivalent
width (3)
150-153 F4.2 mag E(B-V) [0/0.8] Nebular dust extinction (4)
155-158 F4.2 mag e_E(B-V) [0/0.4] Lower 16% uncertainty in E(B-V)
160-163 F4.2 mag E_E(B-V) [0.04/0.7] Upper 84% uncertainty in E(B-V)
165-168 F4.2 [Msun/yr] logSFR2 [0.2/2.7] Log star formation rate (5)
170-173 F4.2 [Msun/yr] e_logSFR2 [0.01/0.3] Lower 16% uncertainty in logSFR2
175-178 F4.2 [Msun/yr] E_logSFR2 [0.05/0.9] Upper 84% uncertainty in logSFR2
180-183 F4.2 [-] log(O/H) [7.5/8.6] Log O/H abundance ratio +12 (4)
185-188 F4.2 [-] e_log(O/H) [0/0.3] Lower 16% uncertainty in log(O/H)
190-193 F4.2 [-] E_log(O/H) [0.01/0.7] Upper 84% uncertainty in
log(O/H)
--------------------------------------------------------------------------------
Note (1): From SED fits, as described in Section 2.6.
Note (2): Both lines of the [OIII], [OII] and [NII] doublets are included.
No corrections for dust extinction or stellar absorption are applied.
Note (3): In units of Angstroms. Calculated as described in Appendix A. No
correction for stellar absorption is applied. Uncertainties on the
emission line equivalent widths of individual objects are around 40%.
Note (4): The extinction and metallicity, derived simultaneously, as described
in Appendix C. A measurement uncertainty of zero (in one direction)
indicates that the most likely solution was found at the edge of
the physically allowed parameter space.
Note (5): Derived from Hα, as described in Section 3.2.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 03-Feb-2023