J/ApJ/923/203 CLEAR: HST G102 & G141 grism obs. of CANDELS gal. (Simons+, 2021)
CLEAR: the gas-phase metallicity gradients of star-forming galaxies at
0.6<z<2.6.
Simons R.C., Papovich C., Momcheva I., Trump J.R., Brammer G.,
Estrada-Carpenter V., Backhaus B.E., Cleri N.J., Finkelstein S.L.,
Giavalisco M., Ji Z., Jung I., Matharu J., Weiner B.
<Astrophys. J., 923, 203 (2021)>
=2021ApJ...923..203S 2021ApJ...923..203S
ADC_Keywords: Galaxies, optical; Spectra, infrared; Redshifts; Abundances
Keywords: Galactic and extragalactic astronomy ; Metallicity ;
Chemical abundances ; Galaxy evolution ; Galaxy chemical evolution
Abstract:
We report on the gas-phase metallicity gradients of a sample of
238 star-forming galaxies at 0.6<z<2.6, measured through deep
near-infrared Hubble Space Telescope slitless spectroscopy. The
observations include 12 orbit depth Hubble/WFC3 G102 grism spectra
taken as a part of the CANDELS Lyα Emission at Reionization
(CLEAR) survey, and archival WFC3 G102+G141 grism spectra overlapping
the CLEAR footprint. The majority of galaxies in this sample are
consistent with having a zero or slightly positive metallicity
gradient (dZ/dR≥0, i.e., increasing with radius) across the full mass
range probed (8.5<logM*/M☉<10.5). We measure the intrinsic
population scatter of the metallicity gradients, and show that it
increases with decreasing stellar mass-consistent with previous
reports in the literature, but confirmed here with a much larger
sample. To understand the physical mechanisms governing this scatter,
we search for correlations between the observed gradient and various
stellar population properties at fixed mass. However, we find no
evidence for a correlation with the galaxy properties we
consider-including star formation rates, sizes, star formation rate
surface densities, and star formation rates per gravitational
potential energy. We use the observed weakness of these correlations
to provide material constraints for predicted intrinsic correlations
from theoretical models.
Description:
The Hubble Wide Field Camera 3 (HST/WFC3) slitless spectra used in
this paper are taken from a collection of programs. The root program
is the Cycle 23 CANDELS Lyα Emission at Reionization survey
(CLEAR; GO-14227, PI Papovich). The CLEAR footprint covers
12 pointings in the GOODS-S deep and GOODS-N deep CANDELS fields.
Each pointing includes 10-12 orbit depth (10 for GOODS-N and 12 for
GOODS-S) HST/WFC3 G102 (0.80-1.15um, R∼210) grism spectroscopy and
companion HST/WFC3 F105W direct imaging.
Given their location in the well-studied GOODS-S and GOODS-N fields,
the CLEAR observations are supported with extensive ancillary
photometry spanning the ultraviolet to the near-infrared. We use an
augmented version of the v4.1 3D-HST GOODS-S and GOODS-N photometric
catalogs (Skelton+ 2014, J/ApJS/214/24) --adding Y-band photometry
measured from the CLEAR F105W imaging and archival HST/WFC3 F098M
and/or F105W imaging.
To extend the spectral coverage and maximize the depth of our grism
observations, we query the Mikulski Archive for Space Telescopes
(MAST) for all publicly available HST/WFC3 G102 and G141 (1.08-1.70um,
R∼130) grism observations (and their associated direct imaging) that
overlap with the root CLEAR footprint. Of note, we retrieve an
ultra-deep 40hr G102 pointing in the GOODS-S/UDF from the Faint
Infrared Grism Survey (FIGS; Pirzkal+ 2017ApJ...846...84P 2017ApJ...846...84P).
The archival G141 observations were acquired by the following
programs: GO-11600 ("AGHAST"; PI Weiner), GO-12461 ("SN COLFAX",
PI Reiss), GO-13871 (PI Oesch), GO/DD-11359 ("ERS", PI: O'Connell),
GO-12099 ("GEORGE, PRIMO", PI Reiss), and GO-12177 ("3D-HST",
PI van Dokkum). The archival G102 observations are from: GO-13420
(PI Barro), GO/DD-11359 ("ERS", PI O'Connell), and GO-13779 ("FIGS",
PI Malhotra).
The full collection of G102+G141 observations used in this paper is
packaged in http://doi.org/10.17909/t9-ctff-wx60
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 73 238 Metallicity gradients of the CLEAR+ sample (0.6<z<2.6)
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See also:
J/AJ/116/2805 : H II regions in spiral galaxies (Van Zee+, 1998)
J/ApJ/758/135 : DEEP2 galaxies with UV spectra in the EGS (Kornei+, 2012)
J/ApJS/203/24 : Structural param. of gal. in CANDELS (van der Wel+, 2012)
J/ApJS/208/10 : κ-distribution in HII regions (Dopita+, 2013)
J/ApJ/768/74 : PHIBSS: CO obs. of star-forming galaxies (Tacconi+, 2013)
J/ApJS/214/24 : 3D-HST+CANDELS catalog (Skelton+, 2014)
J/ApJS/225/27 : 3D-HST Survey: grism spectra master cat. (Momcheva+, 2016)
J/ApJ/830/14 : SIGMA: Keck sp. of z∼2 gal. in CANDELS (Simons+, 2016)
J/ApJ/827/74 : [NII]/Hα ratio in gal. with KMOS3D (Wuyts+, 2016)
J/ApJS/224/15 : Improved 2Ms and 250ks Chandra catalogs (Xue+, 2016)
J/ApJS/228/2 : Chandra Deep Field-South survey: 7Ms sources (Luo+, 2017)
J/MNRAS/478/4293 : 0.1<z<0.8 gal. gas-phase metallicity grad. (Carton+, 2018)
J/MNRAS/474/5076 : KMOS Redshift One Spectroscopic Survey (Johnson+, 2018)
J/MNRAS/486/175 : HiZELS star-forming galaxies at z=0.8-3.3 (Gillman+, 2019)
J/ApJ/886/124 : Completed KMOS3D survey NIR obs. (Wisnioski+, 2019)
J/MNRAS/492/821 : KLEVER Survey: metallicity maps and gradients (Curti+, 2020)
J/ApJ/898/171 : CLEAR. II. SFRs of quiescent gal. (Estrada-Carpenter+, 2020)
J/ApJ/900/183 : HST NIR sp. of strong-lensing galaxy clusters (Wang+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Field Field ("GOODS-N" or "GOODS-S")
9- 13 I5 --- [SWM2014] [10964/49330] Galaxy ID (1)
15- 25 F11.7 deg RAdeg [53/189.4] Right Ascension (J2000)
27- 37 F11.7 deg DEdeg [-28/62.4] Declination (J2000)
39- 42 F4.2 --- z [0.74/2.44] Redshift
44- 48 F5.2 [Msun] logMs [8.34/10.83] Log of stellar mass
50- 55 F6.3 [kpc-1] m [-0.12/0.22] Log of metallicity gradient
slope; dex/kpc (2)
57- 61 F5.3 [kpc-1] e_m [0.006/0.08] uncertainty in m
63- 67 F5.3 [-] b [8.3/9.3] Log of metallicity gradient
intercept, dex (2)
69- 73 F5.3 [-] e_b [0.04/0.6] uncertainty in b
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Note (1): IDs are matched to the 3D-HST photometric catalog
(Skelton+ 2014, J/ApJS/214/24 ; <[SWM2014] @{Field} NNNNN> in Simbad).
Note (2): Linear fits to the radial profiles of the gas-phase metallicity,
taking the form log(O/H)(R)=m*R+b, where R is the projected radial
distance from the galaxy center.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 26-May-2023