J/ApJ/900/183 HST NIR grism sp. of strong-lensing galaxy clusters (Wang+, 2020)
A census of sub-kiloparsec resolution metallicity gradients in star-forming
galaxies at cosmic noon from HST slitless spectroscopy.
Wang X., Jones T.A., Treu T., Daddi E., Brammer G.B., Sharon K.,
Morishita T., Abramson L.E., Colbert J.W., Henry A.L., Hopkins P.F.,
Malkan M.A., Schmidt K.B., Teplitz H.I., Vulcani B.
<Astrophys. J., 900, 183 (2020)>
=2020ApJ...900..183W 2020ApJ...900..183W
ADC_Keywords: Clusters, galaxy; Gravitational lensing; Spectra, infrared;
Abundances; Redshifts; Extinction
Keywords: Galaxy evolution ; Galaxy abundances ; Galaxy formation ;
High-redshift galaxies ; Strong gravitational lensing ; Dwarf galaxies
Abstract:
We present the hitherto largest sample of gas-phase metallicity radial
gradients measured at sub-kpc resolution in star-forming galaxies in
the redshift range of 1.2<z≤2.3. These measurements are enabled by
the synergy of slitless spectroscopy from the Hubble Space Telescope
near-infrared channels and the lensing magnification from foreground
galaxy clusters. Our sample consists of 76 galaxies with stellar mass
ranging from 107 to 1010M_☉, an instantaneous star formation
rate in the range of [1,100]M☉/yr, and global metallicity
[1/12,2] of solar. At a 2σ confidence level, 15/76 galaxies in
our sample show negative radial gradients, whereas 7/76 show inverted
gradients. Combining ours and all other metallicity gradients obtained
at a similar resolution currently available in the literature, we
measure a negative mass dependence of
Δlog(O/H)/Δr[dex/kpc]=(-0.020±0.007)+(-0.016±0.008)
log(M*/109.4M☉), with the intrinsic scatter being
σ=0.060±0.006 over 4 orders of magnitude in stellar mass. Our
result is consistent with strong feedback, not secular processes,
being the primary governor of the chemostructural evolution of
star-forming galaxies during the disk mass assembly at cosmic noon. We
also find that the intrinsic scatter of metallicity gradients
increases with decreasing stellar mass and increasing specific star
formation rate. This increase in the intrinsic scatter is likely
caused by the combined effect of cold-mode gas accretion and
merger-induced starbursts, with the latter more predominant in the
dwarf mass regime of M*≲109M☉.
Description:
The spectroscopic data analyzed in this work are acquired by the Grism
Lens-Amplified Survey from Space (GLASS; Proposal ID 13459,
PI: Treu; Schmidt+ 2014ApJ...782L..36S 2014ApJ...782L..36S & Treu+ 2015, J/ApJ/812/114).
It is a cycle 21 HST large program allocated 140 orbits of Wide-Field
Camera 3 (WFC3) near-infrared slitless spectroscopy on the centers of
10 strong-lensing galaxy clusters. For each cluster center field, we
have 10 orbits of G102 (covering 0.8-1.15um) and four orbits of G141
(covering 1.1-1.7um) exposures, amounting to ∼22ks of G102 and ∼9ks of
G141 in total, together with ∼7ks of F105W+F140W direct imaging for
wavelength/flux calibration and astrometric alignment.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 84 10 Summary of the HST observations
tablea1.dat 269 76 Measured quantities of our sample galaxies
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See also:
J/ApJS/199/25 : CLASH sources for MACS1149.6+2223 (Postman+, 2012)
J/ApJ/762/L30 : CLASH MCS J0416.1-2403 strong lensing analysis (Zitrin+, 2013)
J/ApJ/801/44 : HST lensing analysis of the CLASH sample (Zitrin+, 2015)
J/ApJ/806/16 : CHemical Abundances of Spirals. I. NGC628 (Berg+, 2015)
J/ApJ/811/29 : GLASS. IV. Lensing cluster Abell 2744 (Wang+, 2015)
J/ApJ/812/114 : Grism Lens-Amplified Survey from Space. I. (Treu+, 2015)
J/A+A/587/A70 : CALIFA face-on spiral gal. oxygen (Sanchez-Menguiano+, 2016)
J/ApJ/819/114 : Strong lensing mass modeling of 4 HFF cl. (Kawamata+, 2016)
J/ApJ/827/74 : [NII]/Hα ratio in gal. with KMOS3D (Wuyts+, 2016)
J/ApJ/831/182 : GLASS. VI. MCS J0416.1-2403 HFF imaging & sp. (Hoag+, 2016)
J/ApJ/833/178 : GLASS. VII. Hα maps (Vulcani+, 2016)
J/ApJS/224/33 : CLASH-VLT: the FF cluster MCS J0416.1-2403 (Balestra+, 2016)
J/ApJ/835/254 : GLASS. IX. Param. from HFF & GLASS (Morishita+, 2017)
J/ApJ/854/73 : Full-data results of HFF: galaxies z∼6-9 (Ishigaki+, 2018)
J/MNRAS/478/4293 : 0.1<z<0.8 gal. gas-phase metallicity grad. (Carton+, 2018)
J/A+A/633/A139 : Abundances of RXC J2248.7-4431 galaxies (Ciocan+, 2020)
J/MNRAS/506/928 : Stellar mass-size relation for low M* gal. (Nedkova+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Cluster field name
18 A1 --- f_Name Flag on Name (1)
20- 26 A7 --- Cl Cluster alias (as in Table 3)
28- 32 F5.3 --- z [0.3/0.7] Cluster redshift
34- 35 I2 h RAh Hour of right ascension (J2000)
37- 38 I2 min RAm Minute of right ascension (J2000)
40- 43 F4.1 s RAs Second of right ascension (J2000)
45 A1 --- DE- Sign of declination (J2000)
46- 47 I2 deg DEd Degree of declination (J2000)
49- 50 I2 arcmin DEm Arcminute of declination (J2000)
52- 55 F4.1 arcsec DEs Arcsecond of declination (J2000)
57- 71 A15 deg GrismPA Grism position angle(s) (2)
73- 81 A9 --- Img HST imaging
83- 84 I2 --- Ngal [2/13] Number of galaxies in which we secure
sub-kpc resolution metallicity gradient
measurements from HST spectroscopy
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Note (1): Flag as follows:
c = The detailed analyses of gradient measurements have already been
presented in our earlier paper (Wang+ 2017ApJ...837...89W 2017ApJ...837...89W). Here we
update the SED fitting results associated with these galaxies.
Note (2): The PAs are represented by the "PA_V3" values reported in the
corresponding raw image headers. The PA of the actual dispersion axis
of slitless spectroscopy, in degrees east of north, is given by
PAdisp∼PA_V3-45.2. For each of the GLASS PAs (i.e., excluding
PAs 111 and 119 for MACS 1149), two orbits of G141 and five orbits of
G102 exposures have been taken, amounting to ∼4.5 and ∼11ks science
exposure times for G141 and G102, respectively.
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Cl Cluster
9- 13 I5 --- ID [94/3834] Identifier within Cluster
15- 24 F10.6 deg RAdeg Right Ascension, decimal degree (J2000)
26- 35 F10.6 deg DEdeg Declination, decimal degree (J2000)
37- 40 F4.2 --- zspec [1.23/2.31] Spectroscopic redshift
42- 47 F6.3 [-] dZ/dr [-0.26/0.21] Metallicity gradient,
Δlog(O/H)/Δr in dex/kpc
49- 53 F5.3 [-] e_dZ/dr [0.008/0.25] Uncertainty in dZ/dr
55- 59 F5.2 mag F140W [20.8/25] Observed HST J+H-band
AB magnitude (1)
61- 64 F4.2 --- rF140W [0.1/1] Reduction factor of J+H-band
flux (2)
66- 70 F5.2 10-17mW/m2 FOII [0.07/34] Emission line flux, [OII]
72- 75 F4.2 10-17mW/m2 e_FOII [0.3/6.32] Uncertainty in FOII
77- 81 F5.2 10-17mW/m2 FHg [0.01/16.6]? Emission line flux, Hγ
83- 86 F4.2 10-17mW/m2 e_FHg [0.22/8.7]? Uncertainty in fHg
88- 92 F5.2 10-17mW/m2 FHb [0.16/24.9] Emission line flux, HΒ
94- 97 F4.2 10-17mW/m2 e_FHb [0.19/3.1] Uncertainty in FHb
99-104 F6.2 10-17mW/m2 FOIII [1.27/118] Emission line flux, [OIII]
106-109 F4.2 10-17mW/m2 e_FOIII [0.22/3.1] Uncertainty in FOIII
111-115 F5.2 10-17mW/m2 FHa [3.8/48.5]? Emission line flux, Hα
117-120 F4.2 10-17mW/m2 e_FHa [0.29/1.6]? Uncertainty in FHa
122-126 F5.2 10-17mW/m2 FSII [0.25/18]? Emission line flux, [SII]
128-131 F4.2 10-17mW/m2 e_FSII [0.28/2.31]? Uncertainty in FSII
133-137 F5.2 --- mu [1.13/56.3] Lensing magnification (3)
139-142 F4.2 --- e_mu [0/7.6] Lower uncertainty on mu
144-148 F5.2 --- E_mu [0/11.7] Upper uncertainty on mu
150-154 F5.2 [Msun] logM* [6.2/10.03] log of stellar mass,
continuum SED fit (5)
156-159 F4.2 [Msun] e_logM* [0.01/0.54] Lower uncertainty on logM*
161-164 F4.2 [Msun] E_logM* [0.01/0.35] Upper uncertainty on logM*
166-171 F6.2 Msun/yr SFR [0.02/210.95] Star formation rate,
stellar continuum SED fit (5)
173-178 F6.2 Msun/yr e_SFR [0.0/149.96] Lower uncertainty on SFR
180-185 F6.2 Msun/yr E_SFR [0.01/263.5] Upper uncertainty on SFR
187-190 F4.2 mag Avmag [0.0/1.8] Visual extinction,
stellar continuum SED fit
192-195 F4.2 mag e_Avmag [0.0/1.0] Lower uncertainty on Avmag
197-200 F4.2 mag E_Avmag [0.0/1.0] Upper uncertainty on Avmag
202-205 F4.2 --- NII/Ha [0.04/0.22] [NII]/Hα flux ratio (4)
207-210 F4.2 --- e_NII/Ha [0.0/0.07] Lower uncertainty on
212-215 F4.2 --- E_NII/Ha [0.0/0.09] Upper uncertainty on
217-220 F4.2 --- Z [7.58/8.96] Metallicity 12+log(O/H),
nebular emission diagnostic
222-225 F4.2 --- e_Z [0.06/0.52] Lower uncertainty on
227-230 F4.2 --- E_Z [0.06/0.41] Upper uncertainty on
232-232 A1 --- l_AvN Limit flag on AvN
234-237 F4.2 mag AvN [0.02/2.94] Visual extinction,
nebular emission diagnostic
239-242 F4.2 mag e_AvN [0.14/1.79]? Lower uncertainty on AvN
244-247 F4.2 mag E_AvN [0.14/1.63]? Upper uncertainty on AvN
249-249 A1 --- l_SFRN Limit flag on SFRN
251-256 F6.2 Msun/yr SFRN [0.49/87.0] Star formation rate,
nebular emission diagnostic (5)
258-262 F5.2 Msun/yr e_SFRN [0.13/44.42]? Lower uncertainty on SFRN
264-269 F6.2 Msun/yr E_SFRN [0.15/242.09]? Upper uncertainty on SFRN
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Note (1): The observed JH140-band magnitude before accounting for lensing
magnification.
Note (2): The reduction factor of JH140-band flux after subtracting the
nebular emission that falls within the corresponding wavelength window.
Note (3): The lensing magnification estimated from various mass models of
galaxy clusters. For all HFF clusters, we use the Sharon & Johnson
version 4corr models (J14; Johnson+ 2014ApJ...797...48J 2014ApJ...797...48J). For all
CLASH-only clusters, except RX J1347, we use the Zitrin PIEMD+eNFW
version 2 models (Zitrin+ 2015, J/ApJ/801/44). For RX J1347, we use
our own model built closely following the approach in J14.
Note (4): The flux ratio of [NII] and Hα, estimated from the prescription
of Faisst+ (2018ApJ...855..132F 2018ApJ...855..132F). This value is used to correct for
the blended Hα-[NII] fluxes in grism spectra, if necessary.
Note (5): Values presented here are corrected for lensing magnification.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 03-Jan-2022