J/PASJ/76/219 z=4-10 galaxies UV and Opt magnitudes (Ono+, 2024)
Census for the rest-frame optical and UV morphologies of galaxies at z = 4-10.
First phase of inside-out galaxy formation.
Ono Y., Harikane Y., Ouchi M., Nakajima K., Isobe Y., Shibuya T., Nakane M.,
Umeda H., Xu Y., Zhang Y.
<Publ. Astron. Soc. Jap.,, 76, 219-250>
=2024PASJ...76..219O 2024PASJ...76..219O (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Photometry, ultraviolet ; Optical ;
Redshifts
Keywords: galaxies: evolution - galaxies: formation - galaxies: high-redshift -
galaxies: structure
Abstract:
We present the rest-frame optical and UV surface brightness (SB)
profiles for 149 galaxies with Mopt←19.4mag at z=4-10 (29 of which
are spectroscopically confirmed with JWST NIRSpec), securing high
signal-to-noise ratios of 10-135 with deep JWST NIRCam 1-5um images
obtained by the CEERS survey. We derive morphologies of our high-z
galaxies, carefully evaluating the systematics of SB profile
measurements with Monte Carlo simulations as well as the impacts of a)
AGNs, b) multiple clumps including galaxy mergers, c) spatial
resolution differences with previous HST studies, and d) strong
emission lines, e.g., Hα and [OIII], on optical morphologies
with medium-band F410M images. Conducting Sersic profile fitting for
our high-z galaxy SBs with GALFIT, we obtain effective radius ranges
for optical re,opt and UV re,UV wavelengths of re,opt=0.05-1.6kpc
and re,UV=0.03-1.7kpc that are consistent with previous results
within large scatters in the size-luminosity relations. However, we
find that the effective radius ratio, re,opt/re,UV, is almost
unity, 1.01+0.35-0.22, over z=4-10 with no signatures of past
inside- out star formation such as found at z∼0-2. There are no
spatial offsets exceeding 3σ between the optical and UV
morphology centers in cases of no mergers, indicative of major
star-forming activity only being found near mass centers of galaxies
at z≳4 probably experiencing the first phase of inside-out galaxy
formation.
Description:
In this study, we have performed SB profile fittings for the 149
galaxies at z∼4-10 with SN values exceeding 10, 29 of which have been
spectroscopically confirmed, using the deep JWST NIRCam images
obtained by the CEERS survey. The F150W and F444W images allow for
probing their rest-frame UV and optical continuum emission.
The best-fitting parameters obtained from the SB profile fittings for
the individual sources are summarized in table 6.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 86 177 z∼4-10 galaxies in the CEERS fields reported
in the literature
table6.dat 182 149 GALFIT results
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- ID Identifier (CNN_NN)
8- 16 F9.5 deg RAdeg Right ascension (J2000)
18- 25 F8.5 deg DEdeg Declination (J2000)
27- 36 A10 --- IDN Nakajima et al. (2023ApJS..269...33N 2023ApJS..269...33N) ID
38- 41 F4.2 --- zspN ?=- Nakajima et al. (2023ApJS..269...33N 2023ApJS..269...33N)
spectroscopic redshift
43- 46 I4 --- IDF ?=- Finkelstein et al. (2023ApJ...946L..13F 2023ApJ...946L..13F)
ID, [FBF2023] CEERS1 NNNN in Simbad
48- 51 F4.2 --- zphF ?=- Finkelstein et al. (2023ApJ...946L..13F 2023ApJ...946L..13F)
photometric redshift
53- 67 A15 --- IDB Bouwens et al. (2015ApJ...803...34B 2015ApJ...803...34B) ID,
[BIO2015] EGSY-NNNNNNNNNN in Simbad
69- 72 F4.2 --- zphB ?=- Bouwens et al. (2015ApJ...803...34B 2015ApJ...803...34B)
photometric redshift
74- 78 I5 --- IDS ?=- Shibuya, Ouchi & Harikane
(2015ApJS..219...15S 2015ApJS..219...15S) ID
80 I1 --- zphS ?=- Shibuya, Ouchi & Harikane
(2015ApJS..219...15S 2015ApJS..219...15S) photometric redshift
82- 86 A5 --- Refs Other references (1)
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Note (1): Other references as follows:
1 = Donnan et al. (2023MNRAS.518.6011D 2023MNRAS.518.6011D)
2 = Fujimoto et al. (2023ApJ...949L..25F 2023ApJ...949L..25F)
3 = Bouwens et al. (2023MNRAS.523.1009B 2023MNRAS.523.1009B)
4 = Tang et al. (2023MNRAS.526.1657T 2023MNRAS.526.1657T)
5 = Harikane et al. (2024ApJ...960...56H 2024ApJ...960...56H)
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- ID Identifier (CNN_NN)
8- 12 F5.2 mag mUVF150W Total apparent UV magnitude in F150W
13 A1 --- --- [+]
14- 17 F4.2 mag E_mUVF150W Total apparent UV magnitude in F150W
upper error
18 A1 --- --- [-]
19- 22 F4.2 mag e_mUVF150W Total apparent UV magnitude in F150W
lower error
24- 29 F6.2 mag MUVF150W Total absolute UV magnitude in F150W
30 A1 --- --- [+]
31- 34 F4.2 mag E_MUVF150W Total absolute UV magnitude in F150W
upper error
35 A1 --- --- [-]
36- 39 F4.2 mag e_MUVF150W Total absolute UV magnitude in F150W
lower error
41- 44 F4.2 kpc reF150W UV size measured in F150W
45 A1 --- --- [+]
46- 49 F4.2 kpc E_reF150W UV size measured in F150W upper error
50 A1 --- --- [-]
51- 54 F4.2 kpc e_reF150W UV size measured in F150W lower error
56- 60 F5.2 mag mUVF150WP ?=- Total apparent UV magnitude measured in
the smoothed F150W images
61 A1 --- --- [+]
62- 65 F4.2 mag E_mUVF150WP ?=- Total apparent UV magnitude measured in
the smoothed F150W images upper error
66 A1 --- --- [-]
67- 70 F4.2 mag e_mUVF150WP ?=- Total apparent UV magnitude measured in
the smoothed F150W images lower error
72- 77 F6.2 mag MUVF150WP ?=- Total absolute UV magnitude measured in
the smoothed F150W images
78 A1 --- --- [+]
79- 82 F4.2 mag E_MUVF150WP ?=- Total absolute UV magnitude measured in
the smoothed F150W images upper error
83 A1 --- --- [-]
84- 87 F4.2 mag e_MUVF150WP ?=- Total absolute UV magnitude measured in
the smoothed F150W images lower error
89- 92 F4.2 kpc reF150WP ?=- UV size measured in the smoothed F150W
images
93 A1 --- --- [+]
94- 97 F4.2 kpc E_reF150WP ?=- UV size measured in the smoothed F150W
images upper error
98 A1 --- --- [-]
99-102 F4.2 kpc e_reF150WP ?=- UV size measured in the smoothed F150W
images lower error
104-108 F5.2 mag mUVF144W ?=- Total apparent optical magnitude
in F444W
109 A1 --- --- [+]
110-113 F4.2 mag E_mUVF144W ?=- Total apparent optical magnitude
in F444W upper error
114 A1 --- --- [-]
115-118 F4.2 mag e_mUVF144W ?=- Total apparent optical magnitude
in F444W lower error
120-125 F6.2 mag MUVF144W ?=- Total absolute optical magnitude
in F444W
126 A1 --- --- [+]
127-130 F4.2 mag E_MUVF144W ?=- Total absolute optical magnitude
in F444W upper error
131 A1 --- --- [-]
132-135 F4.2 mag e_MUVF144W ?=- Total absolute optical magnitude
in F444W lower error
137-140 F4.2 kpc reF144W ?=- Optical size measured in F444W
141 A1 --- --- [+]
142-145 F4.2 kpc E_reF144W ?=- Optical size measured in F444W
upper error
146 A1 --- --- [-]
147-150 F4.2 kpc e_reF144W ?=- Optical size measured in F444W
lower error
152-155 F4.2 --- reopt/UV ?=- The component fitted in the smoothed
F150W image and/or the F444W image is a
single component in the original
F150W image
156 A1 --- --- [+]
157-160 F4.2 --- E_reopt/UV ?=- The component fitted in the smoothed
F150W image and/or the F444W image is a
single component in the original F150W
image upper error
161 A1 --- --- [-]
162-165 F4.2 --- e_reopt/UV ?=- The component fitted in the smoothed
F150W image and/or the F444W image is a
single component in the original F150W
image lower error
167-170 F4.2 --- taureopt/UV ?=- The component fitted in the smoothed
F150W image and/or the F444W image consists
of multiple components in the original
F150W image
171 A1 --- --- [+]
172-175 F4.2 --- E_taureopt/UV ?=- The component fitted in the smoothed
F150W image and/or the F444W image consists
of multiple components in the original
F150W image upper error
176 A1 --- --- [-]
177-180 F4.2 --- e_taureopt/UV ?=- The component fitted in the smoothed
F150W image and/or the F444W image consists
of multiple components in the original
F150W image lower error
182 A1 --- Flag [012] Flag about blendedness (1)
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Note (1): Flag as follows:
1 = The component fitted in the smoothed F150W image and/or the F444W image
is a single component in the original F150W image
2 = The component fitted in the smoothed F150W image and/or the F444W image
consists of multiple components in the original F150W image
0 = Too faint or the SB profile fitting encounters numerical convergence
issues
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 06-Aug-2024