J/A+A/691/A299 Massive star-forming galaxies from JWST and ALMA (Gillman+, 2024)
The structure of massive star-forming galaxies from JWST and ALMA:
Dusty, high redshift disk galaxies.
Gillman S., Smail I., Gullberg B., Swinbank A.M., Vijayan A.P. , Lee M.,
Brammer G., Dudzeviciute U., Greve T.R., Almaini O., Brinch M.,
Chapman S.C., Chen C.-C., Ikarashi S., Matsuda Y., Wang W.-H., Walter F.,
van der Werf P.P.
<Astron. Astrophys. 691, A299 (2024)>
=2024A&A...691A.299G 2024A&A...691A.299G (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Star Forming Region ; Redshifts ;
Millimetric/submm sources
Keywords: galaxies: evolution - galaxies: high-redshift - galaxies: structure -
submillimetre: galaxies
Abstract:
We present an analysis of the JWST NIRCam and MIRI morphological and
structural properties of 80 massive (log10(M*[M{sun)])=11.2±0.1)
dusty star-forming galaxies at z=2.7+1.2-0.7, identified as
sub-millimetre galaxies (SMGs) by ALMA, that have been observed as
part of the JWST PRIMER project. To compare the structure of these
massive, active galaxies to more typical less actively star-forming
galaxies, we define two comparison samples. The first of 850 field
galaxies matched in specific star-formation rate and redshift and the
second of 80 field galaxies matched in stellar mass. From visual
classification of the SMGs, we identify 20±5% as candidate
late-stage major mergers, a further 40±10% as potential minor
mergers and 40±10% which have comparatively undisturbed disk-like
morphologies, with no obvious massive neighbours on . 20-30kpc
(projected) scales. These rates are comparable to those for the field
samples and indicate that the majority of the sub-millimetre-detected
galaxies are not late-stage major mergers, but have interaction rates
similar to the general field population at z∼2-3. Through a
multi-wavelength morphological analysis, using parametric and
non-parametric techniques, we establish that SMGs have comparable
near-infrared, mass normalised, sizes to the less active population,
RF444W50=2.7±0.2kpc versus RF444W50=3.1±0.1kpc, but exhibit
lower Sersic indices, consistent with bulge-less disks:
nF444W=1.1±0.1, compared to nF444W=1.9±0.1 for the less active
field and nF444W=2.8±0.2 for the most massive field galaxies. The
SMGs exhibit greater single-Sersic fit residuals and their
morphologies are more structured at 2um relative to 4um when compared
to the field galaxies. This appears to be caused by significant
structured dust content in the SMGs and we find evidence for dust
reddening as the origin of the morphological differences by
identifying a strong correlation between the F200W-F444W pixel colour
and the 870um surface brightness using high-resolution ALMA
observations. We conclude that SMGs and both massive and less massive
star-forming galaxies at the same epochs share a common disk-like
structure, but the weaker bulge components (and potentially lower
black hole masses) of the SMGs result in their gas disks being less
stable. Consequently, the combination of high gas masses and
instabilities triggered either secularly or by minor external
perturbations results in higher levels of activity (and dust content)
in SMGs compared to typical star-forming galaxies.
Description:
We present a multi-wavelength morphological analysis of a complete
sample of ALMA-identified sub-millimetre-selected galaxies from the
AS2UDS and AS2COSMOS surveys (Stach et al., 2019MNRAS.487.4648S 2019MNRAS.487.4648S, cat.
J/MNRAS/487/4648; Simpson et al., 2020MNRAS.495.3409S 2020MNRAS.495.3409S, Cat.
J/MNRAS/495/3409) with >4.5σ ALMA 870um detections and positions.
Utilising public JWST/NIRCam and MIRI imaging from the PRIMER survey,
we have built a sample of 80 SMGs, determining their multi-wavelength
properties through an SED and morphological analysis.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea2.dat 265 80 AS2UDS and AS2COSMOS SMGs identified in the
PRIMER survey listed by source ID
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See also:
J/MNRAS/487/4648 : ALMA survey of the SCUBA-2 UKIDSS/UDS field (Stach+, 2019)
J/MNRAS/495/3409 : SCUBA-2-COSMOS field brightest sub-mm sources
(Simpson+, 2020)
Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- ALMA ALMA ID (AS2UDSNNNN.N)
14- 31 F18.14 deg RAdeg Right ascension (J2000)
33- 51 F19.16 deg DEdeg Declination (J2000)
53- 71 F19.16 mJy S870um Flux density at 870um
73- 91 F19.17 mJy e_S870um Flux density at 870um error
93- 98 F6.1 --- HSTcov HST coverage (see table A.1)
100-105 F6.1 --- JWSTcov JWST coverage (see table A.1)
107-111 F5.3 --- e_z 16th percentile of magphys redshift,
zero indicates spec-z
113-118 F6.4 --- z 50th percentile of magphys redshift
120-124 F5.3 --- E_z 84th percentile of magphys redshift,
zero indicates spec-z
126-130 F5.3 mag e_AV 16th percentile of V-band attenuation
132-136 F5.3 mag AV 50th percentile of V-band attenuation
138-142 F5.3 mag E_AV 84th percentile of V-band attenuation
144-162 F19.16 kpc R50F444W F444W half-light radius,
derived from CoG analysis
164-183 F20.18 kpc e_R50F444W Error on F444W half-light radius,
derived from CoG analysis
185-203 F19.16 --- RRFF444W Residual Flux Fraction RFF in F444W,
derived from GalfitM residuals
205-224 F20.18 --- r_RRFF444W Error on Residual Flux Fraction RFF in F444W
226-244 F19.16 Msun M20F444W F444W M20, derived from statmorph
246-265 F20.18 Msun e_M20F444W Error on F444W M20
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Acknowledgements:
Steven Gillman, srigi(at)space.dtu.dk
(End) Patricia Vannier [CDS] 20-Sep-2024