J/A+A/671/A105 SPT0311-58 JWST, ALMA, and HST images (Alvarez-Marquez+, 2023)
MIRI/JWST observations reveal an extremely obscured starburst in the z=6.9
system SPT0311-58.
Alvarez-Marquez J., Crespo Gomez A., Colina L., Neeleman M., Walter F.,
Labiano A., Perez-Gonzalez P., Bik A., Noorgaard-Nielsen H.U., Ostlin G.,
Wright G., Alonso-Herrero A., Azollini R., Caputi K.I., Eckart A.,
Le Fevre O., Garcia-Marin M., Greve T.R., Hjorth J., Ilbert O., Kendrew S.,
Pye J.P., Tikkanen T., Topinka M., van der Werf P., Ward M.,
van Dishoeck F., Guedel M., Henning T., Lagage P.O., Ray T., Waelkens C.
<Astron. Astrophys. 671, A105 (2023)>
=2023A&A...671A.105A 2023A&A...671A.105A (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Optical ; Infrared
Keywords: galaxies: high-redshift - galaxies: starburst - galaxies: ISM -
galaxies: individual: SPT0311-58
Abstract:
Luminous infrared starbursts in the early universe are thought to be
the progenitors of massive quiescent galaxies identified at redshifts
2 to 4. Using MIRI on-board JWST we present mid-infrared sub-arcsec
imaging (MIRIM) and spectroscopy (MRS) of such a starburst: the
slightly lensed hyperluminous infrared system SPT0311-58 at z=6.9. Our
observations target the stellar (rest-frame 1.26um emission) structure
and ionised (Paα and Hα) medium on kpc scales in the
system. MIRI observations are compared with existing ALMA far-infrared
continuum and [CII]158um imaging at similar angular resolution. Even
though the ALMA observations imply very high star formation rates in
the eastern (E) and western (W) galaxies of the system, the Hα
line is, strikingly, not detected in our MRS observations. This,
together with the detection of the ionised gas phase in Paα,
implies very high internal nebular extinction with lower limits (AV)
of 4.2 (E) and 3.9 mag (W), and even larger (5.6 (E) and 10.0 (W)) for
SED derived values. The extinction-corrected Paα lower limits to
the star formation rates are 383 and 230M☉/yr for the E and W
galaxies, respectively. This represents 50 of the SFRs derived from
the [CII]158um line and infrared light for the E galaxy and as low as
6% for the W galaxy. The specific star formation (sSFR) in the stellar
clumps ranges from 25 to 59Gyr-1 assuming a star formation with a
50-100Myr constant rate. This sSFR is 3 to 10 times larger than the
values measured in galaxies of similar mass at redshifts 6 to 8:
SPT0311-58 thus clearly stands out as a starburst system when compared
with typical massive star-forming galaxies at similar high redshifts.
The MIRI observations reveal a clumpy stellar structure, with each
clump having 3 to 5 x109M☉ mass in stars, leading to a total
stellar mass of 2.0 and 1.5 x10^10M☉ for the E and W galaxies,
respectively. The overall gas mass fraction is Mgas/M*∼3, similar to
that of z∼4.5-6 star-forming galaxies, suggesting a flattening of the
gas mass fraction in massive starbursts up to redshift 7. The
kinematics of the ionised gas in the E galaxy agrees with the known
[CII] gas kinematics, indicating a physical association between the
ionised gas and cold dust/gas clumps. The situation in the W galaxy is
more complex as it appears to be a velocity offset of about +700km/s
in the Paα relative to the [CII] emitting gas. The nature of
this offset, and its reality, is not fully established and requires
further investigation. The observed properties of SPT0311-58 such as
the clumpy distribution at sub(kpc) scales and the very high average
extinction are similar to those observed in low- and intermediate-z
luminous (E galaxy) and ultraluminous (W galaxy) infrared galaxies,
even though SPT0311-58 is observed only ∼800Myr after the Big Bang.
Massive, heavily obscured, clumpy starburst systems like SPT0311-58
likely represent the early phases in the formation of massive
high-redshift bulge/spheroids and luminous quasars. MIRI and JWST will
be able to explore for the first time the rest-frame near-infrared
stellar and ionised gas structure of these galaxies, even during the
Epoch of Reionization as demonstrated by this study.
Description:
SPT0311-58 JWST data were obtained in July 17th, 2022 using
the Mid-Infrared Instrument (MIRI) as part of the European Consortium
MIRI Guaranteed Time (proposal ID 1264).
The [CII]158um observations were carried out with ALMA under
program IDs (2016.1.01293.S and 2017.1.01423.S: PI Marrone). The data
is described in detail in Spilker et al. (2022ApJ...929L...3S 2022ApJ...929L...3S).
HST image of SPT0311-58 were retrieved from the Mikulski
Archive for Space Telescope (MAST). Image was taken with the WPFC3
camera using the near-infrared filter F160W (PI: Marrone, ID: 14740).
Objects:
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RA (2000) DE Designation(s)
--------------------------------------------------------------
03 11 33.14 -58 23 33.3 SPT0311-58 = SPT-S J031132-5823.4
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 141 4 List of fits images
fits/* . 4 Individual fits images
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 24 F5.3 arcsec/pix scale ? Scale of the image
26- 28 I3 --- Nx Number of pixels along X-axis
30- 32 I3 --- Ny Number of pixels along Y-axis
34- 59 A26 "datime" Obs.date Observation date
61- 63 I3 Kibyte size Size of FITS file
65- 89 A25 --- FileName Name of FITS file, in subdirectory fits
91-141 A51 --- Title Title of the FITS file
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History:
15-Mar-2023: From Javier Alvarez-Marquez, javier.alvarez(at)cab.inta-csic.es
17-Jul-2023: Image SPT0311F1000W60mas.fits added
Acknowledgements:
The authors thank to the anonymous referee for useful comments.
J.A-M., A.C-G., L.C., A.L. acknowledge support by grant
PIB2021-127718NB-100, P.G.P-G. by grant PGC2018-093499-B-I00. A.A-H.
by grant PID2021-124665NB-I00 from the Spanish Ministry of Science
and Innovation/State Agency of Research MCIN/AEI/10.1303
9/501100011033 and by "ERDF A way of making Europe". F.W. and M.N.
acknowledge support from the ERC Advanced Grant 740246 (Cosmic_Gas),
A.B. & G.O. acknowledges support from the Swedish National Space
Administration (SNSA). O.I. acknowledges the funding of the French
Agence Nationale de la Recherche for the project iMAGE (grant
ANR-22-CE31-0007), J.H. was supported by a VILLUM FONDEN Investigator
grant (project number 16599). K.I.C. acknowledges funding from the
Netherlands Research School for Astronomy (NOVA) and the Dutch
Research Council (NWO) through the award of the Vici Grant
VI.C.212.036. J.P.P. acknowledges financial support from the UK
Science and Technology Facilities Council, and the UK Space Agency.
T.P.R. would like to acknowledge support from the ERC under advanced
grant 743029 (EASY). The Cosmic Dawn Center (DAWN) is funded by the
Danish National Research Foundation under grant No. 140.
The work presented is the effort of the entire MIRI team and the
enthusiasm with in the MIRI partnership is a significant factor in its
success. MIRI draws on the scientific and technical expertise of the
following organisations: Ames Resear ch Center, USA; Airbus Defence
and Space, UK; CEA-Irfu, Saclay, France; Centre Spatial de Liege,
Belgium; Consejo Superior de Investigaciones Cientificas, Spain; Carl
Zeiss Optronics, Germany; Chalmers University of Technology, Sweden;
Danish Space Research Institute, Denmark; Dublin Institute for
Advanced Studies, Ireland; European Space Agency, Netherlands; ETCA,
Belgium; ETH Zurich, Switzerland; Goddard Space Flight Center, USA;
Institute d'Astrophysique Spatiale, France; Instituto Nacional de
Tecnica Aeroespacial, Spain; Institute for Astronomy, Edinburgh, UK;
Jet Propulsion Laboratory, USA; Laboratoire d'Astrophysique de
Marseille (LAM), France; Leiden University, Netherlands; Lockheed
Advanced Technology Center (USA); NOVA Opt-IR group at Dwingeloo,
Netherlands; Northrop Grumman, USA; Max-Planck Institut fur
Astronomie (MPIA), Heidelberg, Germany; Laboratoire d'Etudes
Spatiales et d'Instrumentation en Astrophysique (LESIA), France; Paul
Scherrer Institut, Switzerland; Raytheon Vision Systems, USA; RUAG
Aerospace, Switzerland; Rutherford Appleton Laboratory (RAL Space),
UK; Space Telescope Science Institute, USA; Toegepast-
Natuurwetenschappelijk Onderzoek (TNO-TPD), Netherlands; UK Astronomy
Technology Centre, UK; University College London, UK; University of
Amsterdam, Netherlands; University of Arizona, USA; University of
Cardiff, UK; University of Cologne, Germany; University of Ghent;
University of Groningen, Netherlands; University of Leicester, UK;
University of Leuven, Belgium; University of Stockholm, Sweden; Utah
State University, USA. A portion of this work was carried out at the
Jet Propulsion Laboratory, California Institute of Technology, under a
contract with the National Aeronautics and Space Administration. We
would like to thank the following National and International Funding
Agencies for their support of the MIRI development: NASA; ESA; Belgian
Science Policy Office; Centre Nationale D'Etudes Spatiales (CNES);
Danish National Space Centre; Deutsches Zentrum fur Luft-und Raumfahrt
(DLR); Enterprise Ireland; Ministerio De Economia y Competitividad;
Netherlands Research School for Astronomy (NOVA); Netherlands
Organisation for Scientific Research (NWO); Science and Technology
Facilities Council; Swiss Space Office; Swedish National Space Board;
UK Space Agency. This work is based on observations made with the
NASA/ESA/CSA James Webb Space Telescope. The data were obtained from
the Mikulski Archive for Space Telescopes at the Space Telescope
Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-03127 for JWST; and from the European JWST archive
(https://jwst.esac.esa.int/archive operated by the ESDC.
This paper makes use of the following ALMA data:
ADS/JAO.ALMA#2016.1.01293.S and ADS/JAO.ALMA#2017.1.01493.S. ALMA is
a partnership of ESO (representing its member states), NSF (USA) and
NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and
KASI (Republic of Korea), in cooperation with the Republic of Chile.
The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.
(End) Patricia Vannier [CDS] 18-Jan-2023