J/A+A/664/A73 Star-forming galaxies at 4.5 < z < 6.2 (Burgarella+, 2022)
The ALMA-ALPINE [CII] survey: The star formation history and the dust emission
of star-forming galaxies at 4.5 < z < 6.2.
Burgarella D., Bogdanoska J., Nanni A., Bardelli S., Bethermin M.,
Boquien M., Buat V., Faisst A.L., Dessauges-Zavadsky M., Fudamoto Y.,
Fujimoto S., Giavalisco M., Ginolfi M., Gruppioni C., Hathi N.P., Ibar E.,
Jones G.C., Koekemoer A.M., Kohno K., Lemaux B.C., Narayanan D., Oesch P.,
Ouchi M., Riechers D.A., Pozzi F., Romano M., Schaerer D., Talia M.,
Theule P., Vergani D., Zamorani G., Zucca E., Cassata P., ALPINE team
<Astron. Astrophys. 664, A73 (2022)>
=2022A&A...664A..73B 2022A&A...664A..73B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Star Forming Region ; Models
Keywords: galaxies: formation - galaxies: evolution - early Universe -
submillimeter: galaxies - ultraviolet: galaxies - infrared: galaxies
Abstract:
Star-forming galaxies are composed of various types of galaxies.
However, the luminosity functions at z≳4-5 suggest that most galaxies
have a relatively low stellar mass (logMstar∼10) and a low dust
attenuation (AFUV∼1.0). The physical properties of these objects are
quite homogeneous. We used an approach where we combined their
rest-frame far-infrared and submillimeter emissions and utilized the
universe and the redshift as a spectrograph to increase the amount of
information in a collective way. From a subsample of 27 ALMA-detected
galaxies at z>4.5, we built an infrared spectral energy distribution
composite template. It was used to fit, with CIGALE, the 105 galaxies
(detections and upper limits) in the sample from the far-ultraviolet
to the far-infrared. The derived physical parameters provide
information to decipher the nature of the dust cycle and of the
stellar populations in these galaxies. The derived IR composite
template is consistent with the galaxies in the studied sample. A
delayed star formation history with τmain=500Myrs is slightly
favored by the statistical analysis as compared to a delayed with a
final burst or a continuous star formation history. The position of
the sample in the star formation rate (SFR) versus Mstar diagram is
consistent with previous papers. The redshift evolution of the log
Mstar versus AFUV relation is in agreement with an evolution in
redshift of this relation. This evolution is necessary to explain the
cosmic evolution of the average dust attenuation of galaxies.
Evolution is also observed in the Ldust/LFUV (IRX) versus UV slope
βFUV diagram: younger galaxies have bluer βFUV. We
modeled the shift of galaxies in the IRX versus the βFUV
diagram with the mass-weighted age as a free parameter, and we provide
an equation to make predictions. The large sample studied in this
paper is generally consistent with models that assume rapid dust
formation from supernovae and removal of dust by outflows and
supernovae blasts. However, we find that high mass dusty star-forming
galaxies cannot be explained by the models.
Description:
We study a sample of star-forming galaxies observed with ALMA in the
redshift range 4.5≲z≲6.2. Some of them, detected in the continuum
with ALMA, were used to build a composite IR SED covering a large
wavelength range from about 15 umto 218um. Using CIGALE, we
modeled the IR composite template and derived a set of physical
properties.
IR template for each of the models, normalized to 200um.
Objects:
---------------------------------------------
RA (2000) DE Designation(s)
---------------------------------------------
03 32 54.024 -27 50 00.82 CANDELSGOODSS12
03 32 18.912 -27 53 02.76 CANDELSGOODSS14
03 32 22.968 -27 46 29.03 CANDELSGOODSS19
03 32 11.928 -27 41 57.08 CANDELSGOODSS21
03 32 16.992 -27 41 13.74 CANDELSGOODSS32
---------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tabled1.dat 28 918 IR template for each of the models,
normalized to 200um
tablee1.dat 680 105 Physical parameters from PL+OTMBB
(Physicalparametersplotmbbfinal21Oct)
tablee2.dat 510 105 Physical parameters from DL2014
(Physicalparametersdl2014final21Oc)
lbghiz.dat 86 47 IR composite built from the sample of
ALMA-detected objects
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See also:
J/A+A/643/A2 : ALPINE DR1 merged catalog (Bethermin+, 2020)
Byte-by-byte Description of file: tabled1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.3 um lambda Wavelength
9- 14 F6.3 --- Fnu(DL2014)/F200um DL2014 flux, normalized to 200um
16- 21 F6.3 --- Fnu(PL+OTMBB)/F200um PL+OTMBB flux, normalized to 200um
23- 28 F6.3 --- Fnu(PL+GMBB)/F200um PL+GMBB flux, normalized to 200um
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Byte-by-byte Description of file: tablee1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 22 A22 --- Name Source name
24- 41 F18.16 --- z ? Redshift
43- 61 F19.16 --- betaFUV UV slope, βFUV
63- 81 F19.17 --- e_betaFUV UV slope error
83-103 E21.17 yr-1 sSFR Specific star formation rate
105-126 E22.17 yr-1 e_sSFR Specific star formation rate error
128-148 E21.19 --- sMdustdl2014 Specific dust mass from DL2014
150-170 E21.19 --- e_sMdustdl2014 Specific dust mass from DL2014 error
172-192 E21.19 --- sMdustpre-shock Pre-shock specific dust mass
194-214 E21.19 --- e_sMdustpre-shock Pre-shock specific dust mass error
216-236 E21.19 --- sMdustpost-shock Post-shock specific dust mass
238-258 E21.19 --- e_sMdustpost-shock Post-shock specific dust mass error
260-279 E20.17 --- Mdustdl2014 Dust mass from dl2014
281-300 E20.17 --- e_Mdustdl2014 Dust mass from dl2014 error
302-321 E20.17 --- Mdustpre-shock Pre-shock dust mass
323-342 E20.17 --- e_Mdustpre-shock Pre-shock dust mass error
344-363 E20.17 --- Mdustpost-shock Pre-shock dust mass
365-383 F19.11 --- e_Mdustpost-shock Pre-shock dust mass error
385-403 F19.17 --- AFUV FUV dust attenuation
405-424 F20.18 --- e_AFUV FUV dust attenuation error
426-446 F21.18 --- IRX Ldust/LFUV ratio
448-467 F20.18 --- e_IRX Ldust/LFUV ratio error
469-488 F20.15 Myr Age Main age
490-509 F20.16 Myr e_Age Main age error
511-531 E21.17 Lsun Ldust Dust luminosity
533-553 E21.17 Lsun e_Ldust Dust luminosity error
555-575 E21.17 Lsun LFUV FUV luminosity
577-597 E21.17 Lsun e_LFUV FUV luminosity error
599-617 F19.15 Msun/yr SFR Star formation rate
619-637 F19.16 Msun/yr e_SFR Star formation rate error
639-659 E21.17 Msun Mstar Star mass
661-680 E20.17 Msun e_Mstar Star mass error
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Byte-by-byte Description of file: tablee2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 22 A22 --- Name Source name
24- 41 F18.16 --- z ? Redshift
43- 61 F19.16 --- betaFUV UV slope, βFUV
63- 81 F19.17 --- e_betaFUV UV slope error
83-103 E21.17 yr-1 sSFR Specific star formation rate
105-126 E22.17 yr-1 e_sSFR Specific star formation rate error
128-148 E21.19 --- sMdust Specific dust mass
150-170 E21.19 --- e_sMdust Specific dust mass error
172-190 F19.17 --- AFUV FUV dust attenuation
192-212 F21.19 --- e_AFUV FUV dust attenuation error
214-234 F21.18 --- IRX Ldust/LFUX ratio
236-255 F20.18 --- e_IRX Ldust/LFUX ratio error
257-276 F20.15 Myr Age Main age
278-297 F20.16 Myr e_Age Main age error
299-319 E21.17 Lsun Ldust Dust luminosity
321-341 E21.17 Lsun e_Ldust Dust luminosity error
343-362 E20.17 Msun Mdust Dust mass
364-383 E20.17 Msun e_Mdust Dust mass error
385-405 E21.17 Lsun LFUV FUV luminosity
407-427 E21.17 Lsun e_LFUV FUV luminosity error
429-447 F19.15 --- SFR Star formation rate
449-467 F19.16 --- e_SFR Star formation rate error
469-489 E21.17 Msun Mstar Star mass
491-510 E20.17 Msun e_Mstar Star mass error
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Byte-by-byte Description of file: lbghiz.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- Id Identifier
19- 25 F7.3 um lambda Wavelength
27- 44 F18.16 --- Fnu/F200um ? Flux, normalized to 200um
46 A1 --- l_Fnu/F200um [-] - indicates upper limit for Fnu/F200um
47- 66 F20.18 --- e_Fnu/F200um ? Error on Fnu/F200um
68- 86 F19.16 --- S/N ? Signal-to-noise ratio (1)
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Note (1): S/N = -1.00 mean that the data in the given band is an upper limit.
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Acknowledgements:
Denis Burgarella, denis.burgarella(at)lam.fr
(End) Patricia Vannier [CDS] 25-Mar-2022