J/MNRAS/501/3926 ALMA/NOEMA high-z star-forming galaxies (Birkin+, 2021)
An ALMA/NOEMA survey of the molecular gas properties of high-redshift
star-forming galaxies.
Birkin J.E., Weiss A., Wardlow J.L., Smail I., Swinbank A.M.,
Dudzeviciute U., An F.X., Ao Y., Chapman S.C., Chen C.-C., da Cunha E.,
Dannerbauer H., Gullberg B., Hodge J.A., Ikarashi S., Ivison R.J.,
Matsuda Y., Stach S.M., Walter F., Wang W.-H., van der Werf P.
<Mon. Not. R. Astron. Soc., 501, 3926-3950 (2021)>
=2021MNRAS.501.3926B 2021MNRAS.501.3926B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Radio sources ; Millimetric/submm sources ;
Star Forming Region ; Redshifts
Keywords: galaxies: evolution - galaxies: star formation -
submillimetre: galaxies
Abstract:
We have used ALMA and NOEMA to study the molecular gas reservoirs in
61 ALMA-identified submillimetre galaxies (SMGs) in the COSMOS, UDS,
and ECDFS fields. We detect 12CO (Jup=2-5) emission lines in 50
sources, and [CI](3P1-3P0) emission in eight, at z=1.2-4.8 and
with a median redshift of 2.9±0.2. By supplementing our data with
literature sources, we construct a statistical CO spectral line energy
distribution and find that the 12CO line luminosities in SMGs peak
at Jup∼6, consistent with similar studies. We also test the
correlations of the CO, [CI], and dust as tracers of the gas mass,
finding the three to correlate well, although the CO and dust mass as
estimated from the 3-mm continuum are preferable. We estimate that
SMGs lie mostly on or just above the star-forming main sequence, with
a median gas depletion timescale, tdep=Mgas/SFR, of 210±40Myr
for our sample. Additionally, tdep declines with redshift across
z∼1-5, while the molecular gas fraction, µgas=Mgas/M*,
increases across the same redshift range. Finally, we demonstrate that
the distribution of total baryonic mass and dynamical line width,
Mbaryon-σ, for our SMGs is consistent with that followed by
early-type galaxies in the Coma cluster, providing strong support to
the suggestion that SMGs are progenitors of massive local spheroidal
galaxies. On the basis of this, we suggest that the SMG populations
above and below an 870-µm flux limit of S870∼5mJy may correspond
to the division between slow and fast rotators seen in local
early-type galaxies.
Description:
Our 61 targets are selected from ALMA-identified 870-µm-selected
SMGs in the AS2COSMOS (Simpson et al. 2020MNRAS.495.3409S 2020MNRAS.495.3409S, Cat.
J/MNRAS/495/3409), AS2UDS (Stach et al. 2019MNRAS.487.4648S 2019MNRAS.487.4648S), and
ALESS (Hodge et al. 2013ApJ...768...91H 2013ApJ...768...91H, Cat. J/ApJ/768/91) surveys.
A total of 31 sources that lack existing spectroscopic redshifts,
which were targeted with scans in the 3-mm band. These sources
comprise two subsets, first SMGs with the brightest 870-µm fluxes
in the AS2COSMOS and AS2UDS surveys, and a second subset of sources
from ALESS that span a wider range in submillimetre flux, but are
chosen to be faint in the optical/near-infrared
A total of 30 sources with existing rest-frame optical/UV
spectroscopic redshifts. Four of these sources are taken from AS2UDS
(Dudzeviciute et al. 2020MNRAS.494.3828D 2020MNRAS.494.3828D, Cat. J/MNRAS/494/3828), and
the remaining 26 are taken from ALESS (Danielson et al.
2017ApJ...840...78D 2017ApJ...840...78D, Cat. J/ApJ/840/78). These sources are typically
brighter in the optical and near-infrared, and fainter in the
submillimetre than the scan sample.
Observations were obtained from six projects, four with ALMA and two
with NOEMA/PolyFix, between 2017 and 2020. Fifteen targets from the
scan sample, five from AS2COSMOS, and ten from AS2UDS, were observed
with NOEMA/PolyFix in projects S18CG and W18EL. The remaining 46
targets were observed with ALMA in projects 2016.1.00564.S,
2017.1.01163.S, 2017.1.01512.S, and 2019.1.00337.S. Sixteen of the
targets in the scan sample (three from AS2UDS, thirteen from ALESS)
were observed using five tunings to achieve 32GHz of bandwidth
covering ∼82-114GHz. All 30 targets in the spec-z sample were observed
using single tunings centred on the frequency of the CO line expected
in the 3-mm band (ALMA band 3).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 76 61 Full list of all sources targeted for this work
tablea2.dat 236 50 Full table of line properties for sources with
CO line detections, along with serendipitously
detected CO emitters
tablea3.dat 161 119 Full table of sources used to construct the CO
SLED in Section 3.3 and also those plotted as
'literature SMGs' in Fig. 7
tablea4.dat 92 8 Table of [CI](3P1-3P0) line properties
from our sample
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See also:
J/MNRAS/495/3409 : SCUBA-2-COSMOS field brightest sub-mm sources
(Simpson+, 2020)
J/ApJ/768/91 : ALMA observations of LESS submm galaxies (Hodge+, 2013)
J/MNRAS/494/3828 : ALMA survey of the SCUBA-2 CLS UDS field
(Dudzeviciute+, 2020)
J/ApJ/840/78 : Redshift survey of ALMA-identified SMGs in ECDFS
(Danielson+, 2017)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- Name Source name
(ALESSNNN.N or AS2COSNNNN.N or AS2UDSNNN.N)
14- 19 A6 --- Subsample Subsample (scan or spec-z) (1)
21- 30 F10.6 deg RAdeg Right ascension (J2000)
32- 41 F10.6 deg DEdeg Declination (J2000)
43- 47 F5.3 --- zphot Photometric redshift
49- 54 F6.4 --- zspec ? Spectroscopic redshift
56- 65 F10.7 mJy S870 ALMA 870um flux density
67- 76 F10.8 mJy e_S870 Error on S870
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Note (1): Subsample as follows:
scan = Source that lacks existing spectroscopic redshifts, which was
targeted with scans in the 3-mm band
spec-z = Source with existing rest-frame optical/UV spectroscopic redshift
See section 2.1 of the article for more details.
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Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- Name Source name (ALESSNNN.N or AS2COSNNNN.N
or AS2UDSNNN.N)
14 I1 --- Jup Total angular momentum of upper level
16- 23 F8.4 GHz Freq Frequency
25- 33 F9.7 Jy.km/s ICO Velocity-integrated intensity of the CO
line
35- 43 F9.7 Jy.km/s e_ICO Error on ICO
45- 51 F7.5 --- zCO CO line redshift
53- 61 F9.4 km/s FWHM FWHM of the CO line
63- 70 F8.4 km/s e_FWHM Error on FWHM
72- 82 F11.8 mJy S870 ? ALMA 870um flux density
84- 93 F10.8 mJy e_S870 ? Error on S870
95- 104 F10.8 mJy S3mm ALMA 3mm continuum flux density
106- 115 F10.8 mJy e_S3mm Error on S3mm
117- 127 E11.6 K.km/s/pc2 LCO CO line luminosity
129- 139 E11.6 K.km/s/pc2 e_LCO Error on LCO
141- 146 F6.3 [Msun] b_logM* ? Lower bound on logM*
148- 153 F6.3 [Msun] logM* ? Logarithm of the stellar mass
155- 160 F6.3 [Msun] B_logM* ? Upper bound on logM*
162- 166 F5.2 [Lsun] b_logLIR ? Lower bound on logLIR
168- 172 F5.2 [Lsun] logLIR ? Logarithm of the dust luminosity
174- 178 F5.2 [Lsun] B_logLIR ? Upper bound on logLIR
180- 184 F5.3 [Msun/yr] b_logSFR ? Lower bound on logSFR
186- 190 F5.3 [Msun/yr] logSFR ? Logarithm of the star formation rate
192- 196 F5.3 [Msun/yr] B_logSFR ? Upper bound on logSFR
198- 202 F5.3 [Msun] b_logMdust ? Lower bound on logMdust
204- 208 F5.3 [Msun] logMdust ? Logarithm of the dust mass
210- 214 F5.3 [Msun] B_logMdust ? Upper bound on logMdust
216- 220 F5.3 Gyr b_Age ? Lower bound on Age
222- 226 F5.3 Gyr Age ? Age
228- 232 F5.3 Gyr B_Age ? Upper bound on Age
234 I1 --- Double [0/1] Indicates if the source displays
double-peaked line profiles
(0: no, 1:yes)
236 I1 --- AGN [0/1] Indicates if the source is
classified as AGN according to the
Donley et al. (2012ApJ...748..142D 2012ApJ...748..142D)
criteria
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Byte-by-byte Description of file: tablea3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- Name Source name
20 I1 --- Jup Total angular momentum of upper level
22- 32 E11.6 K.km/s/pc2 LCO CO line luminosity
34- 40 F7.5 --- zCO CO line redshift
42- 52 E11.6 Lsun LIR Dust luminosity
54- 62 F9.4 km/s FWHM ? FWHM of the CO line
64- 71 F8.4 km/s e_FWHM ? Error on FWHM
73- 161 A89 --- Ref References
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Byte-by-byte Description of file: tablea4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- Name Source name
14- 21 F8.4 GHz Freq Frequency
23- 31 F9.7 Jy.km/s ICI Velocity-integrated intensity of the CI line
33- 41 F9.7 Jy.km/s e_ICI Error on ICI
43- 49 F7.5 --- zCI CI line redshift
51- 59 F9.4 km/s FWHM FWHM of the CI line
61- 68 F8.4 km/s e_FWHM Error on FWHM
70- 80 E11.6 K.km/s/pc2 LCI CI line luminosity
82- 92 E11.6 K.km/s/pc2 e_LCI Error on LCI
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 19-Oct-2023