J/ApJ/903/145 ALMaQUEST. IV. ALMA-MaNGA QUEnching & star formation (Lin+, 2020)
ALMaQUEST.
IV. The ALMA-MaNGA QUEnching and STar Formation (ALMaQUEST) Survey.
Lin L., Ellison S.L., Pan H.-A., Thorp M.D., Su Y.-C., Sanchez S.F.,
Belfiore F., Bothwell M.S., Bundy K., Chen Y.-M., Concas A., Hsieh B.-C.,
Hsieh P.-Y., Li C., Maiolino R., Masters K., Newman J.A., Rowlands K., Shi
Y., Smethurst R., Stark D.V., Xiao T., Yu P.-C.
<Astrophys. J., 903, 145 (2020)>
=2020ApJ...903..145L 2020ApJ...903..145L
ADC_Keywords: Star Forming Region; Interstellar medium; Stars, masses; Surveys;
Spectra, infrared; Spectra, optical; Spectra, millimetric/submm
Keywords: Star formation ; Interstellar medium ; Galaxy quenching ;
Extragalactic astronomy ; Surveys ; Molecular gas
Abstract:
The ALMaQUEST (ALMA-MaNGA QUEnching and STar formation) survey is a
program with spatially resolved 12CO(1-0) measurements obtained with
the Atacama Large Millimeter Array (ALMA) for 46 galaxies selected
from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA)
DR15 optical integral-field spectroscopic survey. The aim of the
ALMaQUEST survey is to investigate the dependence of star formation
activity on the cold molecular gas content at kiloparsec scales in
nearby galaxies. The sample consists of galaxies spanning a wide range
in specific star formation rate (sSFR), including starburst (SB),
main-sequence (MS), and green valley (GV) galaxies. In this paper, we
present the sample selection and characteristics of the ALMA
observations and showcase some of the key results enabled by the
combination of spatially matched stellar populations and gas
measurements. Considering the global (aperture-matched) stellar mass,
molecular gas mass, and star formation rate of the sample, we find
that the sSFR depends on both the star formation efficiency (SFE) and
the molecular gas fraction (fH2), although the correlation with
the latter is slightly weaker. Furthermore, the dependence of sSFR on
the molecular gas content (SFE or fH2) is stronger than that on
either the atomic gas fraction or the molecular-to-atomic gas
fraction, albeit with the small Hi sample size. On kiloparsec scales,
the variations in both SFE and fH2 within individual galaxies can
be as large as 1-2dex, thereby demonstrating that the availability of
spatially resolved observations is essential to understand the details
of both star formation and quenching processes.
Description:
MaNGA is an Integral Field Spectroscopy (IFS) survey conducted with
the loan Digital Sky Survey (SDSS) 2.5m telescope. MaNGA uses the BOSS
spectrographs and couples them with hexagonal fiber bundles of
different sizes. Each spectrum covers a wavelength range of
3500-10000Å with a spectral resolution ∼60km/s. After dithering,
MaNGA data have an effective angular resolution (FWHM) of 2.5",
corresponding to a physical scale of 0.5-6.5kpc.
Molecular gas observations in 12CO(1-0) (rest-frame 115.271204GHz)
were carried out with ALMA during Cycles 3, 5, and 6 using the Band 3
receiver. The observations were taken in the C43-2 configuration
(synthesized beam FWHM ∼2.5"), thus matching the MaNGA resolution. We
used a single pointing with a field of view (FOV) of ∼50". The largest
structure that we expect to be sensitive to is about 23" (∼14kpc). Our
spectral setup includes one high-resolution spectral window (∼10km/s)
targeting 12CO(1-0) and one to three low-resolution spectral window(s)
(∼90km/s) around the target line aimed at detecting/studying the
continuum.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 47 46 ALMaQUEST targets and CO(1-0) sensitivities
table2.dat 74 46 Properties of ALMaQUEST galaxies measured within
1.5Re
table3.dat 66 46 Properties of ALMaQUEST galaxies measured within
the MaNGA bundle coverage
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See also:
J/AJ/136/2782 : Star formation efficiency in nearby galaxies (Leroy+, 2008)
J/MNRAS/415/32 : COLD GASS survey (Saintonge+, 2011)
J/MNRAS/432/2112 : Estimating gas masses from HI and CO data (Brinchmann+ 2013)
J/ApJ/768/74 : PHIBSS: CO observations star-forming galaxies (Tacconi+, 2013)
J/ApJ/846/159 : Interferometric CO obs. of 126 CALIFA galaxies (Bolatto+, 2017)
J/A+A/604/A53 : ALLSMOG final data release. New APEX CO survey (Cicone+, 2017)
J/ApJS/233/22 : xCOLD GASS catalog (Saintonge+, 2017)
J/AJ/154/86 : MaNGA catalog, DR15 (Wake+, 2017)
J/MNRAS/476/875 : xGASS catalog (Catinella+, 2018)
J/ApJ/861/49 : ALFALFA extragalactic HI source catalog (Haynes+, 2018)
J/ApJ/872/16 : Integrated star formation law revisited I (de los Reyes+, 2019)
J/ApJ/892/148 : Molecular ISM in nearby star-forming galaxies (Sun+, 2020)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- ID Identifier
12- 21 F10.6 deg RAdeg [40/359] Right Ascension (J2000)
23- 31 F9.6 deg DEdeg [-8/28] Declination (J2000)
33- 40 F8.6 --- zspec [0.01/0.14] MaNGA spectroscopic redshift
42- 47 F6.4 Jy.km/s/beam sigmaCO [0.0194/0.2599] Sensitivity of integrated
ALMA CO maps (1)
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Note (1): The 1σ sensitivity of the integrated ALMA CO intensity maps
(see Section 2.3), calculated using the spectral window shown as the
yellow area in Figure 2.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- ID Identifier
12- 18 F7.2 kpc2 Area [11/1443] Area
20- 24 F5.2 [Msun] Mass [10.2/11.7] log, stellar mass
26- 30 F5.2 [Msun/yr] SFR [-3.03/1.22] log, star formation rate (1)
32- 36 F5.2 Jy.km/s SCO [1.58/34.3] CO(1-0) integrated intensity
38- 41 F4.2 Jy.km/s e_SCO [0.01/0.3] Uncertainty in SCO
43- 48 F6.3 [Msun] MH2 [8.48/10.5] log, Mass H2 (2)
50- 54 F5.3 [Msun] e_MH2 [0.001/0.02] Uncertainty in logMH2
56- 61 F6.2 [/yr] SSFR [-14.3/-9.42] log, specific star formation rate
63- 68 F6.2 [/yr] SFE [-12.2/-8.12] log, star formation efficiency
70- 74 F5.2 [-] fH2 [-2.61/-0.85] log, molecular hydrogen gas
fraction
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Note (1): Only spaxels classified as star-forming are included.
Note (2): The uncertainty listed here only refers to the measurement error,
not yet including the uncertainty in the CO-to-H2 conversion factor.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- ID Identifier
12- 16 F5.2 [Msun] Mass [10.2/11.8] log, stellar mass
18- 22 F5.2 [Msun/yr] SFR [-3.03/1.29] log, star formation rate (1)
24- 28 F5.2 Jy.km/s SCO [1.43/42.1] CO(1-0) integrated intensity
30- 33 F4.2 Jy.km/s e_SCO [0.01/0.3] Uncertainty in SCO
35- 40 F6.3 [Msun] MH2 [8.41/10.5] log, Mass H2 (2)
42- 46 F5.3 [Msun] e_MH2 [0.001/0.02] Uncertainty in logMH2
48- 53 F6.2 [/yr] SSFR [-14.3/-9.47] log, specific star formation rate
55- 60 F6.2 [/yr] SFE [-12.2/-8.11] log, star formation efficiency
62- 66 F5.2 [-] fH2 [-2.56/-0.9] log, molecular H2 gas fraction
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Note (1): Only spaxels classified as star-forming are included.
Note (2): The uncertainty listed here only refers to the measurement error,
not yet including the uncertainty in the CO-to-H2 conversion factor.
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History:
From electronic version of the journal
References:
Lin et al. Paper I : 2019ApJ...884L..33L 2019ApJ...884L..33L
Ellison et al. Paper II : 2020MNRAS.492.6027E 2020MNRAS.492.6027E
Ellison et al. Paper III : 2020MNRAS.493L..39E 2020MNRAS.493L..39E
Ellison et al. Paper V : 2021MNRAS.501.4777E 2021MNRAS.501.4777E
Ellison et al. Paper VI : 2021MNRAS.502L...6E 2021MNRAS.502L...6E
(End) Prepared by [AAS], Coralie Fix [CDS], 16-Feb-2022