J/ApJ/850/83 DANCING-ALMA. I. submm/mm continuum sources (Fujimoto+, 2017)
Demonstrating A New Census of INfrared Galaxies with ALMA (DANCING-ALMA).
I. FIR size and luminosity relation at z=0-6 revealed with 1034 ALMA sources.
Fujimoto S., Ouchi M., Shibuya T., Nagai H.
<Astrophys. J., 850, 83 (2017)>
=2017ApJ...850...83F 2017ApJ...850...83F
ADC_Keywords: Millimetric/submm sources; Photometry, infrared; Redshifts
Keywords: galaxies: evolution ; galaxies: formation ; galaxies: high redshift ;
galaxies: starburst ; galaxies: star formation
Abstract:
We present the large statistics of the galaxy effective radius Re in
the rest-frame far-infrared (FIR) wavelength Re(FIR) obtained from
1627 Atacama Large Millimeter/submillimeter Array (ALMA) 1mm band maps
that become public by 2017 July. Our ALMA sample consists of 1034
sources with the star formation rate ∼100-1000M☉/yr and the
stellar mass ∼1010-1011.5M☉ at z=0-6. We homogeneously
derive Re(FIR) and FIR luminosity LFIR of our ALMA sources via the
uv-visibility method with the exponential disk model, carefully
evaluating selection and measurement incompletenesses by realistic
Monte-Carlo simulations. We find that there is a positive correlation
between Re(FIR) and LFIR at the >99% significance level. The
best-fit power-law function, Re(FIR)∝LFIRα,
provides α=0.28±0.07, and shows that Re(FIR) at a fixed LFIR
decreases toward high redshifts. The best-fit α and the redshift
evolution of Re(FIR) are similar to those of Re in the rest-frame UV
(optical) wavelength Re(UV) (Re(Opt)) revealed by Hubble Space
Telescope (HST) studies. We identify that our ALMA sources have
significant trends of Re(FIR)≲Re(UV) and Re(Opt), which
suggests that the dusty starbursts take place in compact regions.
Moreover, Re(FIR) of our ALMA sources is comparable to Re(Opt) of
quiescent galaxies at z∼1-3 as a function of stellar mass, supporting
the evolutionary connection between these two galaxy populations. We
also investigate rest- frame UV and optical morphologies of our ALMA
sources with deep HST images, and find that ∼30%-40% of our ALMA
sources are classified as major mergers. This indicates that dusty
starbursts are triggered by not only the major mergers but also the
other mechanism(s).
Description:
To accomplish a complete galaxy effective radius (Re) in the
rest-frame far-infrared (FIR) wavelength (Re(FIR)) study, we make
full use of ALMA archival data in cycles 0-3 that became public by
2017 July. We collect 1627 continuum maps in Band 6/7 from the ALMA
archival data in the regions of HUDF, HFF, Cosmic Evolution Survey
(COSMOS), Subaru/XMM-Newton Deep Survey (SXDS), and The Great
Observatories Origins Deep Survey South (GOODS-S), which have rich
multi-wavelength data.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 84 1627 ALMA maps
table4.dat 136 1034 5σ-peak catalog (ALL5S)
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See also:
II/284 : COSMOS Multi-Wavelength Photometry Catalog (Capak+, 2007)
J/ApJ/622/772 : Redshift survey of submillimeter galaxies (Chapman+, 2005)
J/A+A/434/53 : GOODS-South Field redshifts (Vanzella+, 2005)
J/ApJS/176/1 : Subaru/XMM-Newton deep survey (SXDS). II. (Furusawa+, 2008)
J/ApJS/179/124 : Subaru/XMM-Newton deep survey (SXDS) III. (Ueda+, 2008)
J/ApJ/690/1236 : COSMOS photometric redshift catalog (Ilbert+, 2009)
J/ApJS/195/10 : The CDF-S survey: 4Ms source catalogs (Xue+, 2011)
J/ApJS/201/30 : The Chandra COSMOS survey. III. (Civano+, 2012)
J/ApJS/203/24 : Structural param. of galaxies in CANDELS (van der Wel+, 2012)
J/ApJ/769/80 : Spitzer/IRAC observations of five deep fields (Ashby+, 2013)
J/A+A/556/A55 : Multi-color photom. of star-forming galaxies (Ilbert+, 2013)
J/ApJ/788/125 : An ALMA survey of ECDFS submm galaxies (Simpson+, 2014)
J/ApJ/806/110 : ALESS survey: SMGs in the ECDF-S data (da Cunha+, 2015)
J/ApJ/801/97 : GOODS-S & UDS stellar mass cat. from CANDELS (Santini+, 2015)
J/ApJS/219/15 : Morphologies of z=0-10 galaxies with HST data (Shibuya+, 2015)
J/ApJS/222/1 : Faint ALMA 1.2mm sources down to ∼0.02mJy (Fujimoto+, 2016)
J/A+A/591/A136 : Galaxies & QSOs FIR size and surface brightness (Lutz+, 2016)
J/A+A/597/A41 : ALMA Frontier Fields Survey. I. (Gonzalez-Lopez+, 2017)
J/ApJ/839/58 : ALMA submm galaxies multi-wavelength data (Simpson+, 2017)
http://almascience.eso.org/aq/ : ALMA science archive
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- MID [1/1627] Map ID
6- 19 A14 --- PrID ALMA project code ID
21- 39 A19 --- Target Target name in the initial ALMA observations
41- 44 F4.2 mm lambda [0.8/1.4] Wavelength in the observed frame
46- 48 I3 GHz nu [221/354] Frequency in the observed frame
50- 50 I1 --- Band [6/7] ALMA Band
52- 53 I2 m Min [15/43] Minimum baseline of the antenna
configuration
55- 58 I4 m Max [134/2270] Maximum baseline of the antenna
configuration
60- 63 F4.2 mJy/beam sigma [0.01/1.4] One sigma noise level measured after
the CLEAN process (Section 2.2)
65- 68 F4.2 arcsec amaj [0.1/4.1] Major axis of the synthesized beam
(weight = 'natural')
70- 73 F4.2 arcsec bmin [0.1/1.3] Minor axis of the synthesized beam
(weight = 'natural')
75- 78 F4.2 arcsec Beam [0.1/2.1] Circularized beam size
80- 82 A3 --- sSet Classification of the sub-dataset (1)
84- 84 I1 --- Type [1/2] map type: 1=single field; 2=mosaic (2)
--------------------------------------------------------------------------------
Note (1): We divide the 1627 ALMA continuum maps into 10 sub-data sets based on
the angular resolutions as in Table 1:
------------------------------------------------
sSet θcirc Number of maps
(arcsec)
------------------------------------------------
SB1 0.0-0.2 48
SB2 0.2-0.4 303
SB3 0.4-0.6 394
SB4 0.6-0.8 203
SB5 0.8-1.0 254
SB6 1.0-1.2 154
SB7 1.2-1.4 228
SB8 1.4-1.6 11
SB9 1.6-1.8 18
SB10 1.8-2.0 14
------------------------------------------------
Note (2): We cut out the mosaic maps (M.ID 1599-1627) based on the source
positions identified in the dirty maps to perform the data analyses
(Section 2.2).
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Seq [1/1034] Source ID of ALL5S
6- 19 F14.10 deg RAdeg Right Ascension, decimal degrees (J2000)
21- 34 F14.10 deg DEdeg Declination, decimal degrees (J2000)
36- 40 F5.2 mm lambda [0.8/19.2] Observed wavelength
42- 45 F4.1 --- SNpeak [5/69] Peak signal-to-noise ratio
47- 51 F5.2 mJy/beam Speak [0.08/10.2] Peak flux density per beam
obtained from the peak pixel value
before primary beam correction
53- 56 F4.2 mJy e_Speak [0.01/1.1]? Standard deviation of the pixel
values before primary beam correction,
corresponding to the uncertainty of the
peak pixel values
58- 62 F5.2 mJy Simf [0.06/30.4]? Total flux density measured by
IMFIT after primary beam correction
64- 67 F4.2 mJy e_Simf [0.01/1.1]? Uncertainty in Simf (1)
69- 73 F5.2 mJy Suvf [0.05/35]? Total flux density measured by
UVMULTIFIT after primary beam correction
for ALL10S
75- 80 F6.2 mJy e_Suvf [0.01/425]? Uncertainty in Suvf (2)
82- 86 F5.2 mJy Suvfcrr [0.05/27]? Total flux density measured
by UVMULTIFIT after primary beam
Monte-Carlo simulation (Section 3.3)
corrections for ALL10S (2)
88- 93 F6.2 mJy e_Suvfcrr [0.01/483]? Uncertainty in Suvfcrr (2)
95- 98 F4.2 arcsec Ruvf [0.04/0.9]? Effective Radius measured
by UVMULTIFIT for ALL10S (2)
100-105 F6.2 arcsec e_Ruvf [0/133]? Uncertainty in Ruvf (2)
107-110 F4.2 arcsec Ruvfcrr [0.01/0.9]? Effective Radius measured
by UVMULTIFIT after Monte-Carlo simulation
correction (Section 3.3) for ALL10S (2)
112-117 F6.2 arcsec e_Ruvfcrr [0/111]? Uncertainty in Ruvfcrr (2)
119-119 I1 --- f_uvf ? Reliability of UVMULTIFIT result
(0=reliable) (2)(3)
121-124 F4.2 arcsec offset [0.01/1]? Offset between centers of the ALMA
source and the optical-NIR counterpart
for OC5S (4)
126-131 F6.2 --- zphot [0.01/10]? Photometric redshift of the
optical-NIR counterpart obtained from the
optical-NIR source catalog for OC5S (4)
133-136 F4.1 mag Hmag [1.4/28.3]? H-band AB magnitude for OC5S (4)
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Note (1): Note that IMFIT sometimes shows too small uncertainties in the
fitting results (probably bag of IMFIT). In this case, we adopt the
value of the standard deviation of the pixel values.
Note (2): ALL5S sources that are not included in ALL10S have null values
(blanks) in the columns Suvf, e_Suvf, Suvfcrr, e_Suvfcrr, Ruvf,
e_Ruvf, Ruvfcrr, e_Ruvfcrr, and f_uvf.
Note (3): Reliability of UVMULTIFIT (Marti-Vidal+ 2014A&A...563A.136M 2014A&A...563A.136M) result
based on uv-distance vs. amplitude plot (Section 3.2) for ALL10S.
Code as follows:
0 = reliable;
1 = tentative;
2 = bad.
Note (4): ALL5S sources that are not included in "OC5S" (optical-NIR
counterparts of ALL5S) have the null values (blanks) in the columns of
offset, zphot, and Hmag.
Optical-NIR catalog used in our optical-NIR counterpart
identification (table 5):
-------------------------------------------------------------------------
Field Catalog reference Detection limit (ap.)
-------------------------------------------------------------------------
SXDS Santini+ (2015, J/ApJ/801/97) H<27.5 (0.2")
GOODS-S Wide Santini+ (2015, J/ApJ/801/97) H<27.4 (0.17")
GOODS-S Deep Santini+ (2015, J/ApJ/801/97) H<28.2 (0.17")
HUDF Santini+ (2015, J/ApJ/801/97) H<29.7 (0.17")
COSMOS Wide^a Ilbert+ (2013, J/A+A/556/A55) H<23.9 (2.0")^b
COSMOS Deep^c Momcheva+ (2016ApJS..225...27M 2016ApJS..225...27M) H<26.4 (1.0")^d
HFF Castellano+ (2016, J/A+A/590/A31) H<28.5-29.0 (0.35")
-------------------------------------------------------------------------
Notes:
a = COSMOS field overlapped with 3D-HST.
b = The catalog is constructed with a detection image from the sum of the
UltraVISTA DR1 YJHKs images, where the 5σ detection limit of
the H-band image is H<23.9 in a 2.0" aperture.
c = COSMOS field not overlapped with 3D-HST.
d = The catalog is constructed with the HST JH-band that has the 5σ
detection limit of JH<26.0 in a 1.0" aperture.
-------------------------------------------------------------------------
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 21-Jun-2018