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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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 84 1627 ALMA maps table4.dat 136 1034 5σ-peak catalog (ALL5S)
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) : ALMA science archive Byte-by-byte Description of file: table2.dat
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 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 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).
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
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 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)
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) 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) 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. -------------------------------------------------------------------------
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 21-Jun-2018
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