J/ApJS/275/36 ALMA Lensing Cluster Survey (ALCS) 1.2mm (Fujimoto+, 2024)
ALMA Lensing Cluster Survey: deep 1.2mm number counts and infrared luminosity
functions at z∼1-8.
Fujimoto S., Kohno K., Ouchi M., Oguri M., Kokorev V., Brammer G., Sun F.,
Gonzalez-Lopez J., Bauer F.E., Caminha G.B., Hatsukade B., Richard J.,
Smail I., Tsujita A., Ueda Y., Uematsu R., Zitrin A., Coe D., Kneib J.-P.,
Postman M., Umetsu K., del P. Lagos C., Popping G., Ao Y., Bradley L.,
Caputi K., Dessauges-Zavadsky M., Egami E., Espada D., Ivison R.J.,
Jauzac M., Knudsen K.K., Koekemoer A.M., Magdis G.E., Mahler G.,
Munoz Arancibia A.M., Rawle T., Shimasaku K., Toft S., Umehata H.,
Valentino F., Wang T., Wang W.-H.
<Astrophys. J. Suppl. Ser., 275, 36 (2024)>
=2024ApJS..275...36F 2024ApJS..275...36F
ADC_Keywords: Clusters, galaxy; Millimetric/submm sources; Surveys;
Redshifts; Infrared sources; Interferometry; Gravitational lensing
Keywords: Galaxy formation ; Galaxy evolution ; Starburst galaxies ;
Millimeter astronomy ; Cosmic background radiation ;
Luminosity function ; Interferometry
Abstract:
We present a statistical study of 180 dust continuum sources
identified in 33 massive cluster fields by the Atacama Large
Millimeter/submillimeter Array Lensing Cluster Survey (ALCS) over a
total of 133arcmin2 area, homogeneously observed at 1.2mm. ALCS
enables us to detect extremely faint millimeter sources by lensing
magnification, including near-infrared (NIR) dark objects showing no
counterparts in existing Hubble Space Telescope and Spitzer images.
The dust continuum sources belong to a blind sample (N=141) with
signal-to-noise ratio (S/N)≳5.0 (a purity of >0.99) or a secondary
sample (N=39) with S/N=4.0-5.0 screened by priors. With the blind
sample, we securely derive 1.2mm number counts down to ∼7µJy, and
find that the total integrated 1.2mm flux is
20.7-6.5+8.5Jy/deg2, resolving ∼80% of the cosmic infrared
background light. The resolved fraction varies by a factor of 0.6-1.1
due to the completeness correction depending on the spatial size of
the millimeter emission. We also derive infrared (IR) luminosity
functions (LFs) at z=0.6-7.5 with the 1/Vmax method, finding the
redshift evolution of IR LFs characterized by positive luminosity and
negative density evolution. The total (=UV+IR) cosmic star formation
rate density (SFRD) at z>4 is estimated to be 161-21+25% of the
Madau and Dickinson measurements mostly based on rest-frame UV
surveys. Although our general understanding of the cosmic SFRD is
unlikely to change beyond a factor of 2, these results add to the
weight of evidence for an additional (∼60%) SFRD component contributed
by the faint millimeter population, including NIR-dark objects.
Description:
The Atacama Large Millimeter/submillimeter Array Lensing Cluster
Survey (ALCS) is a cycle-6 ALMA large program (project ID:
2018.1.00035.L; PI: K. Kohno) to map high-magnification regions in
33 massive galaxy clusters at 1.2mm in Band 6. The sample is selected
from the best-studied clusters drawn from HST treasury programs, i.e.,
Hubble Frontier Fields (HFFs; Lotz+ 2017ApJ...837...97L 2017ApJ...837...97L), the Cluster
Lensing and Supernova Survey with Hubble (CLASH;
Postman+ 2012, J/ApJS/199/25), and the Reionization Lensing Cluster
Survey (RELICS; Coe+ 2019, J/ApJ/884/85). Observations were carried
out between 2018 December and 2019 December in compact array
configurations of C43-1 and C43-2, where 26 and seven clusters were
observed in Cycles 6 and 7, respectively. We adopt two frequency
setups with the sky frequencies of 259.4 and 263.2GHz, accomplishing a
15GHz wide spectral scan in ranges of 250.0-257.5GHz and
265.0-272.5GHz to enlarge the survey volume for line-emitting galaxies.
For the five HFF clusters visible with ALMA, ALCS only performed
observations in one of the two frequency setups, because observations
for the other frequency setup had been taken in previous ALMA HFF
surveys (2013.1.00999.S and 2015.1.01425.S;
e.g., Gonzalez-Lopez+ 2017A&A...608A.138G 2017A&A...608A.138G).
The 15GHz frequency coverage of the ALCS data sets sometimes detects
emission lines from the sources serendipitously, which could affect
the continuum flux measurements. To investigate this possibility, we
extract the 15GHz spectra with 1.0" diameter aperture for our ALCS
sources in the two ALCS cubes with velocity channel widths of 30 and
60km/s, respectively. We newly determine a spectroscopic redshift for
eight sources from the serendipitous line detections in 13 ALCS
sources. See Sections 3.4 and 3.5 and Appendix A.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 45 33 ALCS data properties for 33 lensing clusters
table12.dat 101 180 ALCS continuum source catalog
table13.dat 135 160 *Physical properties of ALCS continuum sources
--------------------------------------------------------------------------------
Note on table13.dat: This is after correcting the lensing effect for the
multiply imaged sources, resulting in a slightly lower number than
that in Table 12.
--------------------------------------------------------------------------------
See also:
J/MNRAS/395/1213 : Galaxies in the field of MACS J1206.2-0847 (Ebeling+, 2009)
J/MNRAS/404/325 : Massive galaxy clusters lensing analyse (Richard+, 2010)
J/MNRAS/411/102 : AzTEC/ASTE 1.1mm observations in the ADF-S (Hatsukade+ 2011)
J/ApJS/199/25 : CLASH sources for MACS1149.6+2223 (Postman+, 2012)
J/ApJS/202/2 : VLA 1.4GHz observations of A370 and A2390 (Wold+, 2012)
J/ApJ/762/L30 : CLASH: MCS J0416.1-2403 lensing analysis (Zitrin+, 2013)
J/ApJ/793/115 : UV-continuum slopes beta for z∼4-8 galaxies (Bouwens+, 2014)
J/MNRAS/444/268 : HST Frontier Fields clusters (Richard+, 2014)
J/ApJ/806/110 : ALESS survey: SMGs in the ECDF-S data (da Cunha+, 2015)
J/MNRAS/452/1437 : Abell 2744 strong-lensing analysis (Jauzac+, 2015)
J/ApJ/812/114 : Grism Lens-Amplified Survey from Space. I. (Treu+, 2015)
J/ApJ/811/29 : GLASS. IV. Lensing cluster Abell 2744 (Wang+, 2015)
J/ApJ/801/44 : HST lensing analysis of the CLASH sample (Zitrin+, 2015)
J/ApJS/222/1 : Faint ALMA 1.2mm sources down to ∼0.02mJy (Fujimoto+, 2016)
J/ApJ/819/114 : Strong lensing masses of 4 HFF clusters (Kawamata+, 2016)
J/A+A/600/A90 : MACS J0416.1-2403 redshift catalogue (Caminha+, 2017)
J/ApJ/850/83 : DANCING-ALMA. I. submm/mm cont. sources (Fujimoto+, 2017)
J/A+A/597/A41 : ALMA Frontier Fields Survey. I. (Gonzalez-Lopez+, 2017)
J/MNRAS/464/3369 : SCUBA-2 EGS deep field (Zavala+, 2017)
J/ApJ/855/4 : Lyman break galaxies at z∼6-9 from HFF (Kawamata+, 2018)
J/A+A/609/A130 : [CII] luminosities of gal. in G.A.S.+Cloudy (Lagache+, 2018)
J/ApJ/853/172 : "Super-deblended" dust emission in galaxies. I. (Liu+, 2018)
J/ApJS/235/14 : HFF-DeepSpace phot. cat. of 12 HFF fields (Shipley+, 2018)
J/A+A/632/A36 : Strong lensing models of 8 CLASH clusters (Caminha+, 2019)
J/ApJ/884/85 : RELICS: Reionization Lensing Cluster Survey (Coe+, 2019)
J/MNRAS/485/3738 : 3D structure in the A370 MUSE Mosaic (Lagattuta+, 2019)
J/A+A/643/A2 : ALPINE DR1 merged catalog (Bethermin+, 2020)
J/MNRAS/494/3828 : ALMA survey of SCUBA-2 CLS UDS field (Dudzeviciute+, 2020)
J/A+A/635/A98 : Redshift catalogs of the Abell 2163 core (Rescigno+, 2020)
J/MNRAS/495/3409 : SCUBA-2-COSMOS field brightest smm sources (Simpson+, 2020)
J/ApJ/901/74 : ALMA obs. of UDS & GOODS-S massive galaxies (Tadaki+, 2020)
J/ApJ/923/215 : MORA: ALMA 2mm survey (Casey+, 2021)
J/MNRAS/508/1206 : Galaxy clusters redshifts with VLT/MUSE (Jauzac+, 2021)
J/ApJ/921/40 : FIR of SFGs in GOODS-N & COSMOS fields (Kokorev+, 2021)
J/A+A/646/A83 : 12 massive lensing clusters MUSE obs. (Richard+, 2021)
J/MNRAS/515/3126 : REBELS. Dust Continuum Detections at z>6.5 (Inami+, 2022)
J/A+A/685/A1 : A3COSMOS & A3GOODSS Data Version 20220606 (Adscheid+, 2024)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Prog HST treasury program identifier (1)
8- 14 A7 --- Cluster Cluster identifier
(as in Sun+ 2022, J/ApJ/932/77)
16- 19 F4.2 arcmin2 Area [1/9.3] Sky area observed in ALCS within
the relative sensitivity above 30% to the
deepest part of the mosaic
21- 29 A9 arcsec Beam FWHM of the synthesized beam in the
natural-weighted map
31- 32 I2 uJy/beam sigcont [40/92] Data depth evaluated by the
standard deviation of the pixel with the
CASA task IMSTAT with the by weight
algorithm; σ(cont)
34- 37 I4 uJy/beam sig1 [673/1397] Data depth for the 60km/s width
cube obtained in the frequency setup with
the central sky frequency at 259.4GHz;
σ(cube,tune1)
39- 42 I4 uJy/beam sig2 [643/1706] Data depth for the cube with the
central sky frequency at 263.2GHz;
σ(cube,tune2)
44- 45 I2 --- N [1/20] Number of continuum sources
identified
--------------------------------------------------------------------------------
Note (1): HST treasury programs as follows:
HFF = Hubble Frontier Fields
CLASH = the Cluster Lensing and Supernova Survey with Hubble
RELICS = the Reionization Lensing Cluster Survey
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table12.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Set Catalog set (G1)
7- 13 A7 --- Cluster Cluster identifier as in Table 1
14 A1 --- --- [-]
15- 18 A4 --- ID Continuum source identifier within Cluster
(CNNN)
20- 30 F11.7 deg RAdeg [3.5/348] Right ascension (J2000) (1)
32- 42 F11.7 deg DEdeg [-74/24.5] Declination (J2000) (1)
44- 47 F4.1 --- S/N [4/92] Signal-to-noise ratio of the peak
pixel in the natural-weighted map before
primary beam correction
49- 52 F4.1 --- e_S/N [2/78.4] S/N uncertainty
54- 57 F4.2 --- PBeam [0.3/1] Primary beam sensitivity in the
mosaic map
59- 62 F4.2 mJy/beam Snat [0.2/7] Source flux density at 1.2mm
measured by the peak pixel count in the
natural-weighted map
64- 67 F4.2 mJy/beam e_Snat [0.04/0.3] Snat uncertainty
69- 72 F4.2 mJy/beam Stap [0.18/8.3] Source flux density at 1.2mm
measured by the peak pixel count in the
uv-tapered (2"x2") map
74- 77 F4.2 mJy/beam e_Stap [0.06/0.4] Stap uncertainty
79- 83 F5.2 mJy Sap [-0.15/9.5] Source flux density at 1.2mm
measured by a 2.0" radius aperture in the
natural-weighted map
85- 88 F4.2 mJy e_Sap [0.06/0.4] Sap uncertainty
90- 93 F4.2 mJy Simf [0.16/9]? Source flux density at 1.2mm
measured by 2D elliptical Gaussian fitting
with CASA IMFIT
95- 98 F4.2 mJy e_Simf [0.05/0.6]? Simf uncertainty
100-101 I2 --- Flag [-2/2]? Flag of the IMFIT output (2)
--------------------------------------------------------------------------------
Note (1): Source coordinate of the continuum peak in the natural-weighted map.
Note (2): Flag as follows:
0 = point source (29 occurrences)
1 = marginally resolved (34 occurrences)
2 = fully resolved (109 occurrences)
-1 = fitting error (3 occurrences)
-2 = near the edge of the map (5 occurrences)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table13.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Set Catalog set (G1)
7- 13 A7 --- Cluster Cluster identifier as in Table 1
14 A1 --- --- [-]
15- 18 A4 --- ID Continuum source identifier within Cluster
(CNNN)
20- 24 F5.3 --- zspec [0.18/6.1]? Spectroscopic redshift;
see Section 3.5
26 A1 --- l_zphot [>(] Limit flag on zphot
28- 31 F4.2 --- zphot [0.1/9.62]? Photometric redshift;
see Section 3.5
33- 36 F4.2 --- e_zphot [0/3.4]? Lower uncertainty on zphot
38- 41 F4.2 --- E_zphot [0/2.8]? Upper uncertainty on zphot
43- 46 F4.2 mJy Sobs [0.18/7.8] Observed flux density (3)
48- 51 F4.2 mJy e_Sobs [0.05/0.4] Sobs uncertainty (3)
53- 57 F5.2 Lsun LIR [10.3/13.7] Infrared luminosity estimated by
our SED fitting; see Section 6.1
59- 62 F4.2 Lsun e_LIR [0/0.7] LIR uncertainty
64- 67 F4.1 --- mu [0.2/69.8] Magnification factor based on our
fiducial lens model
69- 72 F4.1 --- e_mu [0/69]? Lower uncertainty on mu (4)
74- 77 F4.1 --- E_mu [0/79]? Upper uncertainty on mu (4)
79 I1 --- f_z [1/5] Redshift category (5)
81- 95 A15 --- Ref Reference (6)
97-135 A39 --- Note Note
--------------------------------------------------------------------------------
Note (3): Observed flux density, including the primary beam correction and
systematic offsets through the MC simulations (Section 3.3), but
without the lens correction. The errors in the flux measurement and
corrections are propagated. For the multiple-image system, we show an
observed flux density calculated by multiplying the average values of
the intrinsic flux densities and magnifications.
Note (4): The error is evaluated from the propagation of the redshift
uncertainty, and the systematic uncertainty from different lens models
(Section 3.6).
Note (5): Redshift category as follows:
1 = zspec;
2 = zphot + multiple images used in the construction of the lens model;
3 = zphot with eazy;
4 = zphot with the composite SED from 707 dusty galaxies in AS2UDS for
the sources without HST counterparts/data (Appendix B);
5 = z=3.0±2.0 assumed for four sources with no counterparts in all bands
other than ALMA; limit flag l_zphot set to "(".
Note (6): Reference as follows:
B13 = Biviano et al. 2013A&A...558A...1B 2013A&A...558A...1B
C21 = Caputi et al. 2021ApJ...908..146C 2021ApJ...908..146C
Ca19 = Caminha et al. 2019, J/A+A/632/A36
Ce18 = Cerny et al. 2018ApJ...859..159C 2018ApJ...859..159C
D17 = Dessauges-Zavadsky et al. 2017A&A...605A..81D 2017A&A...605A..81D
E09 = Ebeling et al. 2009, J/MNRAS/395/1213
E17 = Ebeling et al. 2017MNRAS.471.3305E 2017MNRAS.471.3305E
F21 = Fujimoto et al. 2021ApJ...911...99F 2021ApJ...911...99F
G12 = Gomez et al. 2012AJ....144...79G 2012AJ....144...79G
K22 = Kokorev et al. 2022ApJS..263...38K 2022ApJS..263...38K
L21 = Laporte et al. 2021MNRAS.505.4838L 2021MNRAS.505.4838L
R21 = Richard et al. 2021, J/A+A/646/A83
MA22 = Munoz Arancibia et al. 2023A&A...675A..85M 2023A&A...675A..85M
S04 = Sand et al. 2004ApJ...604...88S 2004ApJ...604...88S
S14 = Schmidt et al. 2014ApJ...782L..36S 2014ApJ...782L..36S
S99 = Soucail et al. 1999A&A...343L..70S 1999A&A...343L..70S
T15 = Treu et al. 2015, J/ApJ/812/114
W15 = Wang et al. 2015, J/ApJ/811/29
W12 = Wold et al. 2012, J/ApJS/202/2
Appendix A = This work
Appendix B = This work
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Global notes:
Note (G1): Catalog as follows:
Blind = Blind catalog (N=144) with purity of p>0.99; see Section 3.1.
Prior = Spitzer/IRAC channel 2 maps prior catalog (N=40); see Section 3.2.
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History:
From electronic version of the journal
* 28-May-2025: Insert into VizieR (Emmanuelle Perret)
* 05-Jun-2025: 4 sources added in Table 12 for R2211 cluster;
update sent by the author
* 17-Jul-2025: 4 sources removed in Table 12 for M0429 and R0949
(were in fact the sources for R2211)
Acknowledgements:
Seiji Fujimoto [fujimoto at utexas.edu]
(End) Emmanuelle Perret [CDS] 28-Mar-2025