ALMA 26 arcmin2 survey of GOODS-S
at 1 mm (ASAGAO):
Physical properties of ALMA-selected galaxies
Yamaguchi et al. 2018, submitted to ApJ

Workshop on Galaxy Evolution 2018 @ Ehime Univ.
2018/06/07 (Thu.)
Institute of Astronomy, The University of Tokyo (D3)
Yuki Yamaguchi

1Outline• Introduction- The evolution of the cosmic SFRD
ü The role of deep continuum observations by ALMA

- Previous studies & this studies• Multi-wavelength analysis of ASAGAO continuum
sources- Star formation properties from SED fitting- What is the difference between ALMA detected andnon-detected sources?
- K-dropout ASAGAO sources?
• The contributions to the cosmic SFRD
• SummaryIntroduction“The evolution of the cosmic SFRD”

2

Red: Dust-obscured star formation

The role of dust-obscured starformation activities
at high-z (z > 3-4)?
How do dusty starburst galaxies
contribute to the SFRD at high-z?

Green: Unobscured star formation

Madau & Dickinson 14

Introduction“The evolution of the cosmic SFRD”

3

Red: Dust-obscured star formation

The role of dust-obscured starformation activities
at high-z (z > 3-4)?
How do dusty starburst galaxies
contribute to the SFRD at high-z?
è deep survey by using ALMA

Green: Unobscured star formation

Madau & Dickinson 14

4Introduction “Previous studies”• Deep continuum observations by ALMA
- ALESS (Hodge+13, da Cunha+15, etc…)- SXDF-ALMA 2 arcmin2 survey (Tadaki+15,Hatsukade+15, Yamaguchi+16, etc…)- ASPEC (Aravena+16, Walter+16)- ALMA deep observation in the HUDF (Dunlop+17)
Follow-up observation of single-dish selected sources
orSmall observation area (~ a few arcmin2)

è Large and deep unbiased survey using ALMA!

5Introduction “ASAGAO”• ALMA twenty-Six Arcmin2 survey of Goods-south At
One-millimeter (ASAGAO)- ALMA Cycle 3 program (PI: K. Kohno)- Band 6 (λobs ~1.2 mm), 26 arcmin2- # of antenna: 38-45- Maximum baseline: ~ 1800 m
ü 0’’.21 ×0’’.17- Sensitivity: rms ~ 38 μJy/beam

Wikipedia

6Introduction “ASAGAO”• ALMA twenty-Six Arcmin2 survey of Goods-south At
One-millimeter (ASAGAO)- ALMA Cycle 3 program (PI: K. Kohno)- Band 6 (λobs ~1.2 mm), 26 arcmin2- # of antenna: 38-45- Maximum baseline: ~ 1800 m
ü 0’’.21 ×0’’.17- Sensitivity: rms ~ 38 μJy/beam7Introduction “ASAGAO”• ALMA twenty-Six Arcmin2 survey of Goods-south At
One-millimeter (ASAGAO)- ASAGAO final map (250 kλ-tapered)ü ASAGAO + Dunlop + Elbaz data
ü Synthesized beam: 0’’.59 × 0’’.45
ü Typical noise: ~ 30-70 μJy/beam
ASAGAOElbazDunlop

Hatsukade+ submitted

8Introduction “ASAGAO”• ALMA twenty-Six Arcmin2 survey of Goods-south At
One-millimeter (ASAGAO)- ASAGAO final map (250 kλ-tapered)ü ASAGAO + Dunlop + Elbaz data
ü Synthesized beam: 0’’.59 × 0’’.45
ü Typical noise: ~ 30-70 μJy/beam

598 candidates with S/N > 3.5

9Multi-wavelength analysis“Counterpart identification”• Multi-wavelength counterpart identification based on
ZFOURGE survey- K-band selected source catalog (Straatman+16)
ü 40 photometry data from U-band to IRAC 8μm- Multi-wavelength counterpart with rsearch < 0.5’’ (p = 0.03)
ü Some extended sources at K-band are included- There are 66 sources have K-band counterpart with
redshift (photo-z or spec-z)

Straatman+16

10Multi-wavelength analysis“Counterpart identification”
JVLA
VLA
IRAC
IRAC
HST
1.2 mm
6 GHz
Ksbasedband on4.5 μm identification• ALMA
Multi-wavelengthcounterpart
F160W
3.6 μmZFOURGE survey- K-band selected source catalog (Straatman+16)
ü 40 photometry data from U-band to IRAC 8μm- Multi-wavelength counterpart with rsearch < 0.5’’ (p = 0.03)
ü Some extended sources at K-band are included- There are 66 sources have multi-wavelengthcounterpart with redshift (photo-z or spec-z)

Straatman+16

Multi-wavelength analysis“Observed flux densities at 1.2 mm”
25

N (S1.2 mm)

2015This work
da Cunha+15
Dunlop+17
Franco+18
Aravena+16

11ALESS sources※(Sub-)mm bright“Classical” SMGs

(Sub-)mm faint“Faint” SMGs

105010 1100
S1.2 mm [mJy]※ Follow-up observation ofSingle dish selected SMGs

Multi-wavelength analysis“Observed flux densities at 1.2 mm”
25N (S1.2 mm)

2015This workda Cunha+15
Dunlop+17
Franco+18
Aravena+16

12

ALESS sources※(Sub-)mm bright“Classical” SMGs

(Sub-)mm faint“Faint” SMGs

10ASAGAO
provides the largest samples
5with the flux range of S1.2 mm < 0.6 mJy
010 1

100
S1.2 mm [mJy]※ Follow-up observation ofSingle dish selected SMGs

13

Multi-wavelength analysis“Redshift distribution”

Normalized N (z)0.4zmed = 1.77 ± 0.23
- Consistent with Dunlop+17
Ø zmed ~ 2.04 ± 0.29
- Lower than da Cunha+15
Ø zmed ~ 2.83 ± 0.22

0.3This workda Cunha+15
Dunlop+17
Straatman+160.2

0.1

0.0

0123Redshift

456

14

Multi-wavelength analysis“Redshift distribution”

Normalized N (z)0.40.3

zmed = 1.77 ± 0.23
- Consistent with Dunlop+17
Ø zmed ~ 2.04 ± 0.29
- Lower than da Cunha+15
Ø zmed ~ 2.83 ± 0.22

This work
da Cunha+15
Dunlop+17
Straatman+16

0.2

0.1

0.0
Faint sources0 tend to1 have lower
redshift
thanSMGs
2
3
4 “classical”
56Redshift function (Koprowski+17)èThe redshift evolution of IR luminosity

Multi-wavelength analysis“SED fitting using MAGPHYS”• SED fitting from optical to mm using MAGPHYS(da Cunha+08,15)
ID3.05Flux density [µJy]

10SPIRE

Stellar mass
104 IR luminosity
UV luminosity
103

PACS
ALMAMIPS

102
101

ZFOURGE100
10 1IRAC

Note: SPIRE de-blended flux isprovided by Wang, T.

100

101
obs [µm]

102

103

15

16

Multi-wavelength analysis“SED fitting using MAGPHYS”

102
101
10100

Flux density [µJy]

104
103
102
101
10100

Flux density [µJy]104103102101101001100
101102103
Observed wavelength [µm]101100103102
101
100104103102101101001100
101102103
Observed wavelength [µm]ID7flag = 1103
102
101010104
103
102
101010104
103
210101010101100
101
102103Observed wavelength [µm]Flux density [µJy]

Flux density [µJy]

100
1100
101
102
103
Observed wavelength [µm]

104

ID8
flag = 1

103
102
101
100
1100
101
102
103
Observed wavelength [µm]

104

ID12
flag = 1

103
102
101
100
10100
101102103
Observed wavelength [µm]ID15flag = 1

1011051105

10210100101102103
Observed wavelength [µm]ID4flag = 1103

105

1ID11flag = 1

104

10100
101
102
103
Observed wavelength [µm]

104

10100
101102103
Observed wavelength [µm]ID14flag = 1

1105

1105

1010100
101102103
Observed wavelength [µm]ID10flag = 10105

1104

10100
101
102
103
Observed wavelength [µm]ID13flag = 1102

105

1105

103

10100
101
102
103
Observed wavelength [µm]ID9flag = 1104

ID6
flag = 1101

10100
101102103
Observed wavelength [µm]

105

1105

1102

Flux density [µJy]

103

0103

105

Flux density [µJy]

Flux density [µJy]

104

ID5
flag = 1

1010100
101102103
Observed wavelength [µm]

105

101

104

ID3
flag = 1

1100
101102103
Observed wavelength [µm]105Flux density [µJy]1

Flux density [µJy]10

Flux density [µJy]

100

102

Flux density [µJy]

101

103

105

Flux density [µJy]

102

104

ID2
flag = 1

Flux density [µJy]

103

105

Flux density [µJy]

104

ID1
flag = 1

Flux density [µJy]

Flux density [µJy]

105

104

ID16
flag = 1103102101100101100
101
102
103
Observed wavelength [µm]Multi-wavelength analysis“SED fitting using MAGPHYS”• SED fitting from optical to mm using MAGPHYS(da Cunha+08,15)
ID3.0
5

Flux density [µJy]

10SPIRE

Stellar mass
104 IR luminosity
UV luminosity
103

PACS
ALMAMIPS

102
101

ZFOURGE

offset ~ 0.3-0.6 dex

100
10 1IRAC

Note: SPIRE de-blended flux isprovided by Wang, T.

100

101
obs [µm]

102

103

17

18

Multi-wavelength analysis“M★ vs. SFR”
Schreiber+15
ZFOURGEALESSASPECS
Yamaguchi+16Dunlop+17
This work (flag = 1)

log(SFRUV+IR [M /yr])

32z  1.5

1.5 < z  2.5

2.5 < z  5.0

ALESSALMAnon-detected

1ASAGAO
078910log(M⇤/M )111278910log(M⇤/M )111278910log(M⇤/M )11• ASAGAO continuum sources (red symbols)- Mainly high-mass end of the main sequence of starformation galaxies- Consistent with previous results of faint SMGs (e.g.,Dunlop+17)
ü Systematical lower SFRs than “classical” SMGs (ALESS)

12

19

Multi-wavelength analysis“M★ vs. SFR”
Schreiber+15
ZFOURGEALESSASPECS
Yamaguchi+16
Dunlop+17This work (flag = 1)

log(SFRUV+IR [M /yr])

32z  1.5

1.5 < z  2.5

2.5 < z  5.0

ALESS
ALMA
non-detected

1ASAGAO
078910log(M⇤/M )111278910log(M⇤/M )111278910log(M⇤/M )11• ASAGAO continuum sources (red symbols)- Mainly high-mass end of the main sequence of stargalaxies
Whatformationis the difference
between ALMA detectedwith previous
results of faint SMGs (e.g.,
and- Consistentnon-detectedsources?
Dunlop+17)
ü Systematical lower SFRs than “classical” SMGs (ALESS)

12

20

Multi-wavelength analysis“What is the difference? (IRX-M★)”
5ZFOURGE
Bouwens+16
ALESS
Dunlop+17This worklog(LIR/LUV )4z  1.5

1.5 < z  2.5

2.5 < z  5.0

3UV-selectedsources

210

78910log(M⇤/M )111278910log(M⇤/M )111278910log(M⇤/M )• IRX-M★ relation- ALMA detected sources show systematic offset
from IRX-M★ relation of UV-selected sources
obtained by Bouwens+16 (especially z > 1.5)

1112

21

Multi-wavelength analysis“What is the difference (IRX-SFR)?”z  1.5

5

ZFOURGE
ALESS
Dunlop+17This work (flag = 1)4log(LIR/LUV )1.5 < z  2.5

2.5 < z  5.0

3210012log(SFR[M yr 1])

3012log(SFR[M yr 1])

3012log(SFR[M yr 1])• IRX-SFR relation- ALMA detected sources show systematic offset
from ZFOURGE sources (especially z > 1.5)èIRX seems to be one of the key parameters?

3

Multi-wavelength analysis“What is difference (IRX-βUV)?”z  1.5

5Meurer+99
Takeuchi+12ZFOURGEThis work (flag = 1)4log(LIR/LUV )1.5 < z  2.5

22

2.5 < z  5.0

3
2
10

4

20
UV

420UV

420UV

• Offset from the relation of local starburst galaxies- Dust compositions, size distribution, or/and spatial
distribution are different (Safarzadeh+17)?
• More observation (e.g., higher resolution) is needed!

Multi-wavelength analysis“K-dropout ASAGAO sources”• We find that 5 ASAGAO sources with S/N > 5 has
no K-band counterpart

Nsources(>S/N)

Positive
Negative
102

101

100
3.5

4.0

4.5

5.0

5.5

S/N

There is only one negative
detection with S/N < -5.0.

6.0

23

24

Multi-wavelength analysis“K-dropout ASAGAO sources”• High-z dust-obscured galaxies (z > 4-5) ?
- SFR ~ 100 M⦿ /yr- M★ ~ 109.5-11 M ⦿?
• Early phase of massive
galaxy formation?
- e.g., Wang+16• Explored only by
ALMA contiguoussurvey!

log(LIR/L ⦿) ~ 12log(M★/M ⦿) ~ 9-10

25Multi-wavelength analysis“K-dropout ASAGAO sources”
Flux density [µJy]104

ALMA band 7(Cowie+18)- SFR ~ 100 M⦿ /yr103- M★ ~ 109.5-11 M ⦿?

102log(LIR/L ⦿) ~ 12log(M★/M ⦿) ~ 9-10

10110010 1
10

Flux density [µJy]

ASAGAO ID20
at ASAGAO• High-z dust-obscured
galaxiesDetected(z > 4-5)? ID22ASAGAO ID174• Early phase of massive
galaxy formation?
- e.g., Wang+16 ASAGAO ID25

ASAGAO ID24

100

101
102103104105Observed wavelength [µm]103

• Explored only by
10
ALMA contiguous
10survey!

z > 4-521

Arp220 @ z = 2.0
Arp220 @ z = 3.0
Arp220 @ z = 4.0
Arp220 @ z = 5.0

100
10 1
100

101
102
103
104
105
Observed wavelength [µm]

100

101
102
103
104
105
Observed wavelength [µm]

26Multi-wavelength analysis“K-dropout ASAGAO sources”• High-z dust-obscured galaxies (z > 4-5) ?
- SFR ~ 100 M⦿ /yr- M★ ~ 109.5-11 M ⦿?
• Early phase of massive
galaxy formation?
- e.g., Wang+16• Explored only by
ALMA contiguoussurvey!

log(LIR/L ⦿) ~ 12log(M★/M ⦿) ~ 9-10

27

The contributions to the cosmic SFRD
• The contribution of ASAGAO sources with K-band
counterparts to the cosmic SFRD
Madau & Dickinson 2014
SFRDtotal (Burgarella+13)
SFRDUV (Burgarella+13)⇢SFR [M yr 1 Mpc 3 ]10 1

SFRDIR (Burgarella+13)
Bouwens+15 (uncorrected)
Bouwens+15 (corrected)
Rowan-Robinson+16

10

Dunlop+17

2

ZFOURGE (ASAGAO field)

IR SFRD

This Work(w/ K-band counterparts)

ASAGAO sources are
not main contributor
10 30123Redshift

4ZFOURGE + ASAGAO

5We resolve
dust-obscured
star-formation atlog (LIR/L⦿) ~ 10-11

28

The contributions to the cosmic SFRD
• The contribution of ASAGAO sources with K-band
counterparts to the cosmic SFRD
Madau & Dickinson 2014
SFRDtotal (Burgarella+13)
SFRDUV (Burgarella+13)⇢SFR [M yr 1 Mpc 3 ]10 1

SFRDIR (Burgarella+13)
Bouwens+15 (uncorrected)
Bouwens+15 (corrected)

102

ASAGAO sources arecomparable with IR SFRD

Rowan-Robinson+16
Dunlop+17
ZFOURGE (ASAGAO field)
This Work(w/ K-band counterparts)
ZFOURGE + ASAGAO

10 30123Redshift45

We resolve
dust-obscured
star-formation atlog (LIR/L⦿) ~ 10-11

29

The contributions to the cosmic SFRD
• The contribution of ASAGAO sources without K-bandcounterparts to the cosmic SFRD
Madau & Dickinson 2014
SFRDtotal (Burgarella+13)⇢SFR [M yr 1 Mpc 3 ]10 1

SFRDUV (Burgarella+13)
SFRDIR (Burgarella+13)
Bouwens+15 (uncorrected)
Bouwens+15 (corrected)
Rowan-Robinson+16102

Dunlop+17
ZFOURGE (ASAGAO field)
This Work(w/ K-band counterparts)
ZFOURGE + ASAGAOThis Work(w/o K-band counterparts)

10 3123
45
Their0contributions
areconsistentwithUV-selectedgalaxies?
Redshift

Multi-wavelength analysis“Summary”• Multi-wavelength counterparts of ASAGAO sources- 66 sources with K-band-selected counterparts(zmed = 1.77)- Mainly high-mass end of the main sequence of starformation galaxy- ALMA detected sources have larger IRX than ALMA
non-detected sourcesü Dust composition, size distribution or/and spatial distribution isdifferent?

• ASAGAO sources are main contributors to the cosmic
SFRD at z > 2.
• Five K-dropout ASAGAO sources (S/N > 5)
- Important contributors to the cosmic SFRD

30