ALMA observa,ons of Lyman alpha blobs at z=3.1 Yuichi Matsuda - - PowerPoint PPT Presentation

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ALMA observa,ons of Lyman alpha blobs at z=3.1 Yuichi Matsuda - - PowerPoint PPT Presentation

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ALMA observa,ons of Lyman alpha blobs at z=3.1 Yuichi Matsuda (NAOJ) Lyman alpha blobs (LABs) Dura%on %me-scale~0.1Gyr (1% of Cosmic %me)? Cosmic cherry blossoms (3 days per year 1%)? NB Ly ! emitter Erb+11 Steidel+00 6 Continuum !

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SLIDE 1

ALMA observa,ons

  • f Lyman alpha blobs

at z=3.1

Yuichi Matsuda (NAOJ)

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SLIDE 2

Lyman alpha blobs (LABs)

  • Dura%on %me-scale~0.1Gyr (1% of Cosmic %me)?
  • Cosmic cherry blossoms (3 days per year – 1%)?

!6 !4 !2 2 4 6 !6 !4 !2 2 4 6 Comoving Mpc Comoving Mpc BLOB 6 BLOB 5 BLOB 4 BLOB 3 BLOB 2 BLOB 1 NB Ly! emitter Continuum!selected z=2.3

Steidel+00 Matsuda+04 Hayes+11

Erb+11

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SLIDE 3

Summary

  • Lya halo is ubiquitous
  • ALMA started to detect dusty sources in LABs
  • One ALMA source in a filamentary LAB may

be in transi,on phase from dusty starburst to passive galaxy

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SLIDE 4

Lyman alpha halo is ubiquitous

Lya halo around the Earth

Kameda+17

PROCYON

Earth

Lya halo is x50 bigger than the Earth

Lya halo around distant galaxies

Steidel+00 Matsuda+04 Hayes+11

Lya halo is x50 bigger than galaxies

Size difference is 1013

300 kpc

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SLIDE 5

ALMA observa,ons of LABs

LAB02

ALMA Band 7 FoV

100 kpc

LAB01

ALMA Band 7 FoV ALMA Band 7 FoV

LAB18

ALMA Band 7 FoV

100 kpc

LAB05

Ø ALMA Band 8 [CII] (Umehata+17) Ø ALMA Band 7 cont + [NII] (Geach+16, Umehata+17, Ao+17, Matsuda+ in prep) Ø ALMA Band 3 cont + CO(4-3) (Kato+ in prep)

3 1

Lya

0.5 0.3

rms=74microJy/beam 1" Taper

2

LAB01

Lya

0.5 0.3

rms=74microJy/beam 1" Taper

1

LAB02

Lya

0.5 0.3

rms=75microJy/beam 1" Taper

1

LAB05

Lya

0.5 0.3

rms=75microJy/beam 1" Taper

4 1 2 3

LAB18

~0.5mJy ~1mJy ~2mJy ~1-4mJy

See also Yiping Ao’s poster

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SLIDE 6

Filamentary LAB at z=3.1 (LAB18)

30 kpc 30 kpc 30 kpc Subaru Lyα HST rest 1985Å Subaru rest 1575Å

b a c d

cyan=850 μm dust

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SLIDE 7

ALMA deep 3mm observations 5 hrs on-source (PI: Yuta Kato)

30 kpc 30 kpc 30 kpc

rest 660μm rest 740μm CO J=4-3 b a c d

Lyα

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SLIDE 8

Ø LIR(8-1000μm) = (2.7 ± 0.4)×1012 Lo (Td=32.5 ± 0.6 K、β=2.3 ± 0.1)

0.5 1 1.5 2 2.5 3 3.5 10 20 30 40 50 60

Temperature [K]

LAB18.b

β

z<0.006 logLFIR (Lo) =8-11 z<0.04 LIRGs
 z<0.5 LIRGs z<0.3 ULIRGs

LAB18.b

Temperature [K]

βISM =1.8

large dust emissivity index β=2.3

transi,on phase from dusty starburst to passive galaxy?

ULIRGs

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SLIDE 9

Short gas depletion time τdep=16Myr

Herschel/SPIRE 250,350,500μm (Kato et al. 2016)

LAB18.b
 CO J=4-3 Ø Mgas = (4.4 ± 0.3) × 109 Mo (r41 = 0.41, α=0.8) Ø SFR = 273 ± 35 Mo/yr τdep = Mgas/SFR = 16 ± 2 Myr

11 12 13 8 9 10 11

log LFIR(8-1000um) [Lo] log L’CO(4-3) [K km s-1 pc2]

Greve et al. (2014) LAB18.b z<0.1 (U)LIRGs z>1 DSFGs z>1 lensed DSFGs

LAB18.b

(τ= 100 Myr) (τ= 16 Myr) . (τ= 200 Myr)

zCO=3.093±0.001 (zLyα=3.104)

transi,on phase from dusty starburst to passive galaxy?

SMGs ULIRGs LIRGs

  • 0.15
  • 0.1
  • 0.05

0.05 0.1 0.15 0.2 112 112.2 112.4 112.6 112.8 113 113.2

  • 1000
  • 500

500 1000 1500

Flux Density [mJy/beam] Frequency (Obs) [GHz] Velocity [km/s]

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SLIDE 10

Summary

  • Lya halo is ubiquitous
  • ALMA started to detect dusty sources in LABs
  • One ALMA source in a filamentary LAB may

be in transi,on phase from dusty starburst to passive galaxy

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SLIDE 11

β reflects dust chemical composition

(κ850 = 0.4-8 cm2 g-1) (κ850 ~0.4 cm2 g-1) Mg-rich
 amorphous silicate
 (1-x) MgO – x SiO2

β~2 steep
 β>2

Mg1.1Fe0.9SiO4

κd

Demyk et al. (2017)

Mass Absorp%on Coefficient (Opacity) Wavelength

Laboratory experiment