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In midinfrared bands, AKARI found zodiacal light is very smooth Fluctua=on can be explained by photon noise (dots) , DGL (black) and faint sources Upper limit of 0.02 % of the sky brightness at the angular scale >100 arcsec, 18μm.

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Page 1: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

In  mid-­‐infrared  bands,  AKARI  found  zodiacal  light  is  very  smooth

Fluctua=on  can  be  explained  by     photon  noise  (dots)  ,     DGL  (black)  and     faint  sources

Upper  limit  of  0.02  %  of  the  sky  brightness  at  the  angular  scale  >100  arcsec,  18µm.

Page 2: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

AKARI  Observa=on  of  the  Fluctua=on    of  the  Near-­‐infrared  Background

Matsumoto,  Toshio

Ins/tute  of  astronomy  and  Astrophysics,  Academia  Sinica,  TaiwanISAS/JAXA

Collaborator:  H.  J.  Seo,  W.-­‐S.  Jeong,  H.  M.  Lee,  S.  Matsuura,  H.  Matsuhara,  S.  Oyabu,  J.  Pyo,  and  T.  Wada    

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Excess  emission  is  significantly  brighter  than  integrated  light  of  faint  galaxies

Pop.III  origin?Redshi]ed  Ly  α?

ProblemTeV  γToo  high  star  forma=on  rate

Uncertainty  of  the  ZL  model?

10

100

0.6 0.8 1 3 5

IRTS

Lavenson & Wright

Arendt & Dwek

Cambrecy

Spitzer, IGL

Bernstein

IGL, Maday & Pozetti

IGL, Totani Yoshii

Model IGL, Totani

Surf

ace B

rightn

ess (

W.m

-2.s

r-2)

Wavelength (µm)

Page 4: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

New  observa=on:  Fluctua=on  of  the  sky

Fluctua=on  provides  model  independent  informa=on• IRAS,  COBE,  ISO  tried  to  detect  fluctua/on  of  zodiacal  emission,  

but  only  upper  limits  were  obtained.• Lowest  upper  limit  is  0.2%  of  sky  brightness  at  25  µm  ,  3  arcmin  

scale  (ISO).

Fluctua=on  may  provide  informa=on  on  structure  forma=on  at  pop.III  era

Page 5: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

AKARI:  First  Japanese  Infrared  astronomy  satellite  

70cm  cooled  infrared  telescope    Launch : February 22, 2006Orbit : sun synchronous orbit, 750km altitudeObserva5on  terminated  on  May  2011

Instruments      IRC  (Infrared  Camera)                   512x412  InSb  array  camera,  1.5”/pixel            NIR  imaging  observaDon  at  2.4,  3.2,  and  4.1  µm            low  resoluDon  spectroscopy         256x256  SiAs  array,  2.4”/pixel              MIR  imaging  observa5on  at  7~24  µm            low  resolu5on  spectroscopy      FIS(Far  Infrared  Surveyor)

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• IRAS,  COBE,  ISO  tried  to  detect  fluctua/on  of  zodiacal  emission,  but  only  upper  limits  were  obtained.

• Lowest  upper  limit  is  0.2%  of  sky  brightness  at  25  µm  ,  3  arcmin  scale  (ISO).

How  smooth  zodiacal  light?

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AKARI  observed  fluctua=on  of  mid-­‐IR  sky  (Pyo  et  al.  2012)

Photon  noise DGL Faint  sources

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AKARI  found  mid-­‐infrared  sky  is  very  smooth!

Observed  fluctua/on  can  be  explained  by       Photon  noise     Diffuse  galac/c  light     Faint  sources

Upper  limit  of  fluctua/on  is       0.02%  at  the  angular  scale  >200  arcseof  zodiacal  emission

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Fluctua=on  of  zodiacal  light  must  be  same  as  zodiacal  emissionDistribu=on  of  volume  emissivity  for  zodiacal  light  (2.2  µm,  blue)  and  zodiacal  emission  (12  µm,  red)  towards  NEP

Total

Circumstellar  ringDust  band

Fluctua=on  of  zodiacal  light  is  <  0.02%

Page 10: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

AKARI  NEP  surveyIRC/AKARI  observed     NEP  monitor  field:    ~2  /mes  in  a  month  with  all  filter  bands   NEP  wide  field:     shallow  survey  over  ~2.5  degree  circle  around  

Compared  with  Spitzer• Dark  frame  can  be  well  obtained  with  cold  shu\er• AKARI  has  2  µm  band• Larger  array,  Large  field  of  view,  Single  frame  (monitor  field)• Larger  pixel  scale  (1.49”/1.2”),  bad  PSF

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Fluctua=on  of  the  sky  at  NEP  monitor  field  

 Images  of  good  quality  for  the  NEP  monitor  field  were  stacked,  and  foreground  sources  are  masked.  For  these    maps,  the  fluctua/on  analysis  was  performed.

10  arcmin  x  10  arcmin1.5  arcsec/pixel

Typical  image,  N2

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Stacked  image  is  circular  (600  arcsec  diameter),  since  posi/on  angle  changes  from  season  to  season.

This  process  loses  some  pixels,  but  smears  out  sensi/vity  fluctua/on  between  pixels,  instrument  noise  and  fluctua/on  of  zodiacal  light  if  exists.  

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       Stacked  image  of  the  sky  and  dark  image2.4  µm                                              3.2  µm                                              4.1  µm                      

Page 14: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

Some  results

Filter  band               N2       N3       N4

Wavelength,  µm              2.4          3.2          4.1  

Number  of  stacked  image             40       39       24  

Number  of  remaining  pixels,  %                    39.2                  37.9       34.8  

Limi/ng  magnitude  (AB  mag)       22.8                  23.3         23.9  

Sky  brightness,    nW.m-­‐2.sr-­‐1                            114                  73                105

1  σ  fluctua/on  of  sky,  nW.m-­‐2.sr-­‐1         2.57       1.54           0.86

1  σ  of  dark,  nW.m-­‐2.sr-­‐1               1.69        0.98         0.49    

Page 15: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

Power  spectrum  analysis2-­‐dimensional  Fourier  transform

Fluctua/on

Page 16: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

 Fluctua=on  spectrum2  dimensional  Fourier  transforma/on  was  applied  both  for  image  and  dark  frame.

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Fluctua=on  spectrum  of  the  skyFluctua/on  of  the  dark  image  was  subtracted

Shot  noise  of  faint  galaxies

Page 18: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

Smoothed  sky  image    (angular  resolu=on~50”)

     2.4  µm                                                  3.2  µm                                                  4.1  µm                      

Large  scale  structure  is  clearly  seen!  

Page 19: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

Analysis  of  NEP-­‐Wide  Field  

2.5  degree  scaleConstruct  mosaic  imageStacking:  6  images  (2.4  and  3.2  µm),  4  images  (4.1  µm)  

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Addi=onal  careful  analysis!

l  Seasonal  varia=on  of  zodiacal  light   Subtract  zodiacal  light  with  sinusoidal  fijng

l  Subtrac=on  of  dark  level   Dark  level  was  es=mated  based  on  subsets  difference

l  Sky  matching  with  using  overlapped  sky

l  Muxbleed  problem:  Masked  affected  pixels  

Page 21: AKARI Observation of the Fluctuation of the Near-infrared ...Collaborator:#H.#J.#Seo,#W.’S.#Jeong,#H.#M.#Lee,#S.#Matsuura,# H.#Matsuhara,#S.#Oyabu,#J.#Pyo,#and#T.#Wada## ... Clustering#of#galaxies,#Red#dwarf#galaxies#at#z…

 N2  band  N3  band  N4  band  In

clud

ing  the  

Exclud

ing  the  

Mosaic  image  (the  contribu=on  of  zodiacal  light)

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Remaining  pixel  ra=o:  23.3  %Limi=ng  mag.  21.5  (AB)

Remaining  pixel  ra=o:  22.6  %Limi=ng  mag.  22.0  (AB)  

Remaining  pixel  ra=o:  18.4  %Limi=ng  mag.  22.7  (AB)

Final  images  of  NEP  wide  field

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Fluctua=on  spectra  of  NEP  wide  field

Excess  fluctua=on  was  observed  up  to  degree  scale

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Fluctua=on  spectrum  combined  with  NEP  monitor  fields

Result  of  NEP  wide  field  is  consistent  with  that  of  NEP  monitor  field

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What  is  the  origin  of  large  scale  fluctua=on?

l Zodiacal  lightl Diffuse  galac=c  lightl Clustering  of  galaxies,  Red  dwarf  galaxies  at  z=1~2

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Zodiacal  light  is  very  smooth

MIR  fluctua=on  of  zodiacal  emission  is  <  0.02  %  at  >200  arcsecFluctua=on  of  zodiacal  light  is  same  levelStacking  process  reduces  the  fluctua/on  of  zodiacal  light,  if  it  exists.

                             2.4µm              3.2µm          4.1µm    

Expected  ZL  fluctua=on            <  0.007     <  0.004       <  0.006(nW.m-­‐2.sr-­‐1  )

Observed  excess  fluctua=on                     0.19            0.08            0.051at  >100  arcsec  (nW.m-­‐2.sr-­‐1  )

Observed  fluctua=on  is  much  larger  than  that  of  zodiacal  light!  

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Origin  of  fluctua=on:  Diffuse  Galac=c  Light  (DGL)?DGL  is  sca\ered  star  light  by  interstellar  dust  and  thermal  emission  of  dustDust  column  density  correlates  with  thermal  emission  of  dust

Comparison  with  AKARI  FIS  deep  survey  toward  NEP!

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There  is  no  correla/on  between  AKARI  fluctua/on  and  FIR  emission

Fluctua=on  observed  by  AKARI  is  not  the  galac=c  origin!

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Chary  et  al.  (2008)  claimed  red  dwarf  galaxies  at  z=1~2  are  origin  of  observed  fluctua/on  by  Spitzer

Spectrum  of  red  dwarf  galaxies  is  quite  different  from  the  spectrum  of  observed  fluctua/ng  component.

Red  dwarf  galaxies  can  not  be  the  origin  of  the  observed  fluctua=on

Ordinary  low  redshij  galaxies  have  redder  color!  

-­‐-­‐-­‐-­‐-­‐-­‐-­‐-­‐-­‐-­‐-­‐-­‐-­‐-­‐

Spectrum  of  fluctua/ng  emission  component

Origin  of  fluctua=on:  clustering  of  faint  galaxies?  

10

100

0.6 0.8 1 3 5

IRTS

Lavenson & Wright

Arendt & Dwek

Cambrecy

Spitzer, IGL

Bernstein

IGL, Maday & Pozetti

IGL, Totani Yoshii

Model IGL, Totani

Surf

ace B

rightn

ess (

W.m

-2.s

r-2)

Wavelength (µm)

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Sullivan  et  al.(2007)  es=mated  fluctua=ng  power  due  to  faint  galaxies.

Expected  fluctua=on  of  galaxies  fainter  than  Ks(Vega)>21  mag

0.03  nW.m-­‐2.sr-­‐1        at  l~1000  (600”)

AKARI  observa=on  at  2.4  µm

0.2    nW.m-­‐2.sr-­‐1  

At  the  L  band

Power  observed  by  Spitzer  is    significantly  higher  than  that  due  to  faint  galaxies

Clustering  is  not  the  source  of  the  observed  fluctua=on!  

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Expected  fluctua=ons  of  zodiacal  light,  DGL  and  clustering  of  galaxies  are  significantly  smaller  than  the  observed  fluctua=on.

Most  probable  source  of  fluctua=on  is  pop.III  stars,  and/or  early  popula=on  stars.  

What  implica=on  on  first  stars  AKARI  fluctua=on  provide?

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Spectrum  of  fluctua=ng  component  is  very  blueConsistent  with  Spitzer  resultSpectrum  of  fluctua/ng  component  (average  value  of  power  at  >100  arcsec)Rayleigh  Jeans  like  spectrum  (  ∝ λ-­‐3)

λ-­‐3

AKARI  fluctua=on  is  also  consistent  with  NICMOS/HST  (~0.4  nW.m-­‐2.sr-­‐1  at  1.6µm  )　if  we  take  small  angular  scale  (<85  arcsec)  into  account.

0.02

0.04

0.06

0.08

0.1

0.3

0.5

2 3 4 5

Average Power, 100"-300"

AKARI NEP

Spitzer

[q

2P

2(q

)/2π

]1/2

(w

/m

2/sr)

Wavelength (µm)

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Spectrum  of  large  scale  fluctua/ng  component  is  similar  to  that  of  excess  emission  observed  by  IRTS

1

10

100

0.1

1

2 3 4 5

IRTS excess emission

AKARI average power

IRT

S e

xces

s em

issi

on (

W.m

-2.s

r-1)

AK

AR

I Average pow

er [q2P2(q)/2É

Œ]1/2 (W

.m-2.sr

-1)

Wavelength (µm)

10

100

0.6 0.8 1 3 5

IRTS

Lavenson & Wright

Arendt & Dwek

Cambrecy

Spitzer, IGL

Bernstein

IGL, Maday & Pozetti

IGL, Totani Yoshii

Model IGL, Totani

Surf

ace B

rightn

ess (

W.m

-2.s

r-2)

Wavelength (µm)

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Correla/on  between  wavelength  bands

Slope  :  0.380R=0.67

Slope  :  0.109R=0.62

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SpectrumFernandez  et  al.  (2010)

Observed    λ・Iλ  ～ λ-­‐3

Fernandez  at  al.  　～  λ-­‐2

   but  model  dependent

Emission  source  of  the  fluctua/on  AKARI  detected  is  stars-­‐>  good  correla5on  between  wavelength  bands

Detec/on  of  Redshi]ed  Lyα  is  important

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Implica=on  of  the  observed  fluctua=on  Comparison  with  theory

Cooray,  Bock,  Kea/ng,  Lange  and  Matsumoto     ApJ  606,  611  (2004)       Analy/cal  es/ma/on  of  CNB  fluctua/on   Linear  theory       Biased  star  forma/on  which  traces  dark  ma\er

Fernandez,  Komatsu,  Iliev  and  Shapiro           ApJ  710,  1089  (2010)Fernandez,    Iliev,    Komatsu  and  Shapiro         ApJ  750:20  (2012)   N  body  simula/on,  radia/on  transfer   Non  linear  effect   Halo  mass  ~  108  -­‐  109  solar  mass   IMF     Salpeter,  Larson   pop.III  and  pop.  II  

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Predic=on  by  Cooray  et  al.  2004

Peak  (turn  over)  at  several  tens  arcminutesBiased  star  forma/on  which  traces  dark  ma\er

 

Thick  line         fesc  ~  0Thin  line     fesc  ~  1

2  µmfesc  ~  0

4  µmfesc  ~  0

Model  B   (pessimis/c  model)    Low  bias  factor,  T>5000K    zmin  ~  15 η (star  forma/on  rate)  ~  0.1

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Comparison  with  theory  (Cooray,  private  communica=on)

Turn  over  at  large  angles  is  not  so  clear.  Observa/on  at  few  degree  is  required.  -­‐>MIRIS

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Predic=on  by  Fernandez  et  al.  (2012)  

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EBL  (Integrated  light  of  galaxies)  amounts  to  ~10  nW.m-­‐2.sr-­‐1    at  KLargest  contribu/on  to  EBL  is    17~18  mag.Fainter  galaxies  than  17~18  mag  have  less  contribu/on  to  EBL

SDF  (Maihara  et  al.)　　

Absolute  brightness  of  CNB?    Observed  fluctua/on  is  very  high!

Keenan  et  al.  （2010）

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EBL  due  to  faint  galaxies  and  excess  fluctua=on

          EBL(Keenan  et  al.  2010)     Fluctua=on

AKARI,  2.4  µm         0.7           0.2     nW.m-­‐2.sr-­‐1  

(lim.  mag.  ~23)

NICMOS/HST,  1.6  µm       ~0.04         0.4     nW.m-­‐2.sr-­‐1  

(lim.  mag.  ~28.5)

Sullivan  et  al.    2.2  µm       4           0.1     nW.m-­‐2.sr-­‐1  

(17-­‐19mag)    

Simple  extrapola=on  of  logN/logS  is  difficult  to  explain  observed  fluctua=on

New  component  is  required  at  faint  end

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Fernandez  et  al.    predict    I/ΔI  >  50This  suggests  high  CNB  brightness

ΔI~    0.2  nW.m-­‐2.sr-­‐1  I  >  10  nW.m-­‐2.sr-­‐1  

Consistent  with  excess  emission  observed  with  IRTS  and  COBE

Fluctua=on  measurement  with  AKARI  supports  high  level  of  CNB

10

100

0.6 0.8 1 3 5

IRTS

Lavenson & Wright

Arendt & Dwek

Cambrecy

Spitzer, IGL

Bernstein

IGL, Maday & Pozetti

IGL, Totani Yoshii

Model IGL, Totani

Surf

ace B

rightn

ess (

W.m

-2.s

r-2)

Wavelength (µm)

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Conclusionn AKARI  detected  excess  fluctua/on  at  large  angular  scale,  100  arcsec  ~1.3  degree

n Detected  excess  fluctua/on  is  larger  than  that  of  foreground  emission  sources,  zodiacal  light,  diffuse  galac/c  light  and  clustering  of  low  redshij  galaxies.  

n Excess  fluctua/on  shows  flat  feature,  and  does  not  show  clear  turn  over  at  large  angles.

n  Observed  fluctua/on  is  fairly  high  and  requires  new  faint  sources  at  >  28  mag

n First  star  (pop.III  star)  is  one  of  possible  origins  of  observed  fluctua/on  (10  arcmin  corresponds  30  Mpc  at  z~10).

n Blue  color  of  wavelength  dependence  of  fluctua/on,  and  good  correla/on  between  wavelength  bands  are  consistent  with  model  of  first  stars.


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