Deep Survey of z=7 Lyα Emitters with the new red-sensitive CCDs on Subaru / Suprime-Cam
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Deep Survey of z=7 Lyα Emitters with the new red-sensitive CCDs on Subaru / Suprime-Cam. Kazuaki Ota Cosmic Radiation Laboratory RIKEN M. Iye, N. Kashikawa (NAOJ), M. Ouchi (Carnegie), K. Shimasaku (Univ. of Tokyo), T. Totani (Kyoto Univ.), M.A.R. Kobayashi, T. Morokuma (NAOJ),

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Deep Survey of z=7 Lyα Emitters with the new red-sensitive CCDs on Subaru / Suprime-Cam

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Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

Deep Survey of z=7 Lyα Emitters with the new red-sensitive CCDs on Subaru / Suprime-Cam

Kazuaki OtaCosmic Radiation LaboratoryRIKEN

M. Iye, N. Kashikawa (NAOJ), M. Ouchi (Carnegie),

K. Shimasaku (Univ. of Tokyo), T. Totani (Kyoto Univ.),

M.A.R. Kobayashi, T. Morokuma (NAOJ),

M. Nagashima (Nagasaki Univ.),

H. Furusawa, T. Hattori (SubaruTelescope),

N. Kodaka, A. Harayama (Saitama Univ.)

Reionization @ Ringberg


Outline

Outline

I. Background & Motivation

(1) Reionization probed by Lyα emitters at z ≿ 6

(2) Weaknesses in the previous z=7 Lyα emitter survey

II. Solution:

- New deeper z=7 survey in SXDS Field

III. Result:

- Deeper Lyα LF and Constraint on XHI

IV. Conclusion


Outline1

Outline

I. Background & Motivation

(1) Reionization probed by Lyα emitters at z ≿ 6

(2) Weaknesses in the previous z=7 Lyα emitter survey

II. Solution:

- New deeper z=7 survey in SXDS Field

III. Result:

- Deeper Lyα LF and Constraint on XHI

IV. Conclusion


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

Neutral Fraction vs Redshift

Neutral Fraction XHI

z=6.3, 6.7

z=7z=6.6Lyα Emitters

Redshift z

Fan et al.2006


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

Reionization Probed by Lyα emitters: Lyα LF

LyαLFdeclines.

Number & Lyα luminosity

density decrease.

n(z=6.6)/n(z=5.7)=0.24

n(z=7.0)/n(z=6.6)=0.17

to L(Lya) > 1043 erg/s

Subaru Deep Field

Project

Subaru Telescope

Suprime-Cam


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

3 weakneses in the previous z=7 survey

(1) Depth was shallow.

(2) Sample is small.

(3) Only one sky field was surveyed.

Subaru Deep Field876 arcmin2

L(Lyα) > 1043 erg/s

Only 1 Lyα emitter


Outline2

Outline

I. Background & Motivation

(1) Reionization probed by Lyα emitters at z ≿ 6

(2) Weaknesses in the previous z=7 Lyα emitter survey

II. Solution:

- New deeper z=7 survey in SXDS Field

III. Result:

- Deeper Lyα LF and Constraint on XHI

IV. Conclusion


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

New fully depleted CCDs on Subaru / Suprime-CamMore sensitive to 0.9 – 1 μm light

Transmission, QE, flux

Wavelenght (A)

>2 x more sensitive to z=7 Lyα


S ubaru x mm newton d eep s urvey field sxds

Target Sky Region

Subaru/XMM-NewtonDeep Survey Field(SXDS)

Spitzer

13 hours imagingNB973 = 25.4 (5σ)(previously, 24.9)

UKIDSS-UDS

Oct, Nov 2008SubaruThis Work


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

Narrowband filter to detect z=7 Lyα emitters

Filter Response

z=7Lyα

NB973

Wavelength(Å)

λc=9755Å⊿λ=200Å


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

New z=7 Lyα emitter candidates

B V R i’ NB816 z’ NB921 NB973

No detection (< 3σ)

NB973 ≤ 25.4 (5σ)

Equivalently, z’ – NB973 > 1

~


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

Color Selection

Visual Inspection

10z=7 Lyα emittercandidates

(tentative)

Remove spurious

& transient objects

using images taken

in different months

#Candidates ≤ 10


Outline3

Outline

I. Background & Motivation

(1) Reionization probed by Lyα emitters at z ≿ 6

(2) Weaknesses in the previous z=7 Lyα emitter survey

II. Solution:

- New deeper z=7 survey in SXDS Field

III. Result:

- Deeper Lyα LF and Constraint on XHI

IV. Conclusion


Neutral fraction z 7 0 49

Lyα Luminosity FunctionAssumption (1): F(Lyα) = F(NB filter)

Neutral Fractionz=7.0~49%

■△ z=5.7

●▲ z=6.6

◆ z=7.0

xHI=0.0

Observed DensitiesnLyα: 3.9x10-5 Mpc-3

ρLyα: 4.7x1038 erg/s/Mpc-3

xHI=0.4

xHI=0.6

Predicted Densities

when xHI=0(Kobayashi et al. 2007

LAE evolution Model)nLyα: 1.1x10-4 Mpc-3

ρLyα: 9.5x1038 erg/s/Mpc-3

Attenuated Schechter LFs(Santos 2004)

>6x1042 erg/s


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

Fraction of Lyα flux in NB filter flux

F(Lyα) ~ 0.7 x F(NB973)

NB973 Filter Total Flux

Spectrum

F(Lyα)

70%

F(Lyα)

30%

F(UV)

F(NB973)= F(Lya) + F(UV)


Neutral fraction z 7 0 66

Lyα Luminosity Function: Assumption (2): F(Lyα) = 0.7 x F(NB973)

Neutral Fractionz=7.0~66%

■△ z=5.7

●▲ z=6.6

◆ z=7.0

xHI=0.0

Observed DensitiesnLyα: 3.9x10-5 Mpc-3

ρLyα: 4.7x1038 erg/s/Mpc-3

xHI=0.4

xHI=0.6

Predicted Densities

when xHI=0(Kobayashi et al. 2007

LAE evolution Model)nLyα: 1.8x10-4 Mpc-3

ρLyα: 1.2x1039 erg/s/Mpc-3

Attenuated Schechter LFs(Santos 2004)

>4.2x1042 erg/s


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

Neutral Fraction vs Redshift

Neutral Fraction XHI

z=6.3, 6.7

z=7z=6.6Lyα Emitters

Redshift z

Fan et al.2006


Outline4

Outline

I. Background & Motivation

(1) Reionization probed by Lyα emitters at z ≿ 6

(2) Weaknesses in the previous z=7 Lyα emitter survey

II. Solution:

- New deeper z=7 survey in SXDS Field

III. Result:

- Deeper Lyα LF and Constraint on XHI

IV. Conclusion


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

Conclusion

Improved statistics & depth, Observed different sky field

(1) Number & Lyα luminosity densities

of Lyα emitters decrease from z=5.7

and 6.6 to z=7.

(2) Neutral Fraction at z=7 is

XHI≿ 0.49 – 0.66.

(3) Reionization seems not to be

complete at z=7.


Deep survey of z 7 ly emitters with the new red sensitive ccds on subaru suprime cam

We are now challenging z=7.3 Lyα

Transmission, QE, flux

Wavelenght (A)

Final survey that can be done by Suprime-Cam + New CCDs


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