EAAGN 2016 mjkimastro1.snu.ac.kr/eaagn/contributions/MKim.pdf · 3. The Origin of Water (Ices) in...
Transcript of EAAGN 2016 mjkimastro1.snu.ac.kr/eaagn/contributions/MKim.pdf · 3. The Origin of Water (Ices) in...
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AGN Science with SPHEREx
Minjin Kim Woong-‐Seob Jeong, KASI SPHEREx team
[Korea Astronomy and Space Science Institute (KASI)]
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Outline
• SPHEREx mission
• AGN science cases with SPHEREx
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SPHEREx mission• Spectro-‐PHotometer for the Extragalactic structure,
Reionization and ices Explorer
• SMEX mission in Phase A (Final selection in Jan. 2017.)
• The first all-sky optical/NIR spectral survey
• wide spectral coverage : 0.75-‐5um, R~40/150
• led by JPL (PI: Jamie Bock) : 7 US institutes + KASI
• Science operation : 2020-‐2013
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How it works?Linear Variable Filter (LVF)
Pluto from New Horizons
7deg
3.5 deg
𝛌
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How it works?
• 24 multiple scan images
-‐> full spectrum
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SPHEREx overview
~PSF size
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Survey strategyAll-Sky Coverage for 2 years
Deep Surveys at Poles
whole sky in 6 months
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deep
all-‐sky survey
Survey Depth• Depth : 18-‐19 mag; Comparable to WISE • Spectral data : better constraint on the redshift
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Main Science Topics1. The Origin of the Universe (large scale structure)
2. The Origin and History of Galaxies (cosmic SF history)
3. The Origin of Water (Ices) in Planetary Systems
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Schedule
1. The Origin of the Universe 2. The Origin and History of Galaxies 3. The Origin of Water (Ices) in Planetary Systems
BOSS
20292027202520232021201720152013 2019
Dark Energy Survey (DES)
Extended BOSS (eBOSS)
HSC imaging PFS spectroscopy
Dark Energy Spec. Instrument (DESI)
Large Synoptic Survey Telescope (LSST)
Euclid
WFIRST-AFTA
BOSS
HETDEX
2031
Blue = imaging Red = spectroscopy
SPHEREx
• Launch : 2020 (2 years of operation)
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KASI’s contribution1. Hardware for electronics : Test of 4 H2RG detectors &
screening
2. Hardware for optics : Baffle tube structure for wide-‐field
telescope
3. Optical Filters : 4 Linear Variable Filters, Dichroic filters
4. Ground support equipment for characterizing the instrument
: cryo. Chamber, integrating sphere, ground station electronics
5. Pipeline development and Science Operation
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Other Science impacts!• Two white papers are posted in Astro-‐ph.
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AGN science with SPHEREx• Structure of AGNs
-‐ Optical/IR reverberation mapping
• AGN unification -‐ Demography of Type 2 Quasars
• BH-‐host coevolution -‐ SFR in AGNs
• And much more!!! (Synergies with other surveys; e.g.,
eRosita, LSST, EUCLID, WFIRST etc.)
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1. Optical/IR reverberation mapping of QSOs
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Optical/IR reverberation
UV,optical continuum
Broad emission line
IR continuumCourtesy : Claudia Ricci
Time lags among UV (optical), broad lines, IR -‐> size of BLR and TORUS
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• SPHEREx data will uniquely provide
1. Simultaneous variability measurement of
broad emission lines (H𝜶 or Pa𝜶) and IR/opt continuum
-‐> structure of accretion disk, BLR and torus at the same
time
2. Variability in IR color -‐> Torus structure : smooth vs. clumpy Torus
Optical/IR reverberation
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Fausnaugh et al. 2016
Time lags among the continuum bands-‐> structure of the accretion disk
Optical/IR reverberation
NGC5548 (STORM project)
Wavelength
Tim
e la
g (d
ays)
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• Requirements
(1) multi-‐epoch data (variability)
-‐ data from each visit
(2) multi-‐wavelength data
(3) relatively high S/N data
Poles > 100 epochs
-> Poles!
Optical/IR reverberation
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• (Distant) Bright QSOs will have
1. large time lags and small amplitude of variability
2. Time dilation : time_lagobs = time_lagrest * (1+z)
• Synergy with other (Korean) facilities -‐ Optical photometry : KMTNet, LOAO, LSG telescope,
several 1m class telescopes in Korea -‐ Optical Spectroscopy : MMT, Gemini, 2-‐4m class telescope
Pre-‐photometric data is crucial!(survey baseline is 2 yrs)
Pre-‐photometric data!
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Difsiculties• large pixel (~ 6”; undersampled PSF)
-‐ host galaxy and/or companion contamination
• low spectral resolution (R~40) -‐ Fe blending (Hβ), narrow emission line blending (Hα)-‐> uncertainty in line flux measurements
• Flux calibration issue-‐ LVF is yet well tested for the absolute flux calibration.
• time difference among the spectral elements
• limited to the brightest AGNs (large time lag?)
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2. Distant type 2 QSOs
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AGN Unisication
Type 2
Type 1
Urry & Padovani 1995
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Modisied Unisication
Merloni et al. 2014
X-‐ray selected AGNs
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Modisied Unisication
Lacy et al. 2015
IR selected AGNs
• Receding Torus model +
disappearing BLR
• Each selection method
has its own different bias!
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Optically selected type 2 QSOs?• Extremely Rare!
SDSS DR7 -‐ type 1 QSOs : 105,783 -‐ type 2 QSOs : a few hundreds (+~2000 from eBoss)
40 41 42 43 44 45 46log (L[OIII])
100
101
102
103
104
105
N
type 1
type 2
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Optically selected type 2 QSOs?• Hard to sind even with SDSS : Targeted spectroscopy
-‐ It does not necessarily mean that it is intrinsically rare! (Zakamska et al. 2003; Sihan et al. 2016)-‐ optical only selection : limited to low-‐z type 2 QSOs (Alexandroff et al. 2013, Greene et al. 2014)
• SPHEREx : high-‐z luminous type 2 QSOs-‐ diagnosed by [OIII] luminosity, H𝛃/[OIII], [OII]/[OIII], hot dust continuum above 1.6um
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0 1 2 3 4redshift
ï17
ï16
ï15
ï14
ï13
log
(F[O
III])
SDSS type 1 QSOs distribution
type 2 QSOs
SPHEREx line slux limit
~ 7000 type 1 QSOs in SDSS sield ~ 10% of type 2 fraction
-‐> 3500 type 2 QSOs from SPHEREx
SPHEREx-‐deep
Shen et al. 2011
Demography of type 2 QSOs
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Demography of type 2 QSOs> 3500 type 2 QSOs from SPHEREx survey
(10% of obscuration fraction)
• The First systematic study of optically (IR) selected type 2 QSOs
• Follow-‐up studies with ground-‐based telescopes (Gemini, GMT
and multi wavelength facilities)-‐ AGN feedback -‐ testing AGN unification -‐ BH-‐host relation
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3. SF activity in AGNs
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BH growth vs. SFR
SF (Galaxy Growth)BH Growth
Time (redshift) Time (redshift) Time (redshift)
1 2 3
BH -‐> Galaxy Galaxy -‐> BHBH = Galaxy
Kenta Matsuoka’s talk yesterday
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PAH 3.3umNGC_6090
1 2 3 4 5wavelength (um)
14.0
13.5
13.0
12.5
12.0
AB
mag
Brown et al. 2014
PAH
Br𝜶
Pa𝜶(SF galaxy)
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PAH as SF indicator
Kim et al. 2012; Woo et al. 2012
Expertise from AKARI mission
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SDSS quasars
• z<0.4 SDSS quasars with expected PAH emission (~ 1/10 of
[OIII]; Woo et al. 2012)~ 600 type 1 quasars
• Statistical study of SFR vs. BH Growth in nearby QSOs
• more abundant sample QSOs with WISE selection
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Summary• SPHEREx will conduct the first all sky spectral survey with
spectral coverage of 0.75-‐5um.
• SPHEREx has the potential to have an impact comparable to
the other great wide-‐field surveys of the 2020’s (M. Strauss).
• The final selection will be made in Jan-‐2017.
• Stay tuned!
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Thank you!