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저작자표시-비영리-변경금지 2.0 대한민국 이용자는 아래의 조건을 따르는 경우에 한하여 자유롭게 l 이 저작물을 복제, 배포, 전송, 전시, 공연 및 방송할 수 있습니다. 다음과 같은 조건을 따라야 합니다: l 귀하는, 이 저작물의 재이용이나 배포의 경우, 이 저작물에 적용된 이용허락조건 을 명확하게 나타내어야 합니다. l 저작권자로부터 별도의 허가를 받으면 이러한 조건들은 적용되지 않습니다. 저작권법에 따른 이용자의 권리는 위의 내용에 의하여 영향을 받지 않습니다. 이것은 이용허락규약 ( Legal Code) 을 이해하기 쉽게 요약한 것입니다. Disclaimer 저작자표시. 귀하는 원저작자를 표시하여야 합니다. 비영리. 귀하는 이 저작물을 영리 목적으로 이용할 수 없습니다. 변경금지. 귀하는 이 저작물을 개작, 변형 또는 가공할 수 없습니다.

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Page 1: Disclaimer - Seoul National UniversityGamma-Ray Burst 111209A ... tically expanding reball with a relativistic ejecta as a shape of shells (Goodman ... internal shocks occur when relatively

저 시-비 리- 경 지 2.0 한민

는 아래 조건 르는 경 에 한하여 게

l 저 물 복제, 포, 전송, 전시, 공연 송할 수 습니다.

다 과 같 조건 라야 합니다:

l 하는, 저 물 나 포 경 , 저 물에 적 된 허락조건 명확하게 나타내어야 합니다.

l 저 터 허가를 면 러한 조건들 적 되지 않습니다.

저 에 른 리는 내 에 하여 향 지 않습니다.

것 허락규약(Legal Code) 해하 쉽게 약한 것 니다.

Disclaimer

저 시. 하는 원저 를 시하여야 합니다.

비 리. 하는 저 물 리 목적 할 수 없습니다.

경 지. 하는 저 물 개 , 형 또는 가공할 수 없습니다.

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이학석사 학위논문

NIR Spectroscopy of EarlyAfterglow of Ultra-Long

Gamma-Ray Burst 111209A

매우 긴 감마선폭발 111209A의 이른 시간 적외선

잔광 스펙트럼 분석

2017년 8월

서울대학교 대학원

물리·천문학부 천문학전공

이 상 윤

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NIR Spectroscopy of Early Afterglowof Ultra-Long Gamma-Ray Burst

111209A

by

Sang-Yun Lee([email protected])

A dissertation submitted in partial fulfillment of the requirements for

the degree of

Master of Science

in

Astronomy

in

Astronomy Program

Department of Physics and Astronomy

Seoul National University

Committee:

Professor Bon-Chul Koo

Professor Myungshin Im

Professor Hyung Mok Lee

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ABSTRACT

In the recent years, few gamma-ray bursts have been observed with extremely

long duration, over 1,000 s or 10,000 s, called ultra-long GRB. Among them, GRB

111209A at redshift z = 0.677 has the longest with an observer frame gamma-ray

prompt emission duration 7 hr. We observed early NIR spectrum of this ULGRB

using NASA’s 3m IRTF. It is the only spectrum data that shows early afterglow in

X-ray to Radio range. We use TAROT R-band data in addition to examining the

flux calibration. The NIR spectra shows synchrotron radiation with β = 1.22± 0.03

with electron power-law energy distribution index p 2.4. The thermal component

was too weak so we cannot figure out any clue about it. To see whether ULGRBs

can have a common origin as short/long GRB, we compare the spectrum of this

GRB with another ULGRB, GRB 101225A so called ”the Christmas burst”. In

contrast with GRB 111209A, GRB 101225A shows an early evolution of strong

blackbody component. These mutually exclusive properties make the two ULGRB

be considered with different progenitor candidates: core-collapse of a low metallicity

blue supergiant for GRB 111209A and merger of helium star with a neutron star

that underwent a common envelope phase for GRB 101225A. We also examine the

validity of external shock model with two characteristic frequencies: νc and νm.

Theoretically, it was possible to satisfy the observation using external shock model,

however, it is not preferable for the real situation. Instead, we see the possibility for

adopting magnetar model using synchrotron radiation theory.

Keywords: gamma-ray burst: general− gamma-ray burst: individual (GRB 111209A,

GRB 101225A)

Student Number: 2015-20363

i

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ii

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Contents

Abstract i

List of Figures v

List of Tables vii

1 Introduction 1

2 Data 9

2.1 IRTF . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9

2.2 TAROT R-band . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 11

2.3 IRTF Reduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12

3 Result 13

4 Discussion 23

4.1 Progenitor Diversity . . . . . . . . . . . . . . . . . . . . . . . . . . . 23

4.2 External Shock Synchrotron Radiation Model . . . . . . . . . . . . . 24

4.3 Magnetars . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 33

5 Conclusion 35

Bibliography 36

iii

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Appendix 39

A Spectrum Data Table 39

요 약 133

iv

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List of Figures

1.1 Standard model . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4

1.2 GRB classification . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6

1.3 SED temporal evolution of the ”Christmas burst” . . . . . . . . . . . 8

2.1 Tarot R-band spline . . . . . . . . . . . . . . . . . . . . . . . . . . . 11

3.1 NIR spectrum of epoch1 . . . . . . . . . . . . . . . . . . . . . . . . . 14

3.2 NIR spectrum of epoch2 . . . . . . . . . . . . . . . . . . . . . . . . . 15

3.3 NIR spectrum of epoch3 . . . . . . . . . . . . . . . . . . . . . . . . . 16

3.4 NIR spectrum of epoch4 . . . . . . . . . . . . . . . . . . . . . . . . . 17

3.5 NIR spectrum of epoch5 . . . . . . . . . . . . . . . . . . . . . . . . . 18

3.6 NIR spectrum of epoch6 . . . . . . . . . . . . . . . . . . . . . . . . . 19

3.7 NIR spectrum of epoch7 . . . . . . . . . . . . . . . . . . . . . . . . . 20

3.8 NIR spectrum of epoch8 . . . . . . . . . . . . . . . . . . . . . . . . . 21

3.9 Simultaneous plot of GRB 111209A and the ”Christmas burst” . . . 22

v

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vi

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List of Tables

2.1 IRTF observation epoch. T0 is Swift’s BAT alert time. . . . . . . . . 10

4.1 Parameters that shows νc, νm < 1013Hz. Test space are−6 ≤ log10 εB ≤

−2, −3 ≤ log10 εe ≤ −1, −3 ≤ log10 n ≤ 1, and 3 ≤ γ ≤ 300 . . . . . 25

4.2 Parameters that shows νc, νm < 1014Hz. Test space are−6 ≤ log10 εB ≤

−2, −2 ≤ log10 εe ≤ −1, −3 ≤ log10 n ≤ 1, and 3 ≤ γ ≤ 300 . . . . . 29

A.1 Spectrum data of first 4 epochs . . . . . . . . . . . . . . . . . . . . . 40

A.2 Spectrum data of last 4 epochs . . . . . . . . . . . . . . . . . . . . . 86

vii

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viii

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Chapter 1

Introduction

Gamma-ray bursts, so called GRBs are flash like events which radiate enormous

energy in a short duration, typically few to tens of seconds. Commonly, they divided

into two classes: short-hard GRB (SGRB) and long-soft GRB (LGRB) based on a

γ-ray duration, δtγ of 2 seconds. For SGRBs, the progenitors are believed as binary

mergers of compact objects such as neutron star + neutron star (NS-NS), black

hole + neutron star (BH-NS), black hole + white dwarf (BH-WD), or black hole +

helium star (BH-He) (Goodman 1986, Paczynski 1991). Also, it is promising that

SGRB will be detected as an electromagnetic (EM) counterpart of gravitational

wave (GW). On the other hand, the connection between LGRB and Type Ic core-

collapse supernovae (SNe) confirmed that the progenitors of LGRBs are massive

stars (Woosley et al. 2006).

Regardless of the class, the emission process is extensively explained using stan-

dard fireball + internal/external shock model. Once progenitors produce a black

hole with high-density accretion disk or torus, the central engines eject relativis-

tically expanding fireball with a relativistic ejecta as a shape of shells (Goodman

1986, Paczynski 1986).

Inside the fast-moving ejecta, internal shocks occur when relatively fast shells

1

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2 Introduction

catch up the precedent shells. This process transforms the difference of kinetic energy

before and after the collision into the internal energy of merged shell. The electrons

accelerated by internal shocks and then emit non-thermal, synchrotron radiation in

the gamma-ray range called the prompt emission.

Meanwhile, the initial part of the ejecta propagates and sweeps the interstellar

medium(ISM). At the beginning, the swept ISM has no influence to the ejecta.

However, when the mass of swept up ISM is comparable to the mass of the ejecta,

deceleration becomes significant and the shells drive shocks into ISM. This is called

external shocks and they transfer the kinetic energy of the ejecta into the thermal

energy of shocked ISM. When the most of the kinetic energy transferred, afterglow

emission begins via synchrotron radiation in the X-ray to radio range.

External shock model is well described by Sari et al. (1998). They calculated

the broadband spectrum and the light curve of synchrotron radiation from electrons

accelerated by an expanding relativistic shock. In their description, it is assumed

that the energy distribution of electrons follows a power-law, with an index p above

a minimal Lorentz factor: N(γe)dγe ∝ γ−pe for γe > γm. If we consider a relativistic

shock propagating through a uniform cold medium with particle density n, then

the particle density and the energy density behind the shock are given as 4γn and

4γ2nmpc2, respectively, where γ is the Lorentz factor of the shock fluid (Blandford

et al. 1976). Sari et al. (1998) assumed that a constant fraction εe of the shock

energy goes into the electrons. Therefore the relation between γm and γ is given as

γm = εe(p− 2)

(p− 1)

mp

meγ (1.1)

They also assumed that the magnetic energy density behind the shock has a constant

fraction of the εB of the shock energy. From this assumption, the magnetic field in

the fluid frame is given as

B = (32πmpεBn)1/2γc (1.2)

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Introduction 3

Meanwhile, the radiation power and the characteristic synchrotron frequency in the

observer frame with Lorentz factor γ >> 1 in the magnetic field B are

P (γe) =4

3σT cγ

2γ2eB2

8π(1.3)

ν(γe) = γγ2eqeB

2πmec(1.4)

From these equations, Sari et al. (1998) defined the two characteristic frequen-

cies: νm and νc. A power-law distribution indicates that most of the electrons have

their energy near Emin = γmmec2. Therefore νm = ν(γm) is typical synchrotron

frequency. νc corresponds to the critical Lorentz factor, γc which is computed from

γγcmec2 = P (γc)t, where t is measured in the observer frame. It is the frequency

that a significant fraction of the electron’s energy will radiate in a duration t.

γc =6πmec

σTγB2t(1.5)

With the relation of the two characteristic frequencies, they defined two regimes:

fast and slow cooling (Figure 1.1). Fast cooling is when νm > νc and slow cooling is

vice-versa. The main difference between the two regimes is the spectral slope. Fast

cooling shows ν−1/2 and ν−p/2, but slow cooling has ν−(p−1)/2 and ν−p/2.

In addition to the synchrotron radiation, some GRBs show thermal emission in

their spectral energy distribution (SED) or light curve. WIth a spectroscopy, ther-

mal component can be easily detected because the spectral shape of Planck function

is totally different with the shape of power-law Fν ∼ t−αν−β. On the other hand,

one can expect thermal component when the light curve does not follow the ten-

dency of power-law component such as later supernova-like bump. In this case, light

curve modelling can reveal the physical parameters of blackbody component. This

indicates the existance of a thermalized region. Generally, it is interpreted as photo-

spheric emission from optically thin part of the fireball. Pe’er et al. (2006) explains

that when the GRB jet breaks out the progenitor’s envelope, the relativistically

expanding hot plasma cocoon also emerges and emits blackbody radiation.

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4 Introduction

Figure 1.1. Synchrotron spectrum of a relativistic shock with power-law electron

distribution. Upper panel (a) is fast cooling regime which is shown late prompt

phase or early afterglow times. During fast colling, νm > νc and the slope between

the two frequency has ν−1/2. Lower panel (b) is slow cooling which is expected at

late afterglow times. νc > νm, therefore the synchrotron emission is not effective as

fast cooling. In this regime, the slope between the two shows ν−(p−1)/2. This figure

was from Sari et al. (1998)

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Introduction 5

Apart from classical short and long GRBs, several GRBs have δtγ > 1000 s or

even 10 ks (Figure 1.2). They are called ultra-long GRB (ULGRB). So far, only 15

GRBs have been confirmed as ULGRBs. This is less than 1% compared to the total

number of GRBs that have been detected since 1967: 7000 GRBs indicating very

rare event.This new classification is not yet strongly defined and still has opened

the debate on whether it can be classified as a new one or just the long tail of the

standard LGRB. Some research tried to analyze ULGRB with wolf-rayet(WR) star

progenitor (Gao et al. 2016) but a majority of research indicate that ULGRBs show

clear deviation from LGRBs. According to the latter case, their long durations are

hard to resolve using standard wolf-rayet star progenitor (Nakauchi et al. 2013,

Levan et al. 2014) and also statistically distinct from the standard LGRBs (Boer

et al. 2015).

Many progenitor candidates have been suggested to explain the observational

aspect. Above all, the following two are most probable: core-collapse of a low metal-

licity blue supergiant star (hereafter BSG) (Woosley et al. 2012, Gendre et al. 2013,

Nakauchi et al. 2013), and merger of a helium star with a NS that underwent a

common envelope (CE) phase, expelling its hydrogen envelope (hereafter He-NS)

(Fryer et al. 1998, Zhang et al. 2001, Barkov et al. 2011, Thone et al. 2011).

The GRB emission machanism of the BSG model is similar to the standard

model. This model natrually explains the long duration of ULGRBs. The low metal-

licity makes a weaker stellar wind, then eventually larger and massive envelope

compared to normal WR star can survive. Stellar envelope falls into the central en-

gine as a free fall time scale tff (r) =√r3/GMr therefore BSG can easily achieves

104s duration scale. Nakauchi et al. (2013) adopted cocoon-fireball photospheric

emission (CFPE) to explain the later SLSN-like bump in the light curve of ULGRB.

He-NS model is somewhat different with the BSG model. The main purpose

of He-NS model is to explain the evolution of strong blackbody component starts

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6 Introduction

Figure 1.2. γ-ray duration and the approximate average isotropic luminosity of

transients. The lower luminosity sources categorized as Galactic sources that we

do not concern about. The soft-gamma repeaters (SGRs) in our own Galaxy are

shown in the green box. LGRB and SGRB are indicated by purple and blue boxes

individually. The red box contains the likely population of low-luminosity GRBs

(LLGRBs). The three ultra-long GRBs (GRB 101225A, GRB 111209A, and GRB

121027A) clearly deviate from the other classes. This image was obtained from Levan

et al. (2014).

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Introduction 7

from early afterglow. The relativistic jet emitted from the central engine interacts

with the inner/outer boundary of the envelope. Since the number density of CE

is much higher, the two region become hot and emit blackbody radiation in X-ray

and UV-Optical-Radio range respectively. GRB 101225, so called the ”Christmas

burst” is an ULGRB that shows δtγ 7000s and average isotropic luminosity, Liso =

1.20×1049erg s−1 (Thone et al. 2011). This ULGRB is well described with He-NS

model (Figure 1.3).

As one can see, the two models are mutually exclusive. The BSG model shows

synchrotron radiation dominantely but hard to see strong blackbody component.

Therefore, this model cannot be applied to the ”Christmas burst”. On the other

hand, the He-NS model shows strong blackbody component. So, by analysing an

ULGRB’s SED, we can reject one of the two models. If a SED of ULGRB shows

strong blackbody radiation, the BSG model is rejected and it is possible to claim

that ULGRB might have single progenitor as the other two class. On the contrary, if

there exist snchrotron radiation dominantely, He-NS model should be rejected and

then it is natural to claim that ULGRBs have different progenitor.

In this paper, we analysis the early NIR spectrum of GRB 111209A that was

obtained during the prompt phase. GRB 111209A is ULGRB which has the longest

duration ( 7 hrs) among detected (Golenetskii et al. 2011). Swift’s Burst Alert

Telescope (BAT) detected at T0 = 2011 : 12 : 09 − 07 : 12 : 08UT and the

location is RA(J2000) = 00h 57m 22.63s, DEC(J2000) = −46d 48′ 03.8′′.

The redshift of z = 0.677 was calculated using FeII, MgII, MgI, CaII H&K lines

in UV/IR range (Vreeswijk et al. 2011). It shows average isotropic luminosity

Liso = 5.21×1049erg s−1 that is about 4 times larger than the ”Christmas burst”.

We investigate whether the black body component appears in the NIR/Optical range

with additional R-band data. The result makes us to determine which model is

proper to GRB 111209A.

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8 Introduction

Figure 1.3. The UVOIR SED of GRB 101225A at various time. This shows tem-

poral evolution of SED from 0.07 days to 40 days. Filled circles are observation data

and triangles are upper limits. To fit the SED, two different component were needed:

expanding and cooling black body up to 10 days and an additional supernova for

the last four epochs. The Solid lines are the total flux of the two components. The

black body components are shown as dashed lines from day 5. The UVOIR black

body was 43000 K at 0.07 d with radius of 2× 1014cm (from Thone et al. (2011)).

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Chapter 2

Data

2.1 IRTF

Shortly after the alert from the GCN Circulars, we observed GRB 111209A using

NASA’s 3m Infrared Telescope Facility (IRTF) at Mauna Kea, Hawaii, USA. The

SpeX spectrograph was used in the short cross-dispersion mode (SXD, 0.8 µm - 2.5

µm). A 0.8″ × 15″ slit was employed and a spectral resolution is 750. The observation

started at 2011:12:09−07:42:13 UT, or about T0 + 38 m. When the observation

started, the altitude of the target was already low at 20 degree (airmass = 2.8).

However, IRTF is capable to observe targets at very low altitudes due to its design to

observe solar system objects, and the observation continued until the target reached

the altitude of about 17 degree (airmass=3.4). In summary, we were able to obtain

the very early NIR spectra of GRB 111209A with a total of 8 epochs, with the

exposure time of 180 s per each epoch (Table 2.1). For A0V standard star, HD6208

was observed, which was near GRB 111209A.

9

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10 Data

Table 2.1. IRTF observation epoch. T0 is Swift’s BAT alert time.

Epoch 1 2 3 4 5 6 7 8

Start(T0+[s]) 2281 2484 2681 2873 3080 3282 3494 3696

End(T0+[s]) 2460 2663 2860 3062 3259 3461 3673 3875

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Data 11

2.2 TAROT R-band

Stratta et al. (2013) provide R-band data of TAROT ESO (Chile) robotic telescope.

The observation started from T0 + 492 s up to T0 + 3.7 ks (Klotz et al. 2011). We

use this data to verify the flux calibration of IRTF spectra. To do this, there need

to match the epoch of R-band data same as IRTF. So we spline interpolate the data

and take the average of the points which fall within each epoch (figure 2.1)

Figure 2.1. TAROT R-band data and modification. Black squares are law data

from Stratta et al. (2013), red is spline fitting, blue filled diamonds are average of

the points that fall within each epoch.

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12 Data

2.3 IRTF Reduction

NIR data reduction was done by using Spextool v4.1 IDL packages. This process

consists of three steps: extraction, telluric correction, and merging. In order to ex-

tract spectra by orders from raw data, xspextool was used. All preprocess including

flat fielding, wavelength calibration, and background subtraction were done with

this program. Xtellcor performs telluric correction and flux calibration on extracted

multi-order spectra. Using a high-resolution model of Vega and observation data

of A0V standard star, this program modifies the Vega model to match the radial

velocity, reddening, resolving power, and HI equivalent widths of the observed stan-

dard star. The telluric correction spectrum can be obtained from the division of

the observed standard star spectrum by the modified Vega spectrum. Theoretically,

this correction spectrum only contains telluric spectra with a normalized continuum.

Therefore, the division of the source spectrum with telluric correction spectrum can

yield an intrinsic spectrum of the source. The extracted and corrected multi-order

spectra can combine into a single spectrum with xmergeorders. SpeX spectrograph

was designed to overlap the ordered spectra side by side for scaling the flux. How-

ever, it was not effective for this source because of the low signal-to-noise ratio (SNR)

and telluric contamination range from the earth’s atmosphere. The orders which are

hard to make scale factor use unity to combine.

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Chapter 3

Result

NIR data was well fitted by a simple power law (Figure 3.1 − 3.8). In log-log plane,

the linear fitting was done with IDL Sixlin procedure with signal-to-noise ratio (SNR)

cut of 3. The mean value is β = 1.22 ± 0.03. Those spectral indices show good

agreement with the standard model as the slope of −p/2 assuming electron power-

law energy distribution index of p ∼ 2.4 (Figure 1.1) (Sari et al. 1998). We cannot

determine which regime the afterglow is. It is becuase we do not know where is

the frequency of minimum lorentz factor (or synchrotron injection frequency) νm is.

However it is certain that the cooling frequency νc is below the NIR range. On the

other hand, the thermal component is too weak to figure out in the early afterglow

of GRB 111209A. It is totally different from the spectral energy distribution (SED)

of GRB 101225A (“Christmas burst”) that shows evolving black body component

from 0.07d to more than 18 days (Thone et al. 2011) (Figure 3.9).

13

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14 Result

Figure 3.1. NIR spectrum of epoch 1 with TAROT R-band. The start time is T0

+ 2281 s upto T0 + 2460 s. Spectral slope β = 1.26 ±0.04.

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Result 15

Figure 3.2. NIR spectrum of epoch 2 with TAROT R-band. The start time is T0

+ 2484 s upto T0 + 2663 s. Spectral slope β = 1.08 ±0.02.

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16 Result

Figure 3.3. NIR spectrum of epoch 3 with TAROT R-band. The start time is T0

+ 2681 s upto T0 + 2860 s. Spectral slope β = 1.32 ±0.02.

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Result 17

Figure 3.4. NIR spectrum of epoch 4 with TAROT R-band. The start time is T0

+ 2873 s upto T0 + 3062 s. Spectral slope β = 1.24 ±0.02.

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18 Result

Figure 3.5. NIR spectrum of epoch 5 with TAROT R-band. The start time is T0

+ 3080 s upto T0 + 3259 s. Spectral slope β = 1.23 ±0.02.

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Result 19

Figure 3.6. NIR spectrum of epoch 6 with TAROT R-band. The start time is T0

+ 3282 s upto T0 + 3461 s. Spectral slope β = 1.17 ±0.02.

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20 Result

Figure 3.7. NIR spectrum of epoch 7 with TAROT R-band. The start time is T0

+ 3494 s upto T0 + 3673 s. Spectral slope β = 1.20 ±0.04.

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Result 21

Figure 3.8. NIR spectrum of epoch 8 with TAROT R-band. The start time is T0

+ 3696 s upto T0 + 3875 s. Spectral slope β = 1.20 ±0.04.

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22 Result

Figure 3.9. Simultaneous plot of GRB 111209A and the ”Christmas burst” at sim-

ilar epoch: T0 + 0.07 d. The two ULGRBs’ SED is totally different. GRB 111209A

is shape of synchrotron radiation, on the other hand, the ”Christmas burst” is black-

body rdaiation of TBB= 47000 K.

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Chapter 4

Discussion

4.1 Progenitor Diversity

ULGRB as a new class of GRB is not strongly defined yet but it is widely accepted

that there is some deviation between classical LGRB and ULGRB phenomenally

and statistically (Boer et al. 2015). This infers that we need somewhat different

progenitor for ULGRB. Many authors suggest various progenitor candidates and

each model has pros and cons. Above all, we’ll examine the two modles: BSG and

He-NS model. As we already mentioned, the two models are mutual independent.

That’s because each concentrate on the different emission component. BSG model

shares the same emission mechanism of the classical LGRB with WR star progenitor.

But the larger envelope of BSG make the central engine possible to last for 104 s.

Therefore, for BSG model, the main emission component is synchrotron radiation.

Blackbody component also can exist as a photospheric emission, however, normally

it is used for the explanation of SN-like or SLSN-like bump (Vreeswijk et al. 2011).

As a result, BSG model can explain GRB 111209A naturally but for the ”Christmas

burst”, it is hard to resolve the early evolution of strong blackbody component. On

the other hand, He-NS model is optimized to the blackbody component, so this

23

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24 Discussion

model is decent explanation for the two blackbody component of the ”Christmas

burst” in X-ray and UVOIR range respectively. Without the blackbody component,

it is impossible to use He-NS model and our results of early NIR spectra of GRB

111209A show only synchrotron radiation. Therefore this model cannot be used

as the progenitor of GRB 111209A. To sum up, it is more natural to claim that

ULGRBs can have different progenitor and it seems unlikely to categorize the whole

ULGRBs with same emission mechanism as classical GRBs.

4.2 External Shock Synchrotron Radiation Model

According to the synchrotron radiation model, β = 1.22 ± 0.03 is corresponds to

the D or H region in figure 1.1 with p ∼ 2.4. This indicates that both characteristic

frequency, νm and νc have to locate below NIR frequency: 1014Hz. Also, in the real

situation, the slope values vary smoothly as time passes, therefore, the characteristic

frequencies should exist further below NIR region. We calculated νm and νc using

equation 1.1-5 with various parameter space and test whether the two frequencies

can satisfy the constraint(Table 4.1 and 4.2). There exist many parameter sets that

can satisfy our constraint, however, the frequencies quite close to the limit and have

similar values. It means that our observation was done right before or after the

transition of the cooling regime which is not preferable. By any chance if so, the

slope should be more gentle since the variation occurs smoothly. Therefore, it might

not possible to adopt external shock model and needs another emission mechanism

for this synchrotron radiation.

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Discussion 25

Table 4.1. Parameters that shows νc, νm < 1013Hz. Test space are −6 ≤ log10 εB ≤

−2, −3 ≤ log10 εe ≤ −1, −3 ≤ log10 n ≤ 1, and 3 ≤ γ ≤ 300

log10 εB log10 εe log10 n log10 γ νc νm

-2.70 -3.00 1.00 2.08 8.66e+012 8.57e+012

-2.60 -3.00 0.90 2.08 8.66e+012 8.57e+012

-2.60 -3.00 1.00 2.08 6.13e+012 9.62e+012

-2.50 -3.00 0.80 2.08 8.66e+012 8.57e+012

-2.50 -3.00 0.90 2.08 6.13e+012 9.62e+012

-2.40 -3.00 0.70 2.08 8.66e+012 8.57e+012

-2.40 -3.00 0.80 2.08 6.13e+012 9.62e+012

-2.40 -3.00 1.00 1.98 7.72e+012 4.82e+012

-2.40 -2.90 1.00 1.98 7.72e+012 7.64e+012

-2.30 -3.00 0.60 2.08 8.66e+012 8.57e+012

-2.30 -3.00 0.70 2.08 6.13e+012 9.62e+012

-2.30 -3.00 0.90 1.98 7.72e+012 4.82e+012

-2.30 -3.00 1.00 1.98 5.47e+012 5.41e+012

-2.30 -2.90 0.90 1.98 7.72e+012 7.64e+012

-2.30 -2.90 1.00 1.98 5.47e+012 8.57e+012

-2.20 -3.00 0.50 2.08 8.66e+012 8.57e+012

-2.20 -3.00 0.60 2.08 6.13e+012 9.62e+012

-2.20 -3.00 0.80 1.98 7.72e+012 4.82e+012

-2.20 -3.00 0.90 1.98 5.47e+012 5.41e+012

-2.20 -3.00 1.00 1.88 9.72e+012 2.42e+012

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26 Discussion

Table 4.1. (Con’d)

log10 εB log10 εe log10 n log10 γ νc νm

-2.20 -3.00 1.00 1.98 3.87e+012 6.07e+012

-2.20 -2.90 0.80 1.98 7.72e+012 7.64e+012

-2.20 -2.90 0.90 1.98 5.47e+012 8.57e+012

-2.20 -2.90 1.00 1.88 9.72e+012 3.83e+012

-2.20 -2.90 1.00 1.98 3.87e+012 9.62e+012

-2.20 -2.80 1.00 1.88 9.72e+012 6.07e+012

-2.20 -2.70 1.00 1.88 9.72e+012 9.62e+012

-2.10 -3.00 0.40 2.08 8.66e+012 8.57e+012

-2.10 -3.00 0.50 2.08 6.13e+012 9.62e+012

-2.10 -3.00 0.70 1.98 7.72e+012 4.82e+012

-2.10 -3.00 0.80 1.98 5.47e+012 5.41e+012

-2.10 -3.00 0.90 1.88 9.72e+012 2.42e+012

-2.10 -3.00 0.90 1.98 3.87e+012 6.07e+012

-2.10 -3.00 1.00 1.88 6.88e+012 2.71e+012

-2.10 -3.00 1.00 1.98 2.74e+012 6.81e+012

-2.10 -2.90 0.70 1.98 7.72e+012 7.64e+012

-2.10 -2.90 0.80 1.98 5.47e+012 8.57e+012

-2.10 -2.90 0.90 1.88 9.72e+012 3.83e+012

-2.10 -2.90 0.90 1.98 3.87e+012 9.62e+012

-2.10 -2.90 1.00 1.88 6.88e+012 4.30e+012

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Discussion 27

Table 4.1. (Con’d)

log10 εB log10 εe log10 n log10 γ νc νm

-2.10 -2.80 0.90 1.88 9.72e+012 6.07e+012

-2.10 -2.80 1.00 1.88 6.88e+012 6.81e+012

-2.10 -2.70 0.90 1.88 9.72e+012 9.62e+012

-2.00 -3.00 0.30 2.08 8.66e+012 8.57e+012

-2.00 -3.00 0.40 2.08 6.13e+012 9.62e+012

-2.00 -3.00 0.60 1.98 7.72e+012 4.82e+012

-2.00 -3.00 0.70 1.98 5.47e+012 5.41e+012

-2.00 -3.00 0.80 1.88 9.72e+012 2.42e+012

-2.00 -3.00 0.80 1.98 3.87e+012 6.07e+012

-2.00 -3.00 0.90 1.88 6.88e+012 2.71e+012

-2.00 -3.00 0.90 1.98 2.74e+012 6.81e+012

-2.00 -3.00 1.00 1.88 4.87e+012 3.04e+012

-2.00 -3.00 1.00 1.98 1.94e+012 7.64e+012

-2.00 -2.90 0.60 1.98 7.72e+012 7.64e+012

-2.00 -2.90 0.70 1.98 5.47e+012 8.57e+012

-2.00 -2.90 0.80 1.88 9.72e+012 3.83e+012

-2.00 -2.90 0.80 1.98 3.87e+012 9.62e+012

-2.00 -2.90 0.90 1.88 6.88e+012 4.30e+012

-2.00 -2.90 1.00 1.88 4.87e+012 4.82e+012

-2.00 -2.80 0.80 1.88 9.72e+012 6.07e+012

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28 Discussion

Table 4.1. (Con’d)

log10 εB log10 εe log10 n log10 γ νc νm

-2.00 -2.80 0.90 1.88 6.88e+012 6.81e+012

-2.00 -2.80 1.00 1.88 4.87e+012 7.64e+012

-2.00 -2.70 0.80 1.88 9.72e+012 9.62e+012

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Discussion 29

Table 4.2. Parameters that shows νc, νm < 1014Hz. Test space are −6 ≤ log10 εB ≤

−2, −2 ≤ log10 εe ≤ −1, −3 ≤ log10 n ≤ 1, and 3 ≤ γ ≤ 300

log10 εB log10 εe log10 n log10 γ νc νm

-2.60 -2.00 1.00 1.78 9.72e+013 6.07e+013

-2.60 -1.90 1.00 1.78 9.72e+013 9.62e+013

-2.50 -2.00 0.90 1.78 9.72e+013 6.07e+013

-2.50 -2.00 1.00 1.78 6.88e+013 6.81e+013

-2.50 -1.90 0.90 1.78 9.72e+013 9.62e+013

-2.40 -2.00 0.80 1.78 9.72e+013 6.07e+013

-2.40 -2.00 0.90 1.78 6.88e+013 6.81e+013

-2.40 -2.00 1.00 1.78 4.87e+013 7.64e+013

-2.40 -1.90 0.80 1.78 9.72e+013 9.62e+013

-2.30 -2.00 0.70 1.78 9.72e+013 6.07e+013

-2.30 -2.00 0.80 1.78 6.88e+013 6.81e+013

-2.30 -2.00 0.90 1.78 4.87e+013 7.64e+013

-2.30 -2.00 1.00 1.68 8.66e+013 3.41e+013

-2.30 -2.00 1.00 1.78 3.45e+013 8.57e+013

-2.30 -1.90 0.70 1.78 9.72e+013 9.62e+013

-2.30 -1.90 1.00 1.68 8.66e+013 5.41e+013

-2.30 -1.80 1.00 1.68 8.66e+013 8.57e+013

-2.20 -2.00 0.60 1.78 9.72e+013 6.07e+013

-2.20 -2.00 0.70 1.78 6.88e+013 6.81e+013

-2.20 -2.00 0.80 1.78 4.87e+013 7.64e+013

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30 Discussion

Table 4.2. (Con’d)

log10 εB log10 εe log10 n log10 γ νc νm

-2.20 -2.00 0.90 1.68 8.66e+013 3.41e+013

-2.20 -2.00 0.90 1.78 3.45e+013 8.57e+013

-2.20 -2.00 1.00 1.68 6.13e+013 3.83e+013

-2.20 -2.00 1.00 1.78 2.44e+013 9.62e+013

-2.20 -1.90 0.60 1.78 9.72e+013 9.62e+013

-2.20 -1.90 0.90 1.68 8.66e+013 5.41e+013

-2.20 -1.90 1.00 1.68 6.13e+013 6.07e+013

-2.20 -1.80 0.90 1.68 8.66e+013 8.57e+013

-2.20 -1.80 1.00 1.68 6.13e+013 9.62e+013

-2.10 -2.00 0.50 1.78 9.72e+013 6.07e+013

-2.10 -2.00 0.60 1.78 6.88e+013 6.81e+013

-2.10 -2.00 0.70 1.78 4.87e+013 7.64e+013

-2.10 -2.00 0.80 1.68 8.66e+013 3.41e+013

-2.10 -2.00 0.80 1.78 3.45e+013 8.57e+013

-2.10 -2.00 0.90 1.68 6.13e+013 3.83e+013

-2.10 -2.00 0.90 1.78 2.44e+013 9.62e+013

-2.10 -2.00 1.00 1.68 4.34e+013 4.30e+013

-2.10 -1.90 0.50 1.78 9.72e+013 9.62e+013

-2.10 -1.90 0.80 1.68 8.66e+013 5.41e+013

-2.10 -1.90 0.90 1.68 6.13e+013 6.07e+013

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Discussion 31

Table 4.2. (Con’d)

log10 εB log10 εe log10 n log10 γ νc νm

-2.10 -1.90 1.00 1.68 4.34e+013 6.81e+013

-2.10 -1.80 0.80 1.68 8.66e+013 8.57e+013

-2.10 -1.80 0.90 1.68 6.13e+013 9.62e+013

-2.00 -2.00 0.40 1.78 9.72e+013 6.07e+013

-2.00 -2.00 0.50 1.78 6.88e+013 6.81e+013

-2.00 -2.00 0.60 1.78 4.87e+013 7.64e+013

-2.00 -2.00 0.70 1.68 8.66e+013 3.41e+013

-2.00 -2.00 0.70 1.78 3.45e+013 8.57e+013

-2.00 -2.00 0.80 1.68 6.13e+013 3.83e+013

-2.00 -2.00 0.80 1.78 2.44e+013 9.62e+013

-2.00 -2.00 0.90 1.68 4.34e+013 4.30e+013

-2.00 -2.00 1.00 1.58 7.72e+013 1.92e+013

-2.00 -2.00 1.00 1.68 3.07e+013 4.82e+013

-2.00 -1.90 0.40 1.78 9.72e+013 9.62e+013

-2.00 -1.90 0.70 1.68 8.66e+013 5.41e+013

-2.00 -1.90 0.80 1.68 6.13e+013 6.07e+013

-2.00 -1.90 0.90 1.68 4.34e+013 6.81e+013

-2.00 -1.90 1.00 1.58 7.72e+013 3.04e+013

-2.00 -1.90 1.00 1.68 3.07e+013 7.64e+013

-2.00 -1.80 0.70 1.68 8.66e+013 8.57e+013

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32 Discussion

Table 4.2. (Con’d)

log10 εB log10 εe log10 n log10 γ νc νm

-2.00 -1.80 0.80 1.68 6.13e+013 9.62e+013

-2.00 -1.80 1.00 1.58 7.72e+013 4.82e+013

-2.00 -1.70 1.00 1.58 7.72e+013 7.64e+013

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Discussion 33

4.3 Magnetars

One of an alternative explanation is magnetar. In the recent years, magnetars have

been suggested for long or ultra-long GRBs (Greiner et al. 2014; Ioka et al. 2016;

Gompertz et al. 2017). According to the precedent studies, magnetar model can

explain the associated supernova-like bump (SN 2011kl) more decently. To consider

this model, we calculated the magnetic field strength using equation 1.4-5.

νc =18πmecqeσ2TγB

3t2(4.1)

B = (18πmecqeσ2Tγνct

2)1/3 (4.2)

Assume the νc = 2.4µm, γ = 100, εB = 0.01, εe = 0.1, n = 1, p = 2.4 and t = 2400s,

the magnetic field strength is B = 0.46G. This value is the lower limit since the

smaller characteristic frequencies make larger magnetic field. This result indicates

that the real magnetic field should has at least few Gauss and that is quite big for

external shock model. On the other hand, if magnetar has 1015G then few Gauss

can easily obtained around R = 1016cm due to flux conservation. This argument is

quite simplified and needs more detailed analysis but still has a positive outlook for

the magnetar model.

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34 Discussion

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Chapter 5

Conclusion

Rarely but certainly, GRBs outburst with δtν over 1000 s or even 10000 s. Now they

are classified as a new class of GRB: ultra-long GRB. To explain these exceptionally

long burst, many authors suggest various progenitor candiidates. Among them, we

concentrate two models: BSG model and He-NS model. BSG model is similar to the

WR star progenitor and emits synchrotron radiation dominantly. He-NS model is

optimized to the blackbody component of GRB 101225, so called the ”Christmas

burst”. To examine the two model, we used NIR spectroscopy of early afterglow

of GRB 111209A which has the longest duration ever detected. The results shows

only synchrotron radiation without blackbody component. This is totally different

from the SED of the ”Christmas burst”, so we conclude that the two ULGRBs

have different progenitor and emission mechanism. One step forward, we tested

external shock model with a constraint for characteristic frequencies. Theoretically, it

is possible to make the two frequencies locate below the frequency limit, however, it is

quite far from the real situation. Therefore, we consider another emission mechanism

that uses magnetars as a progenitor. It was quite simplified analysis but still open

the possibility for the magnetar model.

35

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36 Bibliography

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Appendix A

Spectrum Data Table

39

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40 Appendices

Table

A.1.

Sp

ectr

um

dat

aof

firs

t4

epoch

s

[h]

Wav

elen

gth

Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.8

104

1.6

30.6

41.

340.

731.

050.

431.5

81.0

5

0.81

16

0.8

30.5

22.

060.

581.

110.

600.9

80.8

9

0.81

28

0.9

70.2

92.

320.

921.

150.

680.5

90.6

2

0.81

40

1.0

90.6

81.

800.

701.

120.

260.6

60.3

1

0.81

52

0.5

70.4

61.

520.

410.

940.

210.1

40.3

2

0.81

63

0.8

90.1

71.

150.

921.

320.

451.1

10.3

8

0.81

75

0.6

40.4

21.

180.

461.

010.

151.1

20.4

7

0.81

87

0.8

70.6

21.

560.

420.

740.

541.3

10.2

2

0.81

98

1.1

50.9

91.

110.

540.

130.

740.9

30.2

4

0.82

10

0.5

90.5

40.

870.

820.

520.

571.3

10.5

7

0.82

22

1.0

20.5

80.

920.

591.

250.

470.7

60.4

1

0.82

33

0.1

20.9

01.

660.

451.

290.

480.6

70.6

0

0.82

45

1.0

80.5

21.

070.

751.

080.

660.6

30.6

4

0.82

57

1.5

20.5

91.

620.

450.

560.

591.0

40.4

5

0.82

68

0.5

80.3

90.

950.

611.

130.

300.6

00.5

6

0.82

80

1.0

20.4

11.

270.

781.

220.

520.9

50.3

6

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gth

Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.82

91

1.80

0.6

21.4

20.

391.

180.

501.1

00.1

9

0.8

303

0.76

0.4

11.6

90.

900.

750.

481.4

60.4

4

0.8

315

0.83

0.4

72.1

00.

451.

830.

481.0

90.4

5

0.8

326

1.12

0.3

81.2

70.

231.

140.

670.8

80.5

8

0.8

338

1.27

0.4

21.5

60.

291.

450.

340.8

30.4

6

0.8

350

0.82

0.3

51.6

60.

291.

480.

520.4

00.7

8

0.8

361

1.44

0.4

71.6

40.

750.

770.

300.6

70.5

2

0.8

373

1.60

0.4

61.6

60.

761.

020.

621.4

40.7

1

0.8

385

2.07

0.6

61.0

00.

470.

600.

441.3

00.5

5

0.8

396

1.25

0.5

21.4

40.

391.

040.

211.1

20.4

1

0.8

408

1.06

0.2

01.3

20.

431.

420.

411.0

40.2

4

0.8

419

1.52

0.4

81.2

80.

331.

200.

261.2

50.5

9

0.8

431

1.49

0.3

31.6

80.

211.

430.

760.9

10.2

2

0.8

443

1.36

0.2

41.2

60.

420.

910.

421.2

10.5

5

0.8

454

1.42

0.5

01.3

20.

500.

880.

701.4

70.4

4

0.8

466

1.26

0.5

22.0

30.

350.

990.

331.5

20.5

0

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Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.84

78

1.24

0.4

01.7

20.

251.

440.

501.1

20.4

5

0.8

489

0.88

0.4

30.9

60.

601.

450.

461.3

80.3

1

0.8

501

1.10

0.9

01.4

30.

801.

450.

481.0

50.5

9

0.8

512

1.80

0.2

61.6

60.

160.

750.

330.5

70.5

6

0.8

524

1.46

1.4

02.0

30.

501.

270.

210.4

70.6

3

0.8

536

1.05

0.8

91.6

30.

411.

530.

350.0

50.3

7

0.8

547

1.35

0.3

41.3

40.

231.

610.

520.7

70.3

7

0.8

559

1.37

0.2

70.4

50.

571.

190.

181.3

30.7

4

0.8

570

1.93

0.3

81.4

40.

581.

020.

351.0

70.5

3

0.8

582

1.39

0.7

31.4

60.

251.

060.

671.0

30.4

6

0.8

594

1.26

0.4

11.6

10.

601.

110.

280.9

90.4

7

0.8

605

1.65

0.4

61.5

80.

550.

780.

261.5

10.4

5

0.8

617

1.15

0.4

20.9

90.

320.

950.

261.3

20.3

8

0.8

628

1.35

0.5

91.5

20.

520.

930.

550.8

00.3

6

0.8

640

1.29

0.3

61.7

30.

341.

050.

271.6

90.5

2

0.8

652

1.16

0.4

51.2

20.

310.

820.

321.1

40.2

3

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Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.86

63

1.37

0.5

41.3

30.

631.

410.

231.1

50.4

4

0.8

675

1.55

0.5

61.2

50.

431.

310.

271.2

80.2

8

0.8

686

1.46

0.4

91.9

00.

311.

120.

361.6

20.2

8

0.8

699

1.52

0.9

22.2

10.

451.

470.

371.1

40.5

3

0.8

713

1.66

0.5

71.8

70.

461.

080.

431.3

10.5

8

0.8

727

1.70

0.5

11.5

20.

591.

160.

431.0

90.2

2

0.8

741

1.42

0.6

00.9

90.

390.

940.

331.5

00.3

3

0.8

755

1.83

0.4

31.8

40.

521.

260.

251.1

50.5

5

0.8

769

1.43

0.6

91.4

40.

580.

960.

251.8

20.3

8

0.8

783

1.38

0.6

31.7

10.

750.

990.

251.5

10.3

1

0.8

797

1.11

0.6

71.6

90.

531.

730.

291.1

70.2

6

0.8

810

1.70

0.5

62.2

50.

761.

780.

421.4

90.2

5

0.8

824

1.41

0.5

91.7

30.

561.

320.

221.3

90.4

5

0.8

838

0.95

0.4

62.3

60.

551.

460.

551.7

80.3

9

0.8

852

1.54

0.6

31.4

50.

641.

220.

181.6

50.4

8

0.8

866

1.20

0.6

51.4

70.

451.

070.

341.9

10.2

8

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Ep

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1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.88

80

0.96

0.5

21.7

30.

361.

370.

401.0

80.2

6

0.8

894

1.54

0.9

12.0

91.

721.

580.

301.7

30.2

2

0.8

908

1.57

0.6

81.9

60.

491.

320.

491.4

20.6

8

0.8

921

1.47

0.4

61.4

70.

631.

590.

521.2

70.6

3

0.8

935

1.44

0.8

41.6

60.

681.

200.

261.7

50.6

3

0.8

949

1.18

0.4

31.9

40.

601.

390.

581.2

80.2

6

0.8

963

1.49

0.4

32.3

00.

210.

770.

431.4

30.5

9

0.8

977

1.09

0.5

92.5

90.

741.

420.

251.2

90.6

4

0.8

991

1.25

0.8

21.8

40.

911.

570.

511.1

10.2

8

0.9

005

1.44

0.9

61.9

00.

921.

280.

271.4

10.5

4

0.9

019

1.80

0.4

71.9

70.

560.

770.

361.0

90.1

6

0.9

032

1.58

0.3

82.3

70.

991.

090.

371.5

90.5

6

0.9

046

1.56

0.5

81.6

60.

561.

160.

431.1

10.7

5

0.9

060

2.14

0.4

01.4

20.

331.

180.

441.7

20.5

3

0.9

074

1.22

0.5

61.6

40.

691.

300.

451.1

60.3

9

0.9

088

1.66

0.6

10.5

70.

401.

130.

351.3

80.3

6

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Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.91

02

2.03

1.1

51.7

40.

271.

670.

701.0

60.3

7

0.9

116

1.70

0.5

21.5

10.

481.

710.

371.2

70.2

8

0.9

130

1.61

0.7

32.4

30.

891.

750.

681.4

60.6

5

0.9

143

1.04

0.4

31.4

70.

361.

320.

361.5

60.3

4

0.9

157

1.52

0.5

11.7

41.

091.

660.

591.3

70.4

6

0.9

171

1.75

0.6

31.5

20.

561.

410.

291.3

40.6

7

0.9

185

2.31

0.7

82.4

10.

591.

091.

591.3

21.3

4

0.9

199

1.59

0.8

11.4

50.

601.

070.

331.2

00.6

7

0.9

213

1.62

0.6

91.6

40.

241.

410.

201.3

00.3

3

0.9

227

1.09

0.6

41.6

10.

261.

460.

281.2

70.4

9

0.9

240

1.24

0.5

91.7

20.

591.

900.

571.5

10.5

6

0.9

254

1.41

1.1

61.9

90.

871.

040.

481.3

30.4

8

0.9

268

2.11

0.8

62.1

10.

611.

600.

641.8

40.3

6

0.9

282

1.48

0.7

43.1

30.

731.

130.

421.7

90.4

6

0.9

296

1.95

0.6

12.3

50.

621.

340.

531.8

70.5

8

0.9

310

1.62

1.1

91.4

31.

001.

290.

821.9

30.6

2

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Ep

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1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.93

23

1.50

0.8

31.9

71.

370.

860.

541.7

20.6

5

0.9

337

2.02

1.1

31.1

60.

690.

720.

851.0

95.0

5

0.9

351

2.94

1.0

7-0

.22

1.22

0.45

0.81

1.6

80.6

9

0.9

364

1.92

1.8

01.4

90.

921.

080.

791.8

30.5

4

0.9

378

2.27

1.0

21.9

30.

861.

920.

351.5

50.6

6

0.9

392

2.17

0.7

41.5

20.

541.

190.

451.5

20.6

7

0.9

405

1.23

0.5

41.9

10.

451.

330.

311.4

40.3

6

0.9

419

2.08

0.4

21.8

50.

421.

350.

372.2

10.5

9

0.9

432

1.69

0.6

11.7

50.

361.

450.

721.7

10.7

0

0.9

446

1.44

0.5

11.2

80.

371.

620.

271.6

10.5

6

0.9

460

1.20

0.5

41.1

50.

641.

780.

541.2

30.4

6

0.9

473

1.34

0.7

72.3

20.

531.

800.

790.7

80.5

3

0.9

487

1.18

0.9

51.2

20.

451.

520.

601.4

00.3

9

0.9

500

1.16

0.4

21.5

10.

381.

620.

671.6

30.5

1

0.9

514

1.01

0.7

02.0

20.

301.

310.

511.7

60.3

6

0.9

527

1.81

0.3

31.4

80.

431.

160.

561.0

70.3

9

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Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.95

41

1.91

0.4

41.7

90.

241.

400.

551.5

50.5

4

0.9

555

1.96

0.7

01.0

10.

431.

320.

381.4

20.8

4

0.9

568

2.06

0.3

91.8

90.

361.

560.

531.5

40.7

5

0.9

582

2.04

0.4

11.9

80.

681.

300.

561.7

00.5

1

0.9

595

1.25

0.2

12.5

40.

460.

980.

551.1

50.3

1

0.9

609

0.78

0.4

62.3

30.

401.

760.

291.2

60.4

2

0.9

622

0.96

0.4

82.0

00.

471.

170.

501.1

90.5

9

0.9

636

1.74

0.5

31.9

40.

571.

360.

621.3

00.7

2

0.9

649

1.65

0.4

82.0

10.

251.

270.

321.7

40.3

2

0.9

663

2.28

0.3

41.6

40.

301.

480.

111.2

90.2

8

0.9

676

2.15

0.4

21.7

10.

280.

920.

351.7

10.4

9

0.9

690

1.71

0.3

21.6

90.

301.

550.

411.3

40.4

4

0.9

703

1.74

0.3

51.7

10.

221.

320.

141.5

70.4

4

0.9

717

1.78

0.3

31.7

70.

421.

300.

391.4

70.4

7

0.9

731

1.72

0.4

11.5

20.

401.

670.

471.2

60.4

0

0.9

744

2.00

0.5

01.6

80.

281.

650.

341.1

40.2

4

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poch

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poch

3E

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4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.97

58

1.61

0.4

42.0

70.

251.

390.

171.7

20.2

3

0.9

771

1.95

0.3

21.9

70.

301.

320.

441.8

20.1

5

0.9

785

2.37

0.2

61.6

90.

171.

420.

291.8

40.3

2

0.9

798

1.46

0.2

62.3

40.

611.

830.

531.2

90.1

4

0.9

812

1.86

0.2

92.0

40.

261.

580.

211.4

90.3

4

0.9

825

1.68

0.4

11.9

50.

391.

100.

351.6

90.4

4

0.9

839

1.68

0.4

62.2

50.

241.

700.

271.5

30.5

3

0.9

852

1.67

0.3

22.3

20.

181.

700.

191.8

00.2

2

0.9

866

1.82

0.2

92.0

10.

471.

810.

271.6

50.2

2

0.9

879

1.75

0.2

31.8

10.

261.

560.

501.4

60.1

6

0.9

893

2.20

0.1

51.9

10.

171.

820.

301.5

80.1

6

0.9

906

1.41

0.6

21.8

20.

281.

770.

291.5

30.1

6

0.9

920

1.95

0.7

32.0

90.

231.

740.

201.8

70.3

7

0.9

933

1.85

0.2

32.2

40.

101.

930.

151.6

80.2

2

0.9

947

1.68

0.5

32.2

60.

551.

680.

261.7

20.2

5

0.9

960

2.10

0.4

01.9

00.

381.

470.

211.3

30.4

5

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Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.99

74

1.80

0.6

22.1

80.

371.

650.

211.4

10.2

2

0.9

987

1.60

0.3

21.5

80.

511.

710.

211.3

90.3

6

1.0

001

1.60

0.4

12.0

70.

211.

650.

401.3

90.2

4

1.0

014

1.84

0.3

31.9

70.

501.

690.

051.6

70.1

6

1.0

028

1.82

0.2

61.8

20.

161.

390.

361.7

90.3

5

1.0

041

1.82

0.3

21.6

60.

161.

710.

461.3

50.4

1

1.0

055

1.69

0.4

21.6

50.

441.

600.

291.2

40.2

0

1.0

068

2.00

0.4

91.8

60.

141.

860.

371.5

70.1

8

1.0

082

1.77

0.7

51.8

90.

121.

780.

251.2

40.2

6

1.0

095

1.89

0.3

12.0

10.

151.

960.

361.4

10.2

7

1.0

109

2.15

0.2

81.9

80.

321.

650.

132.0

40.4

4

1.0

122

1.81

0.4

41.9

80.

341.

570.

221.7

40.3

2

1.0

137

2.04

0.5

22.1

30.

581.

880.

191.3

50.2

1

1.0

153

2.22

0.3

71.9

10.

251.

650.

171.4

10.2

2

1.0

170

1.79

0.2

31.8

50.

281.

570.

221.1

30.2

1

1.0

186

2.39

0.4

51.8

40.

441.

650.

301.4

60.2

1

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poch

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poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.02

02

2.11

0.4

61.9

40.

401.

550.

261.4

30.2

0

1.0

218

1.72

0.3

91.6

90.

471.

610.

241.6

10.2

0

1.0

234

1.69

0.4

01.8

50.

251.

480.

251.4

70.2

1

1.0

251

1.82

0.3

61.8

80.

331.

400.

331.6

50.1

7

1.0

267

2.08

0.4

02.3

00.

431.

620.

141.5

10.1

8

1.0

283

1.91

0.3

51.6

90.

491.

350.

191.5

60.1

2

1.0

299

2.01

0.5

02.0

70.

291.

790.

441.5

50.3

8

1.0

315

1.74

0.2

52.1

60.

521.

390.

101.6

20.2

6

1.0

331

1.83

0.4

71.8

80.

431.

770.

401.6

10.2

9

1.0

348

2.73

0.4

61.6

90.

381.

650.

071.5

20.2

5

1.0

364

1.83

0.3

22.0

10.

481.

850.

461.5

10.1

1

1.0

380

2.07

0.4

92.0

10.

211.

780.

421.9

80.3

0

1.0

396

2.08

0.5

62.1

90.

661.

920.

271.4

60.2

7

1.0

412

1.73

0.3

71.7

30.

401.

510.

451.1

90.2

8

1.0

429

1.88

0.5

72.1

20.

581.

550.

231.6

70.2

6

1.0

445

2.07

0.4

71.6

20.

271.

550.

331.5

90.2

9

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Ep

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1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.04

61

1.89

0.4

12.1

90.

451.

830.

311.4

20.4

8

1.0

477

2.00

0.2

82.4

20.

561.

800.

351.4

40.2

8

1.0

493

1.31

0.3

42.6

10.

401.

840.

231.4

00.2

0

1.0

509

1.76

0.7

42.0

70.

391.

740.

221.5

20.3

0

1.0

525

1.96

0.6

72.0

10.

291.

690.

191.2

00.3

3

1.0

542

1.66

0.4

01.6

80.

461.

740.

201.3

30.2

6

1.0

558

2.14

0.5

51.6

30.

331.

570.

211.5

80.3

0

1.0

574

2.36

0.4

41.7

70.

561.

650.

371.7

40.2

3

1.0

590

2.12

0.5

01.6

50.

541.

510.

131.7

20.3

0

1.0

606

1.80

0.3

52.2

10.

311.

650.

291.6

80.3

0

1.0

622

1.86

0.5

71.8

50.

681.

590.

281.4

40.1

7

1.0

639

1.47

0.4

31.7

10.

461.

610.

211.4

80.2

8

1.0

655

1.81

0.7

32.0

60.

421.

730.

351.7

50.2

1

1.0

671

1.36

0.4

31.3

10.

461.

670.

201.6

90.3

4

1.0

687

2.23

0.8

31.4

20.

491.

860.

491.8

30.2

7

1.0

703

1.84

0.4

31.9

90.

641.

820.

091.6

80.1

6

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poch

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poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.07

19

2.61

0.4

43.0

10.

531.

950.

602.1

60.5

4

1.0

735

2.36

0.5

73.4

90.

741.

880.

291.2

60.4

1

1.0

752

2.08

0.7

82.1

00.

391.

770.

141.0

91.2

0

1.0

768

2.25

0.6

33.0

70.

471.

900.

450.9

76.7

5

1.0

784

2.96

0.5

93.7

80.

281.

630.

261.8

60.1

8

1.0

800

3.10

0.4

62.9

60.

201.

620.

211.5

00.2

9

1.0

816

2.70

0.4

32.8

10.

121.

770.

341.4

80.2

7

1.0

832

2.14

1.5

41.5

50.

422.

010.

401.8

20.4

4

1.0

848

3.67

16.2

42.1

30.

751.

690.

410.6

80.4

2

1.0

865

2.81

0.7

92.2

40.

561.

720.

271.3

60.3

4

1.0

881

2.03

0.3

42.3

30.

422.

030.

261.3

80.4

9

1.0

897

1.95

0.8

61.4

60.

621.

650.

271.5

20.2

5

1.0

913

2.74

0.5

31.9

90.

412.

200.

231.6

40.2

3

1.0

929

1.45

0.6

22.5

00.

521.

620.

381.4

50.4

7

1.0

945

1.92

0.5

42.5

40.

671.

640.

241.7

90.2

3

1.0

961

2.62

0.9

22.2

40.

711.

730.

371.8

90.3

4

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Ep

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poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.09

78

2.57

0.4

41.8

70.

641.

770.

401.8

30.3

8

1.0

994

1.92

0.5

12.2

50.

481.

820.

231.7

70.2

3

1.1

010

2.66

0.7

81.7

00.

921.

580.

511.9

50.2

5

1.1

026

2.55

2.9

61.7

20.

711.

620.

211.8

30.3

8

1.1

042

2.79

1.0

72.0

60.

491.

880.

311.4

40.3

7

1.1

058

2.16

0.4

62.2

70.

861.

620.

281.5

90.2

6

1.1

074

1.93

0.6

41.5

40.

451.

850.

331.5

90.3

2

1.1

090

2.45

0.4

91.7

51.

032.

060.

461.6

70.3

6

1.1

107

2.08

0.7

81.3

60.

631.

700.

191.6

00.4

1

1.1

123

2.13

0.7

21.8

40.

621.

360.

441.7

90.3

5

1.1

139

2.82

0.7

11.2

80.

651.

910.

201.8

70.5

7

1.1

155

2.91

1.0

61.5

80.

902.

241.

011.2

80.6

5

1.1

171

3.24

0.2

91.9

70.

912.

020.

402.8

00.5

7

1.1

187

3.01

1.1

21.7

41.

382.

020.

372.4

70.8

5

1.1

203

3.11

0.8

42.0

51.

732.

270.

452.3

80.5

6

1.1

219

2.97

1.4

62.7

61.

602.

311.

752.1

51.1

8

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poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.12

36

3.81

1.0

62.2

30.

941.

861.

031.6

91.0

3

1.1

251

1.93

0.5

53.1

91.

612.

620.

741.6

70.4

6

1.1

268

2.42

0.8

32.4

50.

501.

850.

371.7

80.6

5

1.1

285

2.89

0.3

62.8

40.

332.

260.

261.9

90.3

7

1.1

301

3.28

0.3

72.2

40.

261.

940.

371.9

90.4

2

1.1

317

2.64

0.2

31.9

20.

231.

680.

201.8

10.1

5

1.1

333

2.95

0.3

32.6

00.

412.

500.

901.9

20.1

3

1.1

350

2.31

0.5

91.9

90.

412.

200.

701.6

10.4

5

1.1

366

2.98

0.2

32.4

50.

161.

710.

491.6

90.5

8

1.1

382

2.90

0.3

32.6

90.

301.

600.

121.8

50.3

0

1.1

398

2.71

0.1

92.4

30.

211.

660.

391.8

10.3

0

1.1

415

2.72

0.1

82.1

40.

242.

060.

211.9

20.3

8

1.1

431

3.16

0.5

11.9

80.

261.

920.

341.4

20.5

1

1.1

447

2.29

0.4

22.3

40.

232.

180.

621.7

70.2

7

1.1

463

3.14

0.4

72.6

90.

351.

580.

542.5

60.8

6

1.1

480

2.82

0.1

52.2

90.

361.

800.

122.1

90.2

6

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Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.14

96

2.47

0.2

72.4

10.

312.

260.

161.9

60.1

2

1.1

512

2.66

0.2

32.1

70.

261.

810.

311.9

70.1

8

1.1

528

2.51

0.2

12.3

60.

641.

890.

342.0

80.2

1

1.1

545

2.82

0.2

92.5

40.

292.

000.

231.9

00.2

7

1.1

561

2.37

0.2

62.5

00.

352.

070.

111.5

10.2

1

1.1

577

2.36

0.3

62.6

40.

492.

030.

331.9

20.0

7

1.1

593

2.27

0.3

02.4

40.

422.

070.

321.8

90.1

6

1.1

609

2.49

0.4

02.7

20.

591.

990.

371.9

80.2

1

1.1

626

2.39

0.1

82.5

60.

181.

710.

162.0

10.2

9

1.1

642

2.58

0.4

92.4

80.

331.

920.

212.0

40.2

7

1.1

658

2.42

0.2

92.4

70.

221.

870.

362.0

10.1

2

1.1

674

2.47

0.1

82.1

80.

141.

970.

092.0

70.0

7

1.1

691

2.42

0.0

92.8

00.

152.

060.

162.2

20.1

4

1.1

707

2.46

0.2

22.5

80.

131.

980.

121.7

70.2

0

1.1

723

2.42

0.4

02.5

90.

161.

770.

291.9

90.1

5

1.1

739

2.38

0.4

82.8

10.

352.

010.

302.0

30.3

1

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3E

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4

[µm

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Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.17

55

2.80

0.2

62.6

00.

091.

910.

091.7

30.2

1

1.1

772

2.84

0.1

42.7

20.

241.

870.

221.9

50.1

5

1.1

788

3.25

0.3

32.4

40.

471.

900.

201.8

00.1

5

1.1

804

3.36

0.2

82.3

40.

231.

840.

192.0

00.0

8

1.1

820

3.25

0.3

62.3

50.

191.

910.

212.1

00.0

8

1.1

836

2.90

0.2

82.6

90.

311.

940.

182.0

10.3

4

1.1

853

3.00

0.2

12.6

20.

212.

060.

142.1

70.1

9

1.1

869

3.08

0.1

92.5

70.

101.

880.

082.0

90.1

2

1.1

885

3.25

0.2

42.4

30.

252.

050.

171.9

30.2

8

1.1

901

3.47

0.1

42.4

00.

181.

860.

221.9

00.1

6

1.1

917

3.28

0.1

52.3

80.

301.

930.

152.0

80.1

8

1.1

934

3.28

0.3

22.3

50.

181.

920.

192.1

90.1

6

1.1

950

3.13

0.1

12.3

80.

451.

960.

252.0

20.1

4

1.1

966

3.53

0.2

12.6

50.

401.

830.

211.9

60.2

1

1.1

982

3.28

0.3

72.5

80.

421.

850.

131.8

40.2

3

1.1

998

2.93

0.3

92.7

70.

182.

010.

242.1

40.1

0

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Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.20

15

3.78

0.5

02.7

90.

241.

940.

141.7

90.1

5

1.2

031

3.35

0.2

52.4

80.

151.

760.

332.2

00.4

2

1.2

047

3.24

0.3

32.2

60.

181.

830.

130.6

711.

28

1.2

063

3.38

0.3

92.7

50.

431.

860.

161.8

80.6

3

1.2

079

3.18

0.2

13.0

60.

582.

010.

081.5

00.3

0

1.2

096

3.05

0.2

43.2

10.

201.

930.

141.7

60.2

6

1.2

112

3.05

0.2

82.5

80.

202.

060.

362.0

20.1

4

1.2

128

2.74

0.2

12.6

20.

381.

890.

242.0

10.5

3

1.2

146

3.37

0.5

02.6

60.

311.

920.

152.0

60.2

2

1.2

165

3.36

0.2

12.6

90.

311.

940.

191.9

40.2

3

1.2

185

3.27

0.3

42.7

30.

151.

740.

252.3

60.2

6

1.2

204

3.52

0.3

32.5

00.

202.

030.

362.1

60.1

6

1.2

223

3.37

0.2

42.7

10.

221.

990.

171.9

30.2

7

1.2

243

3.57

0.3

62.6

90.

232.

080.

151.7

90.1

5

1.2

262

3.29

0.4

12.7

00.

362.

130.

191.8

60.2

3

1.2

282

3.44

0.3

52.6

80.

242.

170.

172.0

40.4

3

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poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.23

01

3.46

0.2

73.0

10.

251.

970.

232.1

80.1

0

1.2

320

3.39

0.3

42.8

30.

362.

130.

142.0

50.1

5

1.2

340

3.38

0.4

02.8

20.

381.

990.

071.9

30.1

7

1.2

359

3.62

0.3

22.4

60.

321.

890.

122.3

00.2

6

1.2

379

3.28

0.2

72.4

50.

111.

990.

142.0

60.1

9

1.2

398

3.45

0.3

62.8

50.

172.

160.

131.9

40.1

7

1.2

417

3.23

0.4

02.8

00.

361.

910.

201.9

90.1

5

1.2

437

3.53

0.2

62.6

00.

192.

050.

292.1

00.1

3

1.2

456

3.56

0.7

92.8

40.

342.

090.

202.0

40.1

3

1.2

475

3.31

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02.9

60.

212.

040.

132.2

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7

1.2

495

3.41

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32.9

00.

161.

900.

212.0

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1

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514

3.40

0.2

73.1

10.

212.

200.

181.8

30.2

4

1.2

534

3.16

0.4

73.0

20.

282.

100.

132.2

20.1

7

1.2

553

3.56

0.3

02.7

50.

291.

910.

102.2

00.1

1

1.2

572

3.96

0.4

52.7

00.

192.

120.

141.9

50.2

3

1.2

592

3.81

0.5

42.0

90.

371.

870.

322.2

00.2

4

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Ep

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1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.26

11

4.37

0.2

82.6

20.

242.

260.

362.4

10.4

9

1.2

630

3.56

0.1

72.7

50.

252.

330.

222.1

90.1

2

1.2

650

3.70

0.4

22.4

60.

382.

250.

172.3

90.2

9

1.2

669

3.54

0.4

82.5

90.

632.

080.

211.9

80.2

3

1.2

689

3.75

0.4

32.7

70.

432.

290.

412.5

80.5

6

1.2

708

3.45

0.3

42.5

30.

282.

330.

372.2

10.3

0

1.2

727

3.52

0.3

02.4

00.

252.

220.

172.1

10.1

6

1.2

747

3.14

0.3

63.0

10.

422.

150.

332.1

70.4

2

1.2

766

3.19

0.3

83.5

30.

512.

190.

472.2

30.4

3

1.2

785

3.30

0.3

12.4

80.

331.

990.

161.9

10.2

9

1.2

805

3.26

0.2

72.3

40.

202.

190.

522.1

90.2

0

1.2

824

3.72

0.2

62.6

50.

252.

050.

192.1

30.2

8

1.2

843

3.63

0.5

32.5

70.

122.

210.

322.0

90.2

7

1.2

863

3.69

0.3

12.7

60.

221.

920.

192.1

00.1

6

1.2

882

3.06

0.3

72.7

30.

242.

030.

172.2

00.1

6

1.2

901

2.97

0.4

92.7

90.

422.

090.

672.3

20.4

8

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3E

poch

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[µm

]F

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Jy]

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Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.29

21

3.21

0.4

73.2

70.

752.

180.

332.3

00.4

3

1.2

940

3.16

0.4

63.0

10.

312.

220.

282.4

40.3

3

1.2

960

3.17

0.2

82.8

80.

312.

340.

382.1

60.1

2

1.2

979

3.19

0.2

62.8

70.

282.

180.

222.2

40.2

0

1.2

998

3.20

0.3

23.0

50.

312.

160.

252.2

40.1

5

1.3

018

3.37

0.5

02.6

10.

802.

260.

322.2

70.3

7

1.3

037

3.77

0.6

72.4

30.

322.

410.

172.3

60.2

0

1.3

056

3.36

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12.5

40.

282.

250.

222.2

50.2

4

1.3

076

2.75

0.5

02.8

30.

302.

120.

352.0

90.2

6

1.3

095

3.51

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72.6

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562.

170.

382.3

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2

1.3

114

3.48

0.3

72.8

30.

412.

290.

192.2

20.1

4

1.3

134

3.25

0.2

33.0

30.

442.

310.

462.2

90.2

8

1.3

153

3.63

0.7

52.9

50.

522.

140.

252.3

20.2

8

1.3

172

3.83

0.4

02.9

30.

462.

420.

262.4

70.2

2

1.3

192

3.92

0.3

12.6

80.

342.

200.

182.4

60.1

3

1.3

211

3.66

0.4

32.7

30.

242.

520.

522.2

30.1

7

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poch

2E

poch

3E

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[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.32

30

4.04

0.7

83.2

00.

512.

610.

472.7

90.2

9

1.3

250

3.66

0.3

71.9

71.

062.

860.

802.3

10.1

6

1.3

269

3.78

0.6

73.0

00.

462.

190.

362.3

60.3

1

1.3

288

4.07

0.6

63.5

10.

672.

340.

202.2

80.3

2

1.3

308

3.57

0.6

02.9

70.

912.

640.

262.3

10.1

0

1.3

327

3.98

1.0

72.7

40.

772.

180.

652.8

80.4

8

1.3

346

3.87

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43.6

40.

612.

680.

342.4

90.2

3

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366

3.93

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52.6

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622.

400.

342.8

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0

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385

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10.

672.

800.

353.7

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8

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404

3.66

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73.2

50.

812.

480.

382.8

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1

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080.

162.7

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1

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592.4

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482

4.81

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590.

782.7

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7

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501

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031.

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281.

280.

992.3

20.6

6

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Ep

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poch

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poch

3E

poch

4

[µm

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Err

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Jy]

Err

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Jy]

Err

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1.35

39

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6.1

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132.

972.

181.8

41.7

7

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559

3.66

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84.6

312

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4.13

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578

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217.

344.

684.2

25.0

5

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597

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112

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728

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4-1

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91-2

5.29

73.0

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636

6.29

16.7

85.6

915

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10.7

311

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0

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7-2

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9.53

10.5

847.

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Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

]F

lux[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.38

49

24.2

69.

25

-2.7

420

.59

0.94

18.7

58.1

718.

39

1.3

868

9.20

2.9

63.5

43.

923.

651.

806.0

33.7

0

1.3

887

8.24

5.4

80.7

44.

122.

265.

743.4

53.6

3

1.3

906

7.22

2.0

24.3

22.

753.

823.

005.1

32.5

6

1.3

926

11.3

110

.69

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510

.66

2.81

6.89

2.7

02.7

0

1.3

945

8.45

92.4

92.9

731

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5.23

23.1

8-3

.50

54.1

3

1.39

64

1.24

98.2

725

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75.4

65.

6751

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3.77

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382.3

21.0

3

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003

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888

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276

.74

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714

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49.

17

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4.47

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77.9

09.

395.

333.

834.5

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042

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88

5.5

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583.

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763.2

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8

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100

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0.6

13.6

30.

273.

930.

843.5

01.2

3

1.4

119

4.11

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593.

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8

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40.

703.

180.

481.8

30.5

4

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Ep

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poch

2E

poch

3E

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4

[µm

]F

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Jy]

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Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.41

57

4.09

0.8

94.0

31.

203.

610.

702.1

50.5

9

1.4

177

4.37

0.6

23.8

50.

312.

760.

563.1

80.5

6

1.4

196

5.19

0.7

22.9

20.

784.

460.

912.8

90.3

9

1.4

215

4.32

0.2

43.4

00.

223.

130.

342.5

70.1

9

1.4

235

4.33

0.3

43.4

00.

532.

520.

473.0

20.5

1

1.4

254

4.17

0.1

83.6

70.

132.

450.

273.1

90.2

3

1.4

273

5.31

0.5

33.6

50.

322.

750.

523.4

10.5

6

1.4

293

4.73

0.2

93.7

50.

242.

870.

223.0

50.4

4

1.4

312

4.49

0.4

83.8

50.

352.

950.

312.9

60.3

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1.4

331

4.30

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73.9

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332.

820.

492.8

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1.4

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253.3

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2

1.4

370

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73.7

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452.

950.

183.2

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1

1.4

389

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73.5

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323.

050.

463.1

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6

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408

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94.0

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243.

120.

373.2

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6

1.4

428

3.96

0.2

73.9

10.

273.

150.

223.1

50.4

1

1.4

447

3.80

0.1

33.5

80.

282.

820.

192.9

50.2

5

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Ep

och

1E

poch

2E

poch

3E

poch

4

[µm

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Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.44

66

3.95

0.3

13.3

90.

272.

700.

312.8

40.3

2

1.4

486

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082.7

80.1

6

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352.8

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3

1.4

527

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53.1

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312.

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512.6

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3

1.4

547

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8

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628

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63.4

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142.9

50.1

8

1.4

649

3.77

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73.5

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242.

660.

152.7

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1

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669

4.18

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522.

780.

243.2

80.4

3

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689

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213.

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730

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312.

790.

223.1

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7

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750

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0.4

83.4

70.

172.

480.

382.5

70.3

6

1.4

770

4.30

0.3

93.4

20.

302.

800.

352.5

20.3

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[µm

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Flu

x[m

Jy]

Err

[mJy]

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x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.47

90

4.37

0.4

73.8

90.

512.

740.

262.9

20.5

7

1.4

811

4.39

0.6

03.7

70.

292.

860.

252.6

40.1

1

1.4

831

3.74

0.7

53.5

30.

393.

200.

622.9

50.2

4

1.4

851

4.16

0.3

73.4

00.

393.

040.

252.9

30.2

5

1.4

871

4.23

0.3

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90.

503.

020.

352.8

30.1

8

1.4

892

4.15

0.4

33.7

90.

463.

130.

672.8

80.2

9

1.4

912

3.70

0.4

33.3

50.

322.

720.

152.8

20.2

1

1.4

932

4.06

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80.

352.

570.

253.2

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5

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952

3.85

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43.3

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690.

202.7

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8

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973

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63.2

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93.3

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0

1.5

033

3.77

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93.3

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352.

790.

172.5

80.2

2

1.5

053

3.81

0.4

03.6

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712.

360.

872.8

80.9

4

1.5

074

3.85

0.3

53.7

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372.

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5

1.5

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0.2

53.0

20.

282.

900.

362.8

50.2

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Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.51

14

3.80

0.2

63.5

90.

062.

710.

252.6

60.4

0

1.5

134

3.69

0.2

03.5

00.

262.

630.

302.8

70.1

1

1.5

155

3.64

0.1

23.4

00.

212.

610.

092.9

50.1

2

1.5

177

3.73

0.3

33.5

50.

332.

600.

102.8

20.3

4

1.5

201

3.92

0.2

33.4

70.

182.

670.

452.8

70.2

8

1.5

225

3.70

0.0

73.5

00.

192.

700.

352.9

20.2

9

1.5

249

4.20

0.3

73.6

10.

543.

000.

172.7

80.3

5

1.5

274

4.02

0.2

13.7

50.

423.

020.

212.8

30.2

5

1.5

298

3.71

0.2

63.4

20.

252.

620.

372.9

00.3

1

1.5

322

3.80

0.4

83.6

60.

392.

760.

312.9

00.4

8

1.5

346

4.12

0.2

63.3

80.

162.

680.

372.9

70.4

0

1.5

371

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43.5

40.

172.

870.

172.9

30.2

6

1.5

395

4.04

0.3

83.3

00.

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820.

113.3

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0

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419

4.22

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03.4

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222.

710.

232.9

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3

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443

3.96

0.2

13.5

20.

732.

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152.8

60.3

4

1.5

468

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23.4

20.

282.

910.

172.8

10.1

9

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Jy]

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Jy]

Err

[mJy]

1.54

92

3.80

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03.3

40.

172.

730.

172.9

60.2

3

1.5

516

4.11

0.2

13.4

80.

343.

080.

302.9

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8

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540

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0.3

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00.

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800.

382.8

20.3

3

1.5

564

4.03

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33.6

20.

432.

890.

313.0

50.2

1

1.5

589

4.46

0.3

83.6

70.

442.

860.

603.1

40.5

0

1.5

613

4.46

0.4

03.6

90.

392.

660.

202.9

50.1

8

1.5

637

4.24

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43.7

30.

452.

830.

212.9

50.4

1

1.5

661

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33.6

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452.

550.

373.0

80.3

1

1.5

685

4.25

0.3

33.4

50.

282.

900.

252.9

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1

1.5

710

4.39

0.3

83.4

80.

462.

550.

363.0

40.2

4

1.5

734

4.21

0.4

13.5

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352.

990.

172.9

20.3

0

1.5

758

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252.

700.

153.0

90.1

9

1.5

782

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0.3

53.4

30.

212.

840.

182.6

80.2

4

1.5

806

4.18

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93.5

20.

242.

810.

282.9

70.3

1

1.5

831

4.08

0.4

54.2

10.

672.

810.

523.2

20.7

3

1.5

855

4.14

0.3

33.7

10.

332.

830.

173.0

50.3

2

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Jy]

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Flu

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Jy]

Err

[mJy]

1.58

79

4.16

0.2

13.5

90.

472.

730.

142.9

50.1

7

1.5

903

4.16

0.3

53.4

00.

322.

630.

273.1

70.2

9

1.5

927

4.34

0.2

53.5

60.

282.

870.

162.9

30.1

5

1.5

952

4.27

0.3

93.6

40.

242.

760.

213.0

50.2

8

1.5

976

4.13

0.5

63.7

50.

362.

630.

483.0

30.2

0

1.6

000

4.48

0.4

23.8

20.

393.

150.

263.1

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4

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024

4.49

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93.1

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333.

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373.2

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3

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048

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63.4

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402.

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253.2

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1

1.6

072

4.41

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84.0

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463.

160.

252.8

60.3

3

1.6

097

3.79

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33.7

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192.

690.

172.9

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1.6

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653.

090.

592.9

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253.2

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7

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283.3

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5

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217

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93.5

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542.

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222.9

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6

1.6

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23.5

10.

613.

000.

402.8

00.4

9

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1.62

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223.1

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290

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0

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452.7

80.5

4

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362

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572.

850.

223.4

40.4

1

1.6

387

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653.

300.

333.1

80.1

2

1.6

411

4.40

0.5

43.4

40.

252.

910.

373.2

40.2

0

1.6

435

4.27

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40.

642.

940.

213.0

30.3

8

1.6

459

4.42

0.2

73.8

70.

223.

090.

373.1

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4

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483

4.46

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13.9

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362.

890.

753.3

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5.08

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93.5

80.

392.

990.

433.2

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6

1.6

531

4.58

0.2

93.8

80.

423.

010.

303.2

80.3

6

1.6

556

4.48

0.4

93.5

90.

243.

220.

203.2

30.4

2

1.6

580

4.58

0.4

93.9

60.

353.

070.

273.3

00.1

8

1.6

604

4.56

0.4

33.8

50.

263.

050.

183.2

40.2

2

1.6

628

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00.

202.

930.

133.0

10.1

7

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Flu

x[m

Jy]

Err

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Jy]

Err

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Flu

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Jy]

Err

[mJy]

1.66

52

4.62

0.1

93.6

70.

133.

050.

273.0

00.2

2

1.6

676

4.78

0.5

84.3

40.

713.

410.

623.2

90.5

0

1.6

701

4.66

1.0

13.4

00.

543.

840.

733.3

80.4

7

1.6

725

4.54

0.2

23.8

00.

433.

360.

363.3

10.1

6

1.6

749

4.67

0.4

03.8

80.

292.

930.

263.1

00.2

6

1.6

773

4.61

0.5

44.4

70.

683.

160.

292.9

00.3

9

1.6

797

4.55

0.4

43.8

80.

213.

260.

363.2

90.2

0

1.6

821

4.51

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83.7

80.

103.

190.

313.1

10.1

7

1.6

845

4.48

0.4

84.0

30.

522.

810.

243.2

40.2

0

1.6

870

4.74

0.3

23.9

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313.

220.

273.0

80.2

3

1.6

894

4.53

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53.5

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403.

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783.2

50.5

1

1.6

918

4.67

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90.

443.

530.

263.1

70.4

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942

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443.2

70.4

5

1.6

966

4.75

0.5

33.8

60.

433.

250.

463.4

30.8

2

1.6

990

4.59

0.5

44.2

00.

533.

210.

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80.3

2

1.7

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0.6

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80.

473.

141.

013.2

20.7

6

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Jy]

Err

[mJy]

1.70

38

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93.4

90.

193.

240.

213.4

40.3

4

1.7

063

4.43

0.1

84.0

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563.

350.

323.5

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7

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087

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84.1

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482.

780.

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80.3

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111

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04.2

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362.

880.

273.3

30.5

1

1.7

135

4.52

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553.

270.

583.6

00.6

6

1.7

159

5.15

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503.

270.

373.1

40.3

2

1.7

183

4.66

0.5

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130.

193.5

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7

1.7

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83.7

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443.

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573.4

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543.2

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256

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253.

780.

403.6

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333.7

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1.7

304

4.69

0.7

04.0

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373.

260.

293.5

90.5

5

1.7

328

4.52

0.8

53.8

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312.

960.

443.4

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6

1.7

352

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44.5

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493.

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463.4

90.3

0

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376

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63.8

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513.

480.

473.4

80.5

0

1.7

400

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0.6

24.1

70.

423.

450.

443.1

70.4

3

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Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

1.74

25

4.89

0.6

63.7

50.

593.

250.

403.3

50.6

8

1.7

449

4.29

0.3

23.6

70.

423.

380.

653.7

70.6

1

1.7

473

4.36

0.3

33.8

70.

373.

440.

253.6

40.2

5

1.7

497

4.94

0.8

84.4

10.

513.

380.

503.2

90.5

7

1.7

521

4.66

0.2

34.4

90.

343.

450.

363.2

60.4

5

1.7

545

4.99

0.6

64.1

80.

273.

520.

433.3

50.2

9

1.7

569

4.79

0.8

13.9

80.

203.

170.

553.3

80.4

6

1.7

594

4.66

0.5

24.5

10.

483.

760.

573.3

20.4

6

1.7

618

4.91

0.5

14.3

60.

603.

220.

373.2

80.3

7

1.7

642

4.57

1.3

84.0

60.

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666

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782.7

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5

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738

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2

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787

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90.

583.

550.

463.5

40.5

7

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1.78

11

4.41

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93.9

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553.

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884.4

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835

5.81

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53.7

00.

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823.5

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0.7

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453.1

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53.7

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763.

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9

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907

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554.3

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1.7

932

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573.

770.

624.3

10.7

9

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956

4.12

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44.0

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96N

aN5.7

5N

aN

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1.88

20

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00.

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2

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9

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6

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623.

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9

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52.7

4

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280

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388

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94.6

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374.

160.

494.2

30.1

6

1.9

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6.76

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64.8

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163.

890.

604.8

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469

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631

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80.4

2

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Jy]

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1.96

85

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0.4

14.5

70.

674.

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6

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5.97

0.3

64.5

10.

214.

120.

663.9

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5

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738

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383.7

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6

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34.5

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7

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792

5.63

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134.

100.

273.5

60.2

1

1.9

819

5.25

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34.4

80.

153.

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273.9

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44.4

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263.8

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1

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900

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9

1.9

927

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40.6

0

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2.01

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323

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355

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80.5

6

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2.06

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8

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40.2

1

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5

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Jy]

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2.16

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910.

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7

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9

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574.0

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764.3

50.4

2

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7

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0

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60.

240.

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440.7

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x[m

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Err

[mJy]

Flu

x[m

Jy]

Err

[mJy]

0.91

02

1.30

0.4

41.6

40.

280.

790.

330.7

90.3

9

0.9

116

1.53

0.5

81.4

30.

590.

930.

420.5

60.5

9

0.9

130

1.82

0.3

41.3

80.

450.

760.

390.6

50.6

5

0.9

143

1.73

0.4

61.4

10.

450.

430.

540.7

70.4

0

0.9

157

1.92

0.4

31.3

70.

700.

600.

391.0

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2

0.9

171

1.48

0.5

52.0

30.

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090.

420.7

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9

0.9

185

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81.3

20.

671.

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6

0.9

199

1.82

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11.4

70.

700.

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0.92

13

1.41

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31.9

00.

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460.3

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4

0.9

227

1.66

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01.6

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240

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00.

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240.8

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9

0.9

254

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6

0.9

268

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4

0.9

282

1.51

0.4

41.6

20.

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751.0

10.5

2

0.9

296

1.40

0.6

51.4

30.

591.

060.

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70.3

7

0.9

310

1.48

0.4

61.7

41.

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630.

580.8

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0.93

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0.91

0.93

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9

0.9

392

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450.8

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0.9

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31.2

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360.4

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2

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0.95

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31.9

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1

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9

0.9

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90.3

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0.97

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0.99

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1.04

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1.32

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1.35

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Jy]

Err

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x[m

Jy]

Err

[mJy]

1.38

49

5.13

23.8

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027

.76

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511

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116

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1.38

68

2.92

2.1

33.9

12.

582.

243.

662.1

61.4

5

1.3

887

2.32

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4.95

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0

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5

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1.39

64

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8085

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34

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0

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003

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01.

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311.1

30.2

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1.41

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9

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82.6

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30.1

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Jy]

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1.44

66

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486

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211.7

60.3

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1.47

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1.51

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1.58

79

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5

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80.2

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1.66

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5N

aN

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2.06

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최근 소수의 감마선 폭발 천체가 매우 긴 주기를 보이며 관측되었다. 이들은 매우

긴 감마선 폭발 천체라고 불리며 그 주기가 1,000초 혹은 10,000초를 넘어선다. 그 중

GRB 111209A는 적색편이 z = 0.677에서 관측되었고, 그 주기는 관측자의 입장에서

볼 때 7시간 정도로 지금까지의 감마선 폭발 천체 중 가장 긴 주기를 가지고 있다.

우리는 나사(NASA)의 3m 적외선 망원경 시설(Infrared Telescope Facility, IRTF)을

이용하여 이 매우 긴 감마선 폭발 천체의 이른 시간 근적외선 스펙트럼을 관측하였다.

이 데이터는 X 선부터 라디오에 이르는 영역에서 이른 잔광을 관측한 유일한 스펙트럼

데이터이다. 이 데이터의 플럭스 측정을 비교하기 위해 같은 시간대에 관측된 TAROT

R영역데이터를함께사용하였으며,결과적으로근적외선스펙트럼은 β = 1.22±0.03

에 해당하는 전자의 싱크로트론 복사를 나타내고 있었다. 이로부터 얻어진 전자의 멱

법칙 에너지 분포 지수는 p 2.4로 나타났으며, 이는 일반적으로 사용되는 지수 값과

일치하는 결과이다. 이 매우 긴 감마선 폭발 천체에서 열적 복사에 해당하는 부분은

싱크로트론 복사에 묻혀 전혀 알아볼 수 없었다. 그리고 매우 긴 감마선 폭발 천체가

짧은/긴감마선폭발천체처럼공통적인모체를가질수있는지알아보기위해또다른

매우 긴 감마선 폭발 천체인 GRB 101225A의 스펙트럼과 비교해 보았다. 이 매우 긴

감마선 폭발 천체는 GRB 111209A와 전혀 다르게 강한 열적 복사의 진화양상을 나타

내었으며, 이로부터 두 천체는 다른 모체에서 형성된 것이라는 결론을 내릴 수 있었다.

이때 GRB 111209A는 금속함량이 적고 핵심부가 붕괴하는 청색거성을 모체로 하고,

GRB 101225A는헬륨별과중성자별이합병하는과정에서공통외피의단계에있을때

형성된것으로생각한다.또한,우리는두종류의특성진동수 νc와 νm의계산을통하여

외부 충격파 모형이 유효한지 알아보았다. 그 결과 이론적으로는 스펙트럼에서 보이는

싱크로트론 복사의 기울기가 만족될 수 있으나, 현실에서 그대로 적용하기에는 무리가

있다는 것을 알 수 있었다. 이에 갈음하여 비록 간단한 논의로 이루어졌지만 매우 강한

자기장을 가진 중성자별이 새로운 모체가 될 수 있음을 싱크로트론 복사 이론으로부터

확인할 수 있었다.

주요어: 감마선폭발천체:일반−감마선폭발천체:개별 (GRB 111209A, GRB101225A)

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Page 147: Disclaimer - Seoul National UniversityGamma-Ray Burst 111209A ... tically expanding reball with a relativistic ejecta as a shape of shells (Goodman ... internal shocks occur when relatively

학 번: 2015-20363

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