MIKE High Resolution Observation
and Raman-scattering by Atomic Hydrogenin the Symbiotic Nova RR Telescopii

Jeong-Eun Heo1, Hee-Won Lee1, Rodolfo Angeloni2, Tali Palma3, Francesco Di Miile4
1

Sejong University, Korea
2
Universidad de La Serena, Chile
3
Observatorio Astronómica, Argentina
4
Las Campanas Observatory, Chile

CONTENTS
I. Introduction- [C II] 158 μm- C II 1036, 1037 Doublet- Raman-Scattered C II Lines

II. Observation- RR Tel- MIKE Spectroscopy- Raman Lines in RR Tel

III. Raman C II and ISM- Incident C II 1036, 1037 Emissions- C II 1335 Triplet- Optical Depth of C II Emissions- Extinction of ISM

IV. Summary and Discussion

I. Introduction✓ [C II] 158 μm and ISM
INTRODUCTIONOBSERVATIONSIMULATION-2P3/2 — 2P1/2 : 157.74 μm-

In cold regions, cooling is dominated by collisional excitation of C+ bycollisions with other particles (e.g, H or free electrons and protons).

-An efficient and dominating coolant for neutral gas-

Powerful spectral diagnostics of ISM

C IIDISCUSSION

T*~∆E/k=91.25 K[C II] 157.74 μm2PP3/2
P1/22S2 2P1

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I. Introduction✓ C II 1036, 1037 Doublet
INTRODUCTIONOBSERVATION-2S 2P2 2S1/2 — 2S2 2P1 2P01/2 : 1036.337 Å-

2S 2P2 2S1/2 — 2S2 2P1 2P03/2: 1037.018 ÅSIMULATIONC IIDISCUSSION

2PCCIIII

10103736

2SP3/2
P1/2
2S2 2P1

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2S 2P2

I. Introduction✓ C II 1036, 1037 Doublet
INTRODUCTION-The CII 1036, 1037 photons are incident on H I in the ground state toexcite them in an intermediate level.

OBSERVATIONSIMULATIONHIDISCUSSION

3SC II

703
II 1C@ Ishigaki Island, Japan
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03C603
II 1CEAYAM 2017

II 1

II 1C2S1S

703

62S2P

P3/2
P1/2
2S2 2P1

2S 2P2

I. Introduction✓ Raman-scattered C II Lines
INTRODUCTION-

The H I de-excite to 2S level with re-emission of an optical photon withcenter wavelength at 7025 and 7052, respectively.

OBSERVATION-C II 1036 → Raman scattering by H I → Raman C II at 7023.24 Å-C II 1037 → Raman scattering by H I → Raman C II at 7053.30 Å

SIMULATIONHIDISCUSSION

3S6C

II 103703
II 1C1S
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3Ra n 702aRam

2S

I. Introduction✓ Raman-scattered C II Lines
INTRODUCTIONOBSERVATIONSIMULATIONDISCUSSIONEAYAM 2017
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Only detected in the symbiotic nova V1016 Cyg (Schild & Schmid, 1996)

II. Observation✓INTRODUCTIONRR Telescopii-OBSERVATION-SIMULATION-

D(Dusty)-type symbiotic nova consisting of a Mira variable
and a white dwarf (Whitelock 2003)
After a nova-like outburst in 1944, its brightness is slowly
fading from its peak V∼7mag in 1946 to V∼11.5 mag in 2017.
Distance ~ 2.6 kpc (Schmid & Schild 2002)

DISCUSSION

Basic Parameters for RR Tel(Feast et al. 1983; Mürset & Schmid 1999; Gromadzki et al. 2009)

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Gromadzki et al. (2009)

II. Observation✓INTRODUCTION

MIKE High Resolution Spectroscopy-OBSERVATION-SIMULATION-DISCUSSIONEAYAM 2017
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The Magellan Inamori Kyocera Echelle (MIKE)
6.5m Clay Telescope, Las Campanas Observatory, Chile
Spectral Coverage: (Blue) 3,350~5,000 Å (Red) 4,900~9,500 ÅResolving Power (Blue) R ~ 27,000 (Red) R~ 35,500
Observing Date: 30, July, 2016
Exposure Time: 2000 sec

II. Observation✓Raman-scattered C II Lines in RR Tel

INTRODUCTIONOBSERVATION

7.0

Raman C II

Gaussians

SIMULATIONDISCUSSION

Flux [× 10−14 erg cm−2 s−1 Å−1]

6.0

F(Raman 7023)
6.01x10-14 erg cm-2 s-1

5.0

4.0

F(Raman 7053)
6.74x10-14 erg cm-2 s-1

3.0

2.0

1.00.0
7000

7010

7020

7030

7040

λ[Å]

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-1

7050

7060

7070

7080

7090

-1

III. Raman C II and ISM

INTRODUCTIONOBSERVATION✓ Incident Far-UV C II 1036,1037 Emissions

Incident C II

Raman C II
F(Raman 7023)
6.01x10-14 erg cm-2 s-1

SIMULATIONDISCUSSION

RamanConversion
Eﬃciencies

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F(Raman 7053)
6.74x10-14 erg cm-2 s-1-1-1

III. Raman C II and ISM

INTRODUCTIONOBSERVATIONSIMULATIONDISCUSSION✓ Incident Far-UV C II 1036,1037 Emissions

Incident C II

Raman C II

Fint(1036)
3.15x10-11 erg cm-2 s-1

F(Raman 7023)
6.01x10-14 erg cm-2 s-1

Fint(1037)
4.19x10-11 erg cm-2 s-1

-1-1

Raman
Conversion
Eﬃciencies

η(1036->7023)
0.12
η(1037->7053)
0.10
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F(Raman 7053)
6.74x10-14 erg cm-2 s-1-1-1

III. Raman C II and ISM

OBSERVATIONSIMULATIONDISCUSSION

Incident C II
Fint(1036)
3.15x10-11 erg cm-2 s-1
Fint(1037)
4.19x10-11 erg cm-2 s-1

Expected Spectrum
FUSE(2002−06−14)

3.5-1-1

Flux [× 10−10 erg cm−2 s−1 Å−1]

INTRODUCTION✓ Comparison with FUSE data

C II 1037

32.5

C II 1036

21.5

10.5

01035.8

1036

1036.21036.41036.61036.81037

1037.21037.4λ[Å]✓ A significant amount of C II 1036 and 1037 Å emissions are expected,

however they are clearly absent in FUSE data.
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III. Raman C II and ISMINTRODUCTION✓ C II 1335 Multiplet in IUE Spectrum-2s2p2 2D — 2s22p 2P0: 1334.53, 1335.66 and 1335.71Å

OBSERVATION
3025CI105I 103615I 10DISCUSSION

372S20CI

SIMULATIONC II’rrtel_iue_l.txt’ u 1:($2)*1e13

2D0−51332

1333

1334

1335

1336

1337

Fobs(1335)
4.43x10-13 erg cm-2 s-1
Fobs(1336)
7.15x10-13 erg cm-2 s-1
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5T1338-1-12P

D5/2
D3/2letP3/2 133II
P1/2 C2S 2P22S2 2P1

III. Raman C II and ISM

INTRODUCTION✓ C II 1335 Multiplet-2s2p2 2D — 2s22p 2P0: 1334.53, 1335.66 and 1335.71Å

OBSERVATIONC IISIMULATION

CI

Fint(1335) = Fint(1036) x Υ1335/Υ1036

2P@ Ishigaki Island, Japan
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372Dpir
5TFint(1336) = Fint(1037) x Υ1336/Υ1037

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I 10

DISCUSSION

CI

36

2S

D5/2
D3/2letP3/2 133
IIP1/2 C2S 2P22S2 2P1

III. Raman C II and ISM

INTRODUCTION✓ C II 1335 Multiplet in IUE Spectrum-2s2p2 2D — 2s22p 2P0: 1334.53, 1335.66 and 1335.71Å

OBSERVATION
5000SIMULATION

4000

Expected Spectrum
IUE data

C II 1335

C II 1336

3000

DISCUSSION
2000

100001333.5

1334

Fint(1335) = Fint(1036) x Υ1335/Υ1036
7.41x10-11 erg cm-2 s-1 -1 ~167 Fobs(1335)
Fint(1336) = Fint(1037) x Υ1336/Υ1037
1.425x10-10 erg cm-2 s-1 -1-11~200 Fobs(1336)
EAYAM 2017
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1335.51336

1336.5

III. Raman C II and ISM

INTRODUCTION✓ Optical depth of C II emissions

𝛕=ln(Fint/Fobs)
5000

OBSERVATION

4000SIMULATION

𝛕(1335) ~ 5.1

Expected Spectrum
IUE data

C II 1335

C II 1336

3000

2000

DISCUSSION

𝛕(1336) ~ 5.3

100001333.5

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1334

1334.51335

1335.51336

1336.5

III. Raman C II and ISM

INTRODUCTION✓ Optical depth of C II emissions

𝛕=ln(Fint/Fobs)
5000

OBSERVATION

4000SIMULATION

𝛕(1335) ~ 5.1

Expected Spectrum
IUE data

C II 1335

C II 1336

3000

2000

DISCUSSION

𝛕(1336) ~ 5.3

100001333.5

1334

1334.51335

Flux [× 10−10 erg cm−2 s−1 Å−1]𝛕(1037) ~ 27.24

32.51336

1336.5

Expected Spectrum
FUSE(2002−06−14)

3.5

𝛕(1036) ~ 15.81

1335.5C II 1036

C II 1037

21.5

10.5

01035.8

1036

1036.21036.41036.6λ[Å]EAYAM 2017
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1037.21037.4

III. Raman C II and ISM

INTRODUCTION✓ Optical depth of C II emissions

𝛕=ln(Fint/Fobs)
5000

OBSERVATION

4000SIMULATION

𝛕(1335) ~ 5.1

Expected Spectrum
IUE data

C II 1335

C II 1336

3000

2000

DISCUSSION

𝛕(1336) ~ 5.3

100001333.5

Optically

onsissime
I
ICr
thick ISM fo
1334

1334.51335

Flux [× 10−10 erg cm−2 s−1 Å−1]𝛕(1037) ~ 27.24

32.5

1336

1336.5

Expected Spectrum
FUSE(2002−06−14)

3.5

𝛕(1036) ~ 15.81

1335.5C II 1036

C II 1037

21.5

10.5

01035.8

1036

1036.21036.41036.6λ[Å]EAYAM 2017
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1037.21037.4

III. Raman C II and ISM✓ Extinction of ISM
INTRODUCTIONOBSERVATION-Considering a long distance d ~ 2.5kpc of RR Tel, it can be originatedfrom the heavy extinction along ISM.

-The column density is expressed by the optical depth and the crosssection: N(C II) = 𝛕 / σ-N(CII) ~ 9.87x1013cm-2

SIMULATIONDISCUSSIONEAYAM 2017
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IV. Summary and Discussion

INTRODUCTION✓ We find two Raman-scattered features of C II at 7023 and 7053

Å in the high-resolution spectrum of the symbiotic nova RR Tel.

OBSERVATION✓ A significant amount of C II 1036 and 1037 Å emissions areSIMULATION

expected, however they are clearly absent in FUSE data.

DISCUSSION✓ By comparing with other observed C II emissions in IUE data,

we conclude that the discrepancy between the observed data
and the theoretical expectation is originated from the heavy
extinction along ISM.
✓ We determine the lower limit of the column density of C II in

ISM N(CII) ~ 9.87x1013cm-2.
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THANKSI. Introduction

INTRODUCTIONOBSERVATIONSIMULATIONDISCUSSIONEAYAM 2017
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I. Introduction

INTRODUCTIONOBSERVATIONSIMULATIONDISCUSSIONEAYAM 2017
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I. Introduction✓INTRODUCTION

Symbiotic Stars-Binary systems consisting of a hot radiation source, usuallywhite dwarf, and a cool, mass losing giant-A fraction of the slow stellar wind from the giant isgravitationally captured by the white dwarf to presumable form
an accretion disk.

OBSERVATIONSIMULATIONDISCUSSION

Hen2-104, CH Cyg
R Aqr

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HM SgeSPH Simulation (Mastrodemos and Morris, 1998)

I. Introduction✓INTRODUCTION

Raman Scattering-A far-UV photon blueward of Lyα isincident upon a hydrogen atom in theground state. Subsequently, thehydrogen atom de-excites into the 2sstate, re-emitting an optical Ramanscattered photon.

-Based on the principle of Energy
conservations

OBSERVATIONSIMULATIONDISCUSSION

Schematic energy level diagramfor Raman-Scattering by H I-

The re-emission of a photon has
significantly longer wavelengththan incident photon.
Ly β 1025(1s → 3p)

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Hα 6563(3p →2s)

I. Introduction✓INTRODUCTIONOBSERVATIONSIMULATIONDISCUSSIONEAYAM 2017
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-Raman Scattering in Symbiotic Stars
The white dwarf accretes a fraction of the stellar wind from thegiant, which makes it very hot (~105 K) and luminous(~102-104
Lsun), and thus capable of ionizing the neutral wind from the giant.

I. Introduction✓INTRODUCTIONOBSERVATION-Raman Scattering in Symbiotic Stars
The white dwarf accretes a fraction of the stellar wind from thegiant, which makes it very hot (~105 K) and luminous(~102-104Lsun), and thus capable of ionizing the neutral wind from the giant.

SIMULATIONDISCUSSIONEAYAM 2017
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to.
isbsmeycsor
fpotgnnieremtntaor
ci-snamaThe env
Rethgnivresfor obII. Observation✓INTRODUCTIONOBSERVATION

Raman Lines in RR Tel-We find seven broad features at 4332, 4850, 6545, 6825,7025, 7052 and 7082 Å, which are formed through Ramanscattering of He II, C II and O VI by H I.

SIMULATIONDISCUSSIONRamanHe IIHγRamanHe IIHβRamanHe IITwoRaman RamanC IIO VIRamanO VI

HαFigure 2. Low-resolution optical spectrum of RR Tel (ESO 1.5m + B&C,
Munari & Zwitter, 2002).
Green lines indicate the positions of the observed Raman-scattered lines.

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II. Observation✓INTRODUCTIONOBSERVATIONSIMULATIONDISCUSSIONEAYAM 2017
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Raman Lines in RR Tel

II. Observation✓INTRODUCTIONOBSERVATIONSIMULATIONDISCUSSIONEAYAM 2017
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Raman Lines in RR Tel

III. Monte Carlo Simulations✓ STB ionization front
INTRODUCTION-In STB (Seaquist, Taylor & Button, 1984) model, the ionization front
in the stellar wind region around the giant is determined by thebalance of photoionization by the H-ionizing flux from the hotcomponent and recombination represented by the mass loss
rate of the giant.

-A parameter X in STB geometry is given by X = 4πaLH/αB(mHv∞/Ṁ)2.

OBSERVATIONSIMULATIONDISCUSSION

Figure 4. An ionization structure with STB Geometry (left)
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III. Raman C II and ISM

INTRODUCTIONOBSERVATIONSIMULATIONDISCUSSIONEAYAM 2017
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✓ C II 1335 Triplet

III. Monte Carlo Simulations✓INTRODUCTIONOBSERVATIONSIMULATION

Hierarchical Emission Region Model-In order to reproduce the Raman-scattered line profiles, wesuggest that the emission nebulae around the white dwarf hasa hierarchical structure including inner most part with O
VI disk and the outer part with C II and He II sphere, whichis consistent with the higher ionization potential of O VI thanthose of He II and C II.

DISCUSSION

Figure 4. An ionization structure with STB Geometry (left)
and schematic model for the emission nebula around the WD (right)
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III. Monte Carlo Simulations

Flux [erg cm−2 s−1 Å−1Raman He IIINTRODUCTIONOBSERVATION

2.5e−142.5e−145.0e−142.0e−142.0e−144.0e−141.5e−141.5e−143.0e−141.0e−141.0e−142.0e−145.0e−155.0e−151.0e−140.0e+00

0.0e+00
4330

0.0e+00
6530

4850

λ[Å]

M.C Result6540

λ[Å]

6550

λ[Å]

SIMULATION

Raman O VI

Raman C II
3×10−14DISCUSSION

2.5×10−13

2×10Flux[erg cm−2 s−1 [Å]−1

Flux[erg cm−2 s−1 Å−1

2.5×10−14−14

1.5×10−14

1×10−14

5×10−157010

7020

7030

7040

λ[Å]

--

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2×10−13

8×10−14

1.5×10−13

6×10−14

1×10−13

4×10−14

5×10−142×10−14007050706070701×10−13

M.C. result

data
M.C. Result

6810

68206830

λ[Å]

6840

6850

M.C. result

Mrate=4e−6,vtw=20km/s

07065 7070 7075 7080 7085 7090 7095 7100

λ[Å]A good fit is obtained for the mass loss rate Ṁ ~ 3 x 10-6 M /yrand v∞ =10 km/s, which corresponds to X ~ 7.5.
Raman lines are well fitted with hierarchical emission region
composed of the O VI disk extending 1AU and the He II and C II
spheres with a size of sub AU.

III. Monte Carlo Simulations✓ STB ionization front
INTRODUCTION-In STB (Seaquist, Taylor & Button, 1984) model, the ionization front
in the stellar wind region around the giant is determined by thebalance of photoionization by the H-ionizing flux from the hotcomponent and recombination represented by the mass loss
rate of the giant.

-A parameter X in STB geometry is given by X = 4πaLH/
αB(mHv∞/Ṁ)2.

OBSERVATIONSIMULATIONDISCUSSION

Figure 4. An ionization structure with STB Geometry (left)
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