Spatially-Resolved study of planetary nebulae
withSeimei/KOOLS-IFU;
the case of IC2165
M. Otsuka (Okayama Obs, Kyoto U.),T. Ueta (U. Of Denver), and PEGASuSS consortiumThis work is based on NAOJ open-use time and Kyoto U. time

Backgrounds
Case of planetary nebula (PN) IC418 w KOOLS-IFU
O+/H+O/H

O2+/H+

Sharpee et al.
(2004, optical)

Spitzer/IRS(mid-IR)+=•

The measured abundances determined only from spectroscopic data of a single narrow-slit
exposure DO NOT represent the average abundances PN. For example, Spitzer/IRS mid-IR vs.
Sharpee et al. (2004).

•Elemental abundances are NOT Uniformly distributed within dusty nebula, due tonucleosynthesis history, traps by dust grains/molecules, ionization, mass-loss wind…

To fully understand PNe and obtain the representative abundances, spatiallyresolved spectroscopy is necessary! IFU instruments have advantages over slit-scan!

Aims of this study
We study Galactic PNe using Seimei/KOOLS-IFU andarchive data in multiwavelengths for investigation into(I) spatial distributions of dust extinction, electron densities/
temperatures, and ionic/elemental abundances(II) spatial distributions of gas/dust masses and gas-todust mass ratio by combing use of IR data
(III) evolutionary history of the progenitors by comparing
observed quantities with theoretical AGB modelMapping observations towards
IC2165 w Seimei/KOOLS-IFU(a) HST WFPC2/F437W(a)(b) Fibre positions

IUE SWP/LWR(b)(c) The number of visits

central star
IRS

BOES

10”
2"5"

•We observed IC2165 (panel a) using the VPH-Blue and Red grisms,
covering 0.4-1 µm under clear/stable sky; 4.5-5.2 ℃ in outside
temperature, 76 − 78 % in relative humidity, and 985.5 hpa in pressure.

•We took a single 60s exposure on each 25 dither position (panel b).

•Exposure map (panel c) indicates that we took (13-18) x 60 sec exposure
toward the nebula and central star.

Data Reduction
We improved following points;

sens. function(a)•Displacements in spatial owing to atmospheric dispersion•

Issues on flux calibration database (e.g., magnitude, blue andred spec connection with forcefully removing absorptions in theblue spec, and less data in near-IR, etc) and also telluric removal(panel a)
By comparison of the modelled with the observed spectra, weobtained sensitivity/telluric removal function.

•As a bonus, the issue on transition probabilities of [SIII]9068/9530Å was gone.

FWHM versus wavelength relation (panel b)••

Further correction factor (1.048) by comparing with the KOOLSPSF convolved HST F547M image•Richardson-Lucy (RL) deconvolution•Others•(b)

Now, we can safely compare other spec, e..g.,Spitzer（PSF~3”), IUE（PSF~4.1” ）with KOOLS spec!

De-stripe residual bias pattern （ref. the Messenger, vol. 70,p. 82-84)

FWHM (arcsec)••

drizzled
HR3454 image

EN
λHI10049Å
HeII10124Å[SIII]9530Å

HI9229Å

HI9014Å[ClIV]8045Å[FeV]8197Å
HeII8236Å[ArIV]7171Å[ArIV]＋CII7236Å[ArIV]7263Å
HeI7281Å

CII6781Å

en sPasch
HI9014Å[SIII]9068Å[ArIII]7751Å[ClIV]7531Å
HeII7592Å[ArIII]7135Å[OII]7320/30Å[KIV]6795Å[ArV]7005Å
HeI7065Å

HI6563Å/[NII]6548/83Å
HeI6678Å[SII]6716/31Å

HeII5410Å[ClIII]5517Å[ClIII]5537Å[FIII]5720/21Å[NII]5755Å
CIV5801/12Å
HeI5876Å[CaV]6086Å[KIV]6101Å
HeII6118Å
HeII6233Å[OI]6300Å/[SIII]6312Å[OI]6363Å[ArV]6435Å[NI]5197/5200Å

HI4340Å/[OIII]4363Å
HeI4471Å
HeII4540Å
CIII4648Å/CIV4658Å
HeII4686Å[ArIV]4711/40Å/[NeIV]4724Å
HI4861Å[OIII]4959Å[OIII]5007Å

HI4101ÅKOOLS-IFU 0.4-1µm
RA-DEC-λ CUBEDATA of IC2165
eries

Spectra Fitting

We employ Multiple Gaussian Fitting for the 1-D spectra at every spaxel.
• We detect/identify 105 emission lines in 4300-10200 Å.
•Nebular abundance analysis based on
the 1-D KOOLS, IUE, Spitzer spectraEmission Line Maps
Final FWHM~1.2”

Extinction Map as an indicatorof dust distribution
By comparison between observed F(Hγ, 6 Paschen lines)/F(Hβ) and the theoretical ones as follows;• step1: correct line fluxes with a constant c(Hβ) value; c(Hβ)=1.45E(B-V) with Rv=3.1 and CCM
reddening function• step2: calculate Tε/nε values in each pixel using diagnostic line ratios• step3: compute theoretical H I lines to Hβ ratio values (as a functions of Tε/nε) in each pixel• step4: compare the observed HI lines to Hβ ratios with the theoretical values calculated in step3.
Thus, c(Hβ) was obtained.
• Iterate steps1-4 4 times.
These H I lines are not contaminated with He II lines, which are removed out by employing similar
technique, of course.

ESO NTT/SUSI2 HαE(B-V)

Electron Density (nε) andTemperature (Tε) mapsnε([S II])nε([Cl III])nε([Ar IV])ccTε([S II])

Tε([S III])

Tε([O III])K

Progress and Future Plan
✓ Abundance analysis based 1-D spectra taken by IUE, KOOLS, VLT/VIMOS, andSpitzer (done)✓ KOOLS and VIMOS 2-D emission line image reconstruction (done)✓ 2-D Extinction and Tε/Nε maps (done)✓ Ionic/Elemental abundance maps (doing)✓ Construct 3-D structure using VIMOS PV-maps✓ Construct 3-D photoionisation model✓ Simulate atomic gas emission lines in mid-IR based on the obtained Tε/Nε andionic abundance maps

I hope KOOLS with auto-guider will provide Spectacular data!