赤外線天文衛星「あかり」による新星の近赤外分光観測

左近　樹、尾中 敬、田中雅臣、守屋 尭 ( 東京大学 ) 、新井彰、植村誠、川端弘治 ( 広島大学 )AKARI IRC チーム、新星サイエンス検討チーム、

新星古典新星 (Gehrz et al. 1998) -- a phenomenon resulting from the accretion of matters in the atmosphere 　　 of red-giant or red-dwarf companion onto the white dwarf. Observed Nova rate in the Galaxy ; 35±11yr-1 (Shafter 1997) The mean mass returned by a nova outburst into the ISM; 2x10-4M☉ 7x10-3M☉ yr-1 of processed matter is ejected by novae into the ISM cf. Supernovae rate ~0.02yr-1 in a galaxy The mean mass returned by a supernova into the ISM; 3M ☉ 0.06 M☉ yr-1 of processed matter is ejected by supernova into the ISM

宇宙の化学進化に対する新星の貢献・ Less than ~0.3% of the interstellar matter in the Galaxy ・ Only about 0.1% of the Galactic “stardust” ・ a significant fraction of the 26Al (t1/2~7.2 x 105yr) that exists in Galactic matter

Theoretical studies suggest that large amount of 22Na and 26Al can be produced in outbursts of ONeMg WDs (Weiss & Truran 1990; Nofar et al. 1991); possible candidates that are responsible for the 22Ne (Black 1972) and 26Mg (Truran 1985) anomalies found in meteorites (Gehrz et al. 1998)

新星の赤外線観測CO Novae および ONeMg Novae の赤外スペクトル進化- Hot ejecta gas is initially seen as an expanding photosphere or

“fireball”- When the expanding material becomes optically thin, free-free

and line emission dominate

1). CO Novae; 比較的低質量 (e.g., MWD<1.1M☉) の CO 白色矮星　　　　　の表面上での熱核暴走 (thermonuclear runaway ;TNR) - いくつかのケースで free-free 期に続いてダスト形成が報告　 (e.g., V2362 CYGNI; Lynch et al. 2008)

2). ONeMg Novae; 比較的質量の大きな (e.g., MWD>1.1M☉) の　　　　　 ONeMg 白色矮星の表面上での熱核暴走 (TNR) - free-free 期に引き続いて coronal emission-line 期を迎える - いくつかの例外を除いて観測的にダスト形成の報告は　　　ほとんどない (e.g., V1974 CYGNI; Woodward et al. 1995 )

赤外線天文衛星「あかり」JAXA/ISAS mission

for infrared astronomy with ESA participation

Telescope with 685mm SiC Mirror

cooled by 179l LHe & mechanical coolers

2 instruments: IRC & FIS

Launched on Feb. 22, 2006 Successfully performed near-

to far-infrared observation

LHe: 2006 May - 2007 Aug(phases I&II)

Warm mission: 2008 June –(phase III; 2-5mm imag. & spec.)

「あかり」衛星 近・中間赤外線カメラ近赤外分光素子の波長透過率特性NIR dispersers

AKARI’s spectroscopic ability in the near-infraredin the warm mission is quite unique and valuable

Two Near-Infrared Disperserswith different spectral resolution power

- Near-Infrared Prism (NP)- Near-Infrared Grism (NG)

Effective Coverage Dispersion NP 1.8mm-5.5mm 　 0.06 mm/pix at 3mm NG 2.5mm-5.0mm 0.0097mm/pix

The 1-s noise-equivalent flux for slit-less spectroscopy at the ecliptic poles

Phases I&II Phase III NP ~0.05mJy ~0.1mJy NG ~0.1mJy ~0.2mJy

あかり衛星による新星の観測Phase 3-II AKARI Open Time Program: Spectral Evolution of Novae in the Near-Infrared based on AKARI Observation (SENNA; PI: I. Sakon) Discovery approved observation schedules phase 3-II-1#1 phase 3-II-2#2V1213 CENTAURUS Mar 2009 ○ ○V5582 SAGITTARII Feb 2009 　　　　　　　　 × ○V679 CARINAE Nov 2008 　　　　　　　　 ○　　　　　　　　　 ○ V5580 SAGITTARII Nov 2008 × ○ QY MUSCAE Sep 2008 ○ ○V1309 SCORPII Sep 2008 　　　　　　　　　○ ○V2468 CYGNI Mar 2008 ○ ○V5579 SAGITTARII Apr 2008 　 ○ ○V1280 SCORPII Feb 2007 × ○ #1 Oct. 2009 – Feb. 2010, #2 Mar. 2010– Sep. 2010

・ Continuous 2.5—5mm spectra taken with AKARI/IRC are quite unique・ Collaborative optical (B,V,R) to NIR(J, H, Ks) observations with TRISPEC on the 2m KANATA telescope of Hiroshima University and with other ground-based facilities are important

Nova V2468 CYGNI (R.A., DEC. [J2000]) = (19:58:33.57, +29:52:11.6) 2008 年 3 月に発見 (Munari et al. 2008, Cent. Bur. Electron. Tel. 1431, 1)

Multi-epoch NIR spectroscopic observations of V2468 CYGNI with AKARI/IRCFirst observation; on 2nd Nov., 2008 (t~240days; hereafter first epoch)

Second observation; on 1st May, 2009 (t~420days; hereafter second epoch) Both observations were carried out in the framework of AKARI Director’s Time

Pointing ID’s; 5200318.1 (Nov., 2008), 5200732.1 & 5200733.1 (May, 2009)Near-Infrared Grism (NG) is used to obtain the 2.52mm-5.0mm spectra

with a resolution of R(=l / )Dl ~80 (@3mm)

N3 band reference image of V2468 CYGNI on 1st May. 2009

Raw NG data of V2468 CYGNI on 1st May. 2009

N3 band reference image of V2468 CYGNI on 2nd NOV. 2008

Raw NG data of V2468 CYGNI on 2nd NOV. 2008

あかり衛星による V2468 CYGNI の近赤外分光観測

あかり衛星による V2468 CYGNI の近赤外分光観測1 回目の V2468 CYGNI の近赤外分光観測 (2nd Nov., 2008; t~240 days)

2 回目の V2468 CYGNI の近赤外分光観測 (1st May., 2009; t~420 days)

あかり衛星による V2468 CYGNI の近赤外分光観測

Bra 4.05mm line のライン形状

平均的な放出ガスの視線速度成分は 420 日後の時点で ~1500-1800km s-1

Signal count profile of the Bra line in the spectrum of May 2009

Strength of Hydrogen recombination lines (10-16W/m2); Epoch Bra(4.05mm) Brb(2.63mm) Pfg(3.74mm) Pfb(4.65mm)Nov. 2008 20.2±0.5 12.4±1.2 3.3±0.4 4.3±0.4May. 2009 5.1 ±0.2 4.0±0.4 0.95±0.18 0.91±0.40

Epoch Brb/Bra Pfg/Bra Pfb/Bra Nov. 2008 0.618±0.062 0.164±0.021 0.213±0.020May. 2009 0.790 ±0.088 0.187±0.034 0.178±0.080

Relative Strengths of Hydrogen recombination lines

あかり衛星による V2468 CYGNI の近赤外分光観測 V2468 CYGNI の近赤外スペクトルの進化

Free-free continuum emissionFn ~ 30mJy (on 240 days), ~12mJy (on 420 days)

電子温度 ; Te ~ 数千度 K電子密度 ; ne ~109 cm-3 (on 240 days), ~1011cm-3 (on 420 days)(Case B; Osterbrock 1989; Hummer & Strey 1987; Storey & Hummer 1995)

V2468 CYGNI 近赤外スペクトルの進化あかり衛星による V2468 CYGNI の近赤外分光観測

V2468 CYGNI の近赤外スペクトルの進化 “coronal” lines の強度 (10-16W/m2);

[CaIV] [CaV] [MgIV] [AlV] [AlVI] lc (mm) 3.207 4.150 4.487 2.905 3.650 eion (eV) 67.27 84.50 109.24 153.83 190.48 eex (eV) 50.91 67.27 80.14 120.00 153.83Nov. 2008 4.1±0.7 0.9±0.3 1.5±0.2 -- --May. 2009 4.5±0.3 2.0±0.2 14.2±0.2 2.5±0.3 0.35±0.11

基本的には典型的な ONeMg 新星の近赤外スペクトル進化と一致 ;-- free-free emission line phase の終了段階　に近づくにつれて wind flux は落ちる-- 光学厚さ t~1 で決定される半径が後退 白色矮星の光球のより深く熱い層が　見えるようになる。 (i.e., Lynch et al. 2008)

あかり衛星による V2468 CYGNI の近赤外分光観測

The late time near-Infrared Spectrum of V1280 Sco obtained with AKARI/ IRC on ~940 days after the discovery.

V1280 Scorpii; -Discovered on 2007 Feb 4.86 by Y. Nakamura and Y. Sakurai (Yamaoka et al. 2007)-Dust formation occurred after d~23days (Das et al. 2007)

右上がりの連続光放射に加えて、強い長波長側の wing を有する顕著な PAH 3.3mm バンド放射を検出

2009 年 9 月 9 日にあかり衛星の近・中間赤外線カメラによる近赤外分光観測を遂行

あかり衛星による V1280 Sco の近赤外分光観測

※ 比較的大きな 3.4mm/3.3mm のバンド強度比が V842 Cen でも観測。 (Hyland & McGregor 1988)

赤外線波長域に見られる PAH feature の性質Unidentified Infrared (UIR) BandsPolycyclic Aromatic hydrocarbons (PAHs; Allamandola et al. 1989)

3.3mm feature; aromatic C-H stretch mode3.4mm feature; aliphatic C-H stretch mode

UKIRT で取得された Orion Bar の電離領域 ( 上 ) 　と中性領域 ( 下 ) の近赤外スペクトル (Sloan et al. 1997)

- Nova に見られる hydrocarbon featureが Hydrogenated amorphous carbon によって担われている (Evans & Rawlings 1994) という主張に一貫- 化学進化の観点からの Hydrogenated amorphous carbon と PAHs との関連に関する重要な情報

あかり衛星による V1280 Sco の近赤外分光観測Near infrared spectrum of NGC1333

with UKIRT (Joblin et al. 1996)Red wing in 3.4-3.6mm-- PAH についた aliphatic side group から の C-H strech の振動モードの放射(Jourdain de Muizon et al. 1990)

-- いくつかの Herbig Ae/Be 天体や Nova Cen1986

AKARI Near infrared spectrum of V1280 Sco at the epoch of 980 days

Summary 　(1) Multi-epoch NIR spectroscopic observations of V2468 CYGNI were carried out with AKARI

Infrared Camera (IRC) in the framework of AKARI Director’s TimeFirst epoch; on 2nd Nov., 2008 (t~240days)

Second epoch; on 1st May, 2009 (t~420days)・ The NIR spectrum on first epoch is characterized by strong hydrogen and helium recombination lines and “coronal” lines of [CaIV], [CaV] and [MgIV]・ The NIR spectrum of second epoch is characterized by relatively weaker hydrongen

recombination lines and strong [MgIV], [CaIV], [CaV] together with the lines with higher ionization potential such as [AlV] and [AlVI] (eip>100eV)

No significant signs of dust formation have been found for V2468 CYGNI Consistent with the typical evolution scenario of ONeMg Novae

(2) NIR spectroscopic observations of V1280 Scorpii were carried out With AKARI IRC in the framework of AKARI Director’s Time

First epoch; on 9th Sep., 2009 (t~940 days)・ Clear signs of PAH 3.3mm band accompanied by a strong red-tail in 3.4-3.6mm arising from the aliphatic C-H bonds

consistent with the scenario that hydrocarbon features in novae are carried by hydrogenated amorphous carbon (HAC) (Evans & Rawlings 1994)