可視変動により見つかった

radio-loud narrow line Seyfert 1の多波長観測
諸隈 智貴 (東京大学), 田中 雅臣 (国立天文台), 伊藤 亮介, 秋田谷 洋 (広島大学), !
冨永 望 (甲南大学), 諸隈 佳菜 (国立天文台), 野間 千菜美 (東北大学), !
斉藤 嘉彦 (東京工業大学), 徂徠 和夫 (北海道大学), 藤沢 健太, 新沼 浩太郎, !
元木 業人 (山口大学), 松本 恵未子 (甲南大学)

M. Tanaka et al. ApJ Letters, in press (arXiv:1309.1409)
日本天文学会2014秋季年会(山形大学) 2014/09/11-13可視変動により見つかった

radio-loud narrow line Seyfert 1の多波長観測
諸隈 智貴 (東京大学), 田中 雅臣 (国立天文台), 伊藤 亮介, 秋田谷 洋 (広島大学), !
冨永 望 (甲南大学), 諸隈 佳菜 (国立天文台), 野間 千菜美 (東北大学), !
斉藤 嘉彦 (東京工業大学), 徂徠 和夫 (北海道大学), 藤沢 健太, 新沼 浩太郎, !
元木 業人 (山口大学), 松本 恵未子 (甲南大学)

M.
M. Tanaka
Tanaka etet al.
al. ApJ
ApJ Letters,Letters, inin press
press (arXiv:1309.1409)(arXiv:1309.1409)
日本天文学会2014秋季年会(山形大学) 2014/09/11-13

Narrow Line Seyfert 1 (NLS1)‣ AGN w/ “narrow” broad emission lines‣ <2000 km/s

‣ smaller supermassive black holes (SMBHs)‣ 105-8 Msun SMBH

‣ rare population‣ 15% of broad-line AGN (SDSS)‣ high Eddington ratio ==> high accretion rate (Lbol/LEdd>0.1)‣ growing SMBH

‣ weak [OIII]: [OIII]/Hbeta<3‣ small amplitude of variability(?)‣ radio-quiet‣ Only ~7% of NLS1 are radio-loud (R>10).

日本天文学会2014秋季年会(山形大学) 2014/09/11-13

SDSS J1100+4420 (KISS14k): Peculiar NLS1?

‣ AGN w/ “narrow” broad emission lines‣ <2000 km/s: v(MgII)=2070km/s, v(Hbeta)=1900km/s‣ smaller supermassive black holes (SMBHs)‣ 105-8 Msun SMBH: 1.5x107 Msun SMBH

‣ rare population‣ 15% of broad-line AGN (SDSS)‣ high Eddington ratio ==> high accretion rate (Lbol/LEdd>0.1): Lbol/LEdd~0.3‣ growing SMBH

‣ weak [OIII]: [OIII]/Hbeta<3: high L([OIII]). [OIII]/Hbeta~7‣ small amplitude of variability(?): rapid optical “flare”‣ radio-quiet‣ Only ~7% of NLS1 are radio-loud (R>10). 

‣ radio-loudness R~3000‣ extended radio emission: ~100 kpc?

‣ SED consistent with previous gamma-loud/radio-loud NLS1s
日本天文学会2014秋季年会(山形大学) 2014/09/11-13

Discovery: SDSS J1100+4420 (KISS14k)‣ rapid optical “flare” discovered in high-cadence supernova survey‣ Kiso Supernova Survey (KISS; Morokuma et al. PASJ, in press)‣ Kiso Schmidt (1.05m) + KWFC (4 deg2 FoV)

‣ supernova shock breakout !?!?!?

faint host(g~22)

in SDSS

日本天文学会2014秋季年会(山形大学) 2014/09/11-13

Follow-Up Observation (1): Optical w/ Subaru‣ optical imaging & spectroscopy w/ Subaru/FOCAS‣ rapid decreasing phase

日本天文学会2014秋季年会(山形大学) 2014/09/11-13

Follow-Up Observation (1): Optical w/ Subaru‣ optical imaging & spectroscopy w/ Subaru/FOCAS‣ “narrow” (~2000km/s) broad emission lines (MgII, Hbeta)‣ ==> 1.5x107 Msun SMBH

‣ no changes of power-law indices (spectral slopes)‣ strong [OIII] emission lines ([OIII]/Hbeta>7)

日本天文学会2014秋季年会(山形大学) 2014/09/11-13

KISS14k is very radio-loud !!!
radioIR/opt X-ray gamma-ray

15.76 mJy

radio-loudnesss R~3000
日本天文学会2014秋季年会(山形大学) 2014/09/11-13

Follow-Up Observation (2): optical/NIR

Follow-Up Observation (3): X-ray/UV‣ continuous monitoring w/ Kiso/KWFC (1.05m), Kanata/HONIR (1.5m),
Akeno/MITSuME (0.5m), Kottamia (1.88m, Egypt)
multiple flares?

‣ ToO X-ray & UV imaging
w/ Swift/XRT & UVOT (PI: M. Tanaka)
日本天文学会2014秋季年会(山形大学) 2014/09/11-13

Spectral Energy Distribution of KISS14k
radioIR/opt X-ray gamma-ray
Fermi/2FGL
Swiftsimilar SED to gamma-loud NLS1

日本天文学会2014秋季年会(山形大学) 2014/09/11-13

Follow-Up Observation (4): radio w/ JVN‣ Japan VLBI Network (JVN)‣ August 2, 2014 (UT)

‣ 8 GHz‣ Yamaguchi, Hitachi, Usuda‣ aims‣ flux measurement (==> monitoring)‣ 37.6 mJy@5 GHz‣ spectral shape‣ morphology‣ under reduction‣ simultaneous optical/NIR observations‣ <== failed due to bad weather

日本天文学会2014秋季年会(山形大学) 2014/09/11-13

Follow-Up Observation (4): radio w/ JVNDoi+2012‣ Japan VLBI Network (JVN)‣ August 2, 2014 (UT)

‣ 8 GHz‣ Yamaguchi, Hitachi, Usuda‣ aims‣ flux measurement (==> monitoring)‣ 37.6 mJy@5 GHz‣ spectral shape‣ morphology‣ under reduction‣ simultaneous optical/NIR observations‣ <== failed due to bad weather

日本天文学会2014秋季年会(山形大学) 2014/09/11-13

Nature of KISS14k‣ short (~hours) time scale variability in optical‣ “narrow” broad line ==> 2x107 Msun SMBH

‣ SED consistent with other gamma-loud/radio-loud NLS1‣ very radio-loud‣ constant optical spectral slopes during luminosity change‣ ==> relativistic jet‣ Extended (~100 kpc) radio structure‣ Origin of high [OIII] luminosity? extended narrow line region?

‣ ==> The jets are not aligned to the line-of-sight?

‣ transition to more luminous quasar ???

日本天文学会2014秋季年会(山形大学) 2014/09/11-13

Summary‣ We detected a rapid optical flare from a radio-loud NLS1 in ourhigh-cadence supernova survey KISS. 

‣ Optical spectra‣ “narrow” broad emission line: ‣ v(MgII)=2070km/s, v(Hbeta)=1900km/s‣ 2x107 Msun SMBH

‣ high [OIII] luminosity: [OIII]/Hbeta~7‣ very radio-loud: R~3000‣ extended (~100 kpc) emission!

Future Plans‣ Simultaneous observations over wide wavelength range‣ coordinated observation of OISTER (optical/NIR) & JVN (radio)‣ High-resolution interferometric observation ‣ Deep optical imaging/spectroscopy for the nature of a possible
extended [OIII]?

日本天文学会2014秋季年会(山形大学) 2014/09/11-13