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Tae-Soo Pyo Subaru Telescope/NAOJ

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1 Tae-Soo Pyo Subaru Telescope/NAOJ 2015.11.11
IGRINS High-Resolution Spectroscopy FU Ori Type Object 2MASS J (V960 Mon) Tae-Soo Pyo Subaru Telescope/NAOJ

2 FU Ori type: Long-term Light curve
FU Ori type: ~ 3-4 magnitude brightening ~ 20 objects Distinguish the type of FU Ori outburst with long-term observation Hartmann & Cannon 1996

3 2MASS J 2014. Nov.30 (ATEL#6770): Maehara et al. report an outburst: magnitude (>13 to 11.5): to R~ 600: low-res. spectrum

4 2014. Dec. 19: Heckstein et al. (ATEL#6838)
2014. Dec. 9 : Hillenbrand (#6797) Observation: Keck/HIRES w/ R ~ 72,000 Optical spectrum : early F giant or super giant P-cygni profiles of Ha  strong wind resemble with FU Ori. 2014. Dec. 19: Heckstein et al. (ATEL#6838) - 15cm telescope 2009.Nov – 2014.Dec - Δm=2.6 : Outburst at 2014.Jan - Oct

5 2015. Jan 1 : Reipurth et al (ATEL#6862)
NIR low-res. spectra w/ IRTF/SPEX (R~ 1300) late-K and late-M type star w/ CO absorb. Band. Dec. 21

6 ATel # 6901 IGRINS K-band High-Resolution Spectroscopy of the FU Ori Type Object 2MASS J Tae-Soo Pyo (NAOJ), Heeyoung Oh(UST,KASI), In-Soo Yuk (KASI), Hwihyun Kim (KASI,UT), C. J. Davis (Liverpool John Moors Univ., UK) We confirmed that newly found outburst object 2MASS J showed similar spectrum with FU Ori star: [1] 2.3 – 2.32 mm: CO first overtone band mixed with H2O lines Hartmann et al. 2004 [2] Br g : Absorption not emission OBS: Dec. 25 & 26 UT Report [ATel# 6901]: 2015.Jan.11 Aspin et al.(2009)

7 Monitoring Observation
2014. Dec 2015. Jan. 20,23,27 /1 (by JungEun Lee team)

8 The new FUor candidate V960 Mon (2MASS J06593158-040
, Varricatt et al.(Atel #7578):  Near-IR photometric monitoring of FU Ori Type Object 2MASS J A slight dimming and re-brightening 0.04 mag (2014.Dec.2 – 19) 2015. Sep. 8, Semkov (ATEL#8019): The new FUor candidate V960 Mon (2MASS J 5277) still retains at high brightness level - I = 10.11, R= @ 2015.Sep.2-5

9 Conclusion 2MASS J is showing resemble spectra with FU Ori. Tracing time variation with high spectral resolution will give important clue to identify type of star and a history of accretion and outburst. Efficient pipeline and analysis tools are essential

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