IGRINS Observations of Extended IFOs in the UWIFE Survey 2017. 07. - PowerPoint PPT Presentation

IGRINS Workshop 2017 IGRINS Observations of Extended IFOs in the UWIFE Survey 2017. 07. 28 Seoul National University Yesol Kim Supervisor : Bon - Chul Koo (SNU) Collaborators : Tae - Soo Pyo (NAOJ), Yong - Hyun Lee (SNU), Jae - Joon Lee (KASI), Dirk Froebrich (Univ. of Kent), Heeyoung Oh (SNU)

Contents • Introduction - the UWIFE survey • Previous [Fe II] studies • Spectroscopic follow-up of UWIFE sources with IGRINS 1. G25.8+0.2 (1) Detected lines (2) Position – velocity diagram of [Fe II] and Br-gamma 2. HH 803 (1) Position – velocity diagram • Future Work – other sources to observe

UWIFE survey ■ UKIRT Wide - field Infrared Survey for Fe+ (Lee+2014) Unbiased imaging survey using narrow - band filter with central st Gal wavelength of 1.644 μ m, covers the 1 st quadrant (7 ° < l < 62 ° , b ≤ |1 ° .5|). alactic c qu l = 62 ° l =7 ° Figure 1. Observation coverage of UWIFE survey - Observations were conducted by WFCAM at UKIRT (2012.5 ~ 2013.8) - pixel size: 0.2”, median seeing: 0.83” - 5σ detection limit : 18.7 mag , surface brightness limit : 8.1 × 10 -20 W m -2 → UWIFE is first high - resolution, deep [Fe II] survey for 1st Galactic quadrant. Suitable for systematic [Fe II] study of shocked, dense & unseen material in obscured region! 2

Motivation  IFO : Ionized Fe Object Figure 2. Observation coverage of UWIFE with known sources What about other, unseen [Fe II] - emitting sources? We are compiling a comprehensive catalogue

UWIFE extended IFO catalog • Manual search & automatic search by source detection algorithm. (Developer : Dirk Froebrich) • In total, we identified 202 sources ( 1.23 source in 1 deg 2 ). ■ Extended Ionic Fe Object (IFO) catalog (Kim et al. in prep) Table 1. (left) Catalog of extended IFOs. (right) Number of IFOs classified with counterpart.  Basic physical properties ( coordinate, size, flux, distance , etc) are enlisted, as well as counterpart of IFOs. About half of IFOs are associated with YSOs.  Most of IFOs in this study are newly discovered [Fe II] objects . 4

UWIFE extended IFO catalog  Spatial distribution of IFOs related to early evolutionary phase is clustered, highlighting star - forming regions (e.g. M 16, M 17 in l ~ 16°).  Gaussian-fitted center position of IFO latitude distribution is -0.22° (FWHM ~1.5°), consistent with distribution of Galactic arm (Goodman+2014). Figure 4. Spatial distribution of IFOs 5 on artist’s impression of Milky way. Figure 3. Spatial distribution of IFOs in catalog

Follow-up observations of IFOs • We are conducting spectroscopic follow-up of UWIFE sources with IGRINS . 1. G25.8+0.2 - On-off mode, as a part of mini - queue (2015.08.05) - Exposure time : 340s × 2 - Two slit positions were placed on [Fe II] shell. 2. HH 803 - On-off mode, observed on 2016.10.11. (PI : Heeyoung Oh) - Exposure time : 300s × 2 - Two slit positions where [Fe II] & H2 are bright. 6

Follow-up study 1 : G25.8+0.2 ■ IFO J183740.829-061452.41 Red : Slit position [Fe II]-H - A shell-like IFO located near HII region G25.8+0.2. - [Fe II] flux ~ 2.49 x 10 -16 W/m 2 : Falls in one of the faint SNR in [Fe II] (Lee, in prep). - Radio recombination line was observed with distance of 6.5±0.3kpc (Russeil+2003). : Size of IFO is ~6’, 11 pc Figure 5. IFO J183740.829-061452.41 on UWIFE continuum - subtracted [Fe II] data.

Follow-up observations of IFOs G ~ 26° region • X-ray PWN / SNR candidate and young pulsar AX J1837.6-0610 seem to be associated with [Fe II] shell (Sakamoto+2001, Lin+2008). Red contour : 0.7-2keV New-GPS 20cm GLIMPSE 8um Green contour : 4-10keV Blue * : AX J1837.6-0610 Magenta * : IRAS 18348-0616 SHS H- α UWIFE [Fe II] - H Figure 6. Multiwavelength view of G~ 26º region. 8

Follow-up observations of IFOs G25.8+0.2  [Fe II] 1.64um, He I 2.05um, Br- γ , Br 10, Br 11, Br 12, Br 14 were detected.  [Fe II] structure is distinct from Hydrogen & Helium structures. • Slit position 1 : perpendicular to [Fe II] shell [Fe II] He I Br- γ Br 10 Br 11 Br 12 Br 14 • Slit position 2 : parallel to [Fe II] shell 9 Figure 7. 2D spectrum of detected lines

Follow-up observations of IFOs G25.8+0.2 • [Fe II] is spatially distinct from Br- γ , enhanced where UWIFE [Fe II] shell exists. • A shocked region was revealed, with [Fe II] / Br- γ ratio up to 2. * Slit position 1 * Slit position 2 10 Figure 8. 2D spectrum of [Fe II] and Br- γ

Follow-up study 2 : HH 803 Figure 9. IPHAS H α image of HH 803 region

2D spectrum of detected lines - Twelve molecular hydrogen lines were detected. - All show knots revealed in UWISH2 image (figure 10). P9 Figure 10. H2 and [Fe II] image with IGRINS slit positions P10 Figure 11. 2D spectrum of detected Hydrogen lines 1.68 2.12 2.41 1.74 2.03 2.07 2.22 1.78 2.25 2.45 2.42 2.43

Follow-up study 2 : HH 803 ■ 2D spectrum of [Fe II] shows high velocity component, which is apart from low velocity molecular hydrogen structures. Figure 12. H2 image of HH 803. Figure 13. 2D [Fe II] & H2 spectrum of HH 803

Future Work Candidates to observe • Variety of [Fe II] morphology from YSOs YSO? PN? Figure 14. Continuum-subtracted [Fe II] image of YSO – related IFOs. Red + ,x: H2 14

Candidates to observe (in Eagle Nebula) K [Fe II] J Hα [FeII]-H Figure 15. H α image of Eagle with zoomed-in JHK three-color images.

Future Work Candidates to observe • IFO J190816.78+052506.1 - Clumpy amorphous structure in [Fe II]. - An Hα counterpart was discovered and Figure 16. [Fe II] and GPS H-band image of the IFO. suspected to be a PN, spectroscopic follow-up could not find any PN 29:00.0 emission line (Viironen et al. 2009, Sabin et al. 2014) . N 28:00.0 - Exploiting UWIFE and UWISH2 data, E 27:00.0 we found that this IFO may associate with chains of multiple [Fe II] and H 2 5:26:00.0 knots. These aligned diffuse structures 25:00.0 are located inside an IRDC DOBASHI I F O J 1 9 0 8 1 6 . 7 8 + 0 5 2 5 0 6 . 1 1675 (A v = 8.22). 24:00.0 Figure 17. Wide view around the source in H2. 16 Black ellipse : H2 knots. White circle : IFO. 35.0 30.0 25.0 19:08:20.0 15.0 10.0 23:00.0

Future Work Candidates to observe  IFO J181845.167 -150257.2 - Located inside the SNR G015.9+00.2. - No other possible counterpart was found. - The nearest object is CXOU J181852.0- 150213, an x-ray source which suspected to be related to SNR.  IFO J192348 & J192354 - J192348 is a broken shell surrounding Figure 18. [Fe II] and GPS H-band image of candidate LBV [OMN2000] LS1 IFO J181845.167 -150257.2 (Source 1 in H-band image). - The central source of this IFO is O4 I P- cygni supergiant with initial mass of 120 solar mass, one of the massive and evolved star in Milky way (Clark et al. 2009). - YSO (Source 2 in H-band image) is located in the central position of J192354. Figure 19. [Fe II] and GPS H-band image of 17 IFO J192348.169 +143641.5 and IFO J192354.032 +143558.0.

Summary • We designated [Fe II] 1.644um – emitting sources as IFO s and identified in the UWIFE survey area in unbiased way. • About 202 extended IFOs are identified , often associated with H2. • We conducted spectroscopic follow-up with IGRINS, two sources (SNR candidate G25.8+0.2 & HH 803) were observed so far. • IGRINS successfully carried out follow-up, revealed shock-excited [Fe II] structure in SNR candidate. • IGRINS will be useful for studying newly found [Fe II] & H2 sources in the UWIFE & UWISH2 survey. 18

Complementary search by computer  Source detection algorithm (Developer : Dirk Froebrich) - Median filter to remove remaining stars - Subtract large scale backgrounds - Draw contours above 1σ noise level  Preliminary Results - Results in tens of thousands of contours - About 5% would be real  Remove false detection (manually) - Both method found 189 + 103 only manually + 20 only automatically + α Automatic Manual Automatic Manual Artifacts