IGRINS Spectroscopy on Multiple Outﬂows around LkHα 234ust.kasi.re.kr/JC-ref/HYOh_USTJC_20160217.pdf · IGRINS 2 • Immersion GRating INfrared Spectrograph • Collaboration between

IGRINS Spectroscopy onMultiple Outflows around LkHα 234

2016 ApJ, 817, 148

Heeyoung Oh1,2, Tae-Soo Pyo3,4, In-Soo Yuk1, Byeong-Gon Park1,2, and IGRINS Team1KASI, 2UST, 3Subaru Telescope, 4SOKENDAI

February 17, 2016 @KASI-UST JC

1

Monday, February 22, 2016

IGRINS

2

• Immersion GRating INfrared Spectrograph

• Collaboration between Univ. of Texas & KASI

• 2.7-m HJST on McDonald Observatory

• Simultaneously obtains whole H- (1.49-1.80μm) & K-bands (1.96-2.46μm)

• Spectral resolution R ~ 40,000 (7.5 km s-1)

• 1″ x 14.″8 slit

• Compact size 1m x 0.6m x 0.4m

• Commissioning runs on March, May, July 2014


IGRINS

2.7-m HJST, McDonald Observatory3


SVC frame(Orion BN) Slit-viewing Camera

4


Th-Ar

U-Ne

Flat Lamp OpticsIGRINSWindow

U-Ne

Calibration System

5


6Andre (2000)

accretion/outflow

YSO Outflow Basic Intro

Class 0

Class I


YSO Outflow

7

HH 111 (HST)

HH 212ESO/M. McCaughrean

Outflow is important in accretion: removes angular momentum of infalling material for growth of stellar seed

Basic Intro


Slit Spectroscopy & Position-velocity Diagram

8galaxy UGC 2936 (z~0.013)

blueshifted

redshifted

slit

Basic Intro

grating

Hα


LkHα 234 Complex Region

9

• NGC 7129 star formation region at 1.25 kpc

• LkHα 234: B7 type Herbig Be star, ~8.5 M☉, ~1700 L☉, age ~105 yr

• CO, [S II] outflow, H2 jet

• Water maser sources

• VLA continuum, Millimeter, Mid-IR sources

• No outflow driven by LkHα 234

• IGRINS: The first high-R NIR spectroscopy


1990ApJ...357L..45R

CO / [S II] Outflow

10


1990ApJ...357L..45R

CO / [S II] Outflow

113.6, 4.5, 5.8, 8.0 μmMonday, February 22, 2016

S. Cabrit et al.: Origin of the mid-infrared emission and supersonic jet toward LkH! 234 527

Fig. 3a–d. A montage of 2µm narrow-band images covering a 67!! ! 64!! area around LkH! 234. a (top-left): 2.122µm image, i.e. H2 line

emission + continuum; b (top-right): 2.166µm image, i.e. essentially continuum; c (bottom-left): 2.122µm " 2.166µm difference image, i.e.

pure H2 line emission; d (bottom-right): pure H2 line emission after cosmetic cleaning. The pure continuum image (b) delineates an arc-shaped

reflection nebula 3!! west of LkH! 234, while the pure H2 line image (d) shows a spectacular jet at PA 226", at an angle of 45" with the optical

[Sii] jet of Ray et al. (1990). In each panel, intensity is displayed logarithmically. Resolution is 0.5!! FWHM in original images and 0.65!!

FWHM in the pure H2 images.

10″

H2 Jet

Continuum subtracted, H2 narrow bandCabrit el al. (1997)

12

MM1


13

MM1

VLA 2

NW2

NW1

+VLA 3B

VLA 3A IRS 6

Multiple Outflow & Sources

Background image: JHK (Kato et al. 2011)

– 19 –

Fig. 1.— Key for the LkHα 234 region. a) Three slit positions, outflow source candidates,and axes of outflows. b) Zoom-in of source positions. The 1.��0 (W) × 14.��8 (L) slits atposition angles (P.A.) of 256◦ are superposed on the JHK color composite image (Kato etal. 2011). The slit positions are numbered as 1, 2 and 3 (SP 1, 2, and 3) from the bottomto the top in the figure. c) The slit positions on the continuum subtracted H2 emission lineimage (Cabrit et al. 1997). A dash-dotted line in the inset represents the position of Y =0��, and knots A, B, and C are shown. d) Source subtracted 3.6 cm map taken fromTrinidad et al. (2004). FIRS1-MM1, VLA sources, mid-IR sources NW 1, NW 2 and IRS6 are marked and a dashed ellipse shows the position of the bright [Fe II] knot detected atSP 1 and 2. The positional uncertainties of the sources are described in Section 1.The dotted, dashed, and solid lines marked as Axis1, Axis2, and Axis3 indicate axes of anoptical [S II] jet, a near-IR H2 jet, and an [Fe II] jet which is newly suggested in this study,respectively. Axis1 and Axis2 correspond to A1 and A2 of Fuente et al. (2001). Letter G ismarked in the original image of Kato et al. (2011), indicating the YSO candidate.

[S II]jet axis

H2 jet axis

[Fe II]jet axis


Observation

14

• IGRINS 3rd test run on July 13, 2014 (UT)

• Slit:1″ x 14.8″, 3 slit positions (SP) 1, 2, 3.

• ON(600s) - OFF(600s) at each position


H KRaw Data

15

[FeII]1.644

H2 2.122

[Fe II] and H2: Near-IR outflow tracers


H

K

[Fe II] 1.533

[Fe II] 1.644

[Fe II] 1.677

1-0 S(7)

1-0 S(6)

1-0 S(2)

2-1 S(3)

1-0 S(1)

2-1 S(2)

1-0 S(0)

2-1 S(1)

1-0 Q(1) 1-0 Q(2)

1-0 Q(3) 1-0 Q(4)

H2ro-vibrational

16


!"#$ !"#% !"#&

17

Position-velocity Diagram

• H2 is dominant in low-velocity (0 to -30 km/s) & [Fe II] in higher-velocity (-120 km/s): H2 arise from entrained gas

• Multiple-velocity peaks in H2 at SP 1 and SP 2: bow-shock

• Extended, redshifted component at SP 2 & SP 3: outflow in almost parallel to sky plane, wide opening angle?

• H2 emission at Vsys in all slits: background PDR?

H2 1-0 S(1) (Contour), [Fe II] 1.644μm (Color)


1. H2 jet from FIRS1-MM1

• knot B, C of H2 jet & inner [S II] jet (P.A. ~227°)

• MM1 well aligned with jet axis

2. Outer [S II] jet from VLA 2 (NW2)

• [S II] jet knot D-E, CO outflow (P.A. ~252°)

• Masers around VLA 2: proper motions agree with jet axis

3. [Fe II] jet from VLA 3 (IRS 6, NW1)

Multiple Outflow & Sources – 19 –

Fig. 1.— Key for the LkHα 234 region. a) Three slit positions, outflow source candidates,and axes of outflows. b) Zoom-in of source positions. The 1.��0 (W) × 14.��8 (L) slits atposition angles (P.A.) of 256◦ are superposed on the JHK color composite image (Kato etal. 2011). The slit positions are numbered as 1, 2 and 3 (SP 1, 2, and 3) from the bottomto the top in the figure. c) The slit positions on the continuum subtracted H2 emission lineimage (Cabrit et al. 1997). A dash-dotted line in the inset represents the position of Y =0��, and knots A, B, and C are shown. d) Source subtracted 3.6 cm map taken fromTrinidad et al. (2004). FIRS1-MM1, VLA sources, mid-IR sources NW 1, NW 2 and IRS6 are marked and a dashed ellipse shows the position of the bright [Fe II] knot detected atSP 1 and 2. The positional uncertainties of the sources are described in Section 1.The dotted, dashed, and solid lines marked as Axis1, Axis2, and Axis3 indicate axes of anoptical [S II] jet, a near-IR H2 jet, and an [Fe II] jet which is newly suggested in this study,respectively. Axis1 and Axis2 correspond to A1 and A2 of Fuente et al. (2001). Letter G ismarked in the original image of Kato et al. (2011), indicating the YSO candidate.

[S II]jet axis

H2 jet axis

[Fe II]jet axis


3.6 cm, there are two additional arguments to support theassertion that VLA 2 is a genuine source. First, a weak (3 !)feature at 1.3 cm is observed at that position, and second, itis spatially coincident with a cluster of water maser spots,containing the strongest maser spot in the LkH" 234 region.Furthermore, the geometrical center of the water masers is at" (2000) ! 21h43m06:s330; #(2000) ! 66"06055B93, which isnearly coincident with the nominal VLA 2 position (Table 1).It is interesting to note that in the high-mass-star–formingregions of Cep A, W75N(B), and AFGL 2591, where differentradio continuum sources and water masers are distributedwithin small regions of a few arcseconds (a few thousand AU),thus probably sharing the same molecular environment,brighter masers are associated with weaker radio continuumsources (Torrelles et al. 2001, 2003; Trinidad et al. 2003b). Inorder to establish whether this is a real general tendency in star-forming regions or not, further simultaneous observations ofcontinuum and water maser emission at 1.3 cm toward a largersample of embedded YSO clusters are necessary.

An important result in VLA 2 comes from the spatial dis-tribution of the associated 16 water maser spots (Table 2 andFig. 4). These masers are distributed into two main groupsseparated by ’0B3 (300 AU), one of them to the northeast(8 spots; hereafter the northeast group) and the other one to thewest and southwest (2+5 spots; hereafter the southwest group)of VLA 2. The spectra of these two groups of masers are shownin Fig. 5. The mean velocity of the maser spots associated withVLA 2 is VLSR ! #10:6 km s#1 (with a standard deviation of3.3 km s#1), which is similar to the ambient molecular cloudvelocity (#10.3 km s#1; e.g., Font et al. 2001). On the otherhand, the mean velocity of the maser spots located to thenortheast is #9.1 km s#1 (redshifted), while the mean velocityof the southwest masers is #12.2 km s#1 (blueshifted). Thisspatial-velocity segregation of the water masers is also seen inFigure 6, where we present the position-velocity distribution ofthe masers along the axes with P:A: ! 67" and #23". Thesediagrams show that the northeast maser group is mainly red-shifted, while the southwest one is mainly blueshifted withrespect to the cloud velocity.

The spatio-kinematical distribution of the water masersaround VLA 2 is similar to that found toward the protostarsIRAS 05413#0104 by Claussen et al. (1998) and S106 FIR byFuruya et al. (1999, 2000). For these sources, based on thespatial distribution and relative proper motions of the masercomponents, these authors concluded that the water masers areassociated with a highly collimated compact jetlike flow thatcould originate from a presumed protostar located betweentwo groups of masers. The similarity we find between VLA 2and the YSOs IRAS 05413#0104 and S106 FIR leads us tosuggest that the water masers in VLA 2 are associated with acollimated outflow, with VLA 2 as the central source. Fur-thermore, since the redshifted CO lobe of the LkH" 234 re-gion is detected toward the northeast, while the blueshiftedoptical S [ii] jet is detected toward the southwest, with a po-sition angle similar to that of the major axis of the maserdistribution (P:A: $ 247"), we suggest that the masers inVLA 2 are tracing the base of this large-scale outflow seen inCO/[S ii].

4.3. VLA 3

VLA 3 is the strongest radio continuum source in the fieldat both wavelengths (1.3 and 3.6 cm). It was previouslydetected at 3 mm, 1.3 cm, and 2 cm by Wilking et al. (1986).They estimated a spectral index (S$ / $" ) of 1.6, which was

Fig. 2.—(a) Contour map of the continuum emission of VLA 3 at 3.6 cmusing uniform weighting and the Briggs ‘‘robustness’’ parameter set to #5 (seeBriggs 1995 for more details). Contours are#4,#3, 3, 4, 5, 6, 7, 8, 9, 10, and 12times 47 %Jy beam#1, the rms of the map. The beam (0B26 ; 0B17) is shown inthe lower left corner. From this figure we see that VLA 3 is in fact a binary sys-tem, which is formed by VLA 3A and VLA 3B. (b) Contour map of VLA 3 at1.3 cm using uniformweighting and the Briggs ‘‘robustness’’ parameter set to 0.Contours are#4,#3, 3, 4, 5, 7, 9, 11, and 13 times 0.11 mJy beam#1, the rms ofthe map. The beam (0B12 ; 0B10) is shown in the lower left corner. At this fre-quency, the two sources are completely separated. (c) We have subtracted thesource VLA 3A from the (u, v) data at 3.6 cm. Contours are#4,#3, 3, 4, 5, 6, 7,and 8 times 45 %Jy beam#1, the rms of the map. The beam (0B26 ; 0B17) is shownin the lower left corner. In this panel, only VLA 3B remains and its morphologyis elongated, suggesting a jetlike appearance. In the three panels the small crossesindicate the position of the H2Omaser spots associated with VLA 3 and the largecross indicates the position of IRS 6 (its size represents the error in its position).

OUTFLOWS IN LkH" 234 419No. 1, 2004

3. [Fe II] jet and VLA 3 (IRS 6, NW1)

•1.3 & 3.6 cm continuum: two peaks VLA 3A & 3B, young binary system

• 3B: thermal radio jet with P.A. ~230°

• Green blob in JHK image: provably [Fe II] emission, well matches with [Fe II] peak in SP 1 & 2 (-6″<Y<-2″)

• Axis 230°: VLA 3B, Radio jet & [Fe II] peak

• Mid-IR source IRS 6: less extinction region

• We confirmed -120km/s [Fe II] jet from VLA 3B

Trinidad et al. (2004)

Multiple Outflow & Sources3.6 cm

1.3 cm

VLA 3A subtracted


588 HAYASHI & PYO Vol. 694

Figure 5. Composite color image of L1551 IRS 5. The blue, green, and red colors are assigned to the H, [Fe ii], and H2 filter frames, respectively. North is up and eastis left.

Figure 6. Close-up of L1551 IRS 5. The blue, green, and red colors are assigned to the H, [Fe ii], and Ks filter frames, respectively. North is up and east is left.

H, [FeII], H2. Hayashi & Pyo (2009)L1551-IRS5


21

Electron Density

• ne estimated from Line Ratios of [Fe II] 1.644μm/1.600μm, 1.644μm/1.533μm, 1.644μm/1.677μm

• 0.5-3.1 x 104 cm-3, similar or slightly smaller than outflow fromT-Tauri, intermediate-mass star, Class 0-I YSOs

Model (Nisini et al. 2002)4,000K

15,000K


22

H2 Population Diagram

• Trot at peaks A1, A2, and B

• v =1: ~2,500±200K, v=2: ~3,000±1500 K

• Gases are thermalized in 2,500-3,000 K

• Temperature fitting in single line: Shock excited gas (outflow of low- & high-mass star)

v=1v=2

bow shock


Summary1. We detected 14 H2 and 5 [Fe II] emission lines from

outflow around LkHα 234 in H- and K-band.

2. We confirmed new [Fe II] jet from VLA 3B.

3. H2 is dominant in low-velocity (0 to -30 km/s) while [Fe II] is in high-velocity (-120 km/s): H2 emission is arise from shock gas entrained by fast outflow.

4. Multiple-velocity peaks in H2 emission: low- and high-velocity components arise from typical bow shock

5. H2 population diagram shows that gas is thermalized at Trot ~ 2500-3000 K, and from shock excited gas

6. Electron density from [Fe II] ratios are similar to CTTS & Class 0-I YSOs


Thank you


Documents

IGRINS Spectroscopy on Multiple Outﬂows around LkHα 234ust.kasi.re.kr/JC-ref/HYOh_USTJC_20160217.pdf · IGRINS 2 • Immersion GRating INfrared Spectrograph • Collaboration between