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2 Age Gradients in the Stellar Populations of Massive Star Forming Regions Based on a New Stellar Chronometer Konstantin V. Getman, Eric D. Feigelson, Michael A. Kuhn, Patrick S. Broos, Leisa K. Townsley, Tim Naylor, Matthew S. Povich, Kevin L. Luhman, Gordon P. Garmire (MSFRs) X(Age JX ) L X MX J () Age JX MYStIX31784X5525Age JX 15MSFRs100 MYStIX (Massive Young Star- Forming Complex Study in Infrared and X- ray) X,, 20OB (Feigelson et al. 2013)

MYStIX MSFR,, J- H, Median(AgeJX) [Myr] 3.

0 Figure 7 Orion Nebula A;1.4 B;1.1 C;1.

3 MYStIX MSFR,, J- H, Median(AgeJX) [Myr] Figure 7 Orion Nebula A;1.4 B;1.1 C;1.5 D;2.7 U; Median(J-H) [mag] Figure 6 14

4 Dense molecular globulettes and the dust arc towards the runaway O star AE Aur (HD 34078) P. Gratier, J. Pety P. Boisse, S. Cabrit, P. Lesaffre, M. Gerin, and G. Pineau des Forêts Runaway Stars arc- likeir Runaway O- Star AE Aur (HD 34078) 12 CO(1 0) IRAM30 mpdbi Runaway Star Figure 1 HD Spitzer 24 μm (Gray Scale & Black Contours) () (1000) PdBI

5 1/32 Globuletts (Figure 2 right 1, 2), 2 Globulettes CO Globulettes (Bow Shock?) Figure 5 () 12CO (1 0) () 12CO (2 1) () (30 m) 12CO (1 0) (30 m + PdBI) Figure 2 () 12 CO (1 0) 30 m30 m+pdbi

6 O Globulettes CO Globulletes IR arc, () UV IR arcco Globulettes

7 The tiny globulettes in the Carina Nebula T. Grenman and G. F. Gahm HII Globulettes Carina Nebula Globulettes, HII Hubble Space Telescope Hα Globulettes 6563 Å Figure 1 () Carina Nebula (1.3 x 1.5 deg) GlobulettesHST field η Carina 4

結果今までサーベイされた領域で最も多い288のGlobulettesの位置を確認よくまとまった高密度クランプで, だいたいは薄いおおいや尾をもたない縁の明るいものは少数ではあるが他の領域よりは多いいくつかは若い星団の方向を向いて伸びた構造をしている多くは孤立していて隣の分子構造とは1.5 pc以上離れている Figure 2Nebula ( ) T. Grenman and G.

8 結果今までサーベイされた領域で最も多い288のGlobulettesの位置を確認よくまとまった高密度クランプで, だいたいは薄いおおいや尾をもたない縁の明るいものは少数ではあるが他の領域よりは多いいくつかは若い星団の方向を向いて伸びた構造をしている多くは孤立していて隣の分子構造とは1.5 pc以上離れている Figure 2Nebula ( ) T. Grenman and G. F. Gahm: Figure 3 ( ) The tiny globulettes in the Carina Carina Nebulaで見つかったGlobulettesの例 Carina Nebula の Globulettes の性質上から4行が最も典型的な暗いもの上半径 (arcsec) 次の2行が明るいハローをまとったもの中半径をkAUに直したもの最後の2行が伸びた尾をもつもの下質量 (MJ) T. Grenman and G. F. Gahm: The tiny globulettes in the Carina Nebula Table 1. HST archive data used. T. Grenman and G. F. Gahm: The tiny globulettes in the Carina Nebula Field/Target R.A. Dec. Images Fig. 3. Left: Distribution of average radii as measured for all globulettes found in the Carina Nebula expressed in arcsec. Middle: (J2000.0) (J2000.0) The corresponding distribution of average radii expressed in kau and adopting a distance to the complex of 2.9 kpc. The vertical arrow marks the peak in the corresponding accumulated size distribution for objects in seven H ii regions (De Marco et al. 2006). Right: of masses-59:47:42 for Carina globulettes 1 / PosDistribution 30 10:41:27 J9dk09010 less massive than 10 M J, expressed in Jupiter masses. 2 / Pos 30 10:41:38-59:46:17 J9dk / Pos 30 10:41:40-59:44:41 J9dka9010 iny globulettes in the Carina Nebula 4 / Pos 19 10:42:23-59:20:59 J9dk / Pos 19 10:42:48-59:19:44 J9dk / Tr 14 10:43:07-59:29:34 J900c1010 tion of average radii as measured for all globulettes found in the Carina Nebula expressed in arcsec. Middle: 7 / Tr 14 10:43:23-59:32:06 J900b1010 istribution of average radii expressed in kau and adopting a distance to the complex of 2.9 kpc. The vertical 8 / Tr 14 10:43:24-59:27:55 J900c2010 k in the corresponding accumulated size distribution for objects in seven H ii regions (De Marco et al. 2006). 9 / Tr 14 10:43:39-59:34:37 J900a1010 f masses for Carina globulettes less massive than 10 M J, expressed in Jupiter masses. 10 / Tr14 10:43:41-59:30:17 J900b / Tr 14 10:43:47-59:35:53 J / Tr 14 10:43:55-59:37:09 J / HH :43:58-59:54:39 J900a / Tr 14 10:43:59-59:32:38 J900a / Tr 14 10:44:00-59:28:05 J900b3010 obulettes found in the Carina Nebula expressed in arcsec. Middle: Fig. 2. Examples of globulettes found in the Carina Nebula num16 /tohh :44:01-59:58:42 J900b9010 U and adopting a distance the complex of 2.9 kpc. The vertical 17 / Tr H 16ii regions 10:44:05-59:40:16 J900c5010 bered according to Tables A1-A5 in Appendix A. The most typstribution for objects in seven (De Marco et al. 2006).

9 HII () (10 5 cm - 3 ) Globulettes! (10-19 gr/cm 3 ) Radius (kau) Figure 6 () Carina Nebula Globulettes

The dynamical properties of dense filaments in the infrared dark cloud G035.39 00.33 J. D. Henshaw, P. Caselli, F. Fontani, I.

10 The dynamical properties of dense filaments in the infrared dark cloud G J. D. Henshaw, P. Caselli, F. Fontani, I. Jime ńez- Serra, and J. C. Tan Infrared Dark Cloud (IRDC) G PdBIN 2 H + (1 0) Figure 1 G : N2H+ () () (1 st moment) () (2 nd moment)

(σ NT /c s ~1.5)(F2a, F2b, F3) (<0.7 km/s/pc) (1.5 2.5 km/s/pc) Outflow The dynamics of filaments in G035.39 00.

11 (σ NT /c s ~1.5)(F2a, F2b, F3) (<0.7 km/s/pc) ( km/s/pc) Outflow The dynamics of filaments in G infalling material ( ~ 7±4 e- 5 Msun/yr) expanding shells ( ~ 24±12 Msun km/s) 2 Figure 12. Top: a close-up image of the region surrounding H6. The size and direction of the arrows correspond to the magnitude and direction of the velocity gradient (pointing in the direction of increasing velocity). Dark green and dark red arrows refer to the velocity gradient calculated at each point, using velocities from the surrounding 27 pixels (note this is used for a spatial representation only, and not used in the analysis); light green and light red arrows refer to the velocity gradient calculated from the surrounding 38 pixels, for F2b and F3, respectively (see Section 4.2 for details). The symbols have the same meaning as Downloaded from at National Astronomical Observatory of Japan on May 1, 2014 Figure 6 () Figure 6. Three-dimensional PPV cube showing the centroid velocity of the three velocity components: (cyan) F2a, (red) F2b, and (green) F3, observed across G Additional velocity components, C4, C5, and C6, are shown in purple, blue, and orange, respectively (see Appendix D for more details). Unassigned data points are shown in black. The mass surface density map can be seen at the base of the cube, overlaid with N2H + (1 0) integrated intensity contours. Contour levels increase from 5σ (dotted contour; where σ 0.1 K km s 1 ) in steps of 5σ (solid contours), as with Fig. 1. The vertical dotted line corresponds to the position of H6. 3(cyan F2a, red F2b, green F3) at 3σ (where σ = mjy beam 1 ) and increasing in steps of 2σ. Overlaid are the extended 4.5 µm (green squares; Chambers et al. 2009), 8 µm (red open circles), and 24 µm emission (red open triangles; Carey et al. 2009), as well as the low-mass cores (yellow squares) and high-mass cores (magenta squares) identified using Herschel (Nguyen Luong et al. 2011). The left-centre, right-centre, and right panels show the VLSR maps and spatial location of all three velocity components, as deduced from the Gaussian fitting routine. Overlaid on top of each map are arrows indicating the magnitude and direction of velocity gradients in two dimensions. To achieve this, we have followed the analysis of Goodman et al. (1993). By assuming that the centroid velocities of observed lines take an approximately linear form: VLSR = V0 + Aα + Bδ, (3) whereby α and δ are offsets in right ascension and declination (in radians), least-squares minimization can be used to estimate Figure 12 (Bottom) () 2 values of A and B, usingmpfit2dfun (Markwardt 2009). The velocity gradient, v, canthenbecalculatedforacloudatdistanced, using (Goodman et al. 1993): v = (A2 + B 2 ) 1/2, (4) D and its direction, v (direction of increasing velocity, measured east of north), using ( ) v = tan 1 A. (5) B This method has been adapted following the procedure outlined in Caselli et al. (2002b) to calculate multiple gradients within a given region with a good determination of VLSR (seven contiguous positions with significant measurements of VLSR). In the case of the MNRAS 440, (2014) Downloaded from at National Astronomical Observatory of Japan on May 1, 2014

12 AN OPTICAL SPECTROSCOPIC STUDY OF T TAURI STARS. I. PHOTOSPHERIC PROPERTIES Gregory J. Herczeg and Lynne A. Hillenbrand HR 281T,, TWA1 2

13 Name Continuum Range Band Range Feature x SpT Range Zero-pt rms a (C) (B) G-band G-band C/B x G G0 1 F (5100) F R MgH line (4650) F (4650) F line (5100) b x K0-M0 K0 1.0 TiO TiO log ( C B 1) x +1.73x2 (M0 M4) M0... TiO , TiO C/B x K5 M0.5 K0... TiO TiO log ( C B 1) x +1.57x2 M0 M4.5 M c TiO d TiO C/B x M3 M8 M TiO TiO C/B x M4 M8 M Table 1 (C, B) Figure 2 (Red)

SFN

SFN THE STAR FORMATION NEWSLETTER No.291-14 March 2017 2017/04/28 16-20 16. X-Shooter spectroscopy of young stellar objects in Lupus. Atmospheric parameters, membership and activity diagnostics 17. The evolution