Spectroscopic Follow-Up of HAEBE Binaries Bernadette Rodgersa, Nicole S. van der Bliekb, Ben Brandvigc, Sandrine Thomasb, Greg Doppmanna and Jerome Bouvierd a) Gemini Observatory; b) NOAO Cerro Tololo Observatory; c) CTIO REU Program; d) Observatoire de Grenoble ABSTRACT Binary Candidates We present first results of a program to obtain near-infrared spectra of candidate companions to intermediate mass

SpT Dist. Sep. PA Sep. Object K References pre-main sequence Herbig Ae/Be stars, in order to combine accurate spectral classification with spectral energy (primary) [pc] [asec] [deg] [AU] AFGL961 B2 1600 5.8 254 9280 Maheswar Lada&Gautier 82 distributions (SEDs). We can begin to address two questions: Does companion spectral type correlate with AS 310 NW B1 2500 1.31 78.3 3275 3.7 Bouvier *also Ageorges1997 2500 2.22 240.5 5550 3.4 Bouvier 2500 3.74 233.4 9350 3.7 Bouvier primary spectral type? Do low mass companions look different than “typical” T Tauri stars? 2500 4.34 122 10850 1.1 Bouvier 2500 4.88 0.9 12200 2.7 Bouvier 2500 5 6.1 12500 4.7 Bouvier

BD+46 3471 A0 900 1.31 308.7 1179 5.0 Bouvier HAEBE BINARY PROJECT 

900 4.18 43 3762 4.7 Pirzkal97  900 4.67 40 4203 4.5 Bouvier I.AO-fed near-IR imaging of large, unbiased sample 

900 5.82 205.7 5238 5.2 Bouvier   900 6.01 199.9 5409 Bouvier Expand and repeat previous surveys (Pirzkal et al 1997, Leinert et al !#" $

BF Ori A1 460 2.03 48 934 3.7 Bouvier %&

CO Ori F8 460 2.04 276 938 3.0 Bouvier *also Maheswar 1997, Bouvier & Corporon 2001) *

HD 101412 A0 160 3.06 226.3 490 7.0 Bouvier ')(



$ + , HD 141569 A0 99 6.8 312 673 2.7 Pirzkal97 NIRI+Altair in North (05B program, ~1/2 complete), hopefully 99 8 314 792 2.0 Pirzkal97 HD 144432 A7 160 1.2 354 192 2.5 Bouvier *also Maheswar 160 1.45 4.4 232 2.5 Bouvier VLT+NaCo in South (06A) HD 150193 A0 150 1.1 236 165 2.2 Pirzkal97 *also Bouvier HD 200775 B3 430 2.25 164 968 4.9 Pirzkal97 *also Bouvier II.Near-IR Spectroscopic follow-up of Binary Candidates HD 203024 A? 300 0.23 160.6 69 0.0 Bouvier HD 259431 B6 800 3.12 346.5 2496 5.7 Bouvier III.Combine SED + Spectra for detailed look at HAEBE Multiple Systems

HD 35187 A2 150 1.3 185 195 Maheswar Dunkin et al 98  HD 52721 B2 1150 0.65 194.4 748 1.4 Bouvier *also Maheswar Establish binarity (or not)

HD 53367 B0 1150 0.64 296.9 736 1.8 Bouvier *also Maheswar  HD 76534 B2 830 2.09 303 1735 1.5 Bouvier *also Maheswar Companion spectral type as function of primary mass

Her 4636 B2 630 3.7 214 2331 Maheswar Reipurth&Zinnecker 93  HK Ori B8 460 0.34 41.7 156 2.3 Leinert97 *also Bouvier Effect of primary environment on companion's disk and evolution

460 3.98 354.4 1831 7.4 Bouvier  HR 5999 A7 210 1.43 114.6 300 3.6 Leinert97 *also Bouvier IL Cep B2 690 6.96 147 4802 0.0 Pirzkal97 Provide constraints to star formation theory across mass spectrum 690 7.71 328.6 5320 0.1 Bouvier KK Oph A5 310 1.61 247.2 499 2.0 Leinert97 *also Pirzkal97 Lk Ha 147 B2 ? 1.62 341.7 0 3.0 Bouvier Lk Ha 208 A7 1000 0.12 113.5 115 0.7 Leinert97 Near-IR Spectroscopy Lk Ha 234 B7 1000 1.87 96.6 1870 5.5 Bouvier 1000 2.7 315 2700 >5.2 Leinert97 MWC 349 Be 1200 2.4 280 2880 Maheswar White & Becker 85 of MWC 1080 B0 2200 0.76 267 1672 3.3 Leinert97 *also Bouvier, Pirzkal97 2500 4.69 86 11725 6.2 Pirzkal97 NX Pup A0 450 0.13 62.4 59 1.8 Bouvier *also Maheswar 450 6.98 45.3 3141 4.0 Bouvier Binary Candidates Par 22 A5 ? 1.39 259.9 0 0.6 Bouvier ? 1.85 250.5 0 2.5 Bouvier  R Mon B0 800 0.7 331 560 Maheswar Close 97 Initial Sample from Literature; ~half from Bouvier & Corporon 2001

RCW 34 B3 870 1.55 193 1349 1.6 Bouvier  870 2.21 292.9 1923 4.5 Bouvier Cross-dispersed spectra with Gemini Near-IR Spectrograph (GNIRS)

870 2.89 165.6 2514 3.1 Bouvier  870 4.6 92.1 4002 5.7 Bouvier 1-2.5um; R=1700 in 2005A (shown here); R=5900 in 2005B

870 5.26 65.9 4576 5.2 Bouvier  S Mon O7 760 2.91 112.8 2212 3.5 Bouvier Accurate Spectral Classification of Companions

SV Cep A0 715 1.09 311.6 779 5.5 Bouvier  T Ori A0 460 7.7 72.6 3542 >4.5 Leinert97 Establish binarity V1493 Cyg A2 ? 0.57 293.3 0 3.4 Bouvier 4.21 85.4 0 Bouvier  9.44 258.9 0 Bouvier Constrain SED and measure near-IR excess V1685 Cyg B3 1000 0.72 239.1 720 5.5 Bouvier  V1982 Cyg B8 780 5.36 325.5 4181 5.9 Bouvier Measure Emission Lines

780 5.62 325.3 4384 3.8 Bouvier  V380 Ori B8 460 0.15 204.2 71 1.1 Leinert97 *also Bouvier Indicative of Youth; Trace Accretion, Winds

V586 Ori A2 460 0.99 31.6 455 2.3 Bouvier  V633 Cas B9 600 5.5 3 3300 3.8 Leinert97 For T Tauri Companions, evaluate pre-MS properties from absorption

V892 Tau B8 160 3.72 19 595 4.2 Pirzkal97 *also Leinert97  XY Per A5 160 1.2 255 192 0.0 Pirzkal97 e.g., Effective Temperature, Gravity, Veiling (Doppmann et al 2003) Z CMa B5 1150 0.1 122.5 115 -0.9 Leinert97 Legend: in GNIRS Sample; Observed All Spectral Energy Distributions (SEDs) plot differential photometry from Bouvier & Corporon 2001: system photometry from literature (triangles); primary (diamonds) and secondary (stars)

HD 76534 HR 5999 ¡ Secondary spectra indicate early K star

 Extinction differs from primary

¡ H absorption filled in by emission in primary

HR5999 resolved SED: Distance and ¡ No H emission in extinction fixed by primary; mid G type? HD76534 resolved SED: Secondary is fit to B3 secondary

¡ Primary: B3, strong H emission ¡ Secondary: B3, no emission ¡ Background B3 star? Or ¡ Companion with 1.5 mag of gray extinction? ¡ No NIR excess (either star), but system excess in Far-IR Normalized NIR Spectra of HD76534 ¡ Normalized NIR Spectra of HR5999 HR5999B K-band (center) compared to 2 MS Which star? from Fig. 2H, Hillenbrand et al 1992;

primary (top, black) and companion (blue) open circles are IRAS points primary (top, black) and companion (blue) standards (Wallace & Hinkle, NOAO data archive)

   

HD150193 Preliminary Summary ¤¦¥¨§

¤

©

1.Six stars observed thus far... HD 76534 B3+B3 B3+B3 Companion has no excess ¢ Binarity not yet established or emission; 1.5mag gray

¢ extinction or field star? B+B pairs with different extinction common AS 310 B2+B2 Distant cluster, not close

¢ companion; delta-V~1 T Tauri secondaries to A0 HD150193 A2+K4; A2+~G0 Both emission line stars, primaries have NIR excess, but A2+G2 both large excess little emission

¢ CO Ori F8+F Companion is primary Emission source NOT always emission star HD150193 resolved SED: Distance and primary star HR 5999 A5+K5; A0+~K0 2ndary: some excess, weak

extinction fixed by primary; 2ndary early G type? £ Others in literature: HK Ori, HD35187 A0+G5 emission, more extincted

¡ 2. Spectroscopy is critical

Secondary SED constrained to same HD141569 B9+M Secondary is pair; weak ¢ distance & extinction suggests early G Accurate spectral classification emission lines in N object with large NIR excess ¢ Constrains SED to properly Bouvier & Corporon 2001 IAUS, 200 , 155

¡ Doppmann, Jaffe, White 2003 AJ, 126, 3043 Secondary Spectra show H absorption measure IR excess ¢ Allows detailed analysis of Hillenbrand, Strom, Vrba, Keene 1992 ApJ, 397, 613 (and emission), no HeI and no metal Leinert, Richichi, Haas 1997 A&A, 318, 472 features expected for late type, also evolutionary status Maheswar, Manoj, Bhatt 2002 A&A, 387, 1003 (& refs therein) Normalized Spectra of HD150193B (black, middle) indicating early G type ¢ Identifies peculiar systems Pirzkal, Spillar, Dyck 1997 ApJ, 481, 392 compared to HD76534B (below) and HR5999B (above) Th'e, de Winter, Perez 1994 A&AS, 104, 315