Expanding the Search for Spectroscopic Binaries in Proto-Planetary Nebulae!
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1 Expanding the Search for Spectroscopic Binaries in Proto-Planetary Nebulae! Bruce J. Hrivnak (Valparaiso University)! Motivation! Expectation! Observations! Results! Implications! (expansion of Hrivnak et al. 2011, ApJ, 734, 25)! In collaboration with! David Bohlender! Florian Kerber! Wenxian Lu! Andreas Seifahrt! Griet Van de Steene! Hans Van Winckel! with support from NSF! (Asymmetrical Planetary Nebulae VI, Mexico, )! 1. MOTIVATION: Why search for binaries in post-agbs?! Shaping of planetary nebulae (PNe):! Many have axial or point symmetry! Is this due to binary interaction?! Why search in proto-pne?! Preceding stage, should show evidence! Many already have axial or point symmetry! Spectroscopically easier than PNe:! Many are F-G spectral types! More and relatively narrower lines! Better precision! No strong winds to contend with! Some show an obscured equatorial region! How is this formed? binary?! PPNe! HST images! 1!
2 2. OBSERVATIONAL EXPECTATIONS! Expected binary parameters - Illustration:! PPN: M PPN = 0.62 M! " " " " " # " Companion: Main Seq, M 2 = 0.5 M!! PPN just within Roche lobe at SpT=G!! R PPN = 90 R! $ P orbit = 1.0 yr! $ V PPN = 13 km/s!!(measure K = Vsini but sin 30 o = 0.5)! But if PPN just within Roche lobe tip of AGB! R PPN = 500 R! (2.3 AU) $ P orbit =11 yr $ V PPN = 6.3 km/s! If P orbit = 30 yr $ V PPN = 4.5 km/s! Search for binaries by radial velocity monitoring SB1 " "! 3a. RADIAL VELOCITY OBSERVATIONS! Targets: 7 bright PPNe, SpT = F-G Iab! Many, sharp lines (advantage over hot central stars of PNe)! V = 7 11 mag! Goal - to find binaries (or at least set limits on them)! Observations at the Dominion Astrophysical Obs (Victoria, Canada)! , 2007 present!! Coude on 1.2-m with RVS (early),!! CCD with cross correlation (present)!!!: A! Precision ~ km/s! Observations with the Mercator telescope (La Palma)! 2009 present!! Hermes Spectrograph,!! CCD with cross correlation pipeline!!!: A! Precision ~ km/s! 2!
3 4a. RESULTS: Binaries?! IRAS ! "Vr = 3.6 km/s! One case of clear velocity change beyond (Inc. obs. by Zacs et al 2009)! pulsation! IRAS !"Vr (initial current) = 3.2 km/s! P > 25 years, K = 1.6 km/s! Limiting case: If we assume P = 25 yr, K = 1.6 km/s, M PPN = 0.62 M!, and e = 0, then M 2 = depends on inclination i:! i = 25 o from model (Ueta et al. 2001, mid-ir) $ M 2 = 0.37 (+/-0.05)! If circular orbit, a = 8.5 AU = 1800 R! >> R(AGB) >> R(PPN)! Would survive detached at tip of AGB! 4a. RESULTS: Binaries?! These 3 show no long-term variations beyond pulsation!! HST images! DAO observations (filled/open circles), Hermes (filled triangles), others others (open triangles).! 3!
4 1/20/14! 4a. RESULTS: Binaries?! 1 of these 3 shows long-term variations beyond pulsation! HST images! "Vr = 2.4 km/s! Only 2 of 7 shows long-term variations beyond pulsation, which is consistent with the SB rate for normal F-G stars.! However,! 4a. RESULTS: Constraints on Possible Binaries! What about possible bias - selection effects? - Chose brightest, more likely seen at low inclination (less obscuration), more pole-on. Does this invalidate the results?! Non-detection still sets important constraints on possible binaries! M2! If M2 & i > 15o i > 30o 0.4 M! P > 3.5 yr P > 24.5 yr 0.25 M! P > 1.1yr P > 8 yr i > 45o P > 23 yr or, for example! M2 > 0.3 M! is excluded for P<13 yr at i>30o! P! M2 and P for various inclinations (i)! Any undetected binaries have low mass or/and long periods! (Assuming MPPN=0.62 M!, K=2.0 km/s, circular orbits)! (see Hrivnak et al. 2011, ApJ, 734, 25)! 4!
5 3b. NEW OBSERVATIONS: Edge-on Binaries! Ideally like to observe edge-on PPNe, no inclination ambiguity! but they possess an obscuring torus! HST (visible light)! However, each of which has a visible star in near-ir! HST (near-ir light)! (Different orientation than visible images)! 3b. NEW OBSERVATIONS: Edge-on PPNe with Near-IR Spec! Ideally then, let s observe them in the near-ir! New observing program:! ex. IRAS ! Began 4 years ago Near-IR, high-resolution spec, 8-m telescope! ESO (Kerber, Seifahrt ESO) CRIRES (R=100,000)! Gemini-S (Hinkle NOAO) Phoenix (R=70,000) - discontinued! Data reduction in process, complicated! If "V R > km/s (larger than pulsation) $ (possible/likely) binary! 5!
6 4b. RESULTS: Edge-on PPNe! Preliminary results for IRAS (J & K bands)! 2013! 2011! "Vr (Obs System) ~ 10 km/s! Tantalizing, but more work on data reduction and more observations needed over a longer temporal baseline.! Very preliminary results for IRAS & ! Lower S/N, only in K band, spectra are messy and results less precise in progress.! 5. IMPLICATIONS: of Radial Velocity Study of PPNe! Implications of small or on long-term velocity variations:! Any binaries have long P (> 30 yr) or low mass (<0.3 M! )! (Secondary brown dwarf or a massive planet - would not be detected)! If long P, then effect on shaping is small (Huggins??)! Implications of fact that these stars are F-G supergiants with expanding CSE:! They will not pass through a CE phase! All PPNe are not formed or shaped by CE interaction! Implications of short-term variability! All PPNe vary due to pulsation (we find P(LC) = P(Vr))!$! ! Where are the binaries?! RV Studies continuing! 6!
7 5. Pulsation Studies are giving us new insight to be exploited.! LC! LCs - us! Vr - Zacs et al. (2009) + us! Vr! P=131.9 d!! S!! L!! S! (Hrivnak et al. 2013, ApJ, 766, 116)!! Star is brightest, hottest when smallest (differ from Cepheids)! 7!
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