Pulsation and Granulation in the two PMS stars

Pulsation and Granulation in the two PMS stars V 588 Mon and V 589 Mon using Co. Ro. T data. . . K. Zwintz, T. Kallinger, D. Guenther MOST ST Meeting, Halifax, May 31 - June 1, 2010

V 588 Mon & V 589 Mon • PMS members of NGC 2264 • Discovery of δ Scuti pulsation: Breger (1972) • Recent Observations: • - multi-site campaign 2002 - MOST 2004: 48 days - MOST 2006: 23 days First asteroseismic analysis: Guenther et al. (2009) MOST ST Meeting, Halifax, May 31 - June 1, 2010

Co. Ro. T & NGC 2264 • Dedicated short run (SRa 01): March 2008 for ~23. 4 days • Exo field CCD • 130 candidate targets for asteroseismology • Additional: 14 „Imagettes“ - partially saturated images - V 588 Mon & V 589 Mon MOST ST Meeting, Halifax, May 31 - June 1, 2010

V 588 Mon seen with Co. Ro. T MOST ST Meeting, Halifax, May 31 - June 1, 2010

V 588 Mon seen with Co. Ro. T 8 published pulsation frequencies (Guenther et al. 2009) But there is more. . . MOST ST Meeting, Halifax, May 31 - June 1, 2010

V 588 Mon: Comparison to MOST close to orbit sidelobe ok in MOST; not in gb data MOST ST Meeting, Halifax, May 31 - June 1, 2010

V 589 Mon seen with Co. Ro. T MOST ST Meeting, Halifax, May 31 - June 1, 2010

V 589 Mon seen with Co. Ro. T published 12 pulsation frequencies (Guenther et al. 2009) And again: there is more. . . MOST ST Meeting, Halifax, May 31 - June 1, 2010

Many additional frequencies. . . V 588 Mon: 106 „significant“ frequencies ? 8 known frequencies & 98 „new“ frequencies down to S/N=4 12 known frequencies & 185 „new“ frequencies down to S/N=4 V 589 Mon: 197 „significant“ frequencies MOST ST Meeting, Halifax, May 31 - June 1, 2010

Granulation in A type stars • Kallinger & Matthews (2010): 2 Co. Ro. T targets - power spectra: white noise + sum of power laws + Gaussian > 1000 frequencies published 420 frequencies published 105 frequencies after granulation modelling 55 frequencies after granulation modelling MOST ST Meeting, Halifax, May 31 - June 1, 2010

Granulation in V 588 Mon & V 589 Mon • Prewhitening of the 10 / 15 largest amplitude frequencies - • Gaps in the data are filled by linear interpolation - • Assumption: residual power excess is Gaussian-like standard method for solar-type pulsators Global model fit to residual power spectrum - power law components to correct the frequencydependent background noise - Signal-to-background-noise ratio (SNb. R) to identify additional. MOST pulsation frequencies ST Meeting, Halifax, May 31 - June 1, 2010

Granulation Model for V 588 Mon gap-filled residuals after prewhitening the 10 largest amplitude frequencies solid line: global model fit dotted line: 2 power laws and white noise dashed lines: power laws Peaks with SNb. R > 9: significant additional pulsation frequencies 4 frequencies with SNb. R > 9 MOST ST Meeting, Halifax, May 31 - June 1, 2010

Granulation Model for V 589 Mon gap-filled residuals after prewhitening the 15 largest amplitude frequencies 22 frequencies with SNb. R>9 MOST ST Meeting, Halifax, May 31 - June 1, 2010

Revised pulsation frequencies • • V 588 Mon - 106 significant frequencies ⇒ 10 + 4 after granulation modelling - one published frequency has SNb. R < 9; but has to be included - all 8 published frequencies are confirmed V 589 Mon - 197 significant frequencies ⇒ 15 + 22 after granulation modelling - all 12 published frequencies are confirmed ➡ Revised input for asteroseismic modelling MOST ST Meeting, Halifax, May 31 - June 1, 2010

MOST & PMS stars: Past and Future MOST ST Meeting, Halifax, May 31 - June 1, 2010

MOST & PMS stars in the past • • 5 Herbig Ae stars: HD 142666, UX Ori, HR 5999, V 1247 Ori, HD 34282 - the shortest period δ Scuti pulsator: HD 34282 (in prep. ) - the longest period δ Scuti pulsator: HR 5999 (recent re-observations! to be published) - no pulsational variability: UX Ori (in prep. ) - complex (pulsational) variabilities: HD 142666 (published) - circumstellar matter. . . NGC 2264 stars: no irregular variations MOST ST Meeting, Halifax, May 31 - June 1, 2010

PMS stars - another view A 7 e A 5 e A 7 e A 3 e MOST ST Meeting, Halifax, May 31 - June 1, 2010 HR 5999 (2010)

Circumstellar matter in the 5 stars • emission lines • infrared excess • circumstellar matter - HD 142666 and UX Ori: “edge-on” & studied in detail - HR 5999, V 1247 Ori and HD 34282: presence reported MOST ST Meeting, Halifax, May 31 - June 1, 2010

The case of UX Ori MOST ST Meeting, Halifax, May 31 - June 1, 2010

Spectral energy distributions UX Ori Work in progress. . . MOST ST Meeting, Halifax, May 31 - June 1, 2010

PMS Target Proposal • HD 35929 - RA = 05: 27: 42. 8 DE = -08: 19: 38. 4 GSC 05332 -01468 V = 9. 7, sp = F 2 15‘ V = 8. 13 mag GSC 05332 -01325 V = 10. 2 - A 5 e - single known period: 4. 7 h - switch target - fundamental parameters available Marconi et al. 2000 MOST ST Meeting, Halifax, May 31 - June 1, 2010

Why HD 35929? • Herbig Ae star with similar spectral type to V 1247 Ori - investigating the influence of the circumstellar matter with MOST - check for additional pulsation frequencies at lower amplitudes - similar to HR 5999 concerning length of pulsation period ‣ i. e. one of the longest period PMS pulsators - fundamental parameters known (including parallax!) - possibility for ground-based observations. . . MOST ST Meeting, Halifax, May 31 - June 1, 2010