The Use of Virtual Observatory Databases in Binary Star Research

Geraldine J. Peters Space Sciences Center Department of Physics & Astronomy University of Southern California

From Interacting Binaries to Exoplanets: Essential Modeling Tools IAU Symposium No. 282 Tatranská Lomnica, Slovak Republic July 18, 2011 Databases from Ground-Based Telescopes

Databases from Spacecraft Observatories

Hunt for O Subdwarf Companions to Bright Stars

Double Periodic Variables

Accretion Hot Spots International Virtual Observatory Alliance

Argentina Virtual Observatory European Virtual Observatory Armenian Virtual Observatory German Astrophysical Virtual Observatory Virtual Observatory United Kingdom Hungarian Virtual Observatory Australian Virtual Observatory Japanese Virtual Observatory Brazilian Virtual Observatory Virtual Astronomical Observatory, USA Chinese Virtual Observatory Observatoire Virtuel France Canadian Virtual Observatory Russian Virtual Observatory European Space Agency Spanish Virtual Observatory European Southern Observatory Italian Virtual Observatory Virtual Observatory India MAST - Multimission Archive at STScI

ASTRO - ASTRO Observatory HUT - Hopkins Ultraviolet Explorer UIT - Ultraviolet Imaging Telescope WUPPE - Wisconsin Ultraviolet Photo-Polarimeter Experiment Copernicus - Copernicus DSS - Digitized Sky Survey EUVE - Extreme Ultraviolet Explorer FUSE - Far Ultraviolet Spectrographic Explorer GALEX - Galaxy Evolution Explorer GSC - Guide Star Catalogs HPOL - Halfwave Spectropolarimeter HST - Hubble Space Telescope IUE - International Ultraviolet Explorer KEPLER - Kepler ORFEUS - Orbiting Retrievable Far and Extreme Ultraviolet Spectrometers-SPAS BEFS - Berkeley Extreme and Far-UV Spectrometer TUES - Tübingen Ultraviolet Echelle Spectrometer IMAPS - Interstellar Medium Absorption Profile Spectrograph VLA-FIRST Very Large Array - Faint Images of the Radio Sky at Twenty-cm XMM-OM Xray Multi-Mirror Telescope - Optical Monitor data AGILE - ASI - Italian Space Agency ASCA - Astro-D - Japan Astro-H - NeXT - ISAS/JAXA - Launch 2013 BeppoSAX - ASI, NIVR, ESA COBE - Cosmic Background Explorer CGRO - Compton Gamma Ray Observatory Chandra EUVE - Extreme Ultraviolet Explorer Fermi GALEX - Galaxy Evolution Explorer GEMS - Gravity and Extreme Magnetism Small Explore - 2014 HETE-2 - High Energy Transient Explorer Mission INTEGRAL - INTErnational Gamma-Ray Astrophysics Laboratory ROSAT - Röntgen Satellite RXTE - Rossi X-ray Timing Explorer Mission Suzaku - Astro-E2 - Japan Swift - Gamma Ray Bursts - X-Ray, NUV/Optical Spectra & photometry WMAP - Wilkinson Microwave Anisotropy Probe XMM-Newton - X-ray Multi-Mirror Mission - ESA Other Databases of Note:

NASA/IPAC IRSA -Infrared Science Archive AAVSO – American Association of Variable Star Observers (>20.5 million observations) ASAS - All Sky Automated Survey (photometric monitoring of > 10 million stars) RAVE Survey – Radial velocities, proper motions, distances of > 1 million stars) ELODIE – Database of high-resolution stellar spectra

The Archives of IUE & FUSEThe

IUE – Launched on January 26, 1978 45 cm Ritchey-Chretien telescope Elliptical geosynchronous orbit Operated by NASA & ESA Real time observations for 18 .75 years FUV & NUV spectra at 0.1-0.3 & 6-8 A res. Over 120,000 images 2374 of binary stars – 556 SWP HIRES

FUSE – Launched on June 24, 1999 Operated for NASA and the French & Canadian Space Agencies for 8.3 years FUV spectroscopy (950-1188 A) Resolution of 0.05 A Over 6000 observations 195 of binary stars – 2 large survey programs Search for O Subdwarf Companions to Bright Be Stars

Thaller et al. (1995) used 16 IUE HIRES Images + Doppler tomography code to recover the spectrum of hot secondary in the Be star φ Per (P~126 d).

Gies et al. (1998) used HSt/GHRS observations to improve the stellar parameters. Masses: 9.30 + 1.14 Msun Teff/log g for subdwarf 53kK/ 4.2. Flux Ratio at 1400 A – 0.165

IUE images Reconstructed images: Top – primary Middle – O subdwarf HD 49898 (sdO6) FY Canis Majoris From Peters, Gies, Grundstrom, & McSwain (2008)

P= 37.25 d

11.5 + 1.3 Msun

•March 1995 Observations • 97 IUE HIRES SWP images of N V doublet taken from 1979-96 • One SWP HIRES spectrum • Generated CCF from template per day for 16 days model spectrum generated from • Fortuitously centered on TLUSTY/SYNSPEC conjunction with subdwarf • Used Doppler tomography in front algorithm (Bagnuolo 1994) • Shell feature near phase 0 to reconstruct spectrum of probably caused from shock subdwarf secondary of subdward wind. FY CMa

Teff/log g for subdwarf 45.5kK/ 4.3.

59 Cyg Maintz et al. (2005) Predicted subdwarf from optical spectro- Scopic behavior. The Double Periodic Variable Phenomenon

• First identified by Mennickent et al. (2003) from observations of Be stars in the LMC in the OGLE-II database • First reported in the Algol binaries AU Mon (Lorenzi 1980) and RX Cas (Kalv 1979)

AU Mon – Porbital = 11.113 d Plong = 416.9 d (Desmet et al. 2010)

Other DPVs: Porb (d) Plong (d) RX Cas 32.31 516.1 P (d) ~ 30 P (d) CX Dra 6.70 ~150 long orb β Lyr 12.94 282.4 from LMC binaries V360 Lac 10.09 322.2 V393 Sco 7.71 255.0

IUE Observations of the Eclipse of 1994 December 4/5 FUSE Observations of V356 Sgr During Totality Evidence for Disk Emission Analysis of IUE SWP HIRES Images of AU Mon Use of SHELLSPEC

Inner/Outer radius: 6.6/20 Rsun, Disk hickness: 6 Rsun, Density: 10-13 g cm –3 Mass transfer rate ~1.7 x 10-9 Msun/yr From Atwood-Stone, Miller, Richards, Budaj, & Peters 2011, in prep. 47 SWP HIRES Images in the IUE Archive

Mass Loss/Infall Evidence for Splash Plasma in U Cep Stellar Parameters Determined from FUV Spectra

NLTE model atmospheres computed with TLUSTY/SYNSPEC

FUSE Observations of U Cep

Inferred minimum size of accretion hot spot: 20o 9 -3 Te~30,000 K (2 x Tphot ), Ne~1x10 cm )

(Peters, G. J., Andersson, B.-G., Ake, T. B., & Sankrit, R. 2011, in prep)

Kepler Observations of V850 Cyg During Quarters 2-3 Short (1 min) Cadence V805 Cyg – Kepler Quarter 3 – Long (30 min) Cadence V810 Cyg – Kepler Quarter 2 UZ Lyr – Kepler Quarter 2 – Long Cadence Summary

• Numerous public archives are available. UV archives best developed at this time.

• Due to its long duration of operation the IUE database is excellent for recovering the spectra of hot subdwarfs about bright early-type stars using Doppler tomography.

• Based upon the analysis of AU Mon, the DPV phenomenon Is probably caused from the periodic rebuilding and dissipation of the accretion disk about the primary. The normal state of the star is when it is bright. The disk obscures the light .

• Spacecraft archives can be used to study hot accretion spots in interacting binaries.