3-D Morphology of V723 Cas Nova Ejecta KeckII+LGSAO+OSIRIS

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Randy Campbell and Jim Lyke. [CaVIII] 2.3214 µm. V723 Cas. 3-D Morphology of V723 Cas Nova Ejecta KeckII+LGSAO+OSIRIS. H α images from Classical Novae , ed. Bode and Evans, Ch 12, O’Brien and Bode. v r (km/sec). λ ( μ m). OSIRIS: Integral Field Spectrometer. 0.1”. - PowerPoint PPT Presentation

Transcript of 3-D Morphology of V723 Cas Nova Ejecta KeckII+LGSAO+OSIRIS

  • 3-D Morphology of V723 Cas Nova Ejecta KeckII+LGSAO+OSIRISV723 CasRandy Campbell and Jim LykeH images from Classical Novae, ed. Bode and Evans, Ch 12, OBrien and Bode[CaVIII] 2.3214 m

  • OSIRIS: Integral Field Spectrometer0.1[CaVIII] 2.3214 m2007 Sep 3

  • Stepping Through Velocity Channels[CaVIII] 2.3214 m2007 Sep 30.1 mVr (km/sec)

  • [CaVIII] 2.3214 m2007 Sep 30.1Stepping Through Velocity Channels0.1 mVr (km/sec)

  • 3-D Volume Display27Position Angle Rotation[CaVIII] 2.3214 m2007 Sep 3

  • 3-D Volume Display62Viewing Inclination AngleCube Dimensions:3300 AU / side(dashed cube lines are background)

  • 3-D Volume Display27Position Angle Rotation[CaVIII] 2.3214 m2007 Sep 3

  • 3-D Volume Display-28Viewing Inclination Angle Cube Dimensions:3300 AU / side

  • Comparison of [Ca VIII] and [Al IX]Cube Dimensions: 3300 AU / side[CaVIII] 2.3214 m2007 Sep 3[Al IX] 2.0443 m2007 Sep 3

  • Conclusions

    Integral field spectroscopy + LGSAO yields:High spatial resolution tuned to coronal emission featuresDistance determination: 3.85 0.23 kpcDirect measure of the inclination: 62 1.5Study of the 3-D morphology of V723 Cas ejectaDetection of inhomogeneous shellEquatorial torus with polar globules in [Ca VIII] and most other emission featuresProlate spheroid in [Al IX]

  • Thank YouCube Dimensions: 3300 AU / side[CaVIII] 2.3214 m2007 Sep 3[Al IX] 2.0443 m2007 Sep 3

  • Backups

  • 1D spectra

  • Continuum Subtraction

  • Continuum Subtraction

  • Mosaic of Edge-On Views

  • Mosaic of Face-On Views

  • 2D Spectra 2006Br[Al IX][Si VI][Ti VII]unk

  • V723 CassiopeiaeVery slow multi-peak photometric developmentEvans, et al., 2003, AJ, 126, 1981, Figure 1

  • OSIRIS Overview P.I., James Larkin Fixed grating, lenslet array IFUR=3800ZJHK (1-2.5 mm)4 spatial scales: 20 mas, 35 mas, 50 mas, 100 mas

    Structure of [Si VI] vs. [Al IX] vs. Br gamma is differentOSIRIS with Keck LGSAO gives an unprecedented capability for nova studyhigh spatial resolutionWell suited spectral resolutionhelp reveal the physics insideCoronal lines exist in the ejectaInhomogeneity: Density / temperature /radiaton/ Ionization/ optical depth?well defined ringInfluence of binaryInterested in emission featuresRemove continuumSample continuum outside of features, extrapolate through features.

    Next: no contiuum, toggle back and forth

    Next : isolating individual featuresBrightened for ~100 days before max. Decline took 100s of daysMany novae 1000-2000 km/s lines up to ~5000 km/sNIRSPEC spectra from August 20047 years before these observationsH and CO nb filtersLongest orbital period of classical novae, likely a low mass WD with an evolved secondaryWe may want backup slides on 723 cas, light curves, spectral evolution, other info since some of the questions are likely to be on the nature of this object.

    We deemed the target a worthy challenge for OSIRIS and LGSAO on Keck II

    3 parts: Re-imaging optics, lenslet, spectrographOnly the re-imaging optics and filters move.88 Combinations of spatial and spectral coverage.