Spectroscopic orbits of kepler s gas giants koi 254 a case study
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Spectroscopic Orbits Of Kepler's Gas Giants KOI-254: A Case Study. John A. Johnson Sebastian Pineda Michael Bottom Zach Gazak Josh Winn Kevin Apps Andrew Howard Geoff Marcy Howard Isaacson. R P > 5 R E arth. KOI-254. KOI-254. Cool: T eff < 4000 K (exact value very uncertain )

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Spectroscopic Orbits Of Kepler's Gas Giants KOI-254: A Case Study

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Spectroscopic orbits of kepler s gas giants koi 254 a case study

Spectroscopic Orbits Of Kepler's Gas GiantsKOI-254: A Case Study

John A. Johnson

Sebastian PinedaMichael Bottom

Zach Gazak

Josh Winn

Kevin Apps

Andrew Howard

Geoff Marcy

Howard Isaacson


Spectroscopic orbits of kepler s gas giants koi 254 a case study

RP > 5 REarth

KOI-254


Koi 254

KOI-254

  • Cool: Teff < 4000 K (exact value very uncertain)

  • Faint: V = 16.9

  • R★ = 0.65 R, M★ = 0.53 M

  • Period = 2.455 days

  • Transit Depth = 3.6%


Spectroscopic orbits of kepler s gas giants koi 254 a case study

Kepler

Johnson et al. 2011 in prep

RP = ??

NickelLick Obs.


Spectroscopic orbits of kepler s gas giants koi 254 a case study

??


Spectroscopic orbits of kepler s gas giants koi 254 a case study

Muirhead et al. (2011)

No Main Sequence!


Spectroscopic orbits of kepler s gas giants koi 254 a case study

Rojas Ayala et al. (2010)

Rojas Ayala et al. (2011 in prep)


Spectroscopic orbits of kepler s gas giants koi 254 a case study

Muirhead et al. (2011)

On astro-ph NOW!


An empirical approach

An Empirical Approach

  • No reliance on atmosphere or evolution models

  • Broadly applicable, without need for a parallax


A photometric calibration

A Photometric Calibration

  • J,H,K  MJ,H,K  M★, d(Delfosse et al. 2000)

  • V - K  [Fe/H], M★ (Schlaufman & Laughlin 2010)

  • r - J  MJ  M★ (West et al. 2005, Delfosse et al.)

  • a/R★ M★ (Seager, Mallen-Ornelas 2003)

An example: K-band magnitude to Mass, distance


Spectroscopic orbits of kepler s gas giants koi 254 a case study

Johnson, Gazak, Apps et al. 2011 in prep


Spectroscopic orbits of kepler s gas giants koi 254 a case study

Johnson, Gazak, Apps et al. 2011 in prep

Sample of nearby stars with known parallaxes, and hence known M★


Why not optical spectroscopy

Why not optical spectroscopy?


Keck observatory

Keck Observatory

Keck Observatory

400 Massive, Evolved Stars900 Sun-like dwarfs150 Low-mass M dwarfs with an average of 25 observations per star


Spectroscopic orbits of kepler s gas giants koi 254 a case study

50 individual spectra

Final coadded spectrum


Spectroscopic orbits of kepler s gas giants koi 254 a case study

0.25 M

0.45 M

M★ = 0.68 M

Pseudo- continuum

line region

DecreasingMass


Spectroscopic orbits of kepler s gas giants koi 254 a case study

Bottom, Pineda & Johnson 2011 in prep

Increasing Mass


Spectroscopic orbits of kepler s gas giants koi 254 a case study

Bottom, Pineda & Johnson 2011 in prep

Decreasing [Fe/H]


Spectroscopic orbits of kepler s gas giants koi 254 a case study

Bottom, Pineda & Johnson 2011 in prep

rms = 8.4%


Spectroscopic orbits of kepler s gas giants koi 254 a case study

Photometric

x

Spectroscopic


Spectroscopic orbits of kepler s gas giants koi 254 a case study

KOI-254b

Schlaufman & Laughlin (2010)

Johnson & Apps (2009)


Thank you

Thank You

Sebastian PinedaMichael Bottom

Kevin Apps

Zach Gazak

Josh Winn

Andrew Howard

Geoff Marcy

Howard Isaacson


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