Euclid ASTEROSEISMOLOGY AND KUIPER BELT OBJECTS

Journal of The Korean Astronomical Society.
2016.
Feb,
49(1):
9-18

- Received : April 27, 2015
- Accepted : December 20, 2015
- Published : February 29, 2016

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1. INTRODUCTION

In two earlier papers, we pointed out that
2. EUCLID CHARACTERISTICS

We adopt
3. ASTEROSEISMOLOGY

- 3.1. Bright-Star Photometry

From Equation (16) of
Gould et al. (2015)
, the fractional error (statistical) in the log flux
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- 3.2. Bright-Star Astrometry

From
Gould et al. (2015)
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Fundamental properties and simulation parameters forEuclidsimulations.

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- 3.3. Analytic Error Estimates for Bright Euclid Stars

We summarize the results of Sections 3.1 and 3.2 in the form of analytic expressions for the photometric and astrometric errors for bright stars as a function of magnitude for single-epoch
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- 3.4. Asteroseismic Simulations for Euclid

As for
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- 3.5. Role of Euclid Parallaxes

In
Gould et al. (2015)
, we argued that
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4. KUIPER BELT OBJECTS

Gould (2014) carried out analytic calculations to assess how well
- 4.1. Euclid IR Observations of KBOs

We remind the reader that, in contrast to asteroseismology targets, KBOs are below the sky level and therefore are in a completely different scaling regime. In order to make use of the analytic formulae of Gould (2014), we first note that the
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- 4.2. Correction to Gould (2014) Formula: Number of Trials

To determine the minimum total SNR required for a detection, we must determine the number of trials. In principle, we should be able to simply scale from Equation (18) of Gould (2014). However, this equation contains a significant error in the “radial velocity” term, which must be corrected. We then take this opportunity to rederive the entire formula in order to put it in more general form.
Our guiding assumption is that the predictions of a given trial must match the orbit of a KBO to within half a pixel for all epochs. There are six phase space coordinates, two for transverse position at the midpoint of observations, two for proper motion (
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- 4.3. Euclid Optical Observations of KBOs

To compare optical with IR observations, we first note that the field of view is the same, but with pixels that are smaller by a factor 3. This means that the optical data are nearly critically sampled (100 mas pixels and 180 mas FWHM). The “RIZ” band is centered in
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- 4.4. Detections

The main characteristics of the
- 4.5. Orbital Precision

To determine the precision of the orbit solutions, we first note that the PSF is almost exactly the same size (both mirror and observing wavelength are half as big). Hence, Equation (12) from Gould (2014) remains valid:
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- 4.6. Binaries

Microlensing-style observations can detect KBOs through two distinct channels: resolved companions and unresolved companions detected from center-of-light motion Gould (2014).
For resolved companions, the situation for
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- 4.7. Occultations

Similarly,
- 4.8. Computational Challenges

As mentioned in Section 4.3, a total of 10
- 4.9. Comparison to the DeepHSTSearch

It is of interest to compare the corrected formulae presented here with the practical experience of
Bernstein et al. (2004)
, who searched for KBOs based on
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5. CONCLUSION

We have applied to the
Acknowledgements

Work by AG was supported by NSF grant AST 1103471 and NASA grant NNX12AB99G. DH acknowledges support by the Australian Research Council’s Discovery Projects funding scheme (project number DE140101364) and support by NASA under Grant NNX14AB92G issued through the Kepler Participating Scientist Program. We thank Matthew Penny for seminal discussions. This research was greatly facilitated by the interactive environment at the Galactic Archaeology Workshop at the Kavli Institute for Theoretical Physics in Santa Barbara.

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Citing 'Euclid ASTEROSEISMOLOGY AND KUIPER BELT OBJECTS
'

@article{ CMHHBA_2016_v49n1_9}
,title={Euclid ASTEROSEISMOLOGY AND KUIPER BELT OBJECTS}
,volume={1}
, url={http://dx.doi.org/10.5303/JKAS.2016.49.1.9}, DOI={10.5303/JKAS.2016.49.1.9}
, number= {1}
, journal={Journal of The Korean Astronomical Society}
, publisher={The Korean Astronomical Society}
, author={GOULD, ANDREW
and
HUBER, DANIEL
and
STELLO, DENNIS}
, year={2016}
, month={Feb}