Three Years of Experience with the STELLA Robotic Observatory

Granzer, T.; Weber, M.; Strassmeier, K. G.

doi:10.1155/2010/980182

Cited by 17 publications

(11 citation statements)

References 18 publications

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“…We obtained 11 individual light curves of secondary eclipse events with the 1.2 m STELLA telescope (Strassmeier et al 2004) from 2012 to 2018. The employed instrument was the wide field imager WiFSIP, providing a field of view (FoV) of 22 ′ × 22 ′ on a scale of 0.32 ′′ /pixel (Granzer et al 2010). The detector is a single 4096×4096 back-illuminated thinned CCD with 15 µm pixels.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Low albedos of hot to ultra-hot Jupiters in the optical to near-infrared transition regime

Mallonn

Kohler

Alexoudi

et al. 2019

A&A

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The depth of a secondary eclipse contains information of both the thermally emitted light component of a hot Jupiter and the reflected light component. If the dayside atmosphere of the planet is assumed to be isothermal, it is possible to disentangle both. In this work, we analyzed 11 eclipse light curves of the hot Jupiter HAT-P-32 b obtained at 0.89 µm in the z' band. We obtained a null detection for the eclipse depth with state-of-the-art precision, −0.01 ± 0.10 ppt. We confirm previous studies showing that a noninverted atmosphere model is in disagreement to the measured emission spectrum of HAT-P-32 b. We derive an upper limit on the reflected light component, and thus, on the planetary geometric albedo A g . The 97.5% confidence upper limit is A g < 0.2. This is the first albedo constraint for HAT-P-32 b, and the first z' band albedo value for any exoplanet. This finding disfavors the influence of large-sized silicate condensates on the planetary day side. We inferred z' band geometric albedo limits from published eclipse measurements also for the ultra-hot Jupiters WASP-12 b, WASP-19 b, WASP-103 b, and WASP-121 b, applying the same method. These values consistently point to a low reflectivity in the optical to near-infrared transition regime for hot to ultra-hot Jupiters.

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Section: Observations and Data Reductionmentioning

confidence: 99%

Low albedos of hot to ultra-hot Jupiters in the optical to near-infrared transition regime

Mallonn

Kohler

Alexoudi

et al. 2019

A&A

View full text Add to dashboard Cite

show abstract

“…A1). Further details of the performance of the system were reported by Weber et al (2012) and Granzer et al (2010). Data reduction is performed automatically using the IRAF 1 -based STELLA data-reduction pipeline (Weber et al 2011).…”

Section: New Observations and Data Reductions 21 High-resolution Optmentioning

confidence: 99%

Time‐series high‐resolution spectroscopy and photometry of ε Aurigae from 2006–2013: Another brick in the wall

et al. 2014

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We present continuous and time-resolved R = 55 000 opticaléchelle spectroscopy of Aurigae from [2006][2007][2008][2009][2010][2011][2012][2013] We conclude that Hα is contaminated by changes in the circumstellar environment while the Hβ and V I photometry stems predominantly from the non radial pulsations of the F0 supergiant. We isolate the disk-rotation profile from 61 absorption lines and found that low disk eccentricity generally relates to low disk rotational velocity (but not always) while high disk eccentricity always relates to high velocity. There is also the general trend that the disk-absorption in spectral lines with higher excitation potential comes from disk regions with higher eccentricity and thus also with higher rotational velocity. The dependency on transition probability is more complex and shows a bi-modal trend. The outskirts of the disk is distributed asymmetrically around the disk and appears to have been built up mostly in a tail along the orbit behind the secondary. Our data show that this tail continues to eclipse the F0 Iab primary star even two years after the end of the photometric eclipse. High-resolution spectra were also taken of the other, bona-fide, visual-binary components of Aur (ADS 3605BCDE). Only the C-component, a K3-4-giant, appears at the same distance than Aur but its radial velocity is in disagreement with a bound orbit. The other components are a nearby (≈ 7 pc) cool DA white dwarf, a G8 dwarf, and a B9 supergiant, and not related to Aur. The cool white dwarf shows strong DIB lines that suggest the existence of a debris disk around this star.

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“…We obtained 63 hr of time-series photometry with the 1.2 m robotic STELLA telescope and its wide field imager WiF-SIP (Strassmeier et al 2004). The instrument provides a field of view (FoV) of 22 ′ × 22 ′ on a scale of 0.32 ′′ /pixel (Granzer et al 2010). The detector is a single 4096 × 4096 back-illuminated thinned CCD with 15 μm pixels.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

No further evidence for a transiting inner companion to the hot Jupiter HATS‐50b

Mallonn

2019

Astron Nachr

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Most hot Jupiter exoplanets do not have a nearby planetary companion in their planetary system. One remarkable exception is the system of WASP‐47 with an inner and outer nearby companion to a hot Jupiter, providing detailed constraints on its formation history. In this work, we follow up on a tentative photometric signal of a transiting inner companion to the hot Jupiter HATS‐50 b. If confirmed, it would be the third case of a hot Jupiter with an inner companion. Sixty three hours of new ground‐based photometry were employed to rule out this signal to about 96% confidence. The injection of artificial transit signals showed the data to be of sufficient quality to reveal the potential photometric feature at high significance. However, no transit signal was found. The discrete pattern of observing blocks leaves a slight chance that the transit was missed.

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Three Years of Experience with the STELLA Robotic Observatory

Cited by 17 publications

References 18 publications

Low albedos of hot to ultra-hot Jupiters in the optical to near-infrared transition regime

Low albedos of hot to ultra-hot Jupiters in the optical to near-infrared transition regime

Time‐series high‐resolution spectroscopy and photometry of ε Aurigae from 2006–2013: Another brick in the wall

No further evidence for a transiting inner companion to the hot Jupiter HATS‐50b

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